[
{
"id": "authors:d92et-1ar91",
"collection": "authors",
"collection_id": "d92et-1ar91",
"cite_using_url": "https://authors.library.caltech.edu/records/d92et-1ar91",
"type": "article",
"title": "NASA's Pandora SmallSat Mission: Simulated Modeling and Retrieval of Near-infrared Exoplanet Transmission Spectra",
"author": [
{
"family_name": "Rotman",
"given_name": "Yoav",
"orcid": "0000-0003-4459-9054"
},
{
"family_name": "McGill",
"given_name": "Peter",
"orcid": "0000-0002-1052-6749"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Rackham",
"given_name": "Benjamin V.",
"orcid": "0000-0002-3627-1676"
},
{
"family_name": "Iyer",
"given_name": "Aishwarya",
"orcid": "0000-0003-0971-1709"
},
{
"family_name": "Apai",
"given_name": "D\u00e1niel",
"orcid": "0000-0003-3714-5855"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0001-6247-8323"
},
{
"family_name": "Quintana",
"given_name": "Elisa V.",
"orcid": "0000-0003-1309-2904"
},
{
"family_name": "Dotson",
"given_name": "Jessie L.",
"orcid": "0000-0003-4206-5649"
},
{
"family_name": "Col\u00f3n",
"given_name": "Knicole D.",
"orcid": "0000-0001-8020-7121"
},
{
"family_name": "Barclay",
"given_name": "Thomas",
"orcid": "0000-0001-7139-2724"
},
{
"family_name": "Hedges",
"given_name": "Christina",
"orcid": "0000-0002-3385-8391"
},
{
"family_name": "Rowe",
"given_name": "Jason F.",
"orcid": "0000-0002-5904-1865"
},
{
"family_name": "Gilbert",
"given_name": "Emily A.",
"orcid": "0000-0002-0388-8004",
"clpid": "Gilbert-Emily-A"
},
{
"family_name": "Morris",
"given_name": "Brett M.",
"orcid": "0000-0003-2528-3409"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Foote",
"given_name": "Trevor O.",
"orcid": "0000-0002-6276-1361"
},
{
"family_name": "Soto",
"given_name": "Aylin Garc\u00eda",
"orcid": "0000-0001-9828-3229"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hoffman",
"given_name": "Kelsey",
"orcid": "0000-0001-6541-0754"
},
{
"family_name": "Hord",
"given_name": "Benjamin J.",
"orcid": "0000-0001-5084-4269"
},
{
"family_name": "Kesseli",
"given_name": "Aurora Y.",
"orcid": "0000-0002-3239-5989",
"clpid": "Kesseli-Aurora-Y"
},
{
"family_name": "Kostov",
"given_name": "Veselin B.",
"orcid": "0000-0001-9786-1031"
},
{
"family_name": "Mansfield",
"given_name": "Megan Weiner",
"orcid": "0000-0003-4241-7413"
},
{
"family_name": "Wiser",
"given_name": "Lindsey S.",
"orcid": "0000-0002-3295-1279"
}
],
"abstract": "\n
Pandora is a SmallSat mission dedicated to understanding exoplanets and their host stars by disentangling the impact of stellar heterogeneity on exoplanet transmission spectra. Selected as a NASA Astrophysics Pioneers mission in 2021, Pandora will provide simultaneous long-term visible photometric monitoring (0.4–0.7 μm) and low-resolution near-infrared (NIR) spectroscopy (0.9–1.6 μm) of transiting systems for the purposes of monitoring host star variability and characterizing exoplanetary atmospheres. Pandora’s year-long prime mission from 2026 to 2027 coincides with the middle of a decade defined by targeted efforts for atmospheric characterization of exoplanets, offering a key opportunity to leverage this new resource to maximize science with JWST and other observatories. Here we investigate Pandora’s anticipated performance for the general exoplanet population accessible to transit spectroscopy, from hot Jupiters to temperate sub-Neptunes. By modeling the atmospheres of five test cases broadly consistent with the bulk properties of HD 209458b, HD 189733b, WASP-80 b, HAT-P-18 b, and K2-18 b, we find that Pandora may provide abundance constraints as precise as ∼1.0 dex for main atmospheric absorbers such as H2O and CH4. Then, we explore the synergies between Pandora and JWST. Our results suggest that targets with JWST data in the NIR can benefit from the addition of Pandora observations and result in more reliable abundance estimates than with JWST data alone. Moreover, Pandora can serve the community by providing precursory observations of targets of interest for JWST atmospheric characterization. We conclude by outlining strategies for the use of Pandora as a standalone observatory and in synergy with JWST.
\n
\n
Accretion is the primary driver of protostellar evolution, regulating mass assembly and shaping the physical and chemical environments of young stellar objects. Quantifying accretion in the Class 0 protostellar phase is particularly important, yet remains observationally challenging due to high extinction toward the central protostars. In this paper, we present JWST NIRSpec and Mid-Infrared Instrument/Medium Resolution Spectrograph Integral Field Units data toward the Class 0 protostar L1527 IRS. We extract one-dimensional spectra and find emission from atomic and molecular hydrogen, water, OH, and several ionic species. The atomic hydrogen lines, Brα, Pfα, and Pfγ are the most critical to this study, since they can be used as accretion diagnostics. The existence of these atomic hydrogen lines viewed in scattered light indicates that accretion is likely occurring magnetospherically rather than through a boundary layer. Moment 0 emission maps show that the hydrogen emission is cospatial with the scattered light continuum with a strong east–west asymmetry that is not due to outflow shocks. We additionally present moment 0 maps of other detected species and discuss their emission morphology. By primarily analyzing the Brα line, the strongest of our detected atomic hydrogen lines, we characterize the accretion onto L1527 IRS by estimating the accretion luminosity to be ∼0.4 L\u2299 and the accretion rate to be ∼1 × 10−7 M\u2299 yr−1. Finally, we discuss the implications of our results with respect to both nonsteady and asymmetric accretion possibly occurring in L1527 IRS.
\n
\n
\n
The accretion of icy and rocky solids during the formation of a gas-giant planet is poorly constrained and challenging to model. Refractory species, like sulfur, are present only in solids in the protoplanetary disk where planets form. Measuring their abundance in planetary atmospheres is one of the most direct ways of constraining the extent and mechanism of solid accretion. Here, using the unprecedented sensitivity of NASA’s James Webb Space Telescope, we measure in detail the chemical make-up of three massive gas giants orbiting the star HR 8799, including direct detections of H2O, CO, CH4, CO2, H2S, 13CO and C18O. We find that these planets are uniformly and highly enriched in heavy elements compared with the star, irrespective of their volatile (carbon and oxygen) or refractory (sulfur) nature, which strongly indicates that the accretion of solids was efficient during their formation. This composition closely resembles that of Jupiter and Saturn and demonstrates that this enrichment also occurs in systems with several gas-giant planets orbiting stars beyond the Solar System. This discovery hints at a shared origin for the heavy-element enrichment of giant planets across a wider range of planet masses and orbital separations than previously anticipated.
\n
\n
\n
WD 0806 b is a rare exoplanet companion orbiting a white dwarf, currently with a projected orbital distance of 2500 au. The Spitzer mid-IR photometry suggests that the temperature is as cold as 350 K, making it one of the coldest directly imaged exoplanets. In this paper, we present the Near-infrared Camera (NIRCam) F150W2, F200W, F356W, and F444W broadband photometry and a 3–5 μm Near-Infrared spectroscopy (NIRSpec) G395M spectrum obtained with the James Webb Space Telescope. We develop a new retrieval framework based on the open-source PICASO software that includes additive and multiplicative systematic parameters. Our retrieval results reveal bounded abundances of H2S, CO2, CO, NH3, H2O, and CH4. We present a new chemical analysis framework that utilizes retrieved abundances to measure altitude-dependent eddy diffusion coefficients (Kzz) at multiple quenched pressures. We find that the eddy diffusion coefficients decrease from around 104–102 cm2 s−1 as the atmospheric pressure decreases from from 50 to 20 bar. To our knowledge, this is the first study to report altitude-dependent vertical mixing (or, equivalently, quenched-species-dependent vertical mixing) based on the measured molecular abundances of CO, CH4, and CO2. With the 1–21 μm NIRCam, NIRSpec, and the previously published MIRI data, we measure the bolometric luminosity to be log(L/L\u2299) = −6.75 ± 0.01 and derive the mass to be 8 ± 1MJ. The retrieval results suggest that WD 0806 b has an elevated C/O ratio of 0.76, or 1.3× solar, subsolar metallicity ([M/H ]= −0.25), and a nearly solar C/S ratio (1.17x solar).
\n
With four giant planets (m ∼ 5MJup−10MJup, Teff ∼ 900–1200 K) orbiting between 15 and 70 au, HR 8799 provides an unparalleled test bed for studying giant planet formation and probing compositional trends across the protoplanetary disk. We present new JWST/NIRSpec integral field unit observations (2.85–5.3 μm, R ≈ 2700) that now include the spectrum of HR 8799 b and higher signal-to-noise ratio spectra for HR 8799 c, d, and e compared to those in J.-B. Ruffio et al. We detect CO, CH4, H2O, H2S, CO2, and, for planet b, NH3. We combine the NIRSpec spectra with 1–5 μm photometry to perform atmospheric retrievals that account for disequilibrium chemistry and clouds, and we allow C/H, O/H, N/H, and S/H to scale independently. While the four planets are similarly enriched in carbon and oxygen, with C/H and O/H between 3× and 5× stellar, we observe a tentative trend of increasing S/H—a tracer of refractory solids—from 2× to 5× stellar with increasing orbital distance. From HR 8799 b’s NH3 abundance, we estimate N/H = 21.2_(−8.8)^(+16.2) x stellar, suggesting that the outer planet accreted significant amounts of N-rich gas. Overall, the elemental abundance patterns we observe are consistent with a picture where planet b formed between the CO snowline and the more distant N2 snowline, while the inner planets accreted 3× stellar CO-enriched disk gas within the CO snowline. The excess volatile mass from pebble drift and evaporation implies an integrated pebble flux of 750 ± 200 M⊕. The increase in the planets’ S/H with orbital distance implies more solid accretion further out, which is quantitatively compatible with expectations from both pebble and planetesimal accretion (2× minimum-mass solar nebula) paradigms.
",
"doi": "10.3847/1538-4357/ae448f",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-03-20",
"series_number": "1",
"volume": "1000",
"issue": "1",
"pages": "27"
},
{
"id": "authors:5by5k-q9x75",
"collection": "authors",
"collection_id": "5by5k-q9x75",
"cite_using_url": "https://authors.library.caltech.edu/records/5by5k-q9x75",
"type": "article",
"title": "Cloudy solutions for the clear skies of WASP-80b: 3D cloud feedback on the atmosphere and spectra of a warm Jupiter",
"author": [
{
"family_name": "Mehta",
"given_name": "Nishil",
"orcid": "0000-0001-6086-4175"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Tan",
"given_name": "Xianyu",
"orcid": "0000-0003-2278-6932"
},
{
"family_name": "Lee",
"given_name": "Elspeth K. H.",
"orcid": "0000-0002-3052-7116"
},
{
"family_name": "Guillot",
"given_name": "Tristan",
"orcid": "0000-0002-7188-8428"
},
{
"family_name": "Wiser",
"given_name": "Lindsey S.",
"orcid": "0000-0002-3295-1279"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Arnold",
"given_name": "Kenneth",
"orcid": "0000-0002-3034-8505"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0001-6247-8323"
},
{
"family_name": "Murphy",
"given_name": "Matthew M.",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
}
],
"abstract": "Context. Close-in warm Jupiters orbiting M dwarf stars are expected to exhibit diverse atmospheric chemistry, with clouds playing a key role in shaping their albedo, heat distribution, and spectral properties.
\nAims. We study WASP-80b, a warm Jupiter orbiting an M dwarf star, using the latest JWST panchromatic emission and transmission spectra to comprehensively characterise its atmosphere, including cloud coverage, chemical composition, and particle sizes, and compare the observations with predictions from the general circulation models (GCMs).
\nMethods. We used a GCM, ADAM (ADvanced Atmospheric MITgcm, formerly known as SPARC/MITgcm), combined with the latest JWST data to study the atmosphere of WASP-80b. A cloud module with radiatively active, tracer-based clouds was integrated with the GCM to study the effects on the atmosphere and the spectrum.
\nResults. We find that the emission and transmission spectra of WASP-80b are only compatible with cloudless atmospheres or with clouds composed of sufficiently large particles, namely Na2S (≥10 μm), KCl (≥1 μm), and MgSiO3 (≥5 μm). For these large-particle cloud cases, efficient gravitational settling confines the clouds to deeper atmospheric layers, resulting in weak spectral signatures. Smaller particles are ruled out due to their strong radiative feedback on the atmospheric structure.
\nConclusions. Overall, our results suggest that WASP-80b’s atmosphere is either effectively cloud-free or contains clouds composed of large, settled particles whose opacity has little impact on the observable atmosphere. This underscores the importance of particle size and vertical cloud distribution in interpreting exoplanet spectra. Future observations at shorter wavelengths may help distinguish between large-particle cloud scenarios and a truly cloudless atmosphere.
",
"doi": "10.1051/0004-6361/202557411",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2026-03",
"volume": "707",
"pages": "A394"
},
{
"id": "authors:6kqks-nvq94",
"collection": "authors",
"collection_id": "6kqks-nvq94",
"cite_using_url": "https://authors.library.caltech.edu/records/6kqks-nvq94",
"type": "article",
"title": "Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey",
"author": [
{
"family_name": "Bogat",
"given_name": "Ellis",
"orcid": "0000-0002-7325-5990"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Lawson",
"given_name": "Kellen D.",
"orcid": "0000-0002-6964-8732"
},
{
"family_name": "Li",
"given_name": "Yiting",
"orcid": "0000-0002-6845-9702"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Balmer",
"given_name": "William",
"orcid": "0000-0001-6396-8439"
},
{
"family_name": "Barclay",
"given_name": "Thomas",
"orcid": "0000-0001-7139-2724"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Bryden",
"given_name": "Geoffrey",
"orcid": "0000-0001-5966-837X"
},
{
"family_name": "Calissendorff",
"given_name": "Per",
"orcid": "0000-0002-5335-0616"
},
{
"family_name": "Carter",
"given_name": "Aarynn L.",
"orcid": "0000-0001-5365-4815"
},
{
"family_name": "De Furio",
"given_name": "Matthew",
"orcid": "0000-0003-1863-4960"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438"
},
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"orcid": "0000-0002-3414-784X"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
}
],
"abstract": "\n
The population of giant planets on wide orbits around low-mass M dwarf stars is poorly understood, but the unprecedented sensitivity of JWST NIRCam coronagraphic imaging now provides direct access to planets significantly less massive than Jupiter beyond 10 au around the closest, youngest M dwarfs. We present the design, observations, and results of JWST Guaranteed Time Observation Program 1184, a Cycle 1 NIRCam coronagraphic imaging survey of nine very nearby and young low-mass stars at 3–5 μm wavelengths. In the F356W and F444W filters, we achieve survey median 5σ contrasts deeper than 10−5 at a separation of 1″, corresponding to 0.20 MJup in F444W and 1.30 MJup in F356W at planet–star separations of 10 au. Our results include 3–5 μm debris disk detections and the identification of many extended and point-like sources in the final postprocessed images. In particular, we have identified a marginal point-source candidate having flux and color limits consistent with model predictions for a young sub-Jupiter-mass exoplanet. Under the assumption that the candidate is not confirmed, we place the first direct-imaging occurrence constraints on M dwarf wide-orbit (semimajor axes of 10–100 au), sub-Jupiter-mass exoplanets (0.3–1 MJup). We find frequency limits of <0.10 and <0.16 objects per star with 1σ and 3σ confidence, respectively. This survey showcases the unprecedented capabilities of JWST NIRCam coronagraphic imaging when targeting young, low-mass stars and acts as a precursor to broader surveys to place deep statistical constraints on wide-orbit, sub-Jupiter-mass planets around M dwarfs.
\n
WASP-80 b, a warm sub-Jovian (equilibrium temperature ∼ 820 K, 0.5 Jupiter masses), presents an opportunity to characterize a rare gas giant exoplanet around a low-mass star. In addition, its moderate temperature enables its atmosphere to host a range of carbon and oxygen species (H 2 O, CH 4 , CO, CO 2 , NH 3 ). In this paper, we present a panchromatic emission spectrum of WASP-80 b, the first gas giant around a late K/early M-dwarf star and the coolest planet for which the James Webb Space Telescope has obtained a complete emission spectrum spanning 2.4 to 12 μ m, including NIRCam F322W2 (2.4 to 4 μ m) and F444W (4 to 5 μ m), and MIRI LRS (5 to 12 μ m). We report confident detections of H 2 O, CH 4 , CO, and CO 2 , and a tentative detection of NH 3 . We estimate WASP-80 b's atmospheric metallicity and carbon-to-oxygen ratio and compare them with estimates for other gas giants. Despite the relative rarity of giant planets around low-mass stars, we find that WASP-80 b's composition is consistent with other hot gas giants, suggesting that the formation pathway of WASP-80 b may not be dissimilar from hot gas giants around higher-mass stars.
",
"doi": "10.1073/pnas.2416193122",
"pmcid": "PMC12501160",
"issn": "0027-8424",
"publisher": "National Academy of Sciences",
"publication": "Proceedings of the National Academy of Sciences",
"publication_date": "2025-09-30",
"series_number": "39",
"volume": "122",
"issue": "39",
"pages": "e2416193122"
},
{
"id": "authors:sn2fh-6gx13",
"collection": "authors",
"collection_id": "sn2fh-6gx13",
"cite_using_url": "https://authors.library.caltech.edu/records/sn2fh-6gx13",
"type": "article",
"title": "JWST Observations of Young protoStars (JOYS). Overview of program and early results",
"author": [
{
"family_name": "van Dishoeck",
"given_name": "E. F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Tychoniec",
"given_name": "\u0141.",
"orcid": "0000-0002-9470-2358"
},
{
"family_name": "Rocha",
"given_name": "W. R. M.",
"orcid": "0000-0001-6144-4113"
},
{
"family_name": "Slavicinska",
"given_name": "K.",
"orcid": "0000-0002-7433-1035"
},
{
"family_name": "Francis",
"given_name": "L.",
"orcid": "0000-0001-8822-6327"
},
{
"family_name": "van Gelder",
"given_name": "M. L.",
"orcid": "0000-0002-6312-8525"
},
{
"family_name": "Ray",
"given_name": "T. P.",
"orcid": "0000-0002-2110-1068"
},
{
"family_name": "Beuther",
"given_name": "H.",
"orcid": "0000-0002-1700-090X"
},
{
"family_name": "Caratti o Garatti",
"given_name": "A.",
"orcid": "0000-0001-8876-6614"
},
{
"family_name": "Brunken",
"given_name": "N. G. C.",
"orcid": "0000-0001-7826-7934"
},
{
"family_name": "Chen",
"given_name": "Y.",
"orcid": "0000-0002-3395-5634"
},
{
"family_name": "Devaraj",
"given_name": "R.",
"orcid": "0000-0001-9217-3168"
},
{
"family_name": "Geers",
"given_name": "V. C.",
"orcid": "0000-0003-2692-8926"
},
{
"family_name": "Gieser",
"given_name": "C.",
"orcid": "0000-0002-8120-1765"
},
{
"family_name": "Greene",
"given_name": "T. P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Justtanont",
"given_name": "K.",
"orcid": "0000-0003-1689-9201"
},
{
"family_name": "Le Gouellec",
"given_name": "V. J. M.",
"orcid": "0000-0002-5714-799X"
},
{
"family_name": "Kavanagh",
"given_name": "P. J.",
"orcid": "0000-0001-6872-2358"
},
{
"family_name": "Klaassen",
"given_name": "P. D.",
"orcid": "0000-0001-9443-0463"
},
{
"family_name": "Janssen",
"given_name": "A. G. M.",
"orcid": "0009-0002-5591-1146"
},
{
"family_name": "Navarro",
"given_name": "M. G.",
"orcid": "0000-0002-1860-2304"
},
{
"family_name": "Nazari",
"given_name": "P.",
"orcid": "0000-0002-4448-3871"
},
{
"family_name": "Notsu",
"given_name": "S.",
"orcid": "0000-0003-2493-912X"
},
{
"family_name": "Perotti",
"given_name": "G.",
"orcid": "0000-0002-8545-6175"
},
{
"family_name": "Ressler",
"given_name": "M. E.",
"orcid": "0000-0001-5644-8830"
},
{
"family_name": "Reyes",
"given_name": "S. D.",
"orcid": "0000-0003-0276-5368"
},
{
"family_name": "Sellek",
"given_name": "A. D.",
"orcid": "0000-0003-0330-1506"
},
{
"family_name": "Tabone",
"given_name": "B.",
"orcid": "0000-0002-1103-3225"
},
{
"family_name": "Tap",
"given_name": "C."
},
{
"family_name": "Theijssen",
"given_name": "N. C. M. A.",
"orcid": "0009-0007-5203-157X"
},
{
"family_name": "Colina",
"given_name": "L.",
"orcid": "0000-0002-9090-4227"
},
{
"family_name": "G\u00fcdel",
"given_name": "M.",
"orcid": "0000-0001-9818-0588"
},
{
"family_name": "Henning",
"given_name": "Th.",
"orcid": "0000-0002-1493-300X"
},
{
"family_name": "Lagage",
"given_name": "P.-O."
},
{
"family_name": "\u00d6stlin",
"given_name": "G.",
"orcid": "0000-0002-3005-1349"
},
{
"family_name": "Vandenbussche",
"given_name": "B.",
"orcid": "0000-0002-1368-3109"
},
{
"family_name": "Wright",
"given_name": "G. S.",
"orcid": "0000-0001-7416-7936"
}
],
"abstract": "Context. The embedded phase of star formation is a crucial period in the development of a young star when the system still accretes matter, emerges from its natal cloud with assistance from powerful jets and outflows, and forms a disk, thus setting the stage for the birth of a planetary system. The mid-infrared spectral line observations now possible with unprecedented sensitivity, spectral resolution, and sharpness from the James Webb Space Telescope (JWST) are key for probing many of the physical and chemical processes on subarcsecond scales that occur in highly extincted regions. They provide unique diagnostics and complement millimeter observations.
\nAims. The aim of the JWST Observations of Young protoStars (JOYS) program is to address a wide variety of topics ranging from protostellar accretion and the nature of primeval jets, winds, and outflows to the chemistry of gas and ice in hot cores and cold dense protostellar environments to the characteristics of the embedded disks. We introduce the JOYS program and show representative results.
\nMethods. The JWST Mid-InfraRed Instrument (MIRI) Medium Resolution Spectrometer (MRS) Integral Field Unit (IFU) 5-28 μm maps of 17 low-mass targets (23 if binary components are counted individually) and six high-mass protostellar sources were taken with resolving powers R = λ/Δλ = 1500-4000. We used small mosaics ranging from 1 × 1 to 3 × 3 MRS tiles to cover ~4″ to 20″ fields of view, providing spectral imaging on spatial scales down to ~30 au (low mass) and ~600 au (high mass). For HH 211, the complete ~1′ blue outflow lobe was mapped with the MRS. Atomic lines were interpreted with published shock models, whereas molecular lines were analyzed with simple rotation diagrams and local thermodynamic equilibrium slab models. We stress the importance of taking infrared pumping into account. Inferred abundance ratios were compared with detailed hot core chemical models including X-rays, whereas ice spectra were fit through comparison with laboratory spectra.
\nResults. The JWST MIRI-MRS spectra show a wide variety of features, with their spatial distribution providing key insight into their physical origin. The atomic line maps differ among refractory (e.g., Fe), semi-refractory (e.g., S), and volatile elements (e.g., Ne) and are linked to their different levels of depletion and local (shock) conditions. Jets are prominently seen in lines of [Fe\u202fII] and other refractory elements, whereas the pure rotational H2 lines probe hot (~1000 K) and warm (few ×102 K) gas inside the cavity, as well as gas associated with jets, entrained outflows, and cavity walls for both low- and high-mass sources. Wide-angle winds are found in low-J H2 lines. Nested stratified jet structures containing an inner ionized core with an outer molecular layer are commonly seen in the youngest sources. While [S\u202fI] follows the jet as seen in [Fe\u202fII] in the youngest protostars, it is different in more evolved sources, where it is concentrated on source. Noble gas lines such as [Ne\u202fII] 12.8 μm reveal a mix of jet shock and photoionized emission. The H\u202fI recombination lines serve as a measure of protostellar accretion rates but are also associated with more extended jets. Gaseous molecular emission (CO2, C2H2, HCN, H2O, CH4, SO2, SiO) is seen toward several sources, but it is cool compared with what is found in more evolved disks, with excitation temperatures of only 100-250 K, and likely associated with the warm inner envelopes (“hot cores”). Along the outflow, CO2 is often extended, thus contrasting with C2H2 , which is usually centered on source. Water emission is commonly detected on source, even if relatively weak. Off source, it is seen only in the highest density shocks, such as those associated with NGC 1333 IRAS4B. Some sources show gaseous molecular lines in absorption, including NH3 in one case. Deep ice features are seen toward the protostars, revealing not just the major ice components but also ions (as part of salts) and complex organic molecules, with comparable abundances from low- to high-mass sources. The relative abundances of some gas and ice species are similar, which is consistent with ice sublimation in hot cores. We present a second detection of HDO ice in a solar-mass source, with an HDO/H2O ice ratio of ~0.4%, thus providing a link with HDO/H2O in disks and comets. A deep search for solid O2 suggests that it is not a significant oxygen reservoir. Only a few embedded Class I disks show the same forest of water lines as Class II disks. This may be due to significant dust extinction of the upper layers in young disks caused by less settling of small dust as well as radial drift bringing in fresh dust.
\nConclusions. This paper illustrates the wide range of science questions that a single MIRI-MRS IFU data set can address. Our data suggest many similarities between low- and high-mass sources. Large source samples across evolutionary stages and luminosities are needed to further develop these diagnostics of the physics and chemistry of protostellar systems.
",
"doi": "10.1051/0004-6361/202554444",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2025-07",
"volume": "699",
"pages": "A361"
},
{
"id": "authors:3n43k-hqz73",
"collection": "authors",
"collection_id": "3n43k-hqz73",
"cite_using_url": "https://authors.library.caltech.edu/records/3n43k-hqz73",
"type": "article",
"title": "A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination",
"author": [
{
"family_name": "Murphy",
"given_name": "Matthew M.",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Radica",
"given_name": "Michael",
"orcid": "0000-0002-3328-1203"
},
{
"family_name": "Kennedy",
"given_name": "Thomas D.",
"orcid": "0000-0002-2984-3250"
},
{
"family_name": "Mehta",
"given_name": "Nishil",
"orcid": "0000-0001-6086-4175"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0002-2338-476X"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Wiser",
"given_name": "Lindsey",
"orcid": "0000-0002-3295-1279"
},
{
"family_name": "Triantafillides",
"given_name": "Anastasia",
"orcid": "0000-0002-3034-8505"
},
{
"family_name": "Rauscher",
"given_name": "Emily",
"orcid": "0000-0003-3963-9672"
},
{
"family_name": "Edelman",
"given_name": "Isaac R.",
"orcid": "0000-0001-8745-2613"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "\n
Limb-resolved transmission spectroscopy has the potential to transform our understanding of exoplanetary atmospheres. By separately measuring the transmission spectra of the evening and morning limbs, these atmospheric regions can be individually characterized, shedding light into the global distribution and transport of key atmospheric properties from transit observations alone. In this work, we follow up the recent detection of limb asymmetry on the exoplanet WASP-107 b by reanalyzing literature observations of WASP-107 b using all of James Webb Space Telescope’s science instruments (Near Infrared Imager and Slitless Spectrograph (NIRISS), Near-Infrared Camera, Near Infrared Spectrograph (NIRSpec), and Mid-Infrared Instrument) to measure its limb transmission spectra from ∼1 to 12 μm. We confirm the evening–morning temperature difference inferred previously and find that it is qualitatively consistent with predictions from global circulation models. We find evidence for evening–morning variation in SO2 and CO2 abundance, and significant cloud coverage only on WASP-107 b’s morning limb. We find that the NIRISS and NIRSpec observations are potentially contaminated by occulted starspots, which we leverage to investigate stellar contamination’s impact on limb asymmetry measurements. We find that starspot crossings can significantly bias the inferred evening and morning transmission spectra depending on when they occur during the transit, and develop a simple correction model which successfully brings these instruments’ spectra into agreement with the uncontaminated observations.
\n
The near-infrared (NIR) emission of the youngest protostars still needs to be characterized to better understand the evolution of their accretion and ejection activity. We analyze James Webb Space Telescope NIRSpec 1.7–5.3 μm observations of two deeply embedded sources in the S68N protostellar core in Serpens. The North Central source exhibits a highly obscured spectrum (A K ∼ 4.8 mag) that is modeled with a pre-main-sequence photosphere and a hot disk component. The photospheric parameters are consistent with a young, low-mass photosphere, as suggested by the low surface gravity, log g of 1.95 ±0.15 cm s−2. The hot disk suggests that accretion onto the central protostellar embryo is ongoing, although prototypical accretion-tracing emission lines H i are not detected. The South Central source, which is even more embedded (A K ∼ 8 mag; no continuum is detected shortward of 3.6 μm) appears to be driving the large-scale S68N protostellar outflow, and launches a collimated hot molecular jet detected in H2 and CO rovibrational lines. Shock modeling of the H\u2082 (ro)vibrational lines establishes that fast C-type shocks (≥30 km s\u207b¹), with high pre-shock density (≥10\u2077 cm\u207b³), and strong magnetic field (b ∼ 3–10, where B = b × n H ( cm\u207b³ ) μ G ) best match the data. The bright CO fundamental line forest suggests energetic excitation, with the contribution of non-LTE effects, i.e., irradiation pumping. Detected OH and CH+ rovibrational lines support this hypothesis. These two Class 0 protostars seem to be in very young evolutionary stages and still have to acquire the bulk of their final stellar masses. These results demonstrate that JWST enables unprecedented diagnostics of these first stages of the protostellar evolutionary phase.
",
"doi": "10.3847/1538-4357/adcac4",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-06-01",
"series_number": "2",
"volume": "985",
"issue": "2",
"pages": "225"
},
{
"id": "authors:5kk92-gww62",
"collection": "authors",
"collection_id": "5kk92-gww62",
"cite_using_url": "https://authors.library.caltech.edu/records/5kk92-gww62",
"type": "article",
"title": "A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b",
"author": [
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Murphy",
"given_name": "Matthew M.",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0002-2338-476X"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Wiser",
"given_name": "Lindsey S.",
"orcid": "0000-0002-3295-1279"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "\n
GJ 436b is the archetype warm Neptune exoplanet. The planet’s thermal emission spectrum was previously observed via intensive secondary eclipse campaigns with Spitzer. The atmosphere has long been interpreted to be extremely metal-rich, out of chemical equilibrium, and potentially tidally heated. We present the first panchromatic emission spectrum of GJ 436b observed with JWST’s NIRCAM (F322W2 and F444W) and MIRI (LRS) instruments between 2.4 and 11.9 μm. Surprisingly, the JWST spectrum appears significantly fainter around 3.6 μm than that implied by Spitzer photometry. The molecular absorption features in the spectrum are relatively weak, and we only find tentative evidence of CO2 absorption at 2σ. Under the assumption of a dayside blackbody, we find Tday = 662.8 ± 5.0 K, which is similar to the zero Bond albedo equilibrium temperature. We use it to obtain a 3σ upper limit on the Bond albedo of AB ≤ 0.66. To understand the spectrum, we employ 1D radiative–convective models but find that atmospheric constraints depend strongly on model assumptions. If thermochemical equilibrium is assumed, we find a cloudy metal-enriched atmosphere (metallicity ≥300× solar). We employ 1D photochemical modeling to show that the observed spectrum is also consistent with a cloud-free, relatively lower metallicity atmosphere (metallicity ≥80× solar) with a cold internal temperature (Tint ∼ 60 K). These are much lower metallicities and internal temperatures than inferences from Spitzer photometry. The low Tday and nondetection of transmission features at high spectral resolution do suggest a role for cloud opacity, but this is not definitive.
\n
\n
A successful theory of star formation should predict the number of objects as a function of their mass produced through star-forming events. Previous studies in star-forming regions and the solar neighborhood have identified a mass function increasing from the hydrogen-burning limit down to about 10 MJ. Theory predicts a limit to the fragmentation process, providing a natural turnover in the mass function down to the opacity limit of turbulent fragmentation, thought to be near 1–10 MJ. Programs to date have not been sensitive enough to probe the hypothesized opacity limit of fragmentation. We present the first identification of a turnover in the initial mass function below 12 MJ within NGC 2024, a young star-forming region. With JWST/NIRCam deep exposures across 0.7–5 μm, we identified several free-floating objects down to roughly 3 MJ with sensitivity to 0.5 MJ. We present evidence for a double power-law model increasing from about 60 MJ to roughly 12 MJ, consistent with previous studies, followed by a decrease down to 0.5 MJ. Our results support the predictions of star and brown dwarf formation theory, identifying the theoretical turnover in the mass function and suggesting the fundamental limit of turbulent fragmentation to be near 3 MJ.
\n
Asteroid discoveries are essential for planetary-defence efforts aiming to prevent impacts with Earth, including the more frequent megaton explosions from decametre impactors. Although large asteroids (≥100 kilometres) have remained in the main belt since their formation, small asteroids are commonly transported to the near-Earth object (NEO) population. However, owing to the lack of direct observational constraints, their size–frequency distribution (SFD)—which informs our understanding of the NEOs and the delivery of meteorite samples to Earth—varies substantially among models. Here we report 138 detections of some of the smallest asteroids (\u227310 metres) ever observed in the main belt, which were enabled by JWST's infrared capabilities covering the emission peaks of the asteroids and synthetic tracking techniques. Despite small orbital arcs, we constrain the distances and phase angles of the objects using known asteroids as proxies, allowing us to derive sizes through radiometric techniques. Their SFD shows a break at about 100 metres (debiased cumulative slopes of q = −2.66 ± 0.60 and −0.97 ± 0.14 for diameters smaller and larger than roughly 100 metres, respectively), suggestive of a population driven by collisional cascade. These asteroids were sampled from several asteroid families—most probably Nysa, Polana and Massalia—according to the geometry of pointings considered here. Through further long-stare infrared observations, JWST is poised to serendipitously detect thousands of decametre-scale asteroids across the sky, examining individual asteroid families19 and the source regions of meteorites 'in situ'.
",
"doi": "10.1038/s41586-024-08480-z",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2025-02-06",
"series_number": "8049",
"volume": "638",
"issue": "8049",
"pages": "74-78"
},
{
"id": "authors:wh80v-c2c31",
"collection": "authors",
"collection_id": "wh80v-c2c31",
"cite_using_url": "https://authors.library.caltech.edu/records/wh80v-c2c31",
"type": "article",
"title": "A Possible Metal-dominated Atmosphere below the Thick Aerosols of GJ 1214 b Suggested by Its JWST Panchromatic Transmission Spectrum",
"author": [
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Murphy",
"given_name": "Matthew M.",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Edelman",
"given_name": "Isaac R.",
"orcid": "0000-0001-8745-2613"
},
{
"family_name": "Mehta",
"given_name": "Nishil",
"orcid": "0000-0001-6086-4175"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "GJ 1214b is the archetype sub-Neptune for which thick aerosols have prevented us from constraining its atmospheric properties for over a decade. In this study, we leverage the panchromatic transmission spectrum of GJ 1214b established by the Hubble Space Telescope (HST) and JWST to investigate its atmospheric properties using a suite of atmospheric radiative transfer, photochemistry, and aerosol microphysical models. We find that the combined HST, JWST/NIRSpec, and JWST/MIRI spectrum can be well explained by atmospheric models with an extremely high metallicity of [M/H] \u223c 3.5 and an extremely high haze production rate of Fhaze \u223c 10\u22128 to 10\u22127 g cm\u22122 s\u22121. Such high atmospheric metallicity is suggested by the relatively strong CO2 feature compared to the haze absorption feature or the CH4 feature in the NIRSpec-G395H bandpass of 2.5\u20135 \u03bcm. The flat 5\u201312 \u03bcm MIRI spectrum also suggests a small scale height with a high atmospheric metallicity that is needed to suppress a prominent \u223c6 \u03bcm haze feature. We tested the sensitivity of our interpretation to various assumptions for uncertain haze properties, such as optical constants and production rate, and all models tested here consistently suggest extremely high metallicity. Thus, we conclude that GJ 1214b likely has a metal-dominated atmosphere where hydrogen is no longer the main atmospheric constituent. We also find that different assumptions for the haze production rate lead to distinct inferences for the atmospheric C/O ratio. We stress the importance of high-precision follow-up observations to confirm the metal-dominated atmosphere, as it challenges the conventional understanding of interior structure and evolution of sub-Neptunes.
",
"doi": "10.3847/2041-8213/ada02c",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2025-01-14",
"series_number": "1",
"volume": "979",
"issue": "1",
"pages": "L7"
},
{
"id": "authors:tq8we-mhx34",
"collection": "authors",
"collection_id": "tq8we-mhx34",
"cite_using_url": "https://authors.library.caltech.edu/records/tq8we-mhx34",
"type": "article",
"title": "Retrievals on NIRCam Transmission and Emission Spectra of HD 189733b with PLATON 6, a GPU Code for the JWST Era",
"author": [
{
"family_name": "Zhang",
"given_name": "Michael",
"orcid": "0000-0002-0659-1783"
},
{
"family_name": "Paragas",
"given_name": "Kimberly",
"orcid": "0000-0003-0062-1168",
"clpid": "Paragas-Kimberly"
},
{
"family_name": "Bean",
"given_name": "Jacob L.",
"orcid": "0000-0003-4733-6532"
},
{
"family_name": "Yeung",
"given_name": "Joseph"
},
{
"family_name": "Chachan",
"given_name": "Yayaati",
"orcid": "0000-0003-1728-8269"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Lunine",
"given_name": "Jonathan",
"orcid": "0000-0003-2279-4131",
"clpid": "Lunine-Jonathan-Irving"
},
{
"family_name": "Deming",
"given_name": "Drake",
"orcid": "0000-0001-5727-4094"
}
],
"abstract": "We present the 2.4–5.0 μm JWST/NIRCam emission spectrum of HD 189733b, along with an independent re-reduction of the previously published transmission spectrum at the same wavelengths. We use an upgraded version of PLanetary Atmospheric Tool for Observer Noobs (PLATON) to retrieve atmospheric parameters from both geometries. In transit, we obtain [M/H] = 0.53^(+0.13)_(-0.12) and C/O = 0.41^(+0.13)_(-0.12), assuming a power-law haze and equilibrium chemistry with methane depletion. In eclipse, we obtain [M/H] = 0.68^(+0.15)_(-0.11) and C/O = 0.43^(+0.06)_(-0.05), assuming a clear atmosphere and equilibrium chemistry without methane depletion. These results are consistent with each other, and with a rerun of our previously published joint retrieval of Hubble Space Telescope and Spitzer transmission and emission spectra. Accounting for methane depletion decreases the C/O ratio by 0.14/0.04 (transmission/emission), but changing the limb cloud parameterization does not affect the C/O ratio by more than 0.06. We detect H2O, CO2, CO, and H2S in both the NIRCam transmission and emission spectra, find that methane is depleted on the terminator, and confirm with VULCAN that photochemistry is a potential cause of this depletion. We also find tentative (1.8σ) evidence of a dayside thermal inversion at millibar pressures. Finally, we take this opportunity to introduce a new version of PLATON. PLATON 6 supports GPU computation, speeding up the code up to 10×. It also supports free retrievals using both volume mixing ratio and centered-log ratio priors; emission from planetary surfaces of different compositions; updated opacities at improved resolution; and Pareto smoothed importance sampling leave-one-out cross-validation.
",
"doi": "10.3847/1538-3881/ad8cd2",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2025-01",
"series_number": "1",
"volume": "169",
"issue": "1",
"pages": "38"
},
{
"id": "authors:5rxpv-aa229",
"collection": "authors",
"collection_id": "5rxpv-aa229",
"cite_using_url": "https://authors.library.caltech.edu/records/5rxpv-aa229",
"type": "article",
"title": "JOYS+ study of solid-state \u00b9\u00b2C/\u00b9\u00b3C isotope ratios in protostellar envelopes: Observations of CO and CO\u2082 ice with the James Webb Space Telescope",
"author": [
{
"family_name": "Brunken",
"given_name": "N. G. C.",
"orcid": "0000-0001-7826-7934"
},
{
"family_name": "van Dishoeck",
"given_name": "E. F.",
"orcid": "0000-0001-7591-1907"
},
{
"family_name": "Slavicinska",
"given_name": "K.",
"orcid": "0000-0002-7433-1035"
},
{
"family_name": "le Gouellec",
"given_name": "V. J. M.",
"orcid": "0000-0002-5714-799X"
},
{
"family_name": "Rocha",
"given_name": "W. R. M.",
"orcid": "0000-0001-6144-4113"
},
{
"family_name": "Francis",
"given_name": "L.",
"orcid": "0000-0001-8822-6327"
},
{
"family_name": "Tychoniec",
"given_name": "L.",
"orcid": "0000-0002-9470-2358"
},
{
"family_name": "van Gelder",
"given_name": "M. L.",
"orcid": "0000-0002-6312-8525"
},
{
"family_name": "Navarro",
"given_name": "M. G.",
"orcid": "0000-0002-1860-2304"
},
{
"family_name": "Boogert",
"given_name": "A. C. A.",
"orcid": "0000-0001-9344-0096"
},
{
"family_name": "Kavanagh",
"given_name": "P. J.",
"orcid": "0000-0001-6872-2358"
},
{
"family_name": "Nazari",
"given_name": "P.",
"orcid": "0000-0002-4448-3871"
},
{
"family_name": "Greene",
"given_name": "T.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Ressler",
"given_name": "M. E.",
"orcid": "0000-0001-5644-8830"
},
{
"family_name": "Majumdar",
"given_name": "L.",
"orcid": "0000-0001-7031-8039"
}
],
"abstract": "Context . The carbon isotope ratio is a powerful tool for studying the evolution of stellar systems due to its sensitivity to the local chemical environment. Recent detections of CO isotopologs in disks and exoplanet atmospheres revealed a high variability in the isotope abundance, ponting towards significant fractionation in these systems. In order to fully understand the evolution of this quantity in stellar and planetary systems, however, it is crucial to trace the isotope abundance from stellar nurseries to the time of planet formation. During the protostellar stage, the multiple vibrational modes of CO2and CO ice, which peak in the near- and mid-infrared, provide a unique opportunity to examine the carbon isotope ratio in the solid state. With the current sensitivity and wide spectral coverage of the James Webb Space Telescope, the multiple weak and strong absorption features of CO2and CO have become accessible at a high signal-to-noise ratio in solar-mass systems.
Aims . We aim to study the carbon isotope ratio during the protostellar stage by deriving column densities and ratios from the various absorption bands of CO2and CO ice, and by comparing our results with the ratios derived in other astronomical environments.
Methods . We quantify the12CO2/13CO2and the12CO/13CO isotope ratios in 17 class 0/I low-mass protostars from the12CO2\u03bd1+\u03bd2and 2\u03bd1+\u03bd2combination modes (2.70 \u00b5m and 2.77 \u00b5m), the12CO2\u03bd3stretching mode (4.27 \u00b5m), the13CO2\u03bd3stretching mode (4.39 \u00b5m), the12CO2\u03bd2bending mode (15.2 \u00b5m), the12CO 1-0 stretching mode (4.67 \u00b5m), and the13CO 1-0 stretching mode (4.78 \u00b5m) using the James Webb Space Telescope NIRSpec and MIRI observations. We also report a detection of the 2-0 overtone mode of12CO at 2.35 \u00b5m.
Results . The column densities and12CO2/13CO2ratios derived from the various CO2vibrational modes agree within the reported uncertainties, and we find mean ratios of 85 \u00b1 23, 76 \u00b1 12, and 97 \u00b1 17 for the 2.70 \u00b5m band, the 4.27 \u00b5m band, and the 15.2 \u00b5m band, respectively. The main source of uncertainty on the derived values stems from the error on the band strengths; the observational errors are negligible in comparison. Variation of the12CO2/13CO2ratio is observed from one source to the next, which indicates that the chemical conditions of their envelopes might be genuinely different. The12CO/13CO ratios derived from the 4.67 \u00b5m band are consistent, albeit elevated with respect to the12CO2/13CO2ratios, and we find a mean ratio of 165 \u00b1 52.
Conclusions . These findings indicate that ices leave the prestellar stage with elevated carbon isotope ratios relative to the overall values found in the interstellar medium, and that fractionation becomes a significant factor during the later stages of star and planet formation.
",
"doi": "10.1051/0004-6361/202451794",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2024-12",
"volume": "692",
"pages": "A163"
},
{
"id": "authors:3pb2q-k1m34",
"collection": "authors",
"collection_id": "3pb2q-k1m34",
"cite_using_url": "https://authors.library.caltech.edu/records/3pb2q-k1m34",
"type": "article",
"title": "Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b",
"author": [
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Murphy",
"given_name": "Matthew M.",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Edelman",
"given_name": "Isaac R.",
"orcid": "0000-0001-8745-2613"
},
{
"family_name": "Gill",
"given_name": "Samuel",
"orcid": "0000-0002-4259-0155"
},
{
"family_name": "Anderson",
"given_name": "David R.",
"orcid": "0000-0001-7416-7522"
},
{
"family_name": "Wheatley",
"given_name": "Peter J.",
"orcid": "0000-0003-1452-2240"
},
{
"family_name": "Henry",
"given_name": "Gregory W.",
"orcid": "0000-0003-4155-8513"
},
{
"family_name": "Mehta",
"given_name": "Nishil",
"orcid": "0000-0001-6086-4175"
},
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "Sub-Neptune planets with radii smaller than Neptune (3.9 R\u2295) are the most common type of planet known to exist in the Milky Way, even though they are absent in the solar system. These planets can potentially have a large diversity of compositions as a result of different mixtures of rocky material, icy material, and gas accreted from a protoplanetary disk. However, the bulk density of a sub-Neptune, informed by its mass and radius alone, cannot uniquely constrain its composition; atmospheric spectroscopy is necessary. GJ 1214 b, which hosts an atmosphere that is potentially the most favorable for spectroscopic detection of any sub-Neptune, is instead enshrouded in aerosols (thus showing no spectroscopic features), hiding its composition from view at previously observed wavelengths in its terminator. Here, we present a JWST NIRSpec transmission spectrum from 2.8 to 5.1 \u03bcm that shows signatures of CO2 and CH4, expected at high metallicity. A model containing both these molecules is preferred by 3.3\u03c3 and 3.6\u03c3 as compared to a featureless spectrum for two different data analysis pipelines, respectively. Given the low signal-to-noise of the features compared to the continuum, however, more observations are needed to confirm the CO2 and CH4 signatures and better constrain other diagnostic features in the near-infrared. Further modeling of the planet's atmosphere, interior structure and origins will provide valuable insights about how sub-Neptunes like GJ 1214 b form and evolve.
",
"doi": "10.3847/2041-8213/ad7fef",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-10-01",
"series_number": "2",
"volume": "974",
"issue": "2",
"pages": "L33"
},
{
"id": "authors:djc3q-wbe94",
"collection": "authors",
"collection_id": "djc3q-wbe94",
"cite_using_url": "https://authors.library.caltech.edu/records/djc3q-wbe94",
"type": "article",
"title": "Evidence for morning-to-evening limb asymmetry on the cool low-density exoplanet WASP-107 b",
"author": [
{
"family_name": "Murphy",
"given_name": "Matthew M.",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0001-6247-8323"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Rauscher",
"given_name": "Emily",
"orcid": "0000-0003-3963-9672"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "The atmospheric properties of hot exoplanets are expected to be different between the morning and the evening limbs due to their global atmospheric circulation. Ground-based observations at high spectral resolution have detected this limb asymmetry in several ultra-hot (>2,000\u2009K) exoplanets, but the prevalence of the phenomenon in the broader exoplanetary population remains unexplored. Here we use JWST/NIRCam transmission spectra between 2.5 and 4.0\u2009\u03bcm to find evidence of limb asymmetry on exoplanet WASP-107 b. With its equilibrium temperature of 770\u2009K and low density of 0.126\u2009g\u2009cm\u22123, WASP-107 b probes a very different regime compared to ultra-hot giant planets and was not expected to exhibit substantial spatial heterogeneity according to atmospheric models. We infer instead a morning-to-evening temperature difference of the order of 100\u2009K with a hotter evening limb. Further observations of other cooler exoplanets are needed to determine whether WASP-107 b is an outlier or whether the models have underestimated the presence of limb asymmetry in exoplanets.",
"doi": "10.1038/s41550-024-02367-9",
"issn": "2397-3366",
"publisher": "Nature Publishing Group",
"publication": "Nature Astronomy",
"publication_date": "2024-09-24",
"series_number": "12",
"volume": "8",
"issue": "12",
"pages": "1562-1574"
},
{
"id": "authors:yy1q8-a8d80",
"collection": "authors",
"collection_id": "yy1q8-a8d80",
"cite_using_url": "https://authors.library.caltech.edu/records/yy1q8-a8d80",
"type": "article",
"title": "Hydrogen sulfide and metal-enriched atmosphere for a Jupiter-mass exoplanet",
"author": [
{
"family_name": "Fu",
"given_name": "Guangwei",
"orcid": "0000-0002-3263-2251",
"clpid": "Fu-Guangwei"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564",
"clpid": "Welbanks-Luis"
},
{
"family_name": "Deming",
"given_name": "Drake",
"orcid": "0000-0001-5727-4094",
"clpid": "Deming-Drake"
},
{
"family_name": "Inglis",
"given_name": "Julie",
"orcid": "0000-0001-9164-7966",
"clpid": "Inglis-Julie"
},
{
"family_name": "Zhang",
"given_name": "Michael",
"orcid": "0000-0002-0659-1783",
"clpid": "Zhang-Michael"
},
{
"family_name": "Lothringer",
"given_name": "Joshua",
"orcid": "0000-0003-3667-8633",
"clpid": "Lothringer-Joshua"
},
{
"family_name": "Ih",
"given_name": "Jegug",
"clpid": "Ih-Jegug"
},
{
"family_name": "Moses",
"given_name": "Julianne I.",
"orcid": "0000-0002-8837-0035",
"clpid": "Moses-Julianne-I"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490",
"clpid": "Schlawin-Everett"
},
{
"family_name": "Knutson",
"given_name": "Heather A,",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Henry",
"given_name": "Gregory",
"orcid": "0000-0003-4155-8513",
"clpid": "Henry-Gregory"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Sing",
"given_name": "David K.",
"orcid": "0000-0001-6050-7645",
"clpid": "Sing-David-K"
},
{
"family_name": "Savel",
"given_name": "Arjun B.",
"orcid": "0000-0002-2454-768X",
"clpid": "Savel-Arjun-B"
},
{
"family_name": "Kempton",
"given_name": "Eliza M.-R.",
"orcid": "0000-0002-1337-9051",
"clpid": "Kempton-Eliza-M-R"
},
{
"family_name": "Louie",
"given_name": "Dana R.",
"orcid": "0000-0002-2457-272X",
"clpid": "Louie-Dana-R"
},
{
"family_name": "Line",
"given_name": "Michael",
"orcid": "0000-0001-6247-8323",
"clpid": "Line-Michael"
},
{
"family_name": "Nixon",
"given_name": "Matt",
"orcid": "0000-0001-8236-5553",
"clpid": "Nixon-Matt"
}
],
"abstract": "\n
\n
As the closest transiting hot Jupiter to Earth, HD 189733b has been the benchmark planet for atmospheric characterization. It has also been the anchor point for much of our theoretical understanding of exoplanet atmospheres from composition, chemistry, aerosols to atmospheric dynamics, escape and modelling techniques. Previous studies of HD 189733b have detected carbon and oxygen-bearing molecules H2O and CO (refs. 12-13) in the atmosphere. The presence of CO2 and CH4 has been claimed but later disputed. The inferred metallicity based on these measurements, a key parameter in tracing planet formation locations, varies from depletion to enhancement, hindered by limited wavelength coverage and precision of the observations. Here we report detections of H2O (13.4σ), CO2 (11.2σ), CO (5σ) and H2S (4.5σ) in the transmission spectrum (2.4–5.0 μm) of HD 189733b. With an equilibrium temperature of about 1,200 K, H2O, CO and H2S are the main reservoirs for oxygen, carbon and sulfur. Based on the measured abundances of these three main volatile elements, we infer an atmospheric metallicity of three to five times stellar. The upper limit on the methane abundance at 5σ is 0.1 ppm, which indicates a low carbon-to-oxygen ratio (<0.2), suggesting formation through the accretion of water-rich icy planetesimals. The low oxygen-to-sulfur and carbon-to-sulfur ratios also support the planetesimal accretion formation pathway.
\n
\n
WASP-69 b is a hot, inflated, Saturn-mass planet (0.26 MJup) with a zero-albedo equilibrium temperature of 963 K. Here, we report the JWST 2\u201312 \u03bcm emission spectrum of the planet consisting of two eclipses observed with NIRCam grism time series and one eclipse observed with the MIRI low-resolution spectrometer (LRS). The emission spectrum shows absorption features of water vapor, carbon dioxide, and carbon monoxide, but no strong evidence for methane. WASP-69 b's emission spectrum is poorly fit by cloud-free homogeneous models. We find three possible model scenarios for the planet: (1) a scattering model that raises the brightness at short wavelengths with a free geometric albedo parameter; (2) a cloud-layer model that includes high-altitude silicate aerosols to moderate long-wavelength emission; and (3) a two-region model that includes significant dayside inhomogeneity and cloud opacity with two different temperature\u2013pressure profiles. In all cases, aerosols are needed to fit the spectrum of the planet. The scattering model requires an unexpectedly high geometric albedo of 0.64. Our atmospheric retrievals indicate inefficient redistribution of heat and an inhomogeneous dayside distribution, which is tentatively supported by MIRI LRS broadband eclipse maps that show a central concentration of brightness. Our more plausible models (2 and 3) retrieve chemical abundances enriched in heavy elements relative to solar composition by 6\u00d7 to 14\u00d7 solar and a C/O ratio of 0.65\u20130.94, whereas the less plausible highly reflective scenario (1) retrieves a slightly lower metallicity and lower C/O ratio.
",
"doi": "10.3847/1538-3881/ad58e0",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-08-02",
"series_number": "3",
"volume": "168",
"issue": "3",
"pages": "104"
},
{
"id": "authors:ehmc7-5e012",
"collection": "authors",
"collection_id": "ehmc7-5e012",
"cite_using_url": "https://authors.library.caltech.edu/records/ehmc7-5e012",
"type": "article",
"title": "Toward Exoplanet Transit Spectroscopy Using JWST/MIRI's Medium Resolution Spectrometer",
"author": [
{
"family_name": "Deming",
"given_name": "Drake",
"orcid": "0000-0001-5727-4094"
},
{
"family_name": "Fu",
"given_name": "Guangwei",
"orcid": "0000-0002-3263-2251"
},
{
"family_name": "Bouwman",
"given_name": "Jeroen",
"orcid": "0000-0003-4757-2500"
},
{
"family_name": "Dicken",
"given_name": "Daniel",
"orcid": "0000-0003-0589-5969"
},
{
"family_name": "Espinoza",
"given_name": "Nestor",
"orcid": "0000-0001-9513-1449"
},
{
"family_name": "Glasse",
"given_name": "Alistair",
"orcid": "0000-0002-2041-2462"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Kendrew",
"given_name": "Sarah",
"orcid": "0000-0002-7612-0469"
},
{
"family_name": "Law",
"given_name": "David",
"orcid": "0000-0002-9402-186X"
},
{
"family_name": "Lustig-Yaeger",
"given_name": "Jacob",
"orcid": "0000-0002-0746-1980"
},
{
"family_name": "Garcia Marin",
"given_name": "Macarena",
"orcid": "0000-0003-4801-0489"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
}
],
"abstract": "The Mid-Infrared Instrument Medium Resolution Spectrometer (the MRS) on JWST has potentially important advantages for transit and eclipse spectroscopy of exoplanets, including lack of saturation for bright host stars, wavelength span to longward of 20 \u00b5m, and JWST's highest spectral resolving power. We here test the performance of the MRS for time series spectroscopy by observing the secondary eclipse of the bright stellar eclipsing binary R Canis Majoris. Our observations push the MRS into saturation at the shortest wavelength, more than for any currently known exoplanet system. We find strong charge migration between pixels that we mitigate using a custom data analysis pipeline. Our data analysis recovers much of the spatial charge migration by combining detector pixels at the group level, via weighting by the point-spread function. We achieve nearly photon-limited performance in time series data at wavelengths longward of 5.2 \u00b5m. In 2017, Snellen et al. suggested that the MRS could be used to detect carbon dioxide absorption from the atmosphere of the temperate planet orbiting Proxima Centauri. We infer that the relative spectral response of the MRS versus wavelength is sufficiently stable to make that detection feasible. As regards the secondary eclipse of this Algol-type binary, we measure the eclipse depth by summing our spectra over the wavelengths in four channels, and also measuring the eclipse depth as observed by TESS. Those eclipse depths require a temperature for the secondary star that is significantly hotter than previous observations in the optical to near-IR, probably due to irradiation by the primary star. At full spectral resolution of the MRS, we find atomic hydrogen recombination emission lines in the secondary star, from principal quantum levels n = 7, 8, 10, and 14.
",
"doi": "10.1088/1538-3873/ad6692",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2024-08-01",
"series_number": "8",
"volume": "136",
"issue": "8",
"pages": "084402"
},
{
"id": "authors:78nb2-xby34",
"collection": "authors",
"collection_id": "78nb2-xby34",
"cite_using_url": "https://authors.library.caltech.edu/records/78nb2-xby34",
"type": "article",
"title": "Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b",
"author": [
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0002-2338-476X"
},
{
"family_name": "Murphy",
"given_name": "Matthew",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Edelman",
"given_name": "Isaac",
"orcid": "0000-0001-8745-2613"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Henry",
"given_name": "Gregory W.",
"orcid": "0000-0003-4155-8513"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Rauscher",
"given_name": "Emily",
"orcid": "0000-0003-3963-9672"
},
{
"family_name": "Wiser",
"given_name": "Lindsey S.",
"orcid": "0000-0002-3295-1279"
},
{
"family_name": "Triantafillides",
"given_name": "Anastasia",
"orcid": "0000-0002-3034-8505"
}
],
"abstract": "We report observations of the atmospheric transmission spectrum of the sub-Neptune exoplanet GJ 3470 b taken using the Near-Infrared Camera on JWST. Combined with two archival Hubble Space Telescope/Wide-Field Camera 3 transit observations and 15 archival Spitzer transit observations, we detect water, methane, sulfur dioxide, and carbon dioxide in the atmosphere of GJ 3470 b, each with a significance of >3\u03c3. GJ 3470 b is the lowest-mass\u2014and coldest\u2014exoplanet known to show a substantial sulfur dioxide feature in its spectrum, atMp= 11.2M\u2295andTeq= 600 K. This indicates that disequilibrium photochemistry drives sulfur dioxide production in exoplanet atmospheres over a wider range of masses and temperatures than has been reported or expected. The water, carbon dioxide, and sulfur dioxide abundances we measure indicate an atmospheric metallicity of approximately 100\u00d7 solar. We see further evidence for disequilibrium chemistry in our inferred methane abundance, which is significantly lower than expected from equilibrium models consistent with our measured water and carbon dioxide abundances.
",
"doi": "10.3847/2041-8213/ad55e9",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-07-01",
"series_number": "1",
"volume": "970",
"issue": "1",
"pages": "L10"
},
{
"id": "authors:8wndv-9ts52",
"collection": "authors",
"collection_id": "8wndv-9ts52",
"cite_using_url": "https://authors.library.caltech.edu/records/8wndv-9ts52",
"type": "article",
"title": "A roadmap for the atmospheric characterization of terrestrial exoplanets with JWST",
"author": [
{
"family_name": "de Wit",
"given_name": "Julien",
"orcid": "0000-0003-2415-2191",
"clpid": "de-Wit-Julien"
},
{
"family_name": "Doyon",
"given_name": "Ren\u00e9",
"orcid": "0000-0001-5485-4675"
},
{
"family_name": "Rackham",
"given_name": "Benjamin V.",
"orcid": "0000-0002-3627-1676"
},
{
"family_name": "Lim",
"given_name": "Olivia",
"orcid": "0000-0003-4676-0622"
},
{
"family_name": "Ducrot",
"given_name": "Elsa",
"orcid": "0000-0002-7008-6888"
},
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Ribas",
"given_name": "Ignasi",
"orcid": "0000-0002-6689-0312"
},
{
"family_name": "Berardo",
"given_name": "David",
"orcid": "0000-0001-6298-412X"
},
{
"family_name": "Niraula",
"given_name": "Prajwal",
"orcid": "0000-0002-8052-3893"
},
{
"family_name": "Iyer",
"given_name": "Aishwarya"
},
{
"family_name": "Shapiro",
"given_name": "Alexander",
"orcid": "0000-0002-8842-5403"
},
{
"family_name": "Kostogryz",
"given_name": "Nadiia",
"orcid": "0000-0002-6087-3271"
},
{
"family_name": "Witzke",
"given_name": "Veronika",
"orcid": "0000-0002-0929-1612"
},
{
"family_name": "Gillon",
"given_name": "Micha\u00ebl",
"orcid": "0000-0003-1462-7739"
},
{
"family_name": "Agol",
"given_name": "Eric",
"orcid": "0000-0002-0802-9145"
},
{
"family_name": "Meadows",
"given_name": "Victoria",
"orcid": "0000-0002-1386-1710"
},
{
"family_name": "Burgasser",
"given_name": "Adam J.",
"orcid": "0000-0002-6523-9536"
},
{
"family_name": "Owen",
"given_name": "James E.",
"orcid": "0000-0002-4856-7837"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Selsis",
"given_name": "Franck",
"orcid": "0000-0001-9619-5356"
},
{
"family_name": "Bello-Arufe",
"given_name": "Aaron",
"orcid": "0000-0003-3355-1223",
"clpid": "Bello-Arufe-Aaron"
},
{
"family_name": "de Beurs",
"given_name": "Zo\u00eb",
"orcid": "0000-0002-7564-6047"
},
{
"family_name": "Bolmont",
"given_name": "Emeline",
"orcid": "0000-0001-5657-4503"
},
{
"family_name": "Cowan",
"given_name": "Nicolas",
"orcid": "0000-0001-6129-5699"
},
{
"family_name": "Dong",
"given_name": "Chuanfei",
"orcid": "0000-0002-8990-094X"
},
{
"family_name": "Drake",
"given_name": "Jeremy J.",
"orcid": "0000-0002-0210-2276"
},
{
"family_name": "Garcia",
"given_name": "Lionel",
"orcid": "0000-0002-4296-2246"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Haworth",
"given_name": "Thomas",
"orcid": "0000-0002-9593-7618"
},
{
"family_name": "Hu",
"given_name": "Renyu",
"orcid": "0000-0003-2215-8485",
"clpid": "Hu-Renyu"
},
{
"family_name": "Kane",
"given_name": "Stephen R.",
"orcid": "0000-0002-7084-0529"
},
{
"family_name": "Kervella",
"given_name": "Pierre",
"orcid": "0000-0003-0626-1749"
},
{
"family_name": "Koll",
"given_name": "Daniel",
"orcid": "0000-0002-9076-6901"
},
{
"family_name": "Krissansen-Totton",
"given_name": "Joshua",
"orcid": "0000-0001-6878-4866"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Lichtenberg",
"given_name": "Tim",
"orcid": "0000-0002-3286-7683"
},
{
"family_name": "Lustig-Yaeger",
"given_name": "Jacob",
"orcid": "0000-0002-0746-1980"
},
{
"family_name": "Lingam",
"given_name": "Manasvi",
"orcid": "0000-0002-2685-9417"
},
{
"family_name": "Turbet",
"given_name": "Martin",
"orcid": "0000-0003-2260-9856"
},
{
"family_name": "Seager",
"given_name": "Sara",
"orcid": "0000-0002-6892-6948"
},
{
"family_name": "Barkaoui",
"given_name": "Khalid",
"orcid": "0000-0003-1464-9276"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Burdanov",
"given_name": "Artem",
"orcid": "0000-0001-9892-2406"
},
{
"family_name": "Cadieux",
"given_name": "Charles",
"orcid": "0000-0001-9291-5555"
},
{
"family_name": "Charnay",
"given_name": "Benjamin"
},
{
"family_name": "Cloutier",
"given_name": "Ryan",
"orcid": "0000-0001-5383-9393"
},
{
"family_name": "Cook",
"given_name": "Neil J.",
"orcid": "0000-0003-4166-4121"
},
{
"family_name": "Correia",
"given_name": "Alexandre C. M.",
"orcid": "0000-0002-8946-8579"
},
{
"family_name": "Dang",
"given_name": "Lisa",
"orcid": "0000-0003-4987-6591"
},
{
"family_name": "Daylan",
"given_name": "Tansu",
"orcid": "0000-0002-6939-9211"
},
{
"family_name": "Delrez",
"given_name": "Laetitia",
"orcid": "0000-0001-6108-4808"
},
{
"family_name": "Edwards",
"given_name": "Billy",
"orcid": "0000-0002-5494-3237"
},
{
"family_name": "Fauchez",
"given_name": "Thomas J.",
"orcid": "0000-0002-5967-9631"
},
{
"family_name": "Flagg",
"given_name": "Laura",
"orcid": "0000-0001-6362-0571"
},
{
"family_name": "Fraschetti",
"given_name": "Federico",
"orcid": "0000-0002-5456-4771"
},
{
"family_name": "Haqq-Misra",
"given_name": "Jacob",
"orcid": "0000-0003-4346-2611"
},
{
"family_name": "Huang",
"given_name": "Ziyu",
"orcid": "0000-0002-8624-1264"
},
{
"family_name": "Iro",
"given_name": "Nicolas",
"orcid": "0000-0003-2329-418X"
},
{
"family_name": "Jayawardhana",
"given_name": "Ray",
"orcid": "0000-0001-5349-6853"
},
{
"family_name": "Jehin",
"given_name": "Emmanuel",
"orcid": "0000-0001-8923-488X"
},
{
"family_name": "Jin",
"given_name": "Meng",
"orcid": "0000-0002-9672-3873"
},
{
"family_name": "Kite",
"given_name": "Edwin",
"orcid": "0000-0002-1426-1186"
},
{
"family_name": "Kitzmann",
"given_name": "Daniel",
"orcid": "0000-0003-4269-3311"
},
{
"family_name": "Kral",
"given_name": "Quentin",
"orcid": "0000-0001-6527-4684"
},
{
"family_name": "Lafreni\u00e8re",
"given_name": "David",
"orcid": "0000-0002-6780-4252"
},
{
"family_name": "Libert",
"given_name": "Anne-Sophie",
"orcid": "0000-0003-2682-2793"
},
{
"family_name": "Liu",
"given_name": "Beibei",
"orcid": "0000-0001-5830-3619"
},
{
"family_name": "Mohanty",
"given_name": "Subhanjoy",
"orcid": "0000-0002-9896-8313"
},
{
"family_name": "Morris",
"given_name": "Brett M.",
"orcid": "0000-0003-2528-3409"
},
{
"family_name": "Murray",
"given_name": "Catriona A.",
"orcid": "0000-0001-8504-5862"
},
{
"family_name": "Piaulet",
"given_name": "Caroline",
"orcid": "0000-0002-2875-917X"
},
{
"family_name": "Pozuelos",
"given_name": "Francisco J.",
"orcid": "0000-0003-1572-7707"
},
{
"family_name": "Radica",
"given_name": "Michael",
"orcid": "0000-0002-3328-1203"
},
{
"family_name": "Ranjan",
"given_name": "Sukrit",
"orcid": "0000-0002-5147-9053"
},
{
"family_name": "Rathcke",
"given_name": "Alexander",
"orcid": "0000-0002-4227-4953"
},
{
"family_name": "Roy",
"given_name": "Pierre-Alexis",
"orcid": "0000-0001-6809-3520"
},
{
"family_name": "Schwieterman",
"given_name": "Edward W.",
"orcid": "0000-0002-2949-2163"
},
{
"family_name": "Turner",
"given_name": "Jake D.",
"orcid": "0000-0001-7836-1787"
},
{
"family_name": "Triaud",
"given_name": "Amaury",
"orcid": "0000-0002-5510-8751"
},
{
"family_name": "Way",
"given_name": "Michael J.",
"orcid": "0000-0003-3728-0475"
},
{
"literal": "TRAPPIST-1 JWST Community Initiative"
}
],
"abstract": "\n
\n
Ultracool dwarf stars are abundant, long-lived and uniquely suited to enable the atmospheric study of transiting terrestrial companions with the JWST. Among them, the most prominent is the M8.5V star TRAPPIST-1 and its seven planets. While JWST Cycle 1 observations have started to yield preliminary insights into the planets, they have also revealed that their atmospheric exploration requires a better understanding of their host star. Here we propose a roadmap to characterize the TRAPPIST-1 system — and others like it — in an efficient and robust manner with JWST. We notably recommend that — although more challenging to schedule — multi-transit windows be prioritized to mitigate the effects of stellar activity and gather up to twice more transits per JWST hour spent. We conclude that, for such systems, planets cannot be studied in isolation by small programmes but rather need large-scale, joint space- and ground-based initiatives to fully exploit the capabilities of JWST for the exploration of terrestrial planets.
\n
\n
We present the first results of the JWST program PROJECT-J (PROtostellar JEts Cradle Tested with JWST), designed to study the Class I source HH46 IRS and its outflow through NIRSpec and MIRI spectroscopy (1.66\u201328 \u03bcm). The data provide line images (\u223c6.\u20336 in length with NIRSpec, and up to \u223c20\u2033 with MIRI) revealing unprecedented details within the jet, the molecular outflow, and the cavity. We detect, for the first time, the redshifted jet within \u223c90 au from the source. Dozens of shock-excited forbidden lines are observed, including highly ionized species such as [Ne iii] 15.5 \u03bcm, suggesting that the gas is excited by high velocity (>80 km s\u22121) shocks in a relatively high-density medium. Images of H2 lines at different excitations outline a complex molecular flow, where a bright cavity, molecular shells, and a jet-driven bow shock interact with and are shaped by the ambient conditions. Additional NIRCam 2 \u03bcm images resolve the HH46 IRS \u223c110 au binary system and suggest that the large asymmetries observed between the jet and the H2 wide-angle emission could be due to two separate outflows being driven by the two sources. The spectra of the unresolved binary show deep ice bands and plenty of gaseous lines in absorption, likely originating in a cold envelope or disk. In conclusion, JWST has unraveled for the first time the origin of the HH46 IRS complex outflow demonstrating its capability to investigate embedded regions around young stars, which remain elusive even at near-IR wavelengths.
",
"doi": "10.3847/1538-4357/ad3d5a",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2024-05-30",
"series_number": "2",
"volume": "967",
"issue": "2",
"pages": "168"
},
{
"id": "authors:4fdm8-tnx49",
"collection": "authors",
"collection_id": "4fdm8-tnx49",
"cite_using_url": "https://authors.library.caltech.edu/records/4fdm8-tnx49",
"type": "article",
"title": "A high internal heat flux and large core in a warm Neptune exoplanet",
"author": [
{
"family_name": "Welbanks",
"given_name": "Luis",
"orcid": "0000-0003-0156-4564"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Line",
"given_name": "Michael R.",
"orcid": "0000-0001-6247-8323"
},
{
"family_name": "Ohno",
"given_name": "Kazumasa",
"orcid": "0000-0003-3290-6758"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Rauscher",
"given_name": "Emily",
"orcid": "0000-0003-3963-9672"
},
{
"family_name": "McGill",
"given_name": "Peter",
"orcid": "0000-0002-1052-6749"
},
{
"family_name": "Murphy",
"given_name": "Matthew",
"orcid": "0000-0002-8517-8857"
},
{
"family_name": "Parmentier",
"given_name": "Vivien",
"orcid": "0000-0001-9521-6258"
},
{
"family_name": "Tang",
"given_name": "Yao",
"orcid": "0000-0003-3980-7808"
},
{
"family_name": "Edelman",
"given_name": "Isaac",
"orcid": "0000-0001-8745-2613"
},
{
"family_name": "Mukherjee",
"given_name": "Sagnick",
"orcid": "0000-0003-1622-1302"
},
{
"family_name": "Wiser",
"given_name": "Lindsey S.",
"orcid": "0000-0002-3295-1279"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Dyrek",
"given_name": "Achr\u00e8ne",
"orcid": "0000-0001-7189-6463"
},
{
"family_name": "Triantafillides",
"given_name": "Anastasia"
}
],
"abstract": "Interactions between exoplanetary atmospheres and internal properties have long been proposed to be drivers of the inflation mechanisms of gaseous planets and apparent atmospheric chemical disequilibrium conditions1. However, transmission spectra of exoplanets have been limited in their ability to observationally confirm these theories owing to the limited wavelength coverage of the Hubble Space Telescope (HST) and inferences of single molecules, mostly H2O (ref.\u20092). In this work, we present the panchromatic transmission spectrum of the approximately 750\u00a0K, low-density, Neptune-sized exoplanet WASP-107b using a combination of HST Wide Field Camera 3 (WFC3) and JWST Near-Infrared Camera (NIRCam) and Mid-Infrared Instrument (MIRI). From this spectrum, we detect spectroscopic features resulting from H2O (21\u03c3), CH4 (5\u03c3), CO (7\u03c3), CO2 (29\u03c3), SO2 (9\u03c3) and NH3 (6\u03c3). The presence of these molecules enables constraints on the atmospheric metal enrichment (M/H is 10\u201318\u00d7 solar3), vertical mixing strength (log10Kzz\u2009=\u20098.4\u20139.0\u2009cm2\u2009s\u22121) and internal temperature (>345\u2009K). The high internal temperature is suggestive of tidally driven inflation4 acting on a Neptune-like internal structure, which can naturally explain the large radius and low density of the planet. These findings suggest that eccentricity-driven tidal heating is a critical process governing atmospheric chemistry and interior-structure inferences for most of the cool (<1,000\u2009K) super-Earth-to-Saturn-mass exoplanet population.",
"doi": "10.1038/s41586-024-07514-w",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2024-05-20",
"series_number": "8018",
"volume": "630",
"issue": "8018",
"pages": "836-840"
},
{
"id": "authors:a1egy-66m40",
"collection": "authors",
"collection_id": "a1egy-66m40",
"cite_using_url": "https://authors.library.caltech.edu/records/a1egy-66m40",
"type": "article",
"title": "JWST/NIRCam Detection of the Fomalhaut C Debris Disk in Scattered Light",
"author": [
{
"family_name": "Lawson",
"given_name": "Kellen",
"orcid": "0000-0002-6964-8732",
"clpid": "Lawson-Kellen"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062",
"clpid": "Schlieder-Joshua-E"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140",
"clpid": "Leisenring-Jarron-M"
},
{
"family_name": "Bogat",
"given_name": "Ell",
"orcid": "0000-0002-7325-5990",
"clpid": "Bogat-Ell"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Bryden",
"given_name": "Geoffrey",
"orcid": "0000-0001-5966-837X",
"clpid": "Bryden-Geoffrey"
},
{
"family_name": "G\u00e1sp\u00e1r",
"given_name": "Andr\u00e1s",
"orcid": "0000-0001-8612-3236",
"clpid": "G\u00e1sp\u00e1r-Andr\u00e1s"
},
{
"family_name": "Groff",
"given_name": "Tyler D.",
"orcid": "0000-0001-5978-3247",
"clpid": "Groff-Tyler-D"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956",
"clpid": "McElwain-Michael-W"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084",
"clpid": "Meyer-Michael-R"
},
{
"family_name": "Barclay",
"given_name": "Thomas",
"orcid": "0000-0001-7139-2724",
"clpid": "Barclay-Thomas"
},
{
"family_name": "Calissendorff",
"given_name": "Per",
"orcid": "0000-0002-5335-0616",
"clpid": "Calissendorff-Per"
},
{
"family_name": "De Furio",
"given_name": "Matthew",
"orcid": "0000-0003-1863-4960",
"clpid": "De-Furio-Matthew"
},
{
"family_name": "Li",
"given_name": "Yiting",
"orcid": "0000-0002-6845-9702",
"clpid": "Li-Yiting"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170",
"clpid": "Rieke-Marcia-J"
},
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Girard",
"given_name": "Julien H.",
"orcid": "0000-0001-8627-0404",
"clpid": "Girard-Julien-H"
},
{
"family_name": "Gennaro",
"given_name": "Mario",
"orcid": "0000-0002-5581-2896",
"clpid": "Gennaro-Mario"
},
{
"family_name": "Kammerer",
"given_name": "Jens",
"orcid": "0000-0003-2769-0438",
"clpid": "Kammerer-Jens"
},
{
"family_name": "Rest",
"given_name": "Armin",
"orcid": "0000-0002-4410-5387",
"clpid": "Rest-Armin"
},
{
"family_name": "Roellig",
"given_name": "Thomas L.",
"orcid": "0000-0002-6730-5410",
"clpid": "Roellig-Thomas-L"
},
{
"family_name": "Sunnquist",
"given_name": "Ben",
"orcid": "0000-0003-3759-8707",
"clpid": "Sunnquist-Ben"
}
],
"abstract": "Observations of debris disks offer important insights into the formation and evolution of planetary systems. Though M dwarfs make up approximately 80% of nearby stars, very few M dwarf debris disks have been studied in detail—making it unclear how or if the information gleaned from studying debris disks around more massive stars extends to the more abundant M dwarf systems. We report the first scattered-light detection of the debris disk around the M4 star Fomalhaut C using JWST's Near Infrared Camera (NIRCam; 3.6 and 4.4 μm). This result adds to the prior sample of only four M dwarf debris disks with detections in scattered light and marks the latest spectral type and oldest star among them. The size and orientation of the disk in these data are generally consistent with the prior Atacama Large Millimeter/submillimeter Array submillimeter detection. Though no companions are identified, these data provide strong constraints on their presence—with sensitivity sufficient to recover sub-Saturn mass objects in the vicinity of the disk. This result illustrates the unique capability of JWST to uncover elusive M dwarf debris disks in scattered light and lays the groundwork for deeper studies of such objects in the 2–5 μm regime.
",
"doi": "10.3847/2041-8213/ad4496",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2024-05-20",
"series_number": "1",
"volume": "967",
"issue": "1",
"pages": "L8"
},
{
"id": "authors:abs1s-q5e65",
"collection": "authors",
"collection_id": "abs1s-q5e65",
"cite_using_url": "https://authors.library.caltech.edu/records/abs1s-q5e65",
"type": "article",
"title": "New Insights on the Accretion Properties of Class 0 Protostars from 2 \u03bcm Spectroscopy",
"author": [
{
"family_name": "Le Gouellec",
"given_name": "Valentin J. M.",
"orcid": "0000-0002-5714-799X",
"clpid": "Le-Gouellec-Valentin-J-M"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hillenbrand",
"given_name": "Lynne A.",
"clpid": "Hillenbrand-L-A"
},
{
"family_name": "Yates",
"given_name": "Zoe",
"clpid": "Yates-Zoe"
}
],
"abstract": "\n
Sun-like stars are thought to accrete most of their final mass during the protostellar phase, during which the stellar embryo is surrounded by an infalling dense envelope. We present an analysis of 26 K-band spectra of Class 0 protostars, which are the youngest protostars. Of these, 18 are new observations made with the Keck MOSFIRE instrument. H i Brγ, several H2, and CO Δv = 2 features are detected and analyzed. We detect Brγ emission in 62%, CO overtone emission in 50%, and H2 emission in 90% of sources. The H i and CO emission is associated with accretion, while the H2 lines are consistent with shock excitation indicating jets/outflows. Six objects exhibit photospheric absorption features, with almost no outflow activity and no detection of the accretion-related Brγ emission line. Comparing these results with an archival sample of Class I K-band spectra, we find that the CO and Brγ emission lines are systematically more luminous in Class 0s, suggesting that the accretion is on average more vigorous in the Class 0 phase. Typically associated with the heated inner accretion disk, the much higher detection rate of CO overtone emission in Class 0s indicates also that episodes of high accretion activity are more frequent in Class 0 systems. The kinematics of the Class 0 CO overtone emission suggest either an accretion-heated inner disk or material directly infalling onto the central region. This could point toward an accretion mechanism of different nature in Class 0 systems than the typical picture of magnetospheric accretion.
\n
\n
The launch of the James Webb Space Telescope (JWST) marks a pivotal moment for precise atmospheric characterization of Y dwarfs, the coldest brown dwarf spectral type. In this study, we leverage moderate spectral resolution observations (R ∼ 2700) with the G395H grating of the Near-Infrared Spectrograph (NIRSpec) on board JWST to characterize the nearby (9.9 pc) Y dwarf WISEPA J182831.08+265037.8. With the NIRSpec G395H 2.88–5.12 μm spectrum, we measure the abundances of CO, CO2, CH4, H2S, NH3, and H2O, which are the major carbon-, nitrogen-, oxygen-, and sulfur-bearing species in the atmosphere. Based on the retrieved volume mixing ratios with the atmospheric retrieval framework CHIMERA, we report that the C/O ratio is 0.45 ± 0.01, close to the solar C/O value of 0.458, and the metallicity is +0.30 ± 0.02 dex. Comparison between the retrieval results and the forward modeling results suggests that the model bias for C/O and metallicity could be as high as 0.03 and 0.97 dex, respectively. We also report a lower limit of the 12CO/13CO ratio of >40, being consistent with the nominal solar value of 90. Our results highlight the potential for JWST to measure the C/O ratios down to percent-level precision and characterize isotopologues of cold planetary atmospheres similar to WISE 1828.
\n
MWC 758 is a young star hosting a spiral protoplanetary disk. The spirals are likely companion-driven, and two previously identified candidate companions have been identified\u2014one at the end the Southern spiral arm at \u223c0.\u20336, and one interior to the gap at \u223c0.\u20331. With JWST/NIRCam, we provide new images of the disk and constraints on planets exterior to \u223c1\u2033. We detect the two-armed spiral disk, a known background star, and a spatially resolved background galaxy, but no clear companions. The candidates that have been reported are at separations that are not probed by our data with sensitivity sufficient to detect them\u2212nevertheless, these observations place new limits on companions down to \u223c2 MJup at \u223c150 au and \u223c0.5 MJup at \u2273600 au. Owing to the unprecedented sensitivity of JWST and youth of the target, these are among the deepest mass-detection limits yet obtained through direct imaging observations, and provide new insights into the system's dynamical nature.
",
"doi": "10.3847/1538-3881/ad11d5",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-03-27",
"series_number": "4",
"volume": "167",
"issue": "4",
"pages": "181"
},
{
"id": "authors:nkwev-f1h35",
"collection": "authors",
"collection_id": "nkwev-f1h35",
"cite_using_url": "https://authors.library.caltech.edu/records/nkwev-f1h35",
"type": "article",
"title": "JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462",
"author": [
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Wagner",
"given_name": "Kevin R.",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Mullin",
"given_name": "Camryn",
"orcid": "0009-0007-3210-4356"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Boyer",
"given_name": "Martha",
"orcid": "0000-0003-4850-9589"
},
{
"family_name": "Horner",
"given_name": "Scott",
"orcid": "0000-0001-9886-6934"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Kelly",
"given_name": "Doug"
},
{
"family_name": "McCarthy",
"given_name": "Don"
},
{
"family_name": "Roellig",
"given_name": "Thomas",
"orcid": "0000-0002-6730-5410"
},
{
"family_name": "Rieke",
"given_name": "George",
"orcid": "0000-0003-2303-6519"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
},
{
"family_name": "Stansberry",
"given_name": "John",
"orcid": "0000-0003-2434-5225"
},
{
"family_name": "Young",
"given_name": "Erick",
"orcid": "0000-0002-6395-4296"
}
],
"abstract": "We present JWST/NIRCam F187N, F200W, F405N, and F410M direct imaging data of the disk surrounding SAO 206462. Previous images show a very structured disk, with a pair of spiral arms thought to be launched by one or more external perturbers. The spiral features are visible in three of the four filters, with the nondetection in F410M due to the large detector saturation radius. We detect with a signal-to-noise ratio of 4.4 a companion candidate that, if on a coplanar circular orbit, would orbit SAO 206462 at a separation of \u223c300 au, 2.25\u03c3 away from the predicted separation for the driver of the eastern spiral. No other companion candidates were detected. At the location predicted by simulations of both spirals generated by a single massive companion, the NIRCam data exclude objects more massive than \u223c2.2 MJ assuming the BEX evolutionary models. In terms of temperatures, the data are sensitive to objects with Teff \u223c 650\u2013850 K, when assuming planets emit like blackbodies (Rp between 1 and 3RJ). From these results, we conclude that if the spirals are driven by gas giants, these must be either cold or embedded in circumplanetary material. In addition, the NIRCam data provide tight constraints on ongoing accretion processes. In the low extinction scenario we are sensitive to mass accretion rates of the order \\(M^{\u0307}\\sim 10^{-9}M_{\\mathrm{J}}\\) yr\u22121. Thanks to the longer wavelengths used to search for emission lines, we reach unprecedented sensitivities to processes with \\(M^{\u0307}\\sim 10^{-7}M_{\\mathrm{J}}\\) yr\u22121 even toward highly extincted environments (AV \u2248 50 mag).
",
"doi": "10.3847/1538-3881/ad1ffc",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-03-27",
"series_number": "4",
"volume": "167",
"issue": "4",
"pages": "182"
},
{
"id": "authors:pk0s9-27y27",
"collection": "authors",
"collection_id": "pk0s9-27y27",
"cite_using_url": "https://authors.library.caltech.edu/records/pk0s9-27y27",
"type": "article",
"title": "JWST/NIRCam Imaging of Young Stellar Objects. III. Detailed Imaging of the Nebular Environment around the HL Tau Disk",
"author": [
{
"family_name": "Mullin",
"given_name": "Camryn",
"orcid": "0009-0007-3210-4356"
},
{
"family_name": "Dong",
"given_name": "Ruobing",
"orcid": "0000-0001-9290-7846"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Cugno",
"given_name": "Gabriele",
"orcid": "0000-0001-7255-3251"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Wagner",
"given_name": "Kevin R.",
"orcid": "0000-0002-4309-6343"
},
{
"family_name": "Wolff",
"given_name": "Schuyler G.",
"orcid": "0000-0002-9977-8255"
},
{
"family_name": "Boyer",
"given_name": "Martha",
"orcid": "0000-0003-4850-9589"
},
{
"family_name": "Horner",
"given_name": "Scott",
"orcid": "0000-0001-9886-6934"
},
{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "McCarthy",
"given_name": "Don"
},
{
"family_name": "Rieke",
"given_name": "George",
"orcid": "0000-0003-2303-6519"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
},
{
"family_name": "Young",
"given_name": "Erick",
"orcid": "0000-0002-6395-4296"
}
],
"abstract": "As part of the James Webb Space Telescope (JWST) Guaranteed Time Observation program \"Direct Imaging of YSOs\" (program ID 1179), we use JWST NIRCam's direct imaging mode in F187N, F200W, F405N, and F410M to perform high-contrast observations of the circumstellar structures surrounding the protostar HL Tau. The data reveal the known stellar envelope, outflow cavity, and streamers, but do not detect any companion candidates. We detect scattered light from an inflowing spiral streamer previously detected in HCO+ by the Atacama Large Millimeter/submillimeter Array, and part of the structure connected to the c-shaped outflow cavity. For detection limits in planet mass we use BEX evolutionary tracks when Mp < 2 MJ and AMES-COND evolutionary tracks otherwise, assuming a planet age of 1 Myr (youngest available age). Inside the disk region, due to extended envelope emission, our point-source sensitivities are \u223c5 mJy (37 MJ) at 40 au in F187N and \u223c0.37 mJy (5.2 MJ) at 140 au in F405N. Outside the disk region, the deepest limits we can reach are \u223c0.01 mJy (0.75 MJ) at a projected separation \u223c 525 au.
",
"doi": "10.3847/1538-3881/ad2de9",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-03-27",
"series_number": "4",
"volume": "167",
"issue": "4",
"pages": "183"
},
{
"id": "authors:nfvm5-0tp17",
"collection": "authors",
"collection_id": "nfvm5-0tp17",
"cite_using_url": "https://authors.library.caltech.edu/records/nfvm5-0tp17",
"type": "article",
"title": "The Outflow of The Protostar in B335. I.",
"author": [
{
"family_name": "Hodapp",
"given_name": "Klaus W.",
"orcid": "0000-0003-0786-2140"
},
{
"family_name": "Chu",
"given_name": "Laurie L."
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
},
{
"family_name": "Stansberry",
"given_name": "John",
"orcid": "0000-0003-2434-5225"
},
{
"family_name": "Boyer",
"given_name": "Martha",
"orcid": "0000-0003-4850-9589"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Horner",
"given_name": "Scott",
"orcid": "0000-0001-9886-6934"
},
{
"family_name": "Roellig",
"given_name": "Tom",
"orcid": "0000-0002-6730-5410"
},
{
"family_name": "Rieke",
"given_name": "George",
"orcid": "0000-0003-2303-6519"
},
{
"family_name": "Young",
"given_name": "Eric T.",
"orcid": "0000-0002-6395-4296"
}
],
"abstract": "The isolated globule B335 contains a single, low-luminosity Class 0 protostar associated with a bipolar nebula and outflow system seen nearly perpendicular to its axis. We observed the innermost regions of this outflow as part of JWST/NIRCam Guaranteed Time Observations program 1187, primarily intended for wide-field slitless spectroscopy of background stars behind the globule. We find a system of expanding shock fronts with kinematic ages of only a few decades emerging symmetrically from the position of the embedded protostar, which is not directly detected at NIRCam wavelengths. The innermost and youngest of the shock fronts studied here shows strong emission from CO. The next older shock front shows less CO and the third shock front shows only H2 emission in our data. This third and most distant of these inner shock fronts shows substantial evolution of its shape since it was last observed with high spatial resolution in 1996 with Keck/NIRC. This may be evidence of a faster internal shock catching up with a slower one and of the two shocks merging.
",
"doi": "10.3847/1538-3881/ad1b55",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2024-02-12",
"series_number": "3",
"volume": "167",
"issue": "3",
"pages": "102"
},
{
"id": "authors:yw0yj-efb51",
"collection": "authors",
"collection_id": "yw0yj-efb51",
"cite_using_url": "https://authors.library.caltech.edu/records/yw0yj-efb51",
"type": "article",
"title": "Clouds and Clarity: Revisiting Atmospheric Feature Trends in Neptune-size Exoplanets",
"author": [
{
"family_name": "Brande",
"given_name": "Jonathan",
"orcid": "0000-0002-2072-6541",
"clpid": "Brande-Jonathan"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-Ian-J-M"
},
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147",
"clpid": "Kreidberg-Laura"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456",
"clpid": "Morley-Caroline-V"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002",
"clpid": "Barman-Travis"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498",
"clpid": "Benneke-Bj\u00f6rn"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X",
"clpid": "Dragomir-Diana"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-Jonathan-J"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hardegree-Ullman",
"given_name": "Kevin K.",
"orcid": "0000-0003-3702-0382",
"clpid": "Hardegree-Ullman-Kevin-K"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Lothringer",
"given_name": "Joshua D.",
"orcid": "0000-0003-3667-8633",
"clpid": "Lothringer-Joshua-D"
},
{
"family_name": "Mikal-Evans",
"given_name": "Thomas",
"orcid": "0000-0001-5442-1300",
"clpid": "Mikal-Evans-Thomas"
}
],
"abstract": "\n
Over the last decade, precise exoplanet transmission spectroscopy has revealed the atmospheres of dozens of exoplanets, driven largely by observatories like the Hubble Space Telescope. One major discovery has been the ubiquity of atmospheric aerosols, often blocking access to exoplanet chemical inventories. Tentative trends have been identified, showing that the clarity of planetary atmospheres may depend on equilibrium temperature. Previous work has often grouped dissimilar planets together in order to increase the statistical power of any trends, but it remains unclear from observed transmission spectra whether these planets exhibit the same atmospheric physics and chemistry. We present a reanalysis of a smaller, more physically similar sample of 15 exo-Neptune transmission spectra across a wide range of temperatures (200–1000 K). Using condensation cloud and hydrocarbon haze models, we find that the exo-Neptune population is best described by low cloud sedimentation efficiency (fsed ∼ 0.1) and high metallicity (100 × solar). There is an intrinsic scatter of ∼0.5 scale height, perhaps evidence of stochasticity in these planets' formation processes. Observers should expect significant attenuation in transmission spectra of Neptune-size exoplanets, up to 6 scale heights for equilibrium temperatures between 500 and 800 K. With JWST's greater wavelength sensitivity, colder (<500 K) planets should be high-priority targets given their clearer atmospheres, and the need to distinguish between the \"super-puffs\" and more typical gas-dominated planets.
\n
In parallel with the multi-messenger revolution, major advances in time-domain astronomy across multiple science disciplines relevant to astrophysics are becoming more urgent to address. Aside from electromagnetic observations of gravitational wave events and explosive counterparts, there are a number of \"classical\" astrophysical areas that require new thinking for proper exploration in the time domain. How NASA, NSF, ESA, and ESO consider the 2020 USA Decadal Survey within the astronomy community, as well as the worldwide call to support and expand time domain and multi-messenger astrophysics, it is crucial that all areas of astrophysics, including stellar, galactic, Solar System, and exoplanetary science participate in the discussion, and that it not be made into an exclusive preserve of cosmological, high-energy, explosive and transient science. Time domain astronomy is used to explore many aspects of astrophysics\u2013particularly concerning ground- and space-based mission science goals of exploring how the Universe works, understanding how did we get here, and are we alone. Time domain studies are already built into the core operations of many currently operating and future space telescopes (e.g., Roman, PLATO) as well as current and planned large areal ground-based surveys (e.g., Rubin). Time-domain observations designed for one scientific purpose, also lead to great discoveries in many other science areas. The recent advent of user-friendly hardware, software, observational approaches, and online data infrastructure has also helped make time domain observations especially suitable and appealing for citizen science projects. We provide a review of the current state of TDAMM alerts and observational protocols, revealing a wide array of software and applications, much of which is incompatible. Any conversation regarding TDAMM astrophysics should include all aspects of the field, including those aspects seen as classical applications.
",
"doi": "10.3389/fspas.2024.1304616",
"issn": "2296-987X",
"publisher": "Frontiers Media SA",
"publication": "Frontiers in Astronomy and Space Sciences",
"publication_date": "2024-01-15",
"volume": "11",
"pages": "1304616"
},
{
"id": "authors:ewxv5-mcs69",
"collection": "authors",
"collection_id": "ewxv5-mcs69",
"cite_using_url": "https://authors.library.caltech.edu/records/ewxv5-mcs69",
"type": "article",
"title": "Searching for Planets Orbiting Fomalhaut with JWST/NIRCam",
"author": [
{
"family_name": "Ygouf",
"given_name": "Marie",
"orcid": "0000-0001-7591-2731",
"clpid": "Ygouf-M"
},
{
"family_name": "Beichman",
"given_name": "Charles A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Llop-Sayson",
"given_name": "Jorge",
"orcid": "0000-0002-3414-784X",
"clpid": "Llop-Sayson-Jorge"
},
{
"family_name": "Bryden",
"given_name": "Geoffrey",
"orcid": "0000-0001-5966-837X",
"clpid": "Bryden-Geoffrey"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140",
"clpid": "LeisenringJarron-M"
},
{
"family_name": "G\u00e1sp\u00e1r",
"given_name": "Andr\u00e1s",
"orcid": "0000-0001-8612-3236",
"clpid": "G\u00e1sp\u00e1r-Andr\u00e1s"
},
{
"family_name": "Krist",
"given_name": "John E.",
"clpid": "Krist-John-E"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170",
"clpid": "Rieke-Marcia-J"
},
{
"family_name": "Rieke",
"given_name": "George H.",
"orcid": "0000-0003-2303-6519",
"clpid": "Rieke-George-H"
},
{
"family_name": "Wolff",
"given_name": "Schuyler Grace",
"orcid": "0000-0002-9977-8255",
"clpid": "Wolff-Schuyler-Grace"
},
{
"family_name": "Roellig",
"given_name": "Thomas L.",
"orcid": "0000-0002-6730-5410",
"clpid": "Roellig-Thomas-L"
},
{
"family_name": "Su",
"given_name": "Kate",
"orcid": "0000-0002-3532-5580",
"clpid": "Su-Kate"
},
{
"family_name": "Hainline",
"given_name": "Kevin N.",
"orcid": "0000-0003-4565-8239",
"clpid": "Hainline-Kevin-N"
},
{
"family_name": "Hodapp",
"given_name": "Klaus W.",
"orcid": "0000-0003-0786-2140",
"clpid": "Hodapp-Klaus-W"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084",
"clpid": "Meyer-Michael-R"
},
{
"family_name": "Kelly",
"given_name": "Douglas M.",
"clpid": "Kelly-Douglas-M"
},
{
"family_name": "Misselt",
"given_name": "Karl",
"clpid": "Misselt-Karl"
},
{
"family_name": "Stansberry",
"given_name": "John",
"orcid": "0000-0003-2434-5225",
"clpid": "Stansberry-John"
},
{
"family_name": "Boyer",
"given_name": "Martha",
"orcid": "0000-0003-4850-9589",
"clpid": "Boyer-Martha"
},
{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X",
"clpid": "Johnstone-Doug"
},
{
"family_name": "Horner",
"given_name": "Scott",
"orcid": "0000-0001-9886-6934",
"clpid": "Horner-Scott"
},
{
"family_name": "Greenbaum",
"given_name": "Alexandra Z.",
"orcid": "0000-0002-7162-8036",
"clpid": "Greenbaum-Alexandra-Z"
}
],
"abstract": "\n
We report observations with the JWST/NIRCam coronagraph of the Fomalhaut (α PsA) system. This nearby A star hosts a complex debris disk system discovered by the IRAS satellite. Observations in F444W and F356W filters using the round 430R mask achieve a contrast ratio of ∼4 × 10−7 at 1'' and ∼4 × 10−8 outside of 3''. These observations reach a sensitivity limit of <1 MJup across most of the disk region. Consistent with the hypothesis that Fomalhaut b is not a massive planet but is a dust cloud from a planetesimal collision, we do not detect it in either F356W or F444W (the latter band where a Jovian-sized planet should be bright). We have reliably detected 10 sources in and around Fomalhaut and its debris disk, all but one of which are coincident with Keck or Hubble Space Telescope sources seen in earlier coronagraphic imaging; we show them to be background objects, including the \"Great Dust Cloud\" identified in Mid-Infrared Instrument (MIRI) data. However, one of the objects, located at the edge of the inner dust disk seen in the MIRI images, has no obvious counterpart in imaging at earlier epochs and has a relatively red [F356W]–[F444W] > 0.7 mag (Vega) color. Whether this object is a background galaxy, brown dwarf, or a Jovian-mass planet in the Fomalhaut system will be determined by an approved Cycle 2 follow-up program. Finally, we set upper limits to any scattered light from the outer ring, placing a weak limit on the dust albedo at F356W and F444W.
\n
High-contrast imaging of debris disk systems permits us to assess the composition and size distribution of circumstellar dust, to probe recent dynamical histories, and to directly detect and characterize embedded exoplanets. Observations of these systems in the infrared beyond 2–3 μm promise access to both extremely favorable planet contrasts and numerous scattered-light spectral features—but have typically been inhibited by the brightness of the sky at these wavelengths. We present coronagraphy of the AU Microscopii (AU Mic) system using JWST’s Near Infrared Camera (NIRCam) in two filters spanning 3–5 μm. These data provide the first images of the system’s famous debris disk at these wavelengths and permit additional constraints on its properties and morphology. Conducting a deep search for companions in these data, we do not identify any compelling candidates. However, with sensitivity sufficient to recover planets as small as ∼0.1 Jupiter masses beyond ∼2″ (∼20 au) with 5σ confidence, these data place significant constraints on any massive companions that might still remain at large separations and provide additional context for the compact, multiplanet system orbiting very close-in. The observations presented here highlight NIRCam’s unique capabilities for probing similar disks in this largely unexplored wavelength range, and they provide the deepest direct imaging constraints on wide-orbit giant planets in this very well-studied benchmark system.
",
"doi": "10.3847/1538-3881/aced08",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2023-10",
"series_number": "4",
"volume": "166",
"issue": "4",
"pages": "150"
},
{
"id": "authors:kvy62-v9a45",
"collection": "authors",
"collection_id": "kvy62-v9a45",
"cite_using_url": "https://authors.library.caltech.edu/records/kvy62-v9a45",
"type": "article",
"title": "Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d",
"author": [
{
"family_name": "Roy",
"given_name": "Pierre-Alexis",
"orcid": "0000-0001-6809-3520"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Piaulet",
"given_name": "Caroline",
"orcid": "0000-0002-2875-917X"
},
{
"family_name": "Gully-Santiago",
"given_name": "Michael A.",
"orcid": "0000-0002-4020-3457"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M."
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Mikal-Evans",
"given_name": "Thomas",
"orcid": "0000-0001-5442-1300"
},
{
"family_name": "Brande",
"given_name": "Jonathan",
"orcid": "0000-0002-2072-6541"
},
{
"family_name": "Delisle",
"given_name": "Simon",
"orcid": "0000-0002-4771-0312"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hardegree-Ullman",
"given_name": "Kevin K.",
"orcid": "0000-0003-3702-0382"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Kosiarek",
"given_name": "Molly R.",
"orcid": "0000-0002-6115-4359"
},
{
"family_name": "Lothringer",
"given_name": "Joshua D.",
"orcid": "0000-0003-3667-8633"
}
],
"abstract": "\n
Recent work on the characterization of small exoplanets has allowed us to accumulate growing evidence that sub-Neptunes with radii greater than ∼2.5 R⊕ often host H2/He-dominated atmospheres both from measurements of their low bulk densities and from direct detections of their low mean molecular mass atmospheres. However, the smaller sub-Neptunes in the 1.5–2.2 R⊕ size regime are much less understood and often have bulk densities that can be explained either by the H2/He-rich scenario or by a volatile-dominated composition known as the \"water world\" scenario. Here we report the detection of water vapor in the transmission spectrum of the 1.96 ± 0.08 R⊕ sub-Neptune GJ 9827 d obtained with the Hubble Space Telescope (HST). We observe 11 HST Wide Field Camera 3 transits of GJ 9827 d and find an absorption feature at 1.4 μm in its transit spectrum, which is best explained (at 3.39σ) by the presence of water in GJ 9827 d's atmosphere. We further show that this feature cannot be caused by unocculted starspots during the transits by combining an analysis of the K2 photometry and transit light source effect retrievals. We reveal that the water absorption feature can be similarly well explained by a small amount of water vapor in a cloudy H2/He atmosphere or a water vapor envelope on GJ 9827 d. Given that recent studies have inferred an important mass-loss rate (>0.5 M⊕ Gyr−1) for GJ 9827 d, making it unlikely to retain a H-dominated envelope, our findings highlight GJ 9827 d as a promising water world candidate that could host a volatile-dominated atmosphere. This water detection also makes GJ 9827 d the smallest exoplanet with an atmospheric molecular detection to date.
\n
We present a sample of four emission-line galaxies at z = 6.11\u20136.35 that were serendipitously discovered using the commissioning data for the James Webb Space Telescope (JWST)/NIRCam wide-field slitless spectroscopy mode. One of them (at z = 6.11) has been reported previously, while the others are new discoveries. These sources are selected by the secure detections of both [O iii] \u03bb5007 and H\u03b1 lines with other fainter lines, which were tentatively detected in some cases (e.g., [O ii] \u03bb3727, [O iii] \u03bb4959). In the [O iii]/H\u03b2\u2013[N ii]/H\u03b1 Baldwin\u2013Phillips\u2013Terlevich diagram, these galaxies occupy the same parameter space as that of z \u223c 2 star-forming galaxies, indicating that they have been enriched rapidly to subsolar metallicities (\u223c0.4 Z\u2299), similar to galaxies with comparable stellar masses at much lower redshifts. The detection of strong H\u03b1 lines suggests a higher ionizing photon production efficiency within galaxies in the early universe. We find brightening of the [O iii] \u03bb5007 line-luminosity function (LF) from z = 3 to 6, and weak or no redshift evolution of the H\u03b1 line LF from z = 2 to 6. Both LFs are underpredicted at z \u223c 6 by a factor of \u223c10 in certain cosmological simulations. This further indicates a global Ly\u03b1 photon escape fraction of 7%\u201310% at z \u223c 6, which is slightly lower than previous estimates through the comparison of the UV-derived star formation rate density and Ly\u03b1 luminosity density. Our sample recovers \\(66_{-44}^{+128}\\) % of z = 6.0\u20136.6 galaxies in the survey volume with stellar masses greater than 5 \u00d7 108M\u2299, suggesting the ubiquity of strong H\u03b1 and [O iii] line emitters in the Epoch of Reionization, which will be further uncovered in the era of JWST.
",
"doi": "10.3847/1538-4357/acd53c",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2023-08-01",
"series_number": "1",
"volume": "953",
"issue": "1",
"pages": "53"
},
{
"id": "authors:zdhk0-a4j58",
"collection": "authors",
"collection_id": "zdhk0-a4j58",
"cite_using_url": "https://authors.library.caltech.edu/records/zdhk0-a4j58",
"type": "article",
"title": "The James Webb Space Telescope Mission",
"author": [
{
"family_name": "Gardner",
"given_name": "Jonathan P.",
"orcid": "0000-0003-2098-9568"
},
{
"family_name": "Mather",
"given_name": "John C.",
"orcid": "0000-0002-6460-0078"
},
{
"family_name": "Abbott",
"given_name": "Randy"
},
{
"family_name": "Abell",
"given_name": "James S."
},
{
"family_name": "Abernathy",
"given_name": "Mark"
},
{
"family_name": "Abney",
"given_name": "Faith E."
},
{
"family_name": "Abraham",
"given_name": "John G.",
"orcid": "0000-0001-6559-6616"
},
{
"family_name": "Abraham",
"given_name": "Roberto",
"orcid": "0000-0002-4542-921X"
},
{
"family_name": "Abul-Huda",
"given_name": "Yasin M.",
"orcid": "0000-0001-5625-4091"
},
{
"family_name": "Acton",
"given_name": "Scott"
},
{
"family_name": "Adams",
"given_name": "Cynthia K."
},
{
"family_name": "Adams",
"given_name": "Evan",
"orcid": "0000-0001-5490-2518"
},
{
"family_name": "Adler",
"given_name": "David S."
},
{
"family_name": "Adriaensen",
"given_name": "Maarten",
"orcid": "0000-0003-0026-3129"
},
{
"family_name": "Aguilar",
"given_name": "Jonathan Albert",
"orcid": "0000-0003-3184-0873"
},
{
"family_name": "Ahmed",
"given_name": "Mansoor"
},
{
"family_name": "Ahmed",
"given_name": "Nasif S."
},
{
"family_name": "Ahmed",
"given_name": "Tanjira"
},
{
"family_name": "Albat",
"given_name": "R\u00fcdeger"
},
{
"family_name": "Albert",
"given_name": "Lo\u00efc",
"orcid": "0000-0003-0475-9375"
},
{
"family_name": "Alberts",
"given_name": "Stacey",
"orcid": "0000-0002-8909-8782"
},
{
"family_name": "Aldridge",
"given_name": "David"
},
{
"family_name": "Allen",
"given_name": "Mary Marsha"
},
{
"family_name": "Allen",
"given_name": "Shaune S."
},
{
"family_name": "Altenburg",
"given_name": "Martin"
},
{
"family_name": "Altunc",
"given_name": "Serhat"
},
{
"family_name": "Alvarez",
"given_name": "Jose Lorenzo",
"orcid": "0000-0002-6845-993X"
},
{
"family_name": "\u00c1lvarez-M\u00e1rquez",
"given_name": "Javier",
"orcid": "0000-0002-7093-1877"
},
{
"family_name": "de Oliveira",
"given_name": "Catarina Alves",
"orcid": "0000-0003-2896-4138"
},
{
"family_name": "Ambrose",
"given_name": "Leslie L."
},
{
"family_name": "Anandakrishnan",
"given_name": "Satya M."
},
{
"family_name": "Andersen",
"given_name": "Gregory C."
},
{
"family_name": "Anderson",
"given_name": "Harry James"
},
{
"family_name": "Anderson",
"given_name": "Jay",
"orcid": "0000-0003-2861-3995"
},
{
"family_name": "Anderson",
"given_name": "Kristen"
},
{
"family_name": "Anderson",
"given_name": "Sara M."
},
{
"family_name": "Aprea",
"given_name": "Julio",
"orcid": "0000-0002-6313-8782"
},
{
"family_name": "Archer",
"given_name": "Benita J."
},
{
"family_name": "Arenberg",
"given_name": "Jonathan W.",
"orcid": "0000-0003-1096-5634"
},
{
"family_name": "Argyriou",
"given_name": "Ioannis",
"orcid": "0000-0003-2820-1077"
},
{
"family_name": "Arribas",
"given_name": "Santiago",
"orcid": "0000-0001-7997-1640"
},
{
"family_name": "Artigau",
"given_name": "\u00c9tienne",
"orcid": "0000-0003-3506-5667"
},
{
"family_name": "Arvai",
"given_name": "Amanda Rose"
},
{
"family_name": "Atcheson",
"given_name": "Paul"
},
{
"family_name": "Atkinson",
"given_name": "Charles B."
},
{
"family_name": "Averbukh",
"given_name": "Jesse",
"orcid": "0000-0002-0041-0363"
},
{
"family_name": "Aymergen",
"given_name": "Cagatay"
},
{
"family_name": "Bacinski",
"given_name": "John J."
},
{
"family_name": "Baggett",
"given_name": "Wayne E."
},
{
"family_name": "Bagnasco",
"given_name": "Giorgio"
},
{
"family_name": "Baker",
"given_name": "Lynn L."
},
{
"family_name": "Balzano",
"given_name": "Vicki Ann"
},
{
"family_name": "Banks",
"given_name": "Kimberly A."
},
{
"family_name": "Baran",
"given_name": "David A.",
"orcid": "0000-0002-1212-4276"
},
{
"family_name": "Barker",
"given_name": "Elizabeth A."
},
{
"family_name": "Barrett",
"given_name": "Larry K."
},
{
"family_name": "Barringer",
"given_name": "Bruce O."
},
{
"family_name": "Barto",
"given_name": "Allison",
"orcid": "0000-0003-0604-8673"
},
{
"family_name": "Bast",
"given_name": "William"
},
{
"family_name": "Baudoz",
"given_name": "Pierre",
"orcid": "0000-0002-2711-7116"
},
{
"family_name": "Baum",
"given_name": "Stefi",
"orcid": "0000-0002-4735-8224"
},
{
"family_name": "Beatty",
"given_name": "Thomas G.",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Beaulieu",
"given_name": "Mathilde"
},
{
"family_name": "Bechtold",
"given_name": "Kathryn",
"orcid": "0000-0002-7722-6900"
},
{
"family_name": "Beck",
"given_name": "Tracy",
"orcid": "0000-0002-6881-0574"
},
{
"family_name": "Beddard",
"given_name": "Megan M."
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Bellagama",
"given_name": "Larry"
},
{
"family_name": "Bely",
"given_name": "Pierre"
},
{
"family_name": "Berger",
"given_name": "Timothy W."
},
{
"family_name": "Bergeron",
"given_name": "Louis E."
},
{
"family_name": "Bernier",
"given_name": "Antoine-Darveau",
"orcid": "0000-0002-7786-0661"
},
{
"family_name": "Bertch",
"given_name": "Maria D."
},
{
"family_name": "Beskow",
"given_name": "Charlotte"
},
{
"family_name": "Betz",
"given_name": "Laura E."
},
{
"family_name": "Biagetti",
"given_name": "Carl P."
},
{
"family_name": "Birkmann",
"given_name": "Stephan",
"orcid": "0000-0001-7058-1726"
},
{
"family_name": "Bjorklund",
"given_name": "Kurt F."
},
{
"family_name": "Blackwood",
"given_name": "James D."
},
{
"family_name": "Blazek",
"given_name": "Ronald Paul"
},
{
"family_name": "Blossfeld",
"given_name": "Stephen"
},
{
"family_name": "Bluth",
"given_name": "Marcel"
},
{
"family_name": "Boccaletti",
"given_name": "Anthony",
"orcid": "0000-0001-9353-2724"
},
{
"family_name": "Boegner Jr",
"given_name": "Martin E."
},
{
"family_name": "Bohlin",
"given_name": "Ralph C.",
"orcid": "0000-0001-9806-0551"
},
{
"family_name": "Boia",
"given_name": "John Joseph"
},
{
"family_name": "B\u00f6ker",
"given_name": "Torsten",
"orcid": "0000-0002-5666-7782"
},
{
"family_name": "Bonaventura",
"given_name": "N.",
"orcid": "0000-0001-8470-7094"
},
{
"family_name": "Bond",
"given_name": "Nicholas A."
},
{
"family_name": "Bosley",
"given_name": "Kari Ann"
},
{
"family_name": "Boucarut",
"given_name": "Rene A."
},
{
"family_name": "Bouchet",
"given_name": "Patrice",
"orcid": "0000-0002-6018-3393"
},
{
"family_name": "Bouwman",
"given_name": "Jeroen",
"orcid": "0000-0003-4757-2500"
},
{
"family_name": "Bower",
"given_name": "Gary"
},
{
"family_name": "Bowers",
"given_name": "Ariel S."
},
{
"family_name": "Bowers",
"given_name": "Charles W."
},
{
"family_name": "Boyce",
"given_name": "Leslye A."
},
{
"family_name": "Boyer",
"given_name": "Christine T."
},
{
"family_name": "Boyer",
"given_name": "Martha L.",
"orcid": "0000-0003-4850-9589"
},
{
"family_name": "Boyer",
"given_name": "Michael"
},
{
"family_name": "Boyer",
"given_name": "Robert"
},
{
"family_name": "Bradley",
"given_name": "Larry D.",
"orcid": "0000-0002-7908-9284"
},
{
"family_name": "Brady",
"given_name": "Gregory R.",
"orcid": "0000-0003-3249-2436"
},
{
"family_name": "Brandl",
"given_name": "Bernhard R.",
"orcid": "0000-0001-9737-169X"
},
{
"family_name": "Brannen",
"given_name": "Judith L."
},
{
"family_name": "Breda",
"given_name": "David"
},
{
"family_name": "Bremmer",
"given_name": "Harold G."
},
{
"family_name": "Brennan",
"given_name": "David"
},
{
"family_name": "Bresnahan",
"given_name": "Pamela A."
},
{
"family_name": "Bright",
"given_name": "Stacey N.",
"orcid": "0000-0001-7951-7966"
},
{
"family_name": "Broiles",
"given_name": "Brian J."
},
{
"family_name": "Bromenschenkel",
"given_name": "Asa"
},
{
"family_name": "Brooks",
"given_name": "Brian H."
},
{
"family_name": "Brooks",
"given_name": "Keira J.",
"orcid": "0000-0002-2780-9593"
},
{
"family_name": "Brown",
"given_name": "Bob"
},
{
"family_name": "Brown",
"given_name": "Bruce"
},
{
"family_name": "Brown",
"given_name": "Thomas M.",
"orcid": "0000-0002-1793-9968"
},
{
"family_name": "Bruce",
"given_name": "Barry W."
},
{
"family_name": "Bryson",
"given_name": "Jonathan G."
},
{
"family_name": "Bujanda",
"given_name": "Edwin D."
},
{
"family_name": "Bullock",
"given_name": "Blake M."
},
{
"family_name": "Bunker",
"given_name": "A. J.",
"orcid": "0000-0002-8651-9879"
},
{
"family_name": "Bureo",
"given_name": "Rafael"
},
{
"family_name": "Burt",
"given_name": "Irving J."
},
{
"family_name": "Bush",
"given_name": "James Aaron"
},
{
"family_name": "Bushouse",
"given_name": "Howard A.",
"orcid": "0000-0001-6664-7585"
},
{
"family_name": "Bussman",
"given_name": "Marie C."
},
{
"family_name": "Cabaud",
"given_name": "Olivier"
},
{
"family_name": "Cale",
"given_name": "Steven"
},
{
"family_name": "Calhoon",
"given_name": "Charles D."
},
{
"family_name": "Calvani",
"given_name": "Humberto"
},
{
"family_name": "Canipe",
"given_name": "Alicia M.",
"orcid": "0009-0002-6366-0957"
},
{
"family_name": "Caputo",
"given_name": "Francis M."
},
{
"family_name": "Cara",
"given_name": "Mihai",
"orcid": "0000-0002-9294-6551"
},
{
"family_name": "Carey",
"given_name": "Larkin"
},
{
"family_name": "Case",
"given_name": "Michael Eli"
},
{
"family_name": "Cesari",
"given_name": "Thaddeus"
},
{
"family_name": "Cetorelli",
"given_name": "Lee D."
},
{
"family_name": "Chance",
"given_name": "Don R."
},
{
"family_name": "Chandler",
"given_name": "Lynn"
},
{
"family_name": "Chaney",
"given_name": "Dave"
},
{
"family_name": "Chapman",
"given_name": "George N."
},
{
"family_name": "Charlot",
"given_name": "S.",
"orcid": "0000-0003-3458-2275"
},
{
"family_name": "Chayer",
"given_name": "Pierre",
"orcid": "0000-0001-7653-0882"
},
{
"family_name": "Cheezum",
"given_name": "Jeffrey I."
},
{
"family_name": "Chen",
"given_name": "Bin"
},
{
"family_name": "Chen",
"given_name": "Christine H.",
"orcid": "0000-0002-8382-0447"
},
{
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"given_name": "Gene"
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"family_name": "Yu",
"given_name": "Susan"
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"family_name": "Zak",
"given_name": "Dean S."
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"given_name": "Christian A."
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],
"abstract": "Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least 4 m. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the 6.5 m James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 yr, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit.
",
"doi": "10.1088/1538-3873/acd1b5",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-06-01",
"series_number": "1048",
"volume": "135",
"issue": "1048",
"pages": "068001"
},
{
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"collection_id": "a9tfe-39v09",
"cite_using_url": "https://authors.library.caltech.edu/records/a9tfe-39v09",
"type": "article",
"title": "The Science Performance of JWST as Characterized in Commissioning",
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"family_name": "Truong",
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{
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{
"family_name": "Tyra",
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"family_name": "Ubeda",
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{
"family_name": "Wolff",
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{
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{
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"family_name": "Yeager",
"given_name": "Christopher"
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{
"family_name": "Yeates",
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{
"family_name": "Yerger",
"given_name": "Ethan"
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{
"family_name": "Yoon",
"given_name": "Jinmi",
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"family_name": "Young",
"given_name": "Alice"
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{
"family_name": "Yu",
"given_name": "Susan"
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{
"family_name": "Zak",
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"family_name": "Zeidler",
"given_name": "Peter",
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{
"family_name": "Zhou",
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{
"family_name": "Zincke",
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"abstract": "This paper characterizes the actual science performance of the James Webb Space Telescope (JWST), as determined from the six month commissioning period. We summarize the performance of the spacecraft, telescope, science instruments, and ground system, with an emphasis on differences from pre-launch expectations. Commissioning has made clear that JWST is fully capable of achieving the discoveries for which it was built. Moreover, almost across the board, the science performance of JWST is better than expected; in most cases, JWST will go deeper faster than expected. The telescope and instrument suite have demonstrated the sensitivity, stability, image quality, and spectral range that are necessary to transform our understanding of the cosmos through observations spanning from near-earth asteroids to the most distant galaxies.
",
"doi": "10.1088/1538-3873/acb293",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-04-01",
"series_number": "1046",
"volume": "135",
"issue": "1046",
"pages": "048001"
},
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"type": "article",
"title": "The Mid-infrared Instrument for JWST and Its In-flight Performance",
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{
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{
"family_name": "Aguilar",
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{
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{
"family_name": "Brandl",
"given_name": "Bernard R.",
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"family_name": "Bright",
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"given_name": "Adrian Michael",
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{
"family_name": "Gordon",
"given_name": "Karl D.",
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"given_name": "Beth A.",
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{
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{
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"given_name": "G. C.",
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"orcid": "0009-0001-8954-7138"
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{
"family_name": "Temim",
"given_name": "Tea",
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{
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"orcid": "0009-0003-6128-2347"
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{
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"orcid": "0009-0005-3498-8808"
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{
"family_name": "van Dishoeck",
"given_name": "Ewine F.",
"orcid": "0000-0001-7591-1907"
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{
"family_name": "Vandenbussche",
"given_name": "Bart",
"orcid": "0000-0002-1368-3109"
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{
"family_name": "Weilert",
"given_name": "Mark"
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{
"family_name": "Whitehouse",
"given_name": "Paul"
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{
"family_name": "Wolff",
"given_name": "Schuyler",
"orcid": "0000-0002-9977-8255"
}
],
"abstract": "The Mid-Infrared Instrument (MIRI) extends the reach of the James Webb Space Telescope (JWST) to 28.5\u03bcm. It provides subarcsecond-resolution imaging, high sensitivity coronagraphy, and spectroscopy at resolutions of\u03bb/\u0394\u03bb\u223c 100\u20133500, with the high-resolution mode employing an integral field unit to provide spatial data cubes. The resulting broad suite of capabilities will enable huge advances in studies over this wavelength range. This overview describes the history of acquiring this capability for JWST. It discusses the basic attributes of the instrument optics, the detector arrays, and the cryocooler that keeps everything at approximately 7 K. It gives a short description of the data pipeline and of the instrument performance demonstrated during JWST commissioning. The bottom line is that the telescope and MIRI are both operating to the standards set by pre-launch predictions, and all of the MIRI capabilities are operating at, or even a bit better than, the level that had been expected. The paper is also designed to act as a roadmap to more detailed papers on different aspects of MIRI.
",
"doi": "10.1088/1538-3873/acbe66",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-04-01",
"series_number": "1046",
"volume": "135",
"issue": "1046",
"pages": "048003"
},
{
"id": "authors:fnhpv-jxp23",
"collection": "authors",
"collection_id": "fnhpv-jxp23",
"cite_using_url": "https://authors.library.caltech.edu/records/fnhpv-jxp23",
"type": "article",
"title": "Thermal emission from the Earth-sized exoplanet TRAPPIST-1 b using JWST",
"author": [
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Ducrot",
"given_name": "Elsa",
"orcid": "0000-0002-7008-6888"
},
{
"family_name": "Dyrek",
"given_name": "Achr\u00e8ne",
"orcid": "0000-0001-7189-6463"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
}
],
"abstract": "The TRAPPIST-1 system is remarkable for its seven planets that are similar in size, mass, density and stellar heating to the rocky planets Venus, Earth and Mars in the Solar System1. All the TRAPPIST-1 planets have been observed with transmission spectroscopy using the Hubble or Spitzer space telescopes, but no atmospheric features have been detected or strongly constrained2\u20135. TRAPPIST-1 b is the closest planet to the M-dwarf star of the system, and it receives four times as much radiation as Earth receives from the Sun. This relatively large amount of stellar heating suggests that its thermal emission may be measurable. Here we present photometric secondary eclipse observations of the Earth-sized exoplanet TRAPPIST-1 b using the F1500W filter of the mid-infrared instrument on the James Webb Space Telescope (JWST). We detect the secondary eclipses in five separate observations with 8.7\u03c3 confidence when all data are combined. These measurements are most consistent with re-radiation of the incident flux of the TRAPPIST-1 star from only the dayside hemisphere of the planet. The most straightforward interpretation is that there is little or no planetary atmosphere redistributing radiation from the host star and also no detectable atmospheric absorption of carbon dioxide (CO2) or other species.",
"doi": "10.1038/s41586-023-05951-7",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2023-03-27",
"series_number": "7963",
"volume": "618",
"issue": "7963",
"pages": "39-42"
},
{
"id": "authors:ta8h9-1v156",
"collection": "authors",
"collection_id": "ta8h9-1v156",
"cite_using_url": "https://authors.library.caltech.edu/records/ta8h9-1v156",
"type": "article",
"title": "Spectroscopic Time Series Performance of the Mid-infrared Instrument on the JWST",
"author": [
{
"family_name": "Bouwman",
"given_name": "Jeroen",
"orcid": "0000-0003-4757-2500"
},
{
"family_name": "Kendrew",
"given_name": "Sarah",
"orcid": "0000-0002-7612-0469"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Bell",
"given_name": "Taylor J.",
"orcid": "0000-0003-4177-2149"
},
{
"family_name": "Lagage",
"given_name": "Pierre-Olivier"
},
{
"family_name": "Schreiber",
"given_name": "J\u00fcrgen"
},
{
"family_name": "Dicken",
"given_name": "Daniel",
"orcid": "0000-0003-0589-5969"
},
{
"family_name": "Sloan",
"given_name": "G. C.",
"orcid": "0000-0003-4520-1044"
},
{
"family_name": "Espinoza",
"given_name": "N\u00e9stor",
"orcid": "0000-0001-9513-1449"
},
{
"family_name": "Scheithauer",
"given_name": "Silvia",
"orcid": "0000-0003-4559-0721"
},
{
"family_name": "Coulais",
"given_name": "Alain",
"orcid": "0000-0001-6492-7719"
},
{
"family_name": "Fox",
"given_name": "Ori D.",
"orcid": "0000-0003-2238-1572"
},
{
"family_name": "Gastaud",
"given_name": "Ren\u00e9",
"orcid": "0009-0007-5200-1362"
},
{
"family_name": "Glauser",
"given_name": "Adrian M.",
"orcid": "0000-0001-9250-1547"
},
{
"family_name": "Jones",
"given_name": "Olivia C.",
"orcid": "0000-0003-4870-5547"
},
{
"family_name": "Labiano",
"given_name": "Alvaro",
"orcid": "0000-0002-0690-8824"
},
{
"family_name": "Lahuis",
"given_name": "Fred",
"orcid": "0000-0002-8443-9488"
},
{
"family_name": "Morrison",
"given_name": "Jane E.",
"orcid": "0000-0002-9288-9235"
},
{
"family_name": "Murray",
"given_name": "Katherine"
},
{
"family_name": "Mueller",
"given_name": "Michael",
"orcid": "0000-0003-3217-5385"
},
{
"family_name": "Nayak",
"given_name": "Omnarayani",
"orcid": "0000-0001-6576-6339"
},
{
"family_name": "Wright",
"given_name": "Gillian S.",
"orcid": "0000-0001-7416-7936"
},
{
"family_name": "Glasse",
"given_name": "Alistair",
"orcid": "0000-0002-2041-2462"
},
{
"family_name": "Rieke",
"given_name": "George",
"orcid": "0000-0003-2303-6519"
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],
"abstract": "We present here the first ever mid-infrared spectroscopic time series observation of the transiting exoplanet L 168-9 b with the Mid-Infrared Instrument (MIRI) on the James Webb Space Telescope. The data were obtained as part of the MIRI commissioning activities, to characterize the performance of the Low Resolution Spectroscopy (LRS) mode for these challenging observations. To assess the MIRI LRS performance, we performed two independent analyses of the data. We find that with a single transit observation we reached a spectro-photometric precision of \u223c50 ppm in the 7\u20138 \u03bcm range at R = 50, consistent with \u223c25 ppm systematic noise. The derived band averaged transit depth is 524 \u00b1 15 ppm and 547 \u00b1 13 ppm for the two applied analysis methods, respectively, recovering the known transit depth to within 1\u03c3. The measured noise in the planet's transmission spectrum is approximately 15%\u201320% higher than random noise simulations over wavelengths 6.8 \u2272 \u03bb \u2272 11 \u03bcm. We observed an larger excess noise at the shortest wavelengths of up to a factor of two, for which possible causes are discussed. This performance was achieved with limited in-flight calibration data, demonstrating the future potential of MIRI for the characterization of exoplanet atmospheres.
",
"doi": "10.1088/1538-3873/acbc49",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-03-01",
"series_number": "1045",
"volume": "135",
"issue": "1045",
"pages": "038002"
},
{
"id": "authors:jfddk-arh79",
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"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230307-206925000.36",
"type": "article",
"title": "Performance of NIRCam on JWST in Flight",
"author": [
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
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{
"family_name": "Kelly",
"given_name": "Douglas M."
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{
"family_name": "Misselt",
"given_name": "Karl"
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{
"family_name": "Stansberry",
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{
"family_name": "Boyer",
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{
"family_name": "Beatty",
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{
"family_name": "Egami",
"given_name": "Eiichi",
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{
"family_name": "Florian",
"given_name": "Michael",
"orcid": "0000-0001-5097-6755"
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{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
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{
"family_name": "Hainline",
"given_name": "Kevin",
"orcid": "0000-0003-4565-8239"
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{
"family_name": "Leisenring",
"given_name": "Jarron",
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{
"family_name": "Roellig",
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{
"family_name": "Schlawin",
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{
"family_name": "Sun",
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"family_name": "Tinnin",
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{
"family_name": "Williams",
"given_name": "Christina C.",
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{
"family_name": "Willmer",
"given_name": "Christopher N. A.",
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{
"family_name": "Wilson",
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{
"family_name": "Clark",
"given_name": "Charles R."
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{
"family_name": "Rohrbach",
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{
"family_name": "Brooks",
"given_name": "Brian"
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{
"family_name": "Canipe",
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{
"family_name": "Correnti",
"given_name": "Matteo",
"orcid": "0000-0001-6464-3257"
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{
"family_name": "DiFelice",
"given_name": "Audrey"
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{
"family_name": "Gennaro",
"given_name": "Mario",
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{
"family_name": "Girard",
"given_name": "Julian",
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{
"family_name": "Hartig",
"given_name": "George"
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{
"family_name": "Hilbert",
"given_name": "Bryan"
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{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048"
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{
"family_name": "Nikolov",
"given_name": "Nikolay K.",
"orcid": "0000-0002-6500-3574"
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{
"family_name": "Pirzkal",
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{
"family_name": "Rest",
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{
"family_name": "Robberto",
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"orcid": "0000-0002-9573-3199"
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{
"family_name": "Sunnquist",
"given_name": "Ben",
"orcid": "0000-0003-3759-8707"
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{
"family_name": "Telfer",
"given_name": "Randal"
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{
"family_name": "Wu",
"given_name": "Chi Rai"
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{
"family_name": "Ferry",
"given_name": "Malcolm"
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{
"family_name": "Lewis",
"given_name": "Dan"
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{
"family_name": "Baum",
"given_name": "Stefi",
"orcid": "0000-0002-4735-8224"
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{
"family_name": "Beichman",
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"clpid": "Beichman-Charles-A"
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{
"family_name": "Doyon",
"given_name": "Ren\u00e9",
"orcid": "0000-0001-5485-4675"
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{
"family_name": "Dressler",
"given_name": "Alan",
"orcid": "0000-0002-6317-0037"
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{
"family_name": "Eisenstein",
"given_name": "Daniel J.",
"orcid": "0000-0002-2929-3121"
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{
"family_name": "Ferrarese",
"given_name": "Laura",
"orcid": "0000-0002-8224-1128"
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{
"family_name": "Hodapp",
"given_name": "Klaus",
"orcid": "0000-0003-0786-2140"
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{
"family_name": "Horner",
"given_name": "Scott",
"orcid": "0000-0001-9886-6934"
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{
"family_name": "Jaffe",
"given_name": "Daniel T.",
"orcid": "0000-0003-3577-3540"
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{
"family_name": "Johnstone",
"given_name": "Doug",
"orcid": "0000-0002-6773-459X"
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{
"family_name": "Krist",
"given_name": "John",
"clpid": "Krist-John-E"
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{
"family_name": "Martin",
"given_name": "Peter",
"orcid": "0000-0002-5236-3896"
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{
"family_name": "McCarthy",
"given_name": "Donald W."
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{
"family_name": "Meyer",
"given_name": "Michael",
"orcid": "0000-0003-1227-3084"
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{
"family_name": "Rieke",
"given_name": "George H.",
"orcid": "0000-0003-2303-6519"
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{
"family_name": "Trauger",
"given_name": "John",
"clpid": "Trauger-John-T"
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{
"family_name": "Young",
"given_name": "Erick T.",
"orcid": "0000-0002-6395-4296"
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],
"abstract": "The Near Infrared Camera for the James Webb Space Telescope (JWST) is delivering the imagery that astronomers have hoped for ever since JWST was proposed back in the 1990s. In the Commissioning Period that extended from right after launch to early 2022 July, NIRCam has been subjected to a number of performance tests and operational checks. The camera is exceeding prelaunch expectations in virtually all areas, with very few surprises discovered in flight. NIRCam also delivered the imagery needed by the Wavefront Sensing Team for use in aligning the telescope mirror segments.",
"doi": "10.1088/1538-3873/acac53",
"issn": "0004-6280",
"publisher": "Astronomical Society of the Pacific",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-02",
"series_number": "1044",
"volume": "135",
"issue": "1044",
"pages": "Art. No. 028001"
},
{
"id": "authors:y99a9-89r71",
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"cite_using_url": "https://authors.library.caltech.edu/records/y99a9-89r71",
"type": "article",
"title": "JWST NIRCam Defocused Imaging: Photometric Stability Performance and How It Can Sense Mirror Tilts",
"author": [
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Beatty",
"given_name": "Thomas",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Brooks",
"given_name": "Brian"
},
{
"family_name": "Nikolov",
"given_name": "Nikolay K.",
"orcid": "0000-0002-6500-3574"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Espinoza",
"given_name": "N\u00e9stor",
"orcid": "0000-0001-9513-1449"
},
{
"family_name": "Glidic",
"given_name": "Kayli",
"orcid": "0000-0003-4669-7088"
},
{
"family_name": "Baka",
"given_name": "Keith"
},
{
"family_name": "Egami",
"given_name": "Eiichi",
"orcid": "0000-0003-1344-9475"
},
{
"family_name": "Stansberry",
"given_name": "John",
"orcid": "0000-0003-2434-5225"
},
{
"family_name": "Boyer",
"given_name": "Martha",
"orcid": "0000-0003-4850-9589"
},
{
"family_name": "Gennaro",
"given_name": "Mario",
"orcid": "0000-0002-5581-2896"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Hilbert",
"given_name": "Bryan",
"orcid": "0000-0002-6875-1543"
},
{
"family_name": "Misselt",
"given_name": "Karl"
},
{
"family_name": "Kelly",
"given_name": "Doug"
},
{
"family_name": "Canipe",
"given_name": "Alicia",
"orcid": "0009-0002-6366-0957"
},
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Correnti",
"given_name": "Matteo",
"orcid": "0000-0001-6464-3257"
},
{
"family_name": "Knight",
"given_name": "J. Scott"
},
{
"family_name": "Jurling",
"given_name": "Alden",
"orcid": "0000-0002-6880-4924"
},
{
"family_name": "Perrin",
"given_name": "Marshall D.",
"orcid": "0000-0002-3191-8151"
},
{
"family_name": "Feinberg",
"given_name": "Lee D."
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Bond",
"given_name": "Nicholas"
},
{
"family_name": "Ciardi",
"given_name": "David",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Kendrew",
"given_name": "Sarah",
"orcid": "0000-0002-7612-0469"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "We use JWST NIRCam short-wavelength photometry to capture a transit lightcurve of the exoplanet HAT-P-14 b to assess performance as part of instrument commissioning. The short-wavelength precision is 152 ppm per 27 s integration as measured over the full time series compared to a theoretical limit of 107 ppm, after corrections to spatially correlated 1/f noise. Persistence effects from charge trapping are well fit by an exponential function with short characteristic timescales, settling on the order of 5\u201315 minutes. The short-wavelength defocused photometry is also uniquely well suited to measure the real-time wave-front error of JWST. Analysis of the images and reconstructed wave-front maps indicates that two different hexagonal primary mirror segments exhibited \"tilt events,\" where they changed orientation rapidly in less than \u223c1.4 s. In some cases, the magnitude and timing of the flux jumps caused by tilt events can be accurately predicted with a telescope model. These tilt events can be sensed by simultaneous longer-wavelength NIRCam grism spectral images alone in the form of changes to the point-spread function, diagnosed from the full width at half maximum. They can also be sensed with the fine guidance sensor instrument from difference images. Tilt events possibly from sudden releases of stress in the backplane structure behind the mirrors were expected during the commissioning period because they were found in ground-based testing. Tilt events have shown signs of decreasing in frequency but have not disappeared completely. The detectors exhibit some minor (less than 1%) deviations from linear behavior in the first few groups of each integration, potentially impacting absolute fluxes and transit depths on bright targets, where only a handful of groups are possible. Overall, the noise is within 50% of the theoretical photon noise and read noise. This bodes well for high-precision measurements of transiting exoplanets and other time variable targets.
",
"doi": "10.1088/1538-3873/aca718",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-01-01",
"series_number": "1043",
"volume": "135",
"issue": "1043",
"pages": "018001"
},
{
"id": "authors:mdnf5-mhc24",
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"collection_id": "mdnf5-mhc24",
"cite_using_url": "https://authors.library.caltech.edu/records/mdnf5-mhc24",
"type": "article",
"title": "Spectroscopic Time-series Performance of JWST/NIRSpec from Commissioning Observations",
"author": [
{
"family_name": "Espinoza",
"given_name": "N\u00e9stor",
"orcid": "0000-0001-9513-1449"
},
{
"family_name": "\u00dabeda",
"given_name": "Leonardo",
"orcid": "0000-0001-7130-2880"
},
{
"family_name": "Birkmann",
"given_name": "Stephan M.",
"orcid": "0000-0001-7058-1726"
},
{
"family_name": "Ferruit",
"given_name": "Pierre",
"orcid": "0000-0001-8895-0606"
},
{
"family_name": "Valenti",
"given_name": "Jeff A.",
"orcid": "0000-0003-3305-6281"
},
{
"family_name": "Sing",
"given_name": "David K.",
"orcid": "0000-0001-6050-7645"
},
{
"family_name": "Rustamkulov",
"given_name": "Zafar",
"orcid": "0000-0003-4408-0463",
"clpid": "Rustamkulov-Zafar"
},
{
"family_name": "Regan",
"given_name": "Michael",
"orcid": "0000-0001-9367-0705"
},
{
"family_name": "Kendrew",
"given_name": "Sarah",
"orcid": "0000-0002-7612-0469"
},
{
"family_name": "Sabbi",
"given_name": "Elena",
"orcid": "0000-0003-2954-7643"
},
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Beatty",
"given_name": "Thomas",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Albert",
"given_name": "Lo\u00efc",
"orcid": "0000-0003-0475-9375"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Nikolov",
"given_name": "Nikolay",
"orcid": "0000-0002-6500-3574"
},
{
"family_name": "Karakla",
"given_name": "Diane"
},
{
"family_name": "Keyes",
"given_name": "Charles"
},
{
"family_name": "Alves de Oliveira",
"given_name": "Catarina",
"orcid": "0000-0003-2896-4138"
},
{
"family_name": "B\u00f6ker",
"given_name": "Torsten",
"orcid": "0000-0002-5666-7782"
},
{
"family_name": "Pena-Guerrero",
"given_name": "Maria",
"orcid": "0000-0003-2314-3453"
},
{
"family_name": "Giardino",
"given_name": "Giovanna",
"orcid": "0000-0002-9262-7155"
},
{
"family_name": "Kumari",
"given_name": "Nimisha",
"orcid": "0000-0002-5320-2568"
},
{
"family_name": "Manjavacas",
"given_name": "Elena",
"orcid": "0000-0003-0192-6887"
},
{
"family_name": "Proffitt",
"given_name": "Charles",
"orcid": "0000-0001-7617-5665"
},
{
"family_name": "Rawle",
"given_name": "Timothy",
"orcid": "0000-0002-7028-5588"
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],
"abstract": "We report on James Webb Space Telescope (JWST) commissioning observations of the transiting exoplanet HAT-P-14 b, obtained using the Bright Object Time Series (BOTS) mode of the NIRSpec instrument with the G395H/F290LP grating/filter combination (3\u20135 \u03bcm). While the data were used primarily to verify that the NIRSpec BOTS mode is working as expected, and to enable it for general scientific use, they yield a precise transmission spectrum which we find is featureless down to the precision level of the instrument, consistent with expectations given HAT-P-14 b's small scale-height and hence expected atmospheric features. The exquisite quality and stability of the JWST/NIRSpec transit spectrum\u2014almost devoid of any systematic effects\u2014allowed us to obtain median uncertainties of 50\u201360 ppm in this wavelength range at a resolution of R = 100 in a single exposure, which is in excellent agreement with pre-flight expectations and close to the (or at the) photon-noise limit for a J = 9.094, F-type star like HAT-P-14. These observations showcase the ability of NIRSpec/BOTS to perform cutting-edge transiting exoplanet atmospheric science, setting the stage for observations and discoveries to be made in Cycle 1 and beyond.
",
"doi": "10.1088/1538-3873/aca3d3",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2023-01-01",
"series_number": "1043",
"volume": "135",
"issue": "1043",
"pages": "018002"
},
{
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"collection_id": "tf2bb-v7z75",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221031-575177800.20",
"type": "article",
"title": "A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b",
"author": [
{
"family_name": "Brande",
"given_name": "Jonathan",
"orcid": "0000-0002-2072-6541",
"clpid": "Brande-Jonathan"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-Ian-J-M"
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{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147",
"clpid": "Kreidberg-Laura"
},
{
"family_name": "Oklop\u010di\u0107",
"given_name": "Antonija",
"orcid": "0000-0002-9584-6476",
"clpid": "Oklop\u010di\u0107-Antonija"
},
{
"family_name": "Polanski",
"given_name": "Alex S.",
"orcid": "0000-0001-7047-8681",
"clpid": "Polanski-Alex-S"
},
{
"family_name": "Barman",
"given_name": "Travis",
"orcid": "0000-0002-7129-3002",
"clpid": "Barman-Travis-S"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498",
"clpid": "Benneke-Bj\u00f6rn"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X",
"clpid": "Dragomir-Diana"
},
{
"family_name": "Foreman-Mackey",
"given_name": "Daniel",
"orcid": "0000-0002-9328-5652",
"clpid": "Foreman-Mackey-Daniel"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-Jonathan-J"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Lothringer",
"given_name": "Joshua D.",
"orcid": "0000-0003-3667-8633",
"clpid": "Lothringer-Joshua-D"
},
{
"family_name": "Mikal-Evans",
"given_name": "Thomas",
"orcid": "0000-0001-5442-1300",
"clpid": "Mikal-Evans-Thomas"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456",
"clpid": "Morley-Caroline-V"
}
],
"abstract": "We report observations of the recently discovered warm Neptune TOI-674 b (5.25 R_\u2295, 23.6 M_\u2295) with the Hubble Space Telescope's Wide Field Camera 3 instrument. TOI-674 b is in the Neptune desert, an observed paucity of Neptune-size exoplanets at short orbital periods. Planets in the desert are thought to have complex evolutionary histories due to photoevaporative mass loss or orbital migration, making identifying the constituents of their atmospheres critical to understanding their origins. We obtained near-infrared transmission spectroscopy of the planet's atmosphere with the G141 grism. After extracting, detrending, and fitting the spectral light curves to measure the planet's transmission spectrum, we used the petitRADTRANS atmospheric spectral synthesis code to perform retrievals on the planet's atmosphere to identify which absorbers are present. These results show moderate evidence for increased absorption at 1.4 \u03bcm due to water vapor at 2.9\u03c3 (Bayes factor = 15.8), as well as weak evidence for the presence of clouds at 2.2\u03c3 (Bayes factor = 4.0). TOI-674 b is a strong candidate for further study to refine the water abundance, which is poorly constrained by our data. We also incorporated new TESS short-cadence optical photometry, as well as Spitzer/IRAC data, and refit the transit parameters for the planet. We find the planet to have the following transit parameters: R\u209a/R_* = 0.1135 \u00b1 0.0006, T\u2080 = 2458544.523792 \u00b1 0.000452 BJD, and P = 1.977198 \u00b1 0.00007 day. These measurements refine the planet radius estimate and improve the orbital ephemerides for future transit spectroscopy observations of this highly intriguing warm Neptune.",
"doi": "10.3847/1538-3881/ac8b7e",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-11",
"series_number": "5",
"volume": "164",
"issue": "5",
"pages": "Art. No. 197"
},
{
"id": "authors:bpfcv-m8651",
"collection": "authors",
"collection_id": "bpfcv-m8651",
"cite_using_url": "https://authors.library.caltech.edu/records/bpfcv-m8651",
"type": "article",
"title": "Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c",
"author": [
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M."
},
{
"family_name": "Thorngren",
"given_name": "Daniel P.",
"orcid": "0000-0002-5113-8558"
},
{
"family_name": "Kawashima",
"given_name": "Yui",
"orcid": "0000-0003-3800-7518"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Mikal-Evans",
"given_name": "Thomas",
"orcid": "0000-0001-5442-1300"
},
{
"family_name": "Berardo",
"given_name": "David",
"orcid": "0000-0001-6298-412X"
},
{
"family_name": "Kosiarek",
"given_name": "Molly R.",
"orcid": "0000-0002-6115-4359"
},
{
"family_name": "Gorjian",
"given_name": "Varoujan",
"orcid": "0000-0002-8990-2101",
"clpid": "Gorjian-Varoujan"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X"
},
{
"family_name": "Dressing",
"given_name": "Courtney D.",
"orcid": "0000-0001-8189-0233"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-Benjamin-J"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hardegree-Ullman",
"given_name": "Kevin K.",
"orcid": "0000-0003-3702-0382",
"clpid": "Hardegree-Ullman-Kevin-K"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Krick",
"given_name": "Jessica E.",
"orcid": "0000-0002-2413-5976",
"clpid": "Krick-Jessica-E"
},
{
"family_name": "Livingston",
"given_name": "John H.",
"orcid": "0000-0002-4881-3620"
},
{
"family_name": "Lothringer",
"given_name": "Joshua D.",
"orcid": "0000-0003-3667-8633"
},
{
"family_name": "Morales",
"given_name": "Farisa Y.",
"orcid": "0000-0001-9414-3851",
"clpid": "Morales-Farisa-Y"
},
{
"family_name": "Petigura",
"given_name": "Erik A.",
"orcid": "0000-0003-0967-2893"
},
{
"family_name": "Rodriguez",
"given_name": "Joseph E.",
"orcid": "0000-0001-8812-0565"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058"
}
],
"abstract": "We present a transmission spectrum for the Neptune-sized exoplanet HD 106315c from optical to infrared wavelengths based on transit observations from the Hubble Space Telescope/Wide Field Camera 3, K2, and Spitzer. The spectrum shows tentative evidence for a water absorption feature in the 1.1–1.7 μm wavelength range with a small amplitude of 30 ppm (corresponding to just 0.8 ± 0.04 atmospheric scale heights). Based on an atmospheric retrieval analysis, the presence of water vapor is tentatively favored with a Bayes factor of 1.7–2.6 (depending on prior assumptions). The spectrum is most consistent with either an enhanced metallicity or high-altitude condensates, or both. Cloud-free solar composition atmospheres are ruled out at >5σ confidence. We compare the spectrum to grids of cloudy and hazy forward models and find that the spectrum is fit well by models with moderate cloud lofting or haze formation efficiency over a wide range of metallicities (1–100× solar). We combine the constraints on the envelope composition with an interior structure model and estimate that the core mass fraction is \u22730.3. With a bulk composition reminiscent of that of Neptune and an orbital distance of 0.15 au, HD 106315c hints that planets may form out of broadly similar material and arrive at vastly different orbits later in their evolution.
",
"doi": "10.3847/1538-3881/ac85be",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-10-01",
"series_number": "4",
"volume": "164",
"issue": "4",
"pages": "124"
},
{
"id": "authors:mtw94-9ns95",
"collection": "authors",
"collection_id": "mtw94-9ns95",
"cite_using_url": "https://authors.library.caltech.edu/records/mtw94-9ns95",
"type": "article",
"title": "First Peek with JWST/NIRCam Wide-field Slitless Spectroscopy: Serendipitous Discovery of a Strong [O iii]/H\u03b1 Emitter at z = 6.11",
"author": [
{
"family_name": "Sun",
"given_name": "Fengwu",
"orcid": "0000-0002-4622-6617"
},
{
"family_name": "Egami",
"given_name": "Eiichi",
"orcid": "0000-0003-1344-9475"
},
{
"family_name": "Pirzkal",
"given_name": "Nor",
"orcid": "0000-0003-3382-5941"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
},
{
"family_name": "Boyer",
"given_name": "Martha",
"orcid": "0000-0003-4850-9589"
},
{
"family_name": "Correnti",
"given_name": "Matteo",
"orcid": "0000-0001-6464-3257"
},
{
"family_name": "Gennaro",
"given_name": "Mario",
"orcid": "0000-0002-5581-2896"
},
{
"family_name": "Girard",
"given_name": "Julien",
"orcid": "0000-0001-8627-0404"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Kelly",
"given_name": "Doug"
},
{
"family_name": "Koekemoer",
"given_name": "Anton M.",
"orcid": "0000-0002-6610-2048"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Misselt",
"given_name": "Karl"
},
{
"family_name": "Nikolov",
"given_name": "Nikolay",
"orcid": "0000-0002-6500-3574"
},
{
"family_name": "Roellig",
"given_name": "Thomas L.",
"orcid": "0000-0002-6730-5410"
},
{
"family_name": "Stansberry",
"given_name": "John",
"orcid": "0000-0003-2434-5225"
},
{
"family_name": "Williams",
"given_name": "Christina C.",
"orcid": "0000-0003-2919-7495"
},
{
"family_name": "Willmer",
"given_name": "Christopher N. A.",
"orcid": "0000-0001-9262-9997"
},
{
"literal": "(Members of the JWST/NIRCam Commissioning Team)"
}
],
"abstract": "We report the serendipitous discovery of an [O iii] \u03bb\u03bb4959/5007 and H\u03b1 line emitter in the Epoch of Reionization (EoR) with the James Webb Space Telescope (JWST) commissioning data taken in the NIRCam wide-field slitless spectroscopy (WFSS) mode. Located \u223c55\u2033 away from the flux calibrator P330-E, this galaxy exhibits bright [O iii] \u03bb\u03bb4959/5007 and H\u03b1 lines detected at 3.7\u03c3, 9.9\u03c3, and 5.7\u03c3, respectively, with a spectroscopic redshift of z = 6.112 \u00b1 0.001. The total H\u03b2+[O iii] equivalent width is 664 \u00b1 98 \u00c5 (454 \u00b1 78 \u00c5 from the [O iii] \u03bb5007 line). This provides direct spectroscopic evidence for the presence of strong rest-frame optical lines (H\u03b2+[O iii] and H\u03b1) in EoR galaxies as inferred previously from the analyses of the Spitzer/IRAC spectral energy distributions (SEDs). Two spatial and velocity components are identified in this source, possibly indicating that this system is undergoing a major merger, which might have triggered the ongoing starburst with strong nebular emission lines over a timescale of \u223c2 Myr, as our SED modeling suggests. The tentative detection of He ii\u03bb4686 line (1.9\u03c3), if real, may indicate the existence of very young and metal-poor star-forming regions with a hard UV radiation field. Finally, this discovery demonstrates the power and readiness of the JWST/NIRCam WFSS mode, and marks the beginning of a new era for extragalactic astronomy, in which EoR galaxies can be routinely discovered via blind slitless spectroscopy through the detection of rest-frame optical emission lines.
",
"doi": "10.3847/2041-8213/ac8938",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2022-08-29",
"series_number": "1",
"volume": "936",
"issue": "1",
"pages": "L8"
},
{
"id": "authors:p6t7g-a6771",
"collection": "authors",
"collection_id": "p6t7g-a6771",
"cite_using_url": "https://authors.library.caltech.edu/records/p6t7g-a6771",
"type": "article",
"title": "Densified Pupil Spectrograph as High-precision Radial Velocimetry: From Direct Measurement of the Universe's Expansion History to Characterization of Nearby Habitable Planet Candidates",
"author": [
{
"family_name": "Matsuo",
"given_name": "Taro",
"orcid": "0000-0001-7694-5885"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Qezlou",
"given_name": "Mahdi",
"orcid": "0000-0001-7066-1240"
},
{
"family_name": "Bird",
"given_name": "Simeon",
"orcid": "0000-0001-5803-5490"
},
{
"family_name": "Ichiki",
"given_name": "Kiyotomo",
"orcid": "0000-0003-1365-8568"
},
{
"family_name": "Fujii",
"given_name": "Yuka",
"orcid": "0000-0002-2786-0786"
},
{
"family_name": "Yamamuro",
"given_name": "Tomoyasu"
}
],
"abstract": "The direct measurement of the universe's expansion history and the search for terrestrial planets in habitable zones around solar-type stars require extremely high-precision radial-velocity measures over a decade. This study proposes an approach for enabling high-precision radial-velocity measurements from space. The concept presents a combination of a high-dispersion densified pupil spectrograph and a novel line-of-sight monitor for telescopes. The precision of the radial-velocity measurements is determined by combining the spectrophotometric accuracy and the quality of the absorption lines in the recorded spectrum. Therefore, a highly dispersive densified pupil spectrograph proposed to perform stable spectroscopy can be utilized for high-precision radial-velocity measures. A concept involving the telescope's line-of-sight monitor is developed to minimize the change of the telescope's line of sight over a decade. This monitor allows the precise measurement of long-term telescope drift without any significant impact on the Airy disk when the densified pupil spectra are recorded. We analytically derive the uncertainty of the radial-velocity measurements, which is caused by the residual offset of the lines of sight at two epochs. We find that the error could be reduced down to approximately 1 cm s\u22121, and the precision will be limited by another factor (e.g., wavelength calibration uncertainty). A combination of the high-precision spectrophotometry and the high spectral resolving power could open a new path toward the characterization of nearby non-transiting habitable planet candidates orbiting late-type stars. We present two simple and compact highly dispersed densified pupil spectrograph designs for cosmology and exoplanet sciences.
",
"doi": "10.3847/1538-3881/ac397b",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2022-01-13",
"series_number": "2",
"volume": "163",
"issue": "2",
"pages": "63"
},
{
"id": "authors:x5npb-p1w50",
"collection": "authors",
"collection_id": "x5npb-p1w50",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211220-495675000",
"type": "article",
"title": "Detecting Biosignatures in the Atmospheres of Gas Dwarf Planets with the James Webb Space Telescope",
"author": [
{
"family_name": "Phillips",
"given_name": "Caprice L.",
"orcid": "0000-0001-5610-5328",
"clpid": "Phillips-Caprice-L"
},
{
"family_name": "Wang",
"given_name": "Ji",
"orcid": "0000-0002-4361-8885",
"clpid": "Wang-Ji"
},
{
"family_name": "Kendrew",
"given_name": "Sarah",
"orcid": "0000-0002-7612-0469",
"clpid": "Kendrew-Sarah"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hu",
"given_name": "Renyu",
"orcid": "0000-0003-2215-8485",
"clpid": "Hu-Renyu"
},
{
"family_name": "Valenti",
"given_name": "Jeff",
"orcid": "0000-0003-3305-6281",
"clpid": "Valenti-Jeff-A"
},
{
"family_name": "Panero",
"given_name": "Wendy R.",
"orcid": "0000-0001-5753-2532",
"clpid": "Panero-Wendy-R"
},
{
"family_name": "Schulze",
"given_name": "Joseph",
"orcid": "0000-0003-3570-422X",
"clpid": "Schulze-Joseph"
}
],
"abstract": "Exoplanets with radii between those of Earth and Neptune have stronger surface gravity than Earth, and can retain a sizable hydrogen-dominated atmosphere. In contrast to gas giant planets, we call these planets gas dwarf planets. The James Webb Space Telescope (JWST) will offer unprecedented insight into these planets. Here, we investigate the detectability of ammonia (NH\u2083, a potential biosignature) in the atmospheres of seven temperate gas dwarf planets using various JWST instruments. We use petitRadTRANS and PandExo to model planet atmospheres and simulate JWST observations under different scenarios by varying cloud conditions, mean molecular weights (MMWs), and NH\u2083 mixing ratios. A metric is defined to quantify detection significance and provide a ranked list for JWST observations in search of biosignatures in gas dwarf planets. It is very challenging to search for the 10.3\u201310.8 \u03bcm NH\u2083 feature using eclipse spectroscopy with the Mid-Infrared Instrument (MIRI) in the presence of photon and a systemic noise floor of 12.6 ppm for 10 eclipses. NIRISS, NIRSpec, and MIRI are feasible for transmission spectroscopy to detect NH3 features from 1.5\u20136.1 \u03bcm under optimal conditions such as a clear atmosphere and low MMWs for a number of gas dwarf planets. We provide examples of retrieval analyses to further support the detection metric that we use. Our study shows that searching for potential biosignatures such as NH\u2083 is feasible with a reasonable investment of JWST time for gas dwarf planets given optimal atmospheric conditions.",
"doi": "10.3847/1538-4357/ac29be",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-12-20",
"series_number": "2",
"volume": "923",
"issue": "2",
"pages": "Art. No. 144"
},
{
"id": "authors:b4x75-hrr06",
"collection": "authors",
"collection_id": "b4x75-hrr06",
"cite_using_url": "https://authors.library.caltech.edu/records/b4x75-hrr06",
"type": "article",
"title": "The Near-stellar Environment of Class 0 Protostars: A First Look with Near-infrared Spectroscopy",
"author": [
{
"family_name": "Laos",
"given_name": "Emily",
"orcid": "0000-0001-8407-2105"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Najita",
"given_name": "Joan R.",
"orcid": "0000-0002-5758-150X"
},
{
"family_name": "Stassun",
"given_name": "Keivan G.",
"orcid": "0000-0002-3481-9052"
}
],
"abstract": "We present near-infrared K-band spectra for a sample of seven Class 0 protostars in the Perseus and Orion star-forming regions. We detect Br\u03b3, CO overtone, and H2 emission, features that probe the near-circumstellar environment of the protostar and reveal evidence of magnetospheric accretion, a hot inner disk atmosphere, and outflows, respectively. Comparing the properties of these features with those of Class I sources from the literature, we find that their Br\u03b3 emission and CO emission are generally consistent in strength and velocity width. The Br\u03b3 line profiles are broad and centrally peaked, with FWHMs of \u223c200 km s\u22121 and wings extending to \u223c300 km s\u22121. The line ratios of our H2 emission features, which are spatially extended for some sources, are consistent with shock excitation and indicate the presence of strong jets or a disk wind. Within our small sample, the frequency of CO band emission (\u223c67%) is high relative to that of Class I samples (\u223c15%), indicating that Class 0 sources have high inner disk accretion rates, similar to those of the most actively accreting Class I sources. Collectively, our results suggest that Class 0 sources have similar accretion mechanisms to the more evolved classes, with strong organized stellar magnetic fields established at the earliest observable stage of evolution.
",
"doi": "10.3847/1538-4357/ac1f1b",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2021-11-01",
"series_number": "2",
"volume": "921",
"issue": "2",
"pages": "110"
},
{
"id": "authors:m220c-1ks32",
"collection": "authors",
"collection_id": "m220c-1ks32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210504-082538165",
"type": "article",
"title": "Origins Space Telescope: trades and decisions leading to the baseline mission concept",
"author": [
{
"family_name": "Leisawitz",
"given_name": "David",
"orcid": "0000-0003-1000-2547",
"clpid": "Leisawitz-David-T"
},
{
"family_name": "Amatucci",
"given_name": "Edward"
},
{
"family_name": "Allen",
"given_name": "Lynn"
},
{
"family_name": "Arenberg",
"given_name": "Jonathan"
},
{
"family_name": "Armus",
"given_name": "Lee",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-Lee"
},
{
"family_name": "Battersby",
"given_name": "Cara"
},
{
"family_name": "Bauer",
"given_name": "James"
},
{
"family_name": "Bell",
"given_name": "Ray"
},
{
"family_name": "Benford",
"given_name": "Dominic"
},
{
"family_name": "Bergin",
"given_name": "Edward"
},
{
"family_name": "Booth",
"given_name": "Jeffrey T.",
"clpid": "Booth-Jeffrey-T"
},
{
"family_name": "Bradford",
"given_name": "Charles M.",
"orcid": "0000-0001-5261-7094",
"clpid": "Bradford-Charles-M"
},
{
"family_name": "Bradley",
"given_name": "Damon"
},
{
"family_name": "Carey",
"given_name": "Sean",
"orcid": "0000-0002-0221-6871",
"clpid": "Carey-Sean-J"
},
{
"family_name": "Carter",
"given_name": "Ruth"
},
{
"family_name": "Cooray",
"given_name": "Asantha"
},
{
"family_name": "Corsetti",
"given_name": "James"
},
{
"family_name": "Dewell",
"given_name": "Larry"
},
{
"family_name": "DiPirro",
"given_name": "Michael"
},
{
"family_name": "Drake",
"given_name": "Bret G."
},
{
"family_name": "East",
"given_name": "Matthew"
},
{
"family_name": "Ennico",
"given_name": "Kimberly"
},
{
"family_name": "Feller",
"given_name": "Greg"
},
{
"family_name": "Flores",
"given_name": "Angel"
},
{
"family_name": "Fortney",
"given_name": "Jonathan"
},
{
"family_name": "Granger",
"given_name": "Zachary"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Howard",
"given_name": "Joseph"
},
{
"family_name": "Kataria",
"given_name": "Tiffany",
"orcid": "0000-0003-3759-9080",
"clpid": "Kataria-Tiffany"
},
{
"family_name": "Knight",
"given_name": "John S."
},
{
"family_name": "Lawrence",
"given_name": "Charles",
"clpid": "Lawrence-Charles-R"
},
{
"family_name": "Lightsey",
"given_name": "Paul"
},
{
"family_name": "Mather",
"given_name": "John C."
},
{
"family_name": "Meixner",
"given_name": "Margaret"
},
{
"family_name": "Melnick",
"given_name": "Gary"
},
{
"family_name": "McMurtry",
"given_name": "Craig"
},
{
"family_name": "Milam",
"given_name": "Stefanie"
},
{
"family_name": "Moseley",
"given_name": "Samuel H."
},
{
"family_name": "Narayanan",
"given_name": "Desika"
},
{
"family_name": "Nordt",
"given_name": "Alison"
},
{
"family_name": "Padgett",
"given_name": "Deborah",
"orcid": "0000-0001-5334-5107",
"clpid": "Padgett-Deborah-L"
},
{
"family_name": "Pontoppidan",
"given_name": "Klaus"
},
{
"family_name": "Pope",
"given_name": "Alexandra"
},
{
"family_name": "Rafanelli",
"given_name": "Gerard"
},
{
"family_name": "Redding",
"given_name": "David C.",
"clpid": "Redding-David-C"
},
{
"family_name": "Rieke",
"given_name": "George"
},
{
"family_name": "Roellig",
"given_name": "Thomas"
},
{
"family_name": "Sakon",
"given_name": "Itsuki"
},
{
"family_name": "Sandin",
"given_name": "Carly"
},
{
"family_name": "Sandstrom",
"given_name": "Karin"
},
{
"family_name": "Sengupta",
"given_name": "Anita",
"clpid": "Sengupta-Anita"
},
{
"family_name": "Sheth",
"given_name": "Kartik"
},
{
"family_name": "Sokolsky",
"given_name": "Lawrence M."
},
{
"family_name": "Staguhn",
"given_name": "Johannes"
},
{
"family_name": "Steeves",
"given_name": "John",
"clpid": "Steeves-John-B"
},
{
"family_name": "Stevenson",
"given_name": "Kevin"
},
{
"family_name": "Su",
"given_name": "Kate"
},
{
"family_name": "Vieira",
"given_name": "Joaquin"
},
{
"family_name": "Webster",
"given_name": "Cassandra"
},
{
"family_name": "Wiedner",
"given_name": "Martina"
},
{
"family_name": "Wright",
"given_name": "Edward L."
},
{
"family_name": "Wu",
"given_name": "Chi"
},
{
"family_name": "Yanatsis",
"given_name": "David"
},
{
"family_name": "Zmuidzinas",
"given_name": "Jonas",
"orcid": "0000-0002-3330-5439",
"clpid": "Zmuidzinas-J"
}
],
"abstract": "The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the universe today? How do habitable planets form? How common are life-bearing worlds? We describe how Origins was designed to answer these alluring questions. We discuss the key decisions taken by the Origins mission concept study team, the rationale for those choices, and how they led through an exploratory design process to the Origins baseline mission concept. To understand the concept solution space, we studied two distinct mission concepts and descoped the second concept, aiming to maximize science per dollar and hit a self-imposed cost target. We report on the study approach and describe the concept evolution. The resulting baseline design includes a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. The chosen architecture is similar to that of the Spitzer Space Telescope and requires very few deployments after launch. The cryo-thermal system design leverages James Webb Space Telescope technology and experience.",
"doi": "10.1117/1.JATIS.7.1.011014",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2021-03-13",
"series_number": "1",
"volume": "7",
"issue": "1",
"pages": "Art. No. 011014"
},
{
"id": "authors:38pg0-z0v63",
"collection": "authors",
"collection_id": "38pg0-z0v63",
"cite_using_url": "https://authors.library.caltech.edu/records/38pg0-z0v63",
"type": "article",
"title": "Mid-infrared spectrometer and camera for the Origins Space Telescope",
"author": [
{
"family_name": "Sakon",
"given_name": "Itsuki",
"orcid": "0000-0001-7641-5497"
},
{
"family_name": "Roellig",
"given_name": "Thomas L."
},
{
"family_name": "Ennico-Smith",
"given_name": "Kimberly A.",
"orcid": "0000-0002-8847-8492"
},
{
"family_name": "Matsuo",
"given_name": "Taro"
},
{
"family_name": "Ikeda",
"given_name": "Yuji"
},
{
"family_name": "Yamamuro",
"given_name": "Tomoyasu"
},
{
"family_name": "Enya",
"given_name": "Keigo"
},
{
"family_name": "Wada",
"given_name": "Takehiko",
"orcid": "0000-0002-9321-4918"
},
{
"family_name": "Kawada",
"given_name": "Mitsunobu"
},
{
"family_name": "Takahashi",
"given_name": "Aoi"
},
{
"family_name": "Sarugaku",
"given_name": "Yuki"
},
{
"family_name": "Fujishiro",
"given_name": "Naofumi"
},
{
"family_name": "Murakami",
"given_name": "Naoshi"
},
{
"family_name": "Nishikawa",
"given_name": "Jun",
"orcid": "0000-0001-9326-8134"
},
{
"family_name": "Kotani",
"given_name": "Takayuki",
"orcid": "0000-0001-6181-3142"
},
{
"family_name": "Goda",
"given_name": "Shohei"
},
{
"family_name": "Ido",
"given_name": "Masayuki"
},
{
"family_name": "Itoh",
"given_name": "Satoshi"
},
{
"family_name": "Tsuboi",
"given_name": "Takahiro"
},
{
"family_name": "Sumi",
"given_name": "Takahiro"
},
{
"family_name": "Kamiura",
"given_name": "Masatsugu",
"orcid": "0000-0002-0733-4383"
},
{
"family_name": "Manome",
"given_name": "Takeo"
},
{
"family_name": "Iida",
"given_name": "Naoto"
},
{
"family_name": "Yanagibashi",
"given_name": "Kentaro"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Helvensteijn",
"given_name": "Bernardus P."
},
{
"family_name": "Hofland",
"given_name": "Lynn"
},
{
"family_name": "Johnson",
"given_name": "Roy R."
},
{
"family_name": "Kashani",
"given_name": "Ali"
},
{
"family_name": "Quigley",
"given_name": "Emmett"
},
{
"family_name": "McMurray",
"given_name": "Robert E."
},
{
"family_name": "Inami",
"given_name": "Hanae",
"orcid": "0000-0003-4268-0393"
},
{
"family_name": "Burgarella",
"given_name": "Denis",
"orcid": "0000-0002-4193-2539"
}
],
"abstract": "The mid-infrared spectrometer and camera transit spectrometer (MISC-T) is one of the three baseline instruments for Origins Space Telescope (Origins) and provides the capability to assess the habitability of nearby exoplanets and search for signs of life. MISC-T employs a densified pupil optical design, and HgCdTe and Si:As detector arrays. This optical design allows the instrument to be relatively insensitive to minor line-of-sight pointing drifts and telescope aberrations, and the detectors do not require a sub-Kelvin refrigerator. MISC-T has three science spectral channels that share the same field-of-view by means of beam splitters, and all channels are operated simultaneously to cover the full spectral range from 2.8 to 20 \u03bcm at once with exquisite stability and precision (<5 ppm between 2.8 to 11 \u03bcm, <20 ppm between 11 and 20 \u03bcm). A Lyot-coronagraph-based tip\u2013tilt sensor located in the instrument fore-optics uses the light reflected by a field stop, which corresponds to 0.3% of the light from the target, to send fine pointing information to the field steering mirror in the Origins telescope. An additional MISC Wide Field Imager (WFI) is studied as an upscope option for the Origins. MISC-WFI offers a wide field imaging (3 \u2032 \u00d7 3 \u2032 ) and low-resolution spectroscopic capability with filters and grating-prisms (grisms) covering 5 to 28 \u03bcm. The imaging capability of the MISC-WFI will be used for general science objectives. The low-resolution spectroscopic capability in MISC-WFI with a resolving power R ( = \u03bb / \u0394\u03bb) of a few hundreds will be used to measure the mid-infrared dust features and ionic lines at z up to \u223c1 in the Origins mission's Rise of Metals and Black Hole Feedback programs. The MISC-WFI also serves as a focal plane pointing and guiding instrument for the observatory, including when the MISC-T channel is performing its exoplanet spectroscopy observations.
",
"doi": "10.1117/1.jatis.7.1.011013",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2021-03-11",
"series_number": "01",
"volume": "7",
"issue": "01",
"pages": "1-27"
},
{
"id": "authors:fzww8-g0b39",
"collection": "authors",
"collection_id": "fzww8-g0b39",
"cite_using_url": "https://authors.library.caltech.edu/records/fzww8-g0b39",
"type": "article",
"title": "JWST Noise Floor. II. Systematic Error Sources in JWST NIRCam Time Series",
"author": [
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Misselt",
"given_name": "Karl"
},
{
"family_name": "Don",
"given_name": "Kenneth"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Beatty",
"given_name": "Thomas",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Nikolov",
"given_name": "Nikolay",
"orcid": "0000-0002-6500-3574"
},
{
"family_name": "Kelly",
"given_name": "Douglas"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "The James Webb Space Telescope (JWST) holds great promise for characterizing atmospheres of transiting exoplanets, potentially providing insights into Earth-sized planets within the habitable zones of M-dwarf host stars if photon-limited performance can be achieved. Here, we discuss the systematic error sources that are expected to be present in grism time-series observations with the NIRCam instrument. We find that pointing jitter and high-gain antenna moves in addition to the detectors' subpixel crosshatch patterns will produce relatively small variations (less than 6 parts per million, ppm). The time-dependent aperture losses due to thermal instabilities in the optics can also be kept to below 2 ppm. To achieve these low noise values, it is important to employ a sufficiently large (more than 11) extraction aperture. Persistence due to charge-trapping will have a minor (less than 3 ppm) effect on the time series 20 minutes into an exposure and is expected to play a much smaller role than it does for the Hubble Space Telescope WFC3 detectors. We expect detector temperature fluctuations to contribute less than 3 ppm. In total, our estimated noise floor from known systematic error sources is only 9 ppm per visit. We urge caution, however, because unknown systematic error sources could be present in flight and will only be measurable on astrophysical sources such as quiescent stars. We find that reciprocity failure may introduce a perennial instrument offset at the 40 ppm level, so corrections may be needed when a multi-instrument multi-observatory spectrum is stitched together over wide wavelength ranges.
",
"doi": "10.3847/1538-3881/abd8d4",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-02-11",
"series_number": "3",
"volume": "161",
"issue": "3",
"pages": "115"
},
{
"id": "authors:rs7ww-w5m15",
"collection": "authors",
"collection_id": "rs7ww-w5m15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210125-121646242",
"type": "article",
"title": "Origins Space Telescope: baseline mission concept",
"author": [
{
"family_name": "Leisawitz",
"given_name": "David",
"orcid": "0000-0003-1000-2547",
"clpid": "Leisawitz-David-T"
},
{
"family_name": "Amatucci",
"given_name": "Edward G."
},
{
"family_name": "Allen",
"given_name": "Lynn N."
},
{
"family_name": "Arenberg",
"given_name": "Jonathan W."
},
{
"family_name": "Armus",
"given_name": "Lee",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-Lee"
},
{
"family_name": "Battersby",
"given_name": "Cara",
"orcid": "0000-0002-6073-9320"
},
{
"family_name": "Bauer",
"given_name": "James M.",
"orcid": "0000-0001-9542-0953"
},
{
"family_name": "Beltran",
"given_name": "Porfirio"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206"
},
{
"family_name": "Burgarella",
"given_name": "Denis"
},
{
"family_name": "Carter",
"given_name": "Ruth C."
},
{
"family_name": "Chi",
"given_name": "Danny"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-Asantha"
},
{
"family_name": "Corsetti",
"given_name": "James A."
},
{
"family_name": "De Beck",
"given_name": "Elvire"
},
{
"family_name": "Dewell",
"given_name": "Larry D."
},
{
"family_name": "DiPirro",
"given_name": "Michael J."
},
{
"family_name": "East",
"given_name": "Matthew"
},
{
"family_name": "Edgington",
"given_name": "Samantha"
},
{
"family_name": "Ennico",
"given_name": "Kimberly",
"orcid": "0000-0002-8847-8492"
},
{
"family_name": "Fantano",
"given_name": "Louis G."
},
{
"family_name": "Folta",
"given_name": "David C."
},
{
"family_name": "Generie",
"given_name": "Joseph A."
},
{
"family_name": "Granger",
"given_name": "Zachary A."
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Griffiths",
"given_name": "Alex"
},
{
"family_name": "Harpole",
"given_name": "George M."
},
{
"family_name": "Helmich",
"given_name": "Frank P."
},
{
"family_name": "Howard",
"given_name": "Joseph M."
},
{
"family_name": "Jamison",
"given_name": "Tracee L."
},
{
"family_name": "Kaltenegger",
"given_name": "Lisa",
"orcid": "0000-0002-0436-1802"
},
{
"family_name": "Kataria",
"given_name": "Tiffany",
"orcid": "0000-0003-3759-9080",
"clpid": "Kataria-Tiffany"
},
{
"family_name": "Lawrence",
"given_name": "Charles R.",
"clpid": "Lawrence-Charles-R"
},
{
"family_name": "Meixner",
"given_name": "Margaret"
},
{
"family_name": "Mooney",
"given_name": "Ted"
},
{
"family_name": "Moseley",
"given_name": "Samuel H."
},
{
"family_name": "Neff",
"given_name": "Susan G."
},
{
"family_name": "Nguyen",
"given_name": "Thanh"
},
{
"family_name": "Nordt",
"given_name": "Alison A."
},
{
"family_name": "Petach",
"given_name": "Michael B."
},
{
"family_name": "Petro",
"given_name": "Susanna"
},
{
"family_name": "Pope",
"given_name": "Alexandra",
"orcid": "0000-0001-8592-2706"
},
{
"family_name": "Ramspacker",
"given_name": "Daniel"
},
{
"family_name": "Rao",
"given_name": "Alison"
},
{
"family_name": "Sakon",
"given_name": "Itsuki",
"orcid": "0000-0001-7641-5497"
},
{
"family_name": "Sandstrom",
"given_name": "Karin",
"orcid": "0000-0002-4378-8534"
},
{
"family_name": "Scott",
"given_name": "Douglas",
"orcid": "0000-0002-6878-9840"
},
{
"family_name": "Seals",
"given_name": "Lenward T."
},
{
"family_name": "Sheth",
"given_name": "Kartik J.",
"orcid": "0000-0002-5496-4118"
},
{
"family_name": "Tompkins",
"given_name": "Steven D."
},
{
"family_name": "Webster",
"given_name": "Cassandra M."
},
{
"family_name": "Wiedner",
"given_name": "Martina C.",
"orcid": "0000-0003-3912-7095"
},
{
"family_name": "Wright",
"given_name": "Edward L.",
"orcid": "0000-0001-5058-1593"
},
{
"family_name": "Wu",
"given_name": "Chi K."
},
{
"family_name": "Zmuidzinas",
"given_name": "Jonas",
"orcid": "0000-0002-3330-5439",
"clpid": "Zmuidzinas-J"
},
{
"family_name": "Beaman",
"given_name": "Bob G."
},
{
"family_name": "Bell",
"given_name": "Raymond M."
},
{
"family_name": "Bergin",
"given_name": "Edward"
},
{
"family_name": "Bolognese",
"given_name": "Jeffrey A."
},
{
"family_name": "Bradford",
"given_name": "Charles M.",
"orcid": "0000-0001-5261-7094",
"clpid": "Bradford-Charles-M"
},
{
"family_name": "Bradley",
"given_name": "Damon C."
},
{
"family_name": "Carey",
"given_name": "Sean J.",
"orcid": "0000-0002-0221-6871"
},
{
"family_name": "D'Asto",
"given_name": "Tom"
},
{
"family_name": "Denis",
"given_name": "Kevin L."
},
{
"family_name": "Derkacz",
"given_name": "Christopher"
},
{
"family_name": "Earle",
"given_name": "C. Paul"
},
{
"family_name": "Feller",
"given_name": "Gregory"
},
{
"family_name": "Fortney",
"given_name": "Jonathan",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Gavares",
"given_name": "Benjamin J."
},
{
"family_name": "Gerin",
"given_name": "Maryvonne"
},
{
"family_name": "Harvey",
"given_name": "Keith"
},
{
"family_name": "Hilliard",
"given_name": "Lawrence M."
},
{
"family_name": "Jacoby",
"given_name": "Michael S."
},
{
"family_name": "Jamil",
"given_name": "Anisa"
},
{
"family_name": "Knight",
"given_name": "J. Scott"
},
{
"family_name": "Knollenberg",
"given_name": "Perry J."
},
{
"family_name": "Lightsey",
"given_name": "Paul A."
},
{
"family_name": "Lipscy",
"given_name": "Sarah J."
},
{
"family_name": "Mamajek",
"given_name": "Eric",
"orcid": "0000-0003-2008-1488",
"clpid": "Mamajek-Eric-E"
},
{
"family_name": "Martins",
"given_name": "Gregory E."
},
{
"family_name": "Mather",
"given_name": "John C."
},
{
"family_name": "Melnick",
"given_name": "Gary J."
},
{
"family_name": "Milam",
"given_name": "Stefanie N."
},
{
"family_name": "Narayanan",
"given_name": "Desika",
"orcid": "0000-0002-7064-4309"
},
{
"family_name": "Olson",
"given_name": "Jeffrey R."
},
{
"family_name": "Padgett",
"given_name": "Deborah L.",
"orcid": "0000-0001-5334-5107"
},
{
"family_name": "Pohner",
"given_name": "John"
},
{
"family_name": "Pontoppidan",
"given_name": "Klaus",
"orcid": "0000-0001-7552-1562"
},
{
"family_name": "Roellig",
"given_name": "Thomas L."
},
{
"family_name": "Sandin",
"given_name": "Carly"
},
{
"family_name": "Sokolsky",
"given_name": "Larry"
},
{
"family_name": "Staguhn",
"given_name": "Johannes G.",
"orcid": "0000-0002-8437-0433"
},
{
"family_name": "Steeves",
"given_name": "John B.",
"clpid": "Steeves-John-B"
},
{
"family_name": "Stevenson",
"given_name": "Kevin B.",
"orcid": "0000-0002-7352-7941"
},
{
"family_name": "Stoneking",
"given_name": "Eric T."
},
{
"family_name": "Su",
"given_name": "Kate",
"orcid": "0000-0002-3532-5580"
},
{
"family_name": "Tajdaran",
"given_name": "Kiarash"
},
{
"family_name": "Vieira",
"given_name": "Joaquin D."
}
],
"abstract": "The Origins Space Telescope will trace the history of our origins from the time dust and heavy elements permanently altered the cosmic landscape to present-day life. How did galaxies evolve from the earliest galactic systems to those found in the Universe today? How do habitable planets form? How common are life-bearing worlds? To answer these alluring questions, Origins will operate at mid- and far-infrared (IR) wavelengths and offer powerful spectroscopic instruments and sensitivity three orders of magnitude better than that of the Herschel Space Observatory, the largest telescope flown in space to date. We describe the baseline concept for Origins recommended to the 2020 US Decadal Survey in Astronomy and Astrophysics. The baseline design includes a 5.9-m diameter telescope cryocooled to 4.5 K and equipped with three scientific instruments. A mid-infrared instrument (Mid-Infrared Spectrometer and Camera Transit spectrometer) will measure the spectra of transiting exoplanets in the 2.8 to 20\u2009\u2009\u03bcm wavelength range and offer unprecedented spectrophotometric precision, enabling definitive exoplanet biosignature detections. The far-IR imager polarimeter will be able to survey thousands of square degrees with broadband imaging at 50 and 250\u2009\u2009\u03bcm. The Origins Survey Spectrometer will cover wavelengths from 25 to 588\u2009\u2009\u03bcm, making wide-area and deep spectroscopic surveys with spectral resolving power R\u2009\u2009\u223c\u2009\u2009300, and pointed observations at R\u2009\u2009\u223c\u2009\u200940,000 and 300,000 with selectable instrument modes. Origins was designed to minimize complexity. The architecture is similar to that of the Spitzer Space Telescope and requires very few deployments after launch, while the cryothermal system design leverages James Webb Space Telescope technology and experience. A combination of current-state-of-the-art cryocoolers and next-generation detector technology will enable Origins' natural background-limited sensitivity.",
"doi": "10.1117/1.jatis.7.1.011002",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2021-01-06",
"series_number": "1",
"volume": "7",
"issue": "1",
"pages": "Art. No. 011002"
},
{
"id": "authors:726gr-9sf85",
"collection": "authors",
"collection_id": "726gr-9sf85",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201208-105039183",
"type": "article",
"title": "Transmission Spectroscopy for the Warm Sub-Neptune HD 3167c: Evidence for Molecular Absorption and a Possible High-metallicity Atmosphere",
"author": [
{
"family_name": "Mikal-Evans",
"given_name": "Thomas",
"orcid": "0000-0001-5442-1300",
"clpid": "Mikal-Evans-Thomas"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891"
},
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498"
},
{
"family_name": "Kreidberg",
"given_name": "Laura",
"orcid": "0000-0003-0514-1147"
},
{
"family_name": "Moses",
"given_name": "Julie",
"orcid": "0000-0002-8837-0035"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456"
},
{
"family_name": "Thorngren",
"given_name": "Daniel",
"orcid": "0000-0002-5113-8558"
},
{
"family_name": "Molli\u00e8re",
"given_name": "Paul",
"orcid": "0000-0003-4096-7067"
},
{
"family_name": "Hardegree-Ullman",
"given_name": "Kevin K.",
"orcid": "0000-0003-3702-0382",
"clpid": "Hardegree-Ullman-Kevin-K"
},
{
"family_name": "Brewer",
"given_name": "John",
"orcid": "0000-0002-9873-1471"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-Jessie-L"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-David-R"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X"
},
{
"family_name": "Dressing",
"given_name": "Courtney",
"orcid": "0000-0001-8189-0233"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Gorjian",
"given_name": "Varoujan",
"orcid": "0000-0002-8990-2101",
"clpid": "Gorjian-Varoujan"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hirsch",
"given_name": "Lea A.",
"orcid": "0000-0001-8058-7443"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Howell",
"given_name": "Steve B.",
"orcid": "0000-0002-2532-2853"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073"
},
{
"family_name": "Kosiarek",
"given_name": "Molly R.",
"orcid": "0000-0002-6115-4359"
},
{
"family_name": "Krick",
"given_name": "Jessica",
"orcid": "0000-0002-2413-5976",
"clpid": "Krick-Jessica-E"
},
{
"family_name": "Livingston",
"given_name": "John H.",
"orcid": "0000-0002-4881-3620"
},
{
"family_name": "Lothringer",
"given_name": "Joshua D.",
"orcid": "0000-0003-3667-8633"
},
{
"family_name": "Morales",
"given_name": "Farisa Y.",
"orcid": "0000-0001-9414-3851",
"clpid": "Morales-Farisa-Y"
},
{
"family_name": "Petigura",
"given_name": "Erik A.",
"orcid": "0000-0003-0967-2893"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062"
},
{
"family_name": "Werner",
"given_name": "Michael",
"clpid": "Werner-Michael-W"
}
],
"abstract": "We present a transmission spectrum for the warm (500\u2212600 K) sub-Neptune HD 3167c obtained using the Hubble Space Telescope Wide Field Camera 3 infrared spectrograph. We combine these data, which span the 1.125\u20131.643 \u03bcm wavelength range, with broadband transit measurements made using Kepler/K2 (0.6\u20130.9 \u03bcm) and Spitzer/IRAC (4\u20135 \u03bcm). We find evidence for absorption by at least one of H\u2082O, HCN, CO\u2082, and CH\u2084 (Bayes factor 7.4; 2.5\u03c3 significance), although the data precision does not allow us to unambiguously discriminate between these molecules. The transmission spectrum rules out cloud-free hydrogen-dominated atmospheres with metallicities \u2264100\u00d7 solar at >5.8\u03c3 confidence. In contrast, good agreement with the data is obtained for cloud-free models assuming metallicities >700\u00d7 solar. However, for retrieval analyses that include the effect of clouds, a much broader range of metallicities (including subsolar) is consistent with the data, due to the degeneracy with cloud-top pressure. Self-consistent chemistry models that account for photochemistry and vertical mixing are presented for the atmosphere of HD 3167c. The predictions of these models are broadly consistent with our abundance constraints, although this is primarily due to the large uncertainties on the latter. Interior structure models suggest that the core mass fraction is >40%, independent of a rock or water core composition, and independent of atmospheric envelope metallicity up to 1000\u00d7 solar. We also report abundance measurements for 15 elements in the host star, showing that it has a very nearly solar composition.",
"doi": "10.3847/1538-3881/abc874",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2021-01",
"series_number": "1",
"volume": "161",
"issue": "1",
"pages": "Art. No. 18"
},
{
"id": "authors:hm8jd-p5x18",
"collection": "authors",
"collection_id": "hm8jd-p5x18",
"cite_using_url": "https://authors.library.caltech.edu/records/hm8jd-p5x18",
"type": "article",
"title": "Mid-infrared detector development for the Origins Space Telescope",
"author": [
{
"family_name": "Roellig",
"given_name": "Thomas L."
},
{
"family_name": "McMurtry",
"given_name": "Craig W.",
"orcid": "0000-0003-1969-4324"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Matsuo",
"given_name": "Taro",
"orcid": "0000-0001-7694-5885"
},
{
"family_name": "Sakon",
"given_name": "Itsuki",
"orcid": "0000-0001-7641-5497"
},
{
"family_name": "Staguhn",
"given_name": "Johannes G.",
"orcid": "0000-0002-8437-0433"
}
],
"abstract": "Mid-infrared detector arrays operating from 2.8 to 20 \u03bcm are baselined in the design of the Origins Space Telescope Mid-Infrared Spectrometer Instrument. This instrument is designed to detect and measure the spectral signatures of gases of biogenic origin in the atmospheres of exoplanets as they transit their host stars. In order to make these detections, the detector array's pixels need to have high-signal stability when exposed to a constant flux in multiple time-series integration over a typical transit time of a few hours. With the use of a densified pupil spectrometer design, pointing effects can be mitigated because pointing variations do not displace spectra on the detector and each wavelength of light is averaged over a large number of pixels, giving good spectrophotometric stabilities. The current state-of-the-art detector arrays do not achieve these stabilities, although with a feasible development program this level of performance should be achievable. Three detector technologies are under consideration for this development, HgCdTe arrays, Si:As impurity band conduction arrays, and transition edge superconductor bolometer arrays. We primarily treat the HgCdTe technology development, but also introduce the paths forward for the other two technologies. After a few years-long investigative programs, a down-select will be undertaken to select the flight technology.
",
"doi": "10.1117/1.jatis.6.4.041503",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2020-12-17",
"series_number": "04",
"volume": "6",
"issue": "04",
"pages": "1-13"
},
{
"id": "authors:p3gm3-t4873",
"collection": "authors",
"collection_id": "p3gm3-t4873",
"cite_using_url": "https://authors.library.caltech.edu/records/p3gm3-t4873",
"type": "article",
"title": "JWST Noise Floor. I. Random Error Sources in JWST NIRCam Time Series",
"author": [
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Leisenring",
"given_name": "Jarron",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Misselt",
"given_name": "Karl"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "McElwain",
"given_name": "Michael W.",
"orcid": "0000-0003-0241-8956"
},
{
"family_name": "Beatty",
"given_name": "Thomas",
"orcid": "0000-0002-9539-4203"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "James Webb Space Telescope (JWST) transmission and emission spectra will provide invaluable glimpses of transiting exoplanet atmospheres, including possible biosignatures. This promising science from JWST, however, will require exquisite precision and understanding of systematic errors that can impact the time series of planets crossing in front of and behind their host stars. Here, we provide estimates of the random noise sources affecting JWST Near-Infrared Camera (NIRCam) time-series data on the integration-to-integration level. We find that 1/f noise can limit the precision of grism time series for two groups (230\u20131000 ppm depending on the extraction method and extraction parameters), but will average down like the square root of N frames/reads. The current NIRCam grism time-series mode is especially affected by 1/f noise because its GRISMR dispersion direction is parallel to the detector fast-read direction, but could be alleviated in the GRISMC direction. Care should be taken to include as many frames as possible per visit to reduce this 1/f noise source: thus, we recommend the smallest detector subarray sizes one can tolerate, four output channels, and readout modes that minimize the number of skipped frames (RAPID or BRIGHT2). We also describe a covariance-weighting scheme that can significantly lower the contributions from 1/f noise as compared to sum extraction. We evaluate the noise introduced by pre-amplifier offsets, random telegraph noise, and high dark current resistor capacitor (RC) pixels and find that these are correctable below 10 ppm once background subtraction and pixel masking are performed. We explore systematic error sources in a companion paper.
",
"doi": "10.3847/1538-3881/abb811",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2020-10-29",
"series_number": "5",
"volume": "160",
"issue": "5",
"pages": "231"
},
{
"id": "authors:k0htx-0qc69",
"collection": "authors",
"collection_id": "k0htx-0qc69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190916-075850280",
"type": "article",
"title": "Water Vapor and Clouds on the Habitable-zone Sub-Neptune Exoplanet K2-18b",
"author": [
{
"family_name": "Benneke",
"given_name": "Bj\u00f6rn",
"orcid": "0000-0001-5578-1498",
"clpid": "Benneke-B"
},
{
"family_name": "Wong",
"given_name": "Ian",
"orcid": "0000-0001-9665-8429",
"clpid": "Wong-Ian"
},
{
"family_name": "Piaulet",
"given_name": "Caroline",
"clpid": "Piaulet-C"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Lothringer",
"given_name": "Joshua",
"orcid": "0000-0003-3667-8633",
"clpid": "Lothringer-J-D"
},
{
"family_name": "Morley",
"given_name": "Caroline V.",
"orcid": "0000-0002-4404-0456",
"clpid": "Morley-C-V"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-I-J-M"
},
{
"family_name": "Gao",
"given_name": "Peter",
"orcid": "0000-0002-8518-9601",
"clpid": "Gao-Peter"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Dressing",
"given_name": "Courtney",
"orcid": "0000-0001-8189-0233",
"clpid": "Dressing-C-D"
},
{
"family_name": "Dragomir",
"given_name": "Diana",
"orcid": "0000-0003-2313-467X",
"clpid": "Dragomir-D"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "McCullough",
"given_name": "Peter R.",
"orcid": "0000-0001-9165-9799",
"clpid": "McCullough-P-R"
},
{
"family_name": "Kempton",
"given_name": "Eliza M.-R.",
"orcid": "0000-0002-1337-9051",
"clpid": "Kempton-E-M-R"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-J-J"
},
{
"family_name": "Fraine",
"given_name": "Jonathan",
"orcid": "0000-0003-0910-5805",
"clpid": "Fraine-J-D"
}
],
"abstract": "Results from the Kepler mission indicate that the occurrence rate of small planets (<3 R\u2295) in the habitable zone of nearby low-mass stars may be as high as 80%. Despite this abundance, probing the conditions and atmospheric properties on any habitable-zone planet is extremely difficult and has remained elusive to date. Here, we report the detection of water vapor and the likely presence of liquid and icy water clouds in the atmosphere of the 2.6 R \u2295 habitable-zone planet K2-18b. The simultaneous detection of water vapor and clouds in the mid-atmosphere of K2-18b is particularly intriguing because K2-18b receives virtually the same amount of total insolation from its host star (1368^(+114)_(-107) W m\u207b\u00b2) as the Earth receives from the Sun (1361 W m\u207b\u00b2), resulting in the right conditions for water vapor to condense and explain the detected clouds. In this study we observed nine transits of K2-18b using Hubble Space Telescope/WFC3 in order to achieve the necessary sensitivity to detect the water vapor, and we supplement this data set with Spitzer and K2 observations to obtain a broader wavelength coverage. While the thick hydrogen-dominated envelope we detect on K2-18b means that the planet is not a true Earth analog, our observations demonstrate that low-mass habitable-zone planets with the right conditions for liquid water are accessible with state-of-the-art telescopes.",
"doi": "10.3847/2041-8213/ab59dc",
"issn": "2041-8213",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2019-12-10",
"series_number": "1",
"volume": "887",
"issue": "1",
"pages": "Art. No. L14"
},
{
"id": "authors:7e7r2-gpy75",
"collection": "authors",
"collection_id": "7e7r2-gpy75",
"cite_using_url": "https://authors.library.caltech.edu/records/7e7r2-gpy75",
"type": "article",
"title": "Photometric Precision of a Si:As Impurity Band Conduction Mid-infrared Detector and Application to Transit Spectroscopy",
"author": [
{
"family_name": "Matsuo",
"given_name": "Taro",
"orcid": "0000-0001-7484-1222"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Johnson",
"given_name": "Roy R."
},
{
"family_name": "Mcmurray",
"given_name": "Robert E.",
"orcid": "0000-0001-7971-5137"
},
{
"family_name": "Roellig",
"given_name": "Thomas L.",
"orcid": "0000-0002-6730-5410"
},
{
"family_name": "Ennico",
"given_name": "Kimberly",
"orcid": "0000-0002-8847-8492"
}
],
"abstract": "Transit spectroscopy is the most promising path toward characterizing nearby terrestrial planets at mid-infrared (3\u201330 \u03bcm) wavelengths in the next 20 yr. The Spitzer Space telescope has achieved moderately good mid-infrared photometric precision in observations of transiting planets, but the intrinsic photometric stability of mid-IR detectors themselves has not been reported in the scientific or technical literature. Here, we evaluated the photometric precision of a James Webb Space Telescope Mid-Infrared Instrument prototype mid-infrared Si:As impurity band conduction detector, using time-series data taken under flood illumination. These measurements of photometric precision were conducted over periods of \u223c10 hr, representative of the time required to observe an exoplanet transit. After selecting multiple sub-regions with a size of 10 \u00d7 10 pixels and compensating for a gain change caused by our warm detector control electronics for the selected sub-regions, we found that the photometric precision was limited to 26.3 ppm at high co-added signal levels due to a gain variation caused by our warm detector control electronics. The photometric precision was improved up to 12.8 ppm after correcting for the gain drift. We also translated the photometric precision to the expected spectro-photometric precision (i.e., relative photometric precision between wavelengths), assuming that an optimized densified pupil spectrograph is used in transit observations. We found that the spectro-photometric precision of an optimized densified pupil spectrograph when used in transit observations is expected to be improved by the square root of the number of pixels per a spectral resolution element. At the high co-added signal levels, the total noise could be reduced down to 7 ppm, which was larger by a factor of 1.3 than the ideal performance that was limited by the Poisson noise and readout noise. The systematic noise hidden behind the simulated transit spectroscopy was 1.7 ppm.",
"doi": "10.1088/1538-3873/ab42f1",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2019-11-04",
"series_number": "1006",
"volume": "131",
"issue": "1006",
"pages": "124502"
},
{
"id": "authors:22gat-ppq03",
"collection": "authors",
"collection_id": "22gat-ppq03",
"cite_using_url": "https://authors.library.caltech.edu/records/22gat-ppq03",
"type": "article",
"title": "A Radial Velocity Survey of Embedded Sources in the Rho Ophiuchi Cluster",
"author": [
{
"family_name": "Sullivan",
"given_name": "Timothy"
},
{
"family_name": "Wilking",
"given_name": "Bruce A.",
"orcid": "0000-0002-5241-8818"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Lisalda",
"given_name": "Lindsey",
"orcid": "0000-0002-5202-1642"
},
{
"family_name": "Gibb",
"given_name": "Erika L.",
"orcid": "0000-0003-0142-5265"
},
{
"family_name": "Ejeta",
"given_name": "Chemeda",
"orcid": "0009-0000-7336-7506"
}
],
"abstract": "We present the results of a radial velocity survey of young stellar objects (YSOs) in early stages of evolution in the core of the L1688 molecular cloud. New and archival spectra obtained with four high-resolution infrared spectrographs were analyzed using Markov chain Monte Carlo techniques that simultaneously fit for the radial velocity, Teff, v sin i, and veiling by comparison with synthetic spectra. The radial velocity distribution for 32 objects, most with Class I or flat-spectrum spectral energy distributions, is marginally Gaussian, with a higher dispersion relative to optical surveys at the 2\u03c3 level. When comparing the results from both proper-motion and radial velocity surveys in L1688, there is a trend for the 1D dispersions to be higher for samples of Class I/flat-spectrum YSOs that reside in the cloud core compared to Class II/III dominated samples, which are located in the lower extinction periphery. In addition, there is a velocity gradient along the major axis of the cloud core that appears more pronounced than that derived from optically visible objects at the cloud edges. If these higher dispersions for Class I/flat-spectrum objects are confirmed by future surveys, this could imply a supervirial state for the less evolved objects in the cloud core and be a signature of the initial collapse and rebound of the cluster as suggested by recent simulations of cluster evolution.
",
"doi": "10.3847/1538-3881/ab24c0",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-07-01",
"series_number": "1",
"volume": "158",
"issue": "1",
"pages": "41"
},
{
"id": "authors:1sp3t-1m936",
"collection": "authors",
"collection_id": "1sp3t-1m936",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190124-122613632",
"type": "article",
"title": "Revisiting the HIP 41378 system with K2 and Spitzer",
"author": [
{
"family_name": "Berardo",
"given_name": "David",
"clpid": "Berardo-D"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-I-J-M"
},
{
"family_name": "Werner",
"given_name": "Michael",
"clpid": "Werner-M-W"
},
{
"family_name": "Petigura",
"given_name": "Erik",
"orcid": "0000-0003-0967-2893",
"clpid": "Petigura-E-A"
},
{
"family_name": "Christiansen",
"given_name": "Jessie",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-J-L"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Dressing",
"given_name": "Courtney",
"orcid": "0000-0001-8189-0233",
"clpid": "Dressing-C-D"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-B-J"
},
{
"family_name": "Gorjian",
"given_name": "Varoujan",
"clpid": "Gorjian-V"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Hardegree-Ullman",
"given_name": "Kevin",
"orcid": "0000-0003-3702-0382",
"clpid": "Hardegree-Ullman-K-K"
},
{
"family_name": "Kane",
"given_name": "Stephen R.",
"orcid": "0000-0002-7084-0529",
"clpid": "Kane-S-R"
},
{
"family_name": "Livingston",
"given_name": "John",
"orcid": "0000-0002-4881-3620",
"clpid": "Livingston-J-H"
},
{
"family_name": "Morales",
"given_name": "Farisa",
"orcid": "0000-0001-9414-3851",
"clpid": "Morales-F-Y"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062",
"clpid": "Schlieder-J-E"
}
],
"abstract": "We present new observations of the multiplanet system HIP 41378, a bright star (V = 8.9, K_s = 7.7) with five known transiting planets. Previous K2 observations showed multiple transits of two Neptune-sized bodies and single transits of three larger planets (R_P = 0.33R_J , 0.47R_J , 0.88R_J ). K2recently observed the system again in Campaign 18 (C18). We observe one new transit each of two of the larger planets d/f, giving maximal orbital periods of 1114/1084 days, as well as integer divisions of these values down to a lower limit of about 50 days. We use all available photometry to determine the eccentricity distributions of HIP 41378 d & f, finding that periods \u227e300 days require non-zero eccentricity. We check for overlapping orbits of planets d and f to constrain their mutual periods, finding that short periods (P < 300 days) for planet f are disfavored. We also observe transits of planets b and c with Spitzer/Infrared Array Camera (IRAC), which we combine with the K2observations to search for transit timing variations (TTVs). We find a linear ephemeris for planet b, but see a significant TTV signal for planet c. The ability to recover the two smaller planets with Spitzer shows that this fascinating system will continue to be detectable with Spitzer, CHEOPS, TESS, and other observatories, allowing us to precisely determine the periods of d and f, characterize the TTVs of planet c, recover the transits of planet e, and further enhance our view of this remarkable dynamical laboratory.",
"doi": "10.3847/1538-3881/ab100c",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2019-05",
"series_number": "5",
"volume": "157",
"issue": "5",
"pages": "Art. No. 185"
},
{
"id": "authors:4f89s-5fy66",
"collection": "authors",
"collection_id": "4f89s-5fy66",
"cite_using_url": "https://authors.library.caltech.edu/records/4f89s-5fy66",
"type": "article",
"title": "Detection of Photospheric Features in the Near-infrared Spectrum of a Class 0 Protostar",
"author": [
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Gully-Santiago",
"given_name": "Michael A.",
"orcid": "0000-0002-4020-3457"
},
{
"family_name": "Barsony",
"given_name": "Mary",
"orcid": "0009-0003-2041-7911"
}
],
"abstract": "We present a near-infrared K-band R \u2243 1500 Keck spectrum of S68N, a Class 0 protostar in the Serpens molecular cloud. The spectrum shows a very red continuum, CO absorption bands, weak or nonexistent atomic metal absorptions, and H2 emission lines. The near-IR H2 emission is consistent with excitation in shocks or by X-rays but not by UV radiation. We model the absorption component as a stellar photosphere plus circumstellar continuum emission with wavelength-dependent extinction. A Markov Chain Monte Carlo analysis shows that the most likely model parameters are consistent with a low-temperature, low-gravity photosphere with significant extinction and no more than modest continuum veiling. Its Teff \u2243 3260 K effective temperature is similar to that of older, more evolved pre-main-sequence stars, but its surface gravity log g \u2243 2.4 cm s\u22122 is approximately 1 dex lower. This implies that the radius of this protostar is a factor of \u223c3 larger than that of 106 year old T Tauri stars. Its low veiling is consistent with a circumstellar disk having intrinsic near-IR emission that is less than or equal to that of more evolved Class I protostars. Along with the high extinction, this suggests that most of the circumstellar material is in a cold envelope, as expected for a Class 0 protostar. This is the first known detection and analysis of a Class 0 protostar absorption spectrum.
",
"doi": "10.3847/1538-4357/aacc6c",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2018-07-20",
"series_number": "1",
"volume": "862",
"issue": "1",
"pages": "85"
},
{
"id": "authors:hkway-b3h11",
"collection": "authors",
"collection_id": "hkway-b3h11",
"cite_using_url": "https://authors.library.caltech.edu/records/hkway-b3h11",
"type": "article",
"title": "Clear and Cloudy Exoplanet Forecasts for JWST: Maps, Retrieved Composition, and Constraints on Formation with MIRI and NIRCam",
"author": [
{
"family_name": "Schlawin",
"given_name": "Everett",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Line",
"given_name": "Michael",
"orcid": "0000-0002-2338-476X"
},
{
"family_name": "Fortney",
"given_name": "Jonathan J.",
"orcid": "0000-0002-9843-4354"
},
{
"family_name": "Rieke",
"given_name": "Marcia",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "The James Webb Space Telescope (JWST) will measure exoplanet transmission and eclipse spectroscopy at unprecedented precisions to better understand planet structure, dynamics, chemistry, and formation. These are essential tools on the march toward biosignature searches on potentially habitable planets. We explore a range of exoplanet atmospheric conditions and forecast the expected results with JWST. We take realistic CHIMERA models that match existing Spitzer and Hubble Space Telescope results and simulate the spectra achievable with the JWST MIRI+NIRCam Guaranteed Time Observations survey, which includes observations of HD 189733 b, WASP-80 b, HAT-P-19 b, WASP-107 b, GJ 436 b, and HAT-P-26 b. We then retrieve atmospheric parameters from these spectra to estimate the precision to which the planets' atmospheric compositions can be measured. We find that emission spectra have well-constrained unimodal solutions but transmission spectra near 10\u00d7 solar abundance and solar C/O ratios can suffer from bimodal solutions. Broad wavelength coverage as well as higher-precision data can resolve bimodal solutions and provide dramatically better atmospheric parameter constraints. We find that metallicities can be measured to within 20%\u2013170%, which approaches the precisions on solar system planets, and C/O ratios can be constrained to \u223c10%\u201360%, assuming that observers can leverage short wavelength data to select the correct solution from the bimodal posteriors. These compositional precisions are sufficient to validate or refute predictions from disk formation models on final atmospheric abundances as long as their history is not erased by planet evolution processes. We also show the extent to which eclipse mapping with JWST is possible on our brightest system HD 189733 b.
",
"doi": "10.3847/1538-3881/aac774",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-07-01",
"series_number": "1",
"volume": "156",
"issue": "1",
"pages": "40"
},
{
"id": "authors:w8m8j-ang16",
"collection": "authors",
"collection_id": "w8m8j-ang16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180328-133305203",
"type": "article",
"title": "Validation and Initial Characterization of the Long-period Planet Kepler-1654 b",
"author": [
{
"family_name": "Beichman",
"given_name": "C. A.",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Giles",
"given_name": "H. A. C.",
"clpid": "Giles-H-A-C"
},
{
"family_name": "Akeson",
"given_name": "R.",
"orcid": "0000-0001-9674-1564",
"clpid": "Akeson-R-L"
},
{
"family_name": "Ciardi",
"given_name": "D.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Christiansen",
"given_name": "J.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-J-L"
},
{
"family_name": "Isaacson",
"given_name": "H.",
"orcid": "0000-0002-0531-1073",
"clpid": "Isaacson-H-T"
},
{
"family_name": "Marcy",
"given_name": "G. M.",
"orcid": "0000-0002-2909-0113",
"clpid": "Marcy-G-W"
},
{
"family_name": "Sinukoff",
"given_name": "E.",
"orcid": "0000-0002-5658-0601",
"clpid": "Sinukoff-E"
},
{
"family_name": "Greene",
"given_name": "T.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Fortney",
"given_name": "J. J.",
"orcid": "0000-0002-9843-4354",
"clpid": "Fortney-J-J"
},
{
"family_name": "Crossfield",
"given_name": "I.",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-I-J-M"
},
{
"family_name": "Hu",
"given_name": "R.",
"clpid": "Hu-R"
},
{
"family_name": "Howard",
"given_name": "A. W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Petigura",
"given_name": "E. A.",
"orcid": "0000-0003-0967-2893",
"clpid": "Petigura-E-A"
},
{
"family_name": "Knutson",
"given_name": "H. A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
}
],
"abstract": "Fewer than 20 transiting Kepler planets have periods longer than one year. Our early search of the Kepler light curves revealed one such system, Kepler-1654b (originally KIC 8410697b), which shows exactly two transit events and whose second transit occurred only five days before the failure of the second of two reaction wheels brought the primary Kepler mission to an end. A number of authors have also examined light curves from the Kepler mission searching for long-period planets and identified this candidate. Starting in 2014 September, we began an observational program of imaging, reconnaissance spectroscopy, and precision radial velocity (RV) measurements that confirm with a high degree of confidence that Kepler-1654b is a bona fide transiting planet orbiting a mature G5V star (T_(eff) = 5580 K, [Fe/H] = \u22120.08) with a semimajor axis of 2.03 au, a period of 1047.84 days, and a radius of 0.82 \u00b1 0.02 R_(Jup). RV measurements using Keck's HIRES spectrometer obtained over 2.5 years set a limit to the planet's mass of <0.5 (3\u03c3) M_(Jup). The bulk density of the planet is similar to that of Saturn or possibly lower. We assess the suitability of temperate gas giants like Kepler-1654b for transit spectroscopy with the James Webb Space Telescope, as their relatively cold equilibrium temperatures (T_(pl) ~ 200 K) make them interesting from the standpoint of exoplanet atmospheric physics. Unfortunately, these low temperatures also make the atmospheric scale heights small and thus transmission spectroscopy challenging. Finally, the long time between transits can make scheduling JWST observations difficult\u2014as is the case with Kepler-1654b.",
"doi": "10.3847/1538-3881/aaaeb6",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2018-04",
"series_number": "4",
"volume": "155",
"issue": "4",
"pages": "Art. No. 158"
},
{
"id": "authors:4614q-h0968",
"collection": "authors",
"collection_id": "4614q-h0968",
"cite_using_url": "https://authors.library.caltech.edu/records/4614q-h0968",
"type": "article",
"title": "The Implications of 3D Thermal Structure on 1D Atmospheric Retrieval",
"author": [
{
"family_name": "Blecic",
"given_name": "Jasmina",
"orcid": "0000-0002-0769-9614"
},
{
"family_name": "Dobbs-Dixon",
"given_name": "Ian",
"orcid": "0000-0002-4989-6501"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
}
],
"abstract": "Using the atmospheric structure from a 3D global radiation-hydrodynamic simulation of HD 189733b and the open-source Bayesian Atmospheric Radiative Transfer (BART) code, we investigate the difference between the secondary-eclipse temperature structure produced with a 3D simulation and the best-fit 1D retrieved model. Synthetic data are generated by integrating the 3D models over the Spitzer , the Hubble Space Telescope ( HST ), and the James Web Space Telescope ( JWST ) bandpasses, covering the wavelength range between 1 and 11\u03bcm where most spectroscopically active species have pronounced features. Using the data from different observing instruments, we present detailed comparisons between the temperature\u2013pressure profiles recovered by BART and those from the 3D simulations. We calculate several averages of the 3D thermal structure and explore which particular thermal profile matches the retrieved temperature structure. We implement two temperature parameterizations that are commonly used in retrieval to investigate different thermal profile shapes. To assess which part of the thermal structure is best constrained by the data, we generate contribution functions for our theoretical model and each of our retrieved models. Our conclusions are strongly affected by the spectral resolution of the instruments included, their wavelength coverage, and the number of data points combined. We also see some limitations in each of the temperature parametrizations, as they are not able to fully match the complex curvatures that are usually produced in hydrodynamic simulations. The results show that our 1D retrieval is recovering a temperature and pressure profile that most closely matches the arithmetic average of the 3D thermal structure. When we use a higher resolution, more data points, and a parametrized temperature profile that allows more flexibility in the middle part of the atmosphere, we find a better match between the retrieved temperature and pressure profile and the arithmetic average. The Spitzer and HST simulated observations sample deep parts of the planetary atmosphere and provide fewer constraints on the temperature and pressure profile, while the JWST observations sample the middle part of the atmosphere, providing a good match with the middle and most complex part of the arithmetic average of the 3D temperature structure.
",
"doi": "10.3847/1538-4357/aa8171",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-10-20",
"series_number": "2",
"volume": "848",
"issue": "2",
"pages": "127"
},
{
"id": "authors:mrc09-kdw59",
"collection": "authors",
"collection_id": "mrc09-kdw59",
"cite_using_url": "https://authors.library.caltech.edu/records/mrc09-kdw59",
"type": "article",
"title": "\u03bb = 2.4 to 5 \u03bcm spectroscopy with the James Webb Space Telescope NIRCam instrument",
"author": [
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Kelly",
"given_name": "Douglas M."
},
{
"family_name": "Stansberry",
"given_name": "John",
"orcid": "0000-0003-2434-5225"
},
{
"family_name": "Leisenring",
"given_name": "Jarron M.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Schlawin",
"given_name": "Everett A.",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Hodapp",
"given_name": "Klaus W.",
"orcid": "0000-0002-1437-4463"
},
{
"family_name": "Rieke",
"given_name": "Marcia J.",
"orcid": "0000-0002-7893-6170"
}
],
"abstract": "The James Webb Space Telescope near-infrared camera (JWST NIRCam) has two 2.\u20322\u00d72.\u20322 fields of view that can be observed with either imaging or spectroscopic modes. Either of two R\u223c1500 grisms with orthogonal dispersion directions can be used for slitless spectroscopy over \u03bb=2.4 to 5.0 \u03bcm in each module, and shorter wavelength observations of the same fields can be obtained simultaneously. We describe the design drivers and parameters of the grisms and present the latest predicted spectroscopic sensitivities, saturation limits, resolving powers, and wavelength coverage values. Simultaneous short wavelength (0.6 to 2.3 \u03bcm) imaging observations of the 2.4 to 5.0 \u03bcm spectroscopic field can be performed in one of several different filter bands, either infocus or defocused via weak lenses internal to the NIRCam. The grisms are available for single-object time-series spectroscopy and wide-field multiobject slitless spectroscopy modes in the first cycle of JWST observations. We present and discuss operational considerations including subarray sizes and data volume limits. Potential scientific uses of the grisms are illustrated with simulated observations of deep extragalactic fields, dark clouds, and transiting exoplanets. Information needed to plan observations using these spectroscopic modes is also provided.
",
"doi": "10.1117/1.jatis.3.3.035001",
"pmcid": "PMC5729281",
"issn": "2329-4124",
"publisher": "SPIE-Intl Soc Optical Eng",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2017-07-17",
"series_number": "03",
"volume": "3",
"issue": "03",
"pages": "1-10"
},
{
"id": "authors:rrthe-5ba37",
"collection": "authors",
"collection_id": "rrthe-5ba37",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170601-135603463",
"type": "article",
"title": "K2-66b and K2-106b: Two Extremely Hot Sub-Neptune-size Planets with High Densities",
"author": [
{
"family_name": "Sinukoff",
"given_name": "Evan",
"orcid": "0000-0002-5658-0601",
"clpid": "Sinukoff-E"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Petigura",
"given_name": "Erik A.",
"orcid": "0000-0003-0967-2893",
"clpid": "Petigura-E-A"
},
{
"family_name": "Fulton",
"given_name": "Benjamin J.",
"orcid": "0000-0003-3504-5316",
"clpid": "Fulton-B-J"
},
{
"family_name": "Crossfield",
"given_name": "Ian J. M.",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-I-J-M"
},
{
"family_name": "Isaacson",
"given_name": "Howard",
"orcid": "0000-0002-0531-1073",
"clpid": "Isaacson-H-T"
},
{
"family_name": "Gonzales",
"given_name": "Erica",
"clpid": "Gonzales-E-J"
},
{
"family_name": "Crepp",
"given_name": "Justin R.",
"orcid": "0000-0003-0800-0593",
"clpid": "Crepp-J-R"
},
{
"family_name": "Brewer",
"given_name": "John M.",
"orcid": "0000-0002-9873-1471",
"clpid": "Brewer-J-M-Astro"
},
{
"family_name": "Hirsch",
"given_name": "Lea",
"orcid": "0000-0001-8058-7443",
"clpid": "Hirsch-L-A"
},
{
"family_name": "Weiss",
"given_name": "Lauren M.",
"orcid": "0000-0002-3725-3058",
"clpid": "Weiss-L-M"
},
{
"family_name": "Ciardi",
"given_name": "David R.",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062",
"clpid": "Schlieder-J-E"
},
{
"family_name": "Benneke",
"given_name": "Bjoern",
"orcid": "0000-0001-5578-1498",
"clpid": "Benneke-B"
},
{
"family_name": "Christiansen",
"given_name": "Jessie L.",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-J-L"
},
{
"family_name": "Dressing",
"given_name": "Courtney D.",
"orcid": "0000-0001-8189-0233",
"clpid": "Dressing-C-D"
},
{
"family_name": "Hansen",
"given_name": "Brad M. S.",
"orcid": "0000-0001-7840-3502",
"clpid": "Hansen-B-M-S"
},
{
"family_name": "Knutson",
"given_name": "Heather A.",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Kosiarek",
"given_name": "Molly",
"orcid": "0000-0002-6115-4359",
"clpid": "Kosiarek-M-R"
},
{
"family_name": "Livingston",
"given_name": "John H.",
"orcid": "0000-0002-4881-3620",
"clpid": "Livingston-J-H"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Rogers",
"given_name": "Leslie A.",
"orcid": "0000-0003-0638-3455",
"clpid": "Rogers-L-A"
},
{
"family_name": "L\u00e9pine",
"given_name": "S\u00e9bastien",
"orcid": "0000-0002-2437-2947",
"clpid": "L\u00e9pine-S"
}
],
"abstract": "We report precise mass and density measurements of two extremely hot sub-Neptune-size planets from the K2 mission using radial velocities, K2 photometry, and adaptive optics imaging. K2-66 harbors a close-in sub-Neptune-sized (2.49_(-0.24)^(+0.34)R_\u2295) planet (K2-66b) with a mass of 21.3 \u00b1 3.6 M_\u2295. Because the star is evolving up the subgiant branch, K2-66b receives a high level of irradiation, roughly twice the main-sequence value. K2-66b may reside within the so-called \"photoevaporation desert,\" a domain of planet size and incident flux that is almost completely devoid of planets. Its mass and radius imply that K2-66b has, at most, a meager envelope fraction (<5%) and perhaps no envelope at all, making it one of the largest planets without a significant envelope. K2-106 hosts an ultra-short-period planet (P = 13.7 hr) that is one of the hottest sub-Neptune-size planets discovered to date. Its radius (1.82_(-0.14)^(+0.20) R_\u2295) and mass (9.0 \u00b1 1.6 M_\u2295) are consistent with a rocky composition, as are all other small ultra-short-period planets with well-measured masses. K2-106 also hosts a larger, longer-period planet (R_p = 2.77_(-0.23^(+0.37)R_\u2295, P = 13.3 days) with a mass less than 24.4 M_\u2295 at 99.7% confidence. K2-66b and K2-106b probe planetary physics in extreme radiation environments. Their high densities reflect the challenge of retaining a substantial gas envelope in such extreme environments.",
"doi": "10.3847/1538-3881/aa725f",
"issn": "1538-3881",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2017-06",
"series_number": "6",
"volume": "153",
"issue": "6",
"pages": "Art. No. 271"
},
{
"id": "authors:r4nmh-9vm75",
"collection": "authors",
"collection_id": "r4nmh-9vm75",
"cite_using_url": "https://authors.library.caltech.edu/records/r4nmh-9vm75",
"type": "article",
"title": "PandExo: A Community Tool for Transiting Exoplanet Science with JWST & HST",
"author": [
{
"family_name": "Batalha",
"given_name": "Natasha E.",
"orcid": "0000-0003-1240-6844"
},
{
"family_name": "Mandell",
"given_name": "Avi",
"orcid": "0000-0002-8119-3355"
},
{
"family_name": "Pontoppidan",
"given_name": "Klaus",
"orcid": "0000-0001-7552-1562"
},
{
"family_name": "Stevenson",
"given_name": "Kevin B.",
"orcid": "0000-0002-7352-7941"
},
{
"family_name": "Lewis",
"given_name": "Nikole K.",
"orcid": "0000-0002-8507-1304"
},
{
"family_name": "Kalirai",
"given_name": "Jason",
"orcid": "0000-0001-9690-4159"
},
{
"family_name": "Earl",
"given_name": "Nick"
},
{
"family_name": "Greene",
"given_name": "Thomas",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Albert",
"given_name": "Lo\u00efc",
"orcid": "0000-0003-0475-9375"
},
{
"family_name": "Nielsen",
"given_name": "Louise D.",
"orcid": "0000-0002-5254-2499"
}
],
"abstract": "As we approach the James Webb Space Telescope (JWST) era, several studies have emerged that aim to (1) characterize how the instruments will perform and (2) determine what atmospheric spectral features could theoretically be detected using transmission and emission spectroscopy. To some degree, all these studies have relied on modeling of JWST's theoretical instrument noise. With under two years left until launch, it is imperative that the exoplanet community begins to digest and integrate these studies into their observing plans, as well as think about how to leverage the Hubble Space Telescope (HST) to optimize JWST observations. To encourage this and to allow all members of the community access to JWST & HST noise simulations, we present here an open-source Python package and online interface for creating observation simulations of all observatory-supported timeseries spectroscopy modes. This noise simulator, called PandExo, relies on some aspects of Space Telescope Science Institute's Exposure Time Calculator, Pandeia. We describe PandExo and the formalism for computing noise sources for JWST. Then we benchmark PandExo's performance against each instrument team's independently written noise simulator for JWST, and previous observations for HST. We find that PandExo is within 10% agreement for HST/WFC3 and for all JWST instruments.",
"doi": "10.1088/1538-3873/aa65b0",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2017-04-11",
"series_number": "976",
"volume": "129",
"issue": "976",
"pages": "064501"
},
{
"id": "authors:y9zqw-snj17",
"collection": "authors",
"collection_id": "y9zqw-snj17",
"cite_using_url": "https://authors.library.caltech.edu/records/y9zqw-snj17",
"type": "article",
"title": "Two NIRCam Channels are Better than One: How JWST Can Do More Science with NIRCam's Short-wavelength Dispersed Hartmann Sensor",
"author": [
{
"family_name": "Schlawin",
"given_name": "E.",
"orcid": "0000-0001-8291-6490"
},
{
"family_name": "Rieke",
"given_name": "M.",
"orcid": "0000-0002-7893-6170"
},
{
"family_name": "Leisenring",
"given_name": "J.",
"orcid": "0000-0002-0834-6140"
},
{
"family_name": "Walker",
"given_name": "L. M."
},
{
"family_name": "Fraine",
"given_name": "J.",
"orcid": "0000-0003-0910-5805"
},
{
"family_name": "Kelly",
"given_name": "D."
},
{
"family_name": "Misselt",
"given_name": "K."
},
{
"family_name": "Greene",
"given_name": "T.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Line",
"given_name": "M.",
"orcid": "0000-0001-6247-8323"
},
{
"family_name": "Lewis",
"given_name": "N.",
"orcid": "0000-0002-8507-1304"
},
{
"family_name": "Stansberry",
"given_name": "J.",
"orcid": "0000-0003-2434-5225"
}
],
"abstract": "The James Webb Space Telescope (JWST) offers unprecedented sensitivity, stability, and wavelength coverage for transiting exoplanet studies, opening up new avenues for measuring atmospheric abundances, structure, and temperature profiles. Taking full advantage of JWST spectroscopy of planets from 0.6 to 28 \u03bcm, however, will require many observations with a combination of the NIRISS, NIRCam, NIRSpec, and MIRI instruments. In this white paper, we discuss a new NIRCam mode (not yet approved or implemented) that can reduce the number of necessary observations to cover the 1.0\u20135.0 \u03bcm wavelength range. Even though NIRCam was designed primarily as an imager, it also includes several grisms for phasing and aligning JWST's 18 hexagonal mirror segments. NIRCam's long-wavelength channel includes grisms that cover 2.4\u20135.0 \u03bcm with a resolving power of R = 1200\u20131550 using two separate configurations. The long-wavelength grisms have already been approved for science operations, including wide field and single object (time series) slitless spectroscopy. We propose a new mode that will simultaneously measure spectra for science targets in the 1.0\u20132.0 \u03bcm range using NIRCam's short-wavelength channel. This mode, if approved, would take advantage of NIRCam's Dispersed Hartmann Sensor (DHS), which produces 10 spatially separated spectra per source at R \u223c 300. We discuss the added benefit of the DHS in constraining abundances in exoplanet atmospheres as well as its ability to observe the brightest systems. The DHS essentially comes for free (at no time cost) with any NIRCam long-wavelength grism observation, but the detector integration parameters have to be selected to ensure that the long-wavelength grism observations do not saturate and that JWST data volume downlink constraints are not violated. Combining both of NIRCam's channels will maximize the science potential of JWST, which is a limited life observatory.",
"doi": "10.1088/1538-3873/129/971/015001",
"issn": "0004-6280",
"publisher": "IOP Publishing",
"publication": "Publications of the Astronomical Society of the Pacific",
"publication_date": "2016-11-28",
"series_number": "971",
"volume": "129",
"issue": "971",
"pages": "015001"
},
{
"id": "authors:zbzyf-2yv16",
"collection": "authors",
"collection_id": "zbzyf-2yv16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161012-073815704",
"type": "article",
"title": "Spitzer Observations of Exoplanets Discovered with The Kepler K2 Mission",
"author": [
{
"family_name": "Beichman",
"given_name": "Charles",
"orcid": "0000-0002-5627-5471",
"clpid": "Beichman-C-A"
},
{
"family_name": "Livingston",
"given_name": "John",
"clpid": "Livingston-J-M"
},
{
"family_name": "Werner",
"given_name": "Michael",
"clpid": "Werner-M-W"
},
{
"family_name": "Gorjian",
"given_name": "Varoujan",
"clpid": "Gorjian-V"
},
{
"family_name": "Krick",
"given_name": "Jessica",
"clpid": "Krick-J-E"
},
{
"family_name": "Deck",
"given_name": "Katherine",
"clpid": "Deck-K-M"
},
{
"family_name": "Knutson",
"given_name": "Heather",
"orcid": "0000-0002-5375-4725",
"clpid": "Knutson-H-A"
},
{
"family_name": "Wong",
"given_name": "Ian",
"orcid": "0000-0001-9665-8429",
"clpid": "Wong-Ian"
},
{
"family_name": "Petigura",
"given_name": "Erik",
"orcid": "0000-0003-0967-2893",
"clpid": "Petigura-E-A"
},
{
"family_name": "Christiansen",
"given_name": "Jessie",
"orcid": "0000-0002-8035-4778",
"clpid": "Christiansen-J-L"
},
{
"family_name": "Ciardi",
"given_name": "David",
"orcid": "0000-0002-5741-3047",
"clpid": "Ciardi-D-R"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Schlieder",
"given_name": "Joshua E.",
"orcid": "0000-0001-5347-7062",
"clpid": "Schlieder-J-E"
},
{
"family_name": "Line",
"given_name": "Mike",
"orcid": "0000-0002-2338-476X",
"clpid": "Line-M-R"
},
{
"family_name": "Crossfield",
"given_name": "Ian",
"orcid": "0000-0002-1835-1891",
"clpid": "Crossfield-I-J-M"
},
{
"family_name": "Howard",
"given_name": "Andrew W.",
"orcid": "0000-0001-8638-0320",
"clpid": "Howard-A-W"
},
{
"family_name": "Sinukoff",
"given_name": "Evan",
"orcid": "0000-0002-5658-0601",
"clpid": "Sinukoff-E"
}
],
"abstract": "We have used the Spitzer Space Telescope to observe two transiting planetary systems orbiting low-mass stars discovered in the Kepler K2 mission. The system K2-3 (EPIC 201367065) hosts three planets, while K2-26 (EPIC 202083828) hosts a single planet. Observations of all four objects in these two systems confirm and refine the orbital and physical parameters of the planets. The refined orbital information and more precise planet radii possible with Spitzer will be critical for future observations of these and other K2 targets. For K2-3b we find marginally significant evidence for a transit timing variation between the K2 and Spitzer epochs.",
"doi": "10.3847/0004-637X/822/1/39",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2016-05-01",
"series_number": "1",
"volume": "822",
"issue": "1",
"pages": "Art. No. 39"
},
{
"id": "authors:vkyad-0em55",
"collection": "authors",
"collection_id": "vkyad-0em55",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161018-070312790",
"type": "article",
"title": "Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph",
"author": [
{
"family_name": "Traub",
"given_name": "Wesley A.",
"clpid": "Traub-W-A"
},
{
"family_name": "Breckinridge",
"given_name": "James",
"orcid": "0000-0002-9488-098X",
"clpid": "Breckinridge-J-B"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Guyon",
"given_name": "Olivier",
"orcid": "0000-0002-1097-9908",
"clpid": "Guyon-O"
},
{
"family_name": "Kasdin",
"given_name": "N. Jeremy",
"clpid": "Kasdin-N-J"
},
{
"family_name": "Macintosh",
"given_name": "Bruce",
"orcid": "0000-0003-1212-7538",
"clpid": "Macintosh-B-A"
}
],
"abstract": "The coronagraph instrument (CGI) on the Wide-Field Infrared Survey Telescope will directly image and spectrally characterize planets and circumstellar disks around nearby stars. Here we estimate the expected science yield of the CGI for known radial-velocity (RV) planets and potential circumstellar disks. The science return is estimated for three types of coronagraphs: the hybrid Lyot and shaped pupil are the currently planned designs, and the phase-induced amplitude apodizing complex mask coronagraph is the backup design. We compare the potential performance of each type for imaging as well as spectroscopy. We find that the RV targets can be imaged in sufficient numbers to produce substantial advances in the science of nearby exoplanets. To illustrate the potential for circumstellar disk detections, we estimate the brightness of zodiacal-type disks, which could be detected simultaneously during RV planet observations.",
"doi": "10.1117/1.JATIS.2.1.011020",
"issn": "2329-4124",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"publication": "Journal of Astronomical Telescopes, Instruments, and Systems",
"publication_date": "2016-01",
"series_number": "1",
"volume": "2",
"issue": "1",
"pages": "Art. No. 011020"
},
{
"id": "authors:0wrk7-4v668",
"collection": "authors",
"collection_id": "0wrk7-4v668",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110506-141702853",
"type": "article",
"title": "Ices in the Quiescent IC 5146 Dense Cloud",
"author": [
{
"family_name": "Chiar",
"given_name": "J. E.",
"clpid": "Chiar-J-E"
},
{
"family_name": "Pendleton",
"given_name": "Y. J.",
"clpid": "Pendleton-Y-J"
},
{
"family_name": "Allamandola",
"given_name": "L. J.",
"clpid": "Allamandola-L-J"
},
{
"family_name": "Boogert",
"given_name": "A. C. A.",
"clpid": "Boogert-A-C-A"
},
{
"family_name": "Ennico",
"given_name": "K.",
"orcid": "0000-0002-8847-8492",
"clpid": "Ennico-K"
},
{
"family_name": "Greene",
"given_name": "T. P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Geballe",
"given_name": "T. R.",
"clpid": "Geballe-T-R"
},
{
"family_name": "Keane",
"given_name": "J. V.",
"clpid": "Keane-J-V"
},
{
"family_name": "Lada",
"given_name": "C. J.",
"clpid": "Lada-C-J"
},
{
"family_name": "Mason",
"given_name": "R. E.",
"clpid": "Maso-R-E"
},
{
"family_name": "Roellig",
"given_name": "T. L.",
"clpid": "Roellig-T-L"
},
{
"family_name": "Sandford",
"given_name": "S. A.",
"clpid": "Sandford-S-A"
},
{
"family_name": "Tielens",
"given_name": "A. G. G. M.",
"clpid": "Tielens-A-G-G-M"
},
{
"family_name": "Werner",
"given_name": "M. W.",
"clpid": "Werner-M-W"
},
{
"family_name": "Whittet",
"given_name": "D. C. B.",
"clpid": "Whittet-D-C-B"
},
{
"family_name": "Decin",
"given_name": "L.",
"clpid": "Decin-L"
},
{
"family_name": "Eriksson",
"given_name": "K.",
"clpid": "Eriksson-K"
}
],
"abstract": "This paper presents spectra in the 2 to 20 \u03bcm range of quiescent cloud material located in the IC 5146 cloud complex. The spectra were obtained with NASA's Infrared Telescope Facility SpeX instrument and the Spitzer Space Telescope's Infrared Spectrometer. We use these spectra to investigate dust and ice absorption features in pristine regions of the cloud that are unaltered by embedded stars. We find that the H_2O-ice threshold extinction is 4.03 \u00b1 0.05 mag. Once foreground extinction is taken into account, however, the threshold drops to 3.2 mag, equivalent to that found for the Taurus dark cloud, generally assumed to be the touchstone quiescent cloud against which all other dense cloud and embedded young stellar object observations are compared. Substructure in the trough of the silicate band for two sources is attributed to CH_3OH and NH_3 in the ices, present at the ~2% and ~5% levels, respectively, relative to H_2O-ice. The correlation of the silicate feature with the E(J \u2013 K) color excess is found to follow a much shallower slope relative to lines of sight that probe diffuse clouds, supporting the previous results by Chiar et al.",
"doi": "10.1088/0004-637X/731/1/9",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2011-04-10",
"series_number": "1",
"volume": "731",
"issue": "1",
"pages": "Art. No. 9"
},
{
"id": "authors:h6327-v2v46",
"collection": "authors",
"collection_id": "h6327-v2v46",
"cite_using_url": "https://authors.library.caltech.edu/records/h6327-v2v46",
"type": "article",
"title": "High-Resolution Near-Infrared Spectroscopy of FUors and FUor-Like Stars",
"author": [
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Aspin",
"given_name": "Colin",
"orcid": "0000-0001-6601-8906"
},
{
"family_name": "Reipurth",
"given_name": "Bo",
"orcid": "0000-0001-8174-1932"
}
],
"abstract": "We present new high-resolution (R \u2243 18, 000) near-infrared spectroscopic observations of a sample of classical FU Orionis stars (FUors) and other young stars with FUor characteristics that are sources of Herbig–Haro (HH) flows. Spectra are presented for the region λ = 2.203–2.236 μm which is rich in absorption lines sensitive to both effective temperatures and surface gravities of stars. Both FUors and FUor-like stars show numerous broad and weak-unidentified spectral features in this region. Spectra of the 2.280–2.300 μm region are also presented, with the 2.2935 μm v = 2–0 CO absorption bandhead being clearly the strongest feature seen in the spectra of all FUors and FUor-like stars. A cross-correlation analysis shows that FUor and FUor-like spectra in the 2.203–2.236 μm region are not consistent with late-type dwarfs, giants, nor embedded protostars. The cross-correlations also show that the observed FUor-like HH energy sources have spectra that are substantively similar to those of FUors. Both object groups also have similar near-infrared colors. The large line widths and double-peaked nature of the spectra of the FUor-like stars are consistent with the established accretion disk model for FUors, also consistent with their near-infrared colors. It appears that young stars with FUor-like characteristics may be more common than projected from the relatively few known classical FUors.
",
"doi": "10.1088/0004-6256/135/4/1421",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2008-03-10",
"series_number": "4",
"volume": "135",
"issue": "4",
"pages": "1421-1429"
},
{
"id": "authors:0k9tt-r3560",
"collection": "authors",
"collection_id": "0k9tt-r3560",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091028-110429977",
"type": "article",
"title": "The Relationship between the Optical Depth of the 9.7 \u03bcm Silicate Absorption Feature and Infrared Differential Extinction in Dense Clouds",
"author": [
{
"family_name": "Chiar",
"given_name": "J. E.",
"clpid": "Chiar-J-E"
},
{
"family_name": "Ennico",
"given_name": "K.",
"orcid": "0000-0002-8847-8492",
"clpid": "Ennico-K"
},
{
"family_name": "Pendleton",
"given_name": "Y. J.",
"clpid": "Pendleton-Y-J"
},
{
"family_name": "Boogert",
"given_name": "A. C. A.",
"clpid": "Boogert-A-C-A"
},
{
"family_name": "Greene",
"given_name": "T.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Knez",
"given_name": "C.",
"clpid": "Knez-C"
},
{
"family_name": "Lada",
"given_name": "C.",
"clpid": "Lada-C"
},
{
"family_name": "Roellig",
"given_name": "T.",
"clpid": "Roellig-T"
},
{
"family_name": "Tielens",
"given_name": "A. G. G. M.",
"clpid": "Tielens-A-G-G-M"
},
{
"family_name": "Werner",
"given_name": "M.",
"clpid": "Werner-M"
},
{
"family_name": "Whittet",
"given_name": "D. C. B.",
"clpid": "Whittet-D-C-B"
}
],
"abstract": "We have examined the relationship between the optical depth of the 9.7 \u03bcm silicate absorption feature (\u03c4_(9.7)) and the near-infrared color excess, E(J - K_s), in the Serpens, Taurus, IC 5146, Chameleon I, Barnard 59, and Barnard 68 dense clouds/cores. Our data set, based largely on Spitzer IRS spectra, spans E(J - K_s) = 0.3-10 mag (corresponding to visual extinction between about 2 and 60 mag). All lines of sight show the 9.7 \u03bcm silicate feature. Unlike in the diffuse ISM where a tight linear correlation between the 9.7 \u03bcm silicate feature optical depth and the extinction (A_V) is observed, we find that the silicate feature in dense clouds does not show a monotonic increase with extinction. Thus, in dense clouds, \u03c4_(9.7) is not a good measure of total dust column density. With few exceptions, the measured \u03c4_(9.7) values fall well below the diffuse ISM correlation line for E(J - K_s) > 2 mag (A_V > 12 mag). Grain growth via coagulation is a likely cause of this effect.",
"doi": "10.1086/521789",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2007-09-10",
"series_number": "2",
"volume": "666",
"issue": "2",
"pages": "L73-L76"
},
{
"id": "authors:c9kwp-63n48",
"collection": "authors",
"collection_id": "c9kwp-63n48",
"cite_using_url": "https://authors.library.caltech.edu/records/c9kwp-63n48",
"type": "article",
"title": "Hubble Space Telescope NICMOS Observations of NGC 1333: The Ratio of Stars to Substellar Objects",
"author": [
{
"family_name": "Greissl",
"given_name": "Julia"
},
{
"family_name": "Meyer",
"given_name": "Michael R.",
"orcid": "0000-0003-1227-3084"
},
{
"family_name": "Wilking",
"given_name": "Bruce A.",
"orcid": "0000-0002-5241-8818"
},
{
"family_name": "Fanetti",
"given_name": "Tina"
},
{
"family_name": "Schneider",
"given_name": "Glenn",
"orcid": "0000-0002-4511-5966"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Young",
"given_name": "Erick",
"orcid": "0000-0002-6395-4296"
}
],
"abstract": "We present an analysis of NICMOS photometry and low-resolution grism spectroscopy of low-mass stars and substellar objects in the young star-forming region NGC 1333. Our goal is to constrain the ratio of low-mass stars to substellar objects down to 20MJup in the cluster, as well as constrain the cluster initial mass function (IMF) down to 30MJup, in combination with a previous survey of NGC 1333 by Wilking et al. Our survey covers four fields of 51.2\u2033 \u00d7 51.2\u2033, centered on brown dwarf candidates previously identified in Wilking et al. We extend previous work based on the use of a water vapor index for spectral typing to wavelengths accessible with NICMOS on the Hubble Space Telescope. Spectral types were derived for the 14 brightest objects in our fields, ranging from \u2264M0 to M8, which, at the age of the cluster (0.3 Myr), correspond to a range in mass of \u22650.25-0.02 M\u2299. In addition to the spectra, we present an analysis of the color-magnitude diagram using pre-main-sequence evolutionary models of D'Antona & Mazzitelli. Using an extinction-limited sample, we derive the ratio of low-mass stars to brown dwarfs. Comparisons of the observed ratio to that expected from the field IMF of Chabrier indicate that the two results are consistent. We combine our data with those of Wilking et al. to compute the ratio of intermediate-mass stars (0.1-1.0 M\u2299) to low-mass objects (0.03-0.1 M\u2299) in the cluster. We also report the discovery of a faint companion to the previously confirmed brown dwarf ASR 28, as well as a possible outflow surrounding ASR 16. If the faint companion is confirmed as a cluster member, it would have a mass of \u22485MJup (mass ratio 0.15) at a projected distance of 350 AU, similar to that of 2MASS 1207-3923B.",
"doi": "10.1086/510901",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2007-02-21",
"series_number": "4",
"volume": "133",
"issue": "4",
"pages": "1321-1330"
},
{
"id": "authors:nefpb-eep89",
"collection": "authors",
"collection_id": "nefpb-eep89",
"cite_using_url": "https://authors.library.caltech.edu/records/nefpb-eep89",
"type": "article",
"title": "High Spectral Resolution Near-IR Observations of ESO-H\u03b1 279A and 279B",
"author": [
{
"family_name": "Aspin",
"given_name": "Colin",
"orcid": "0000-0001-6601-8906"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
}
],
"abstract": "We present high spectral resolution near-IR observations of the stars ESO-H\u03b1 279A and 279B located in the Serpens star formation complex. ESO-H\u03b1 279A is a known young T Tauri star driving a Herbig-Haro flow, while ESO-H\u03b1 279B is a nearby (8\u2033, 2500 AU) extremely red companion. Previous work has suggested that this is not a physically bound system but a chance alignment of a young star and a background giant. Below, we further investigate the nature of ESO-H\u03b1 279B and probe the emission characteristics of ESO-H\u03b1 279A. We find that ESO-H\u03b1 279B shows many narrow absorption features typical of late-type giant stars and unlike those seen in FU Orionis objects and Herbig-Haro energy sources, the only young stars that exhibit such deep CO absorption. This result confirms that ESO-H\u03b1 279B is a background M-type giant viewed through the molecular cloud hosting ESO-H\u03b1 279A, and therefore, the association of ESO-H\u03b1 279A and 279B is fortuitous. For ESO-H\u03b1 279A we find that the Na doublet lines are broadened and self-absorbed and that the v = 2-0 CO overtone band head is similar in shape to that observed in the young pre-main-sequence object SVS 13 in NGC 1333, and not characteristic of a rotating-disk velocity dispersion. We consider the origin of the CO emission in relation to current models and suggest that it perhaps is more indicative of creation in a wind or funnel flow rather than in the inner hot regions of a circumstellar disk.",
"doi": "10.1086/510133",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2007-01-09",
"series_number": "2",
"volume": "133",
"issue": "2",
"pages": "568-575"
},
{
"id": "authors:aj233-mjr31",
"collection": "authors",
"collection_id": "aj233-mjr31",
"cite_using_url": "https://authors.library.caltech.edu/records/aj233-mjr31",
"type": "article",
"title": "Mid-Infrared Observations of Class I/Flat-Spectrum Systems in Six Nearby Molecular Clouds",
"author": [
{
"family_name": "Haisch,\u00a0Jr.",
"given_name": "Karl\u00a0E."
},
{
"family_name": "Barsony",
"given_name": "Mary",
"orcid": "0009-0003-2041-7911"
},
{
"family_name": "Ressler",
"given_name": "Michael\u00a0E.",
"orcid": "0000-0001-5644-8830"
},
{
"family_name": "Greene",
"given_name": "Thomas\u00a0P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
}
],
"abstract": "We have obtained new mid-infrared observations of 65 Class I/flat-spectrum (FS) objects in the Perseus, Taurus, Chamaeleon I and II, \u03c1 Ophiuchi, and Serpens dark clouds. These objects represent a subset of the young stellar objects (YSOs) from our previous near-infrared multiplicity surveys. We detected 45 out of 48 (94%) of the single sources, 16 out of 16 (100%) of the primary components, and 12 out of 16 (75%) of the secondary/triple components of the binary/multiple objects surveyed. One target, IRS 34, a 0.\u203331 separation FS binary, remains unresolved at near-infrared wavelengths. The composite spectral energy distributions for all of our sample YSOs are either Class I or FS, and in 15 out of 16 multiple systems at least one of the individual components displays a Class I or FS spectral index. However, the occurrence of mixed pairings, such as FS with Class I, FS with Class II, and, in one case, an FS with a Class III (Cha I T33B), is suprisingly frequent. Such behavior is not consistent with that of multiple systems among T Tauri stars (TTSs), where the companion of a classical TTS also tends to be a classical TTS, although other mixed pairings have been previously observed among Class II YSOs. Based on an analysis of the spectral indices of the individual binary components, there appears to be a higher proportion of mixed Class I/FS systems (65%-80%) than that of mixed classical and weak-lined TTSs (25%-40%), demonstrating that the envelopes of Class I/FS systems are rapidly evolving during this evolutionary phase. In general, the individual binary/multiple components suffer very similar extinctions, Av, suggesting that most of the line-of-sight material is either in the foreground of the molecular cloud or circumbinary. We report the discovery of a steep spectral index secondary companion to ISO-Cha I 97, detected for the first time via our mid-infrared observations. In our previous near-infrared imaging survey of binary/multiple Class I and FS YSOs, ISO-Cha I 97 appeared to be single. With a spectral index of \u03b1 \u2265 +3.9, the secondary component of this system is a member of a rare class of very steep spectral index YSOs, those with \u03b1 > +3. Only three such objects have previously been reported, all of which are either Class 0 or Class I.",
"doi": "10.1086/508651",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2006-01",
"series_number": "6",
"volume": "132",
"issue": "6",
"pages": "2675-2684"
},
{
"id": "authors:scc30-2cr48",
"collection": "authors",
"collection_id": "scc30-2cr48",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120918-102317394",
"type": "article",
"title": "A tidally interacting disk in the young triple system WL 20?",
"author": [
{
"family_name": "Barsony",
"given_name": "Mary",
"clpid": "Barsony-M"
},
{
"family_name": "Greene",
"given_name": "Thomas P.",
"orcid": "0000-0002-8963-8056",
"clpid": "Greene-Thomas-P"
},
{
"family_name": "Blake",
"given_name": "Geoffrey A.",
"orcid": "0000-0003-0787-1610",
"clpid": "Blake-G-A"
}
],
"abstract": "We present high-resolution \u03bb = 2.7 mm imaging of the close triple pre-main-sequence system WL 20. Compact dust emission with integrated flux density of 12.9 \u00b1 1.3 mJy is associated with two components of the triple system, WL 20W and WL 20S. No emission above a 3 \u03c3 level of 3.9 mJy is detected toward the third component, WL 20E, which lies 3.\"17 (400 AU) due east in projection from its neighbors. A possibly warped structure of ~0.1 M_\u2609 and \u22643.\"2 extent encompasses WL 20W and WL 20S, which have a projected separation of 2.\"25 (~280 AU) along a north-south axis. This structure is most likely a tidally disrupted disk surrounding WL 20S. New near-infrared spectra of the individual components show a remarkable similarity between the two T Tauri stars of the system: WL 20E has a K7 spectral type (T_eff = 4040 K) with r_K = 0.2, and WL 20W has an M0 spectral type (T_eff = 3800 K) with r_K = 0.2. The spectrum of WL 20S is consistent with that of a source intrinsically similar to WL 20W, with r_K < 0.9, but seen through an A_V = 25 in addition to the A_V = 16.3 to the system as a whole. Taken together, these millimeter and infrared data help explain the peculiar nature of the infrared companion, WL 20S, as resulting from a large enhancement in its dusty, circumstellar environment in relation to its companions.",
"doi": "10.1086/341553",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2002-06-10",
"series_number": "1",
"volume": "572",
"issue": "1",
"pages": "L75-L78"
}
]