[ { "id": "authors:37bdj-n7n51", "collection": "authors", "collection_id": "37bdj-n7n51", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220816-192417168", "type": "monograph", "title": "Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field", "author": [ { "family_name": "Kounkel", "given_name": "Marina", "orcid": "0000-0002-5365-1267", "clpid": "Kounkel-Marina-A" }, { "family_name": "Stassun", "given_name": "Keivan G.", "orcid": "0000-0002-3481-9052", "clpid": "Stassun-Keivan-G" }, { "family_name": "Bouma", "given_name": "Luke G.", "orcid": "0000-0002-0514-5538", "clpid": "Bouma-Luke-G" }, { "family_name": "Covey", "given_name": "Kevin", "orcid": "0000-0001-6914-7797", "clpid": "Covey-Kevin-R" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Curtis", "given_name": "Jason Lee", "orcid": "0000-0002-2792-134X", "clpid": "Curtis-Jason-L" } ], "abstract": "We present a catalog of ~100,000 periodic variable stars in TESS FFI data among members of widely distributed moving groups identified with Gaia in the previous papers in the series. By combining the periods from our catalog attributable to rotation with previously derived rotation periods for benchmark open clusters, we develop an empirical gyrochronology relation of angular momentum evolution that is valid for stars with ages 10-1000 Myr. Excluding stars rotating faster than 2 days, which we find are predominantly binaries, we achieve a typical age precision of ~0.2-0.3 dex and improving at older ages. Importantly, these empirical relations apply to not only FGK-type stars but also M-type stars, due to the angular momentum distribution being much smoother, simpler, continuous and monotonic as compared to the rotation period distribution. As a result, we are also able to begin tracing in fine detail the nature of angular momentum loss in low-mass stars as functions of mass and age. We characterize the stellar variability amplitudes of the cool stars as functions of mass and age, which may correlate with the starspot covering fractions. We also identify pulsating variables among the hotter stars in the catalog, including \u03b4 Scuti, \u03b3 Dor and SPB-type variables. These data represent an important step forward in being able to estimate precise ages of FGK- and M-type stars in the field, starting as early as the pre-main-sequence phase of evolution.", "doi": "10.48550/arXiv.2206.13545", "publisher": "arXiv", "publication_date": "2022-06-27" }, { "id": "authors:rnnv4-10154", "collection": "authors", "collection_id": "rnnv4-10154", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220816-192421369", "type": "monograph", "title": "Spectroscopic Confirmation of a Population of Isolated, Intermediate-Mass YSOs", "author": [ { "family_name": "Kuhn", "given_name": "Michael A.", "orcid": "0000-0002-0631-7514", "clpid": "Kuhn-Michael-A" }, { "family_name": "Saber", "given_name": "Ramzi", "clpid": "Saber-Ramzi" }, { "family_name": "Povich", "given_name": "Matthew S.", "orcid": "0000-0001-9062-3583", "clpid": "Povich-Matthew-S" }, { "family_name": "de Souza", "given_name": "Rafael S.", "orcid": "0000-0001-7207-4584", "clpid": "de-Souza-Rafael-S" }, { "family_name": "Krone-Martins", "given_name": "Alberto", "orcid": "0000-0002-2308-6623", "clpid": "Krone-Martins-Alberto" }, { "family_name": "Ishida", "given_name": "Emille E. O.", "orcid": "0000-0002-0406-076X", "clpid": "Ishida-Emile-E-O" }, { "family_name": "Zucker", "given_name": "Catherine", "orcid": "0000-0002-2250-730X", "clpid": "Zucker-Catherine" }, { "family_name": "Benjamin", "given_name": "Robert A.", "orcid": "0000-0002-8109-2642", "clpid": "Benjamin-Robert-A" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Castro-Ginard", "given_name": "Alfred", "orcid": "0000-0002-9419-3725", "clpid": "Castro-Ginard-Alfred" }, { "family_name": "Zhou", "given_name": "Xingyu", "clpid": "Zhou-Xingyu" } ], "abstract": "Wide-field searches for young stellar objects (YSOs) can place useful constraints on the prevalence of clustered versus distributed star formation. The Spitzer/IRAC Candidate YSO (SPICY) catalog is one of the largest compilations of such objects (~120,000 candidates in the Galactic midplane). Many SPICY candidates are spatially clustered, but, perhaps surprisingly, approximately half the candidates appear spatially distributed. To better characterize this unexpected population and confirm its nature, we obtained Palomar/DBSP spectroscopy for 26 of the optically-bright (G<15 mag) \"isolated\" YSO candidates. We confirm the YSO classifications of all 26 sources based on their positions on the Hertzsprung-Russell diagram, H and Ca II line-emission from over half the sample, and robust detection of infrared excesses. This implies a contamination rate of <10% for SPICY stars that meet our optical selection criteria. Spectral types range from B4 to K3, with A-type stars most common. Spectral energy distributions, diffuse interstellar bands, and Galactic extinction maps indicate moderate to high extinction. Stellar masses range from ~1 to 7 M_\u2299, and the estimated accretion rates, ranging from 3 \u00d7 10\u207b\u2078 to 3 \u00d7 10\u207b\u2077 M_\u2299 yr\u207b\u00b9, are typical for YSOs in this mass range. The 3D spatial distribution of these stars, based on Gaia astrometry, reveals that the \"isolated\" YSOs are not evenly distributed in the Solar neighborhood but are concentrated in kpc-scale dusty Galactic structures that also contain the majority of the SPICY YSO clusters. Thus, the processes that produce large Galactic star-forming structures may yield nearly as many distributed as clustered YSOs.", "doi": "10.48550/arXiv.2206.04090", "publisher": "arXiv", "publication_date": "2022-06-08" }, { "id": "authors:d5a0g-ykq23", "collection": "authors", "collection_id": "d5a0g-ykq23", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220816-183020507", "type": "monograph", "title": "Rotation of Low-Mass Stars in Upper Centaurus Lupus and Lower Centaurus Crux with TESS", "author": [ { "family_name": "Rebull", "given_name": "L. M.", "orcid": "0000-0001-6381-515X", "clpid": "Rebull-Luisa-M" }, { "family_name": "Stauffer", "given_name": "J. R.", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-John-R" }, { "family_name": "Hillenbrand", "given_name": "L. A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Cody", "given_name": "A. M.", "orcid": "0000-0002-3656-6706", "clpid": "Cody-Ann-Marie" }, { "family_name": "Kruse", "given_name": "Ethan", "orcid": "0000-0002-0493-1342", "clpid": "Kruse-Ethan" }, { "family_name": "Powell", "given_name": "Brian P.", "orcid": "0000-0003-0501-2636", "clpid": "Powell-Brian-P" } ], "abstract": "We present stellar rotation rates derived from Transiting Exoplanet Survey Satellite (TESS) light curves for stars in Upper Centaurus-Lupus (UCL; ~136 pc, ~16 Myr) and Lower Centaurus-Crux (LCC; ~115 pc, ~17 Myr). We find spot-modulated periods (P) for ~90% of members. The range of light curve and periodogram shapes echoes that found for other clusters with K2, but fewer multi-period stars may be an indication of different noise characteristics of TESS, or a result of the source selection methods here. The distribution of P as a function of color as a proxy for mass fits nicely in between that for both older and younger clusters observed by K2, with fast rotators found among both the highest and lowest masses probed here, and a well-organized distribution of M star rotation rates. About 13% of the stars have an infrared (IR) excess, suggesting a circumstellar disk; this is well-matched to expectations, given the age of the stars. There is an obvious pile-up of disked M stars at P~2 days, and the pile-up may move to shorter P as the mass decreases. There is also a strong concentration of disk-free M stars at P~2 days, hinting that perhaps these stars have recently freed themselves from their disks. Exploring the rotation rates of stars in UCL/LCC has the potential to help us understand the beginning of the end of the influence of disks on rotation, and the timescale on which the star responds to unlocking.", "doi": "10.48550/arXiv.2205.13083", "publisher": "arXiv", "publication_date": "2022-05-25" }, { "id": "authors:35gs8-ncw89", "collection": "authors", "collection_id": "35gs8-ncw89", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220517-214318858", "type": "monograph", "title": "Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association", "author": [ { "family_name": "Bouma", "given_name": "L. G.", "orcid": "0000-0002-0514-5538", "clpid": "Bouma-Luke-G" }, { "family_name": "Kerr", "given_name": "R.", "orcid": "0000-0002-6549-9792", "clpid": "Kerr-Ronan" }, { "family_name": "Curtis", "given_name": "J. L.", "orcid": "0000-0002-2792-134X", "clpid": "Curtis-Jason-L" }, { "family_name": "Isaacson", "given_name": "H.", "orcid": "0000-0002-0531-1073", "clpid": "Isaacson-Howard-T" }, { "family_name": "Hillenbrand", "given_name": "L. A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Howard", "given_name": "A. W.", "orcid": "0000-0001-8638-0320", "clpid": "Howard-A-W" }, { "family_name": "Kraus", "given_name": "A. L.", "orcid": "0000-0001-9811-568X", "clpid": "Kraus-Adam-L" }, { "family_name": "Bieryla", "given_name": "A.", "orcid": "0000-0001-6637-5401", "clpid": "Bieryla-Allyson" }, { "family_name": "Latham", "given_name": "D. W.", "orcid": "0000-0001-9911-7388", "clpid": "Latham-David-W" }, { "family_name": "Petigura", "given_name": "E. A.", "orcid": "0000-0003-0967-2893", "clpid": "Petigura-Erik-A" }, { "family_name": "Huber", "given_name": "D.", "orcid": "0000-0001-8832-4488", "clpid": "Huber-Daniel" } ], "abstract": "Stellar positions and velocities from Gaia are yielding a new view of open cluster dispersal. Here we present an analysis of a group of stars spanning Cepheus to Hercules, hereafter the Cep-Her complex. The group includes four Kepler Objects of Interest: Kepler-1643 b (2.32 \u00b1 0.14 Earth-radii, 5.3 day orbital period), KOI-7368 b (2.22 \u00b1 0.12 Earth-radii, 6.8 days), KOI-7913 Ab (2.34 \u00b1 0.18 Earth-radii, 24.2 days), and Kepler-1627 Ab (3.85 \u00b1 0.11 Earth-radii, 7.2 days). The latter Neptune-sized planet is in part of the Cep-Her complex called the \u03b4 Lyr cluster (Bouma et al. 2022). Here we focus on the former three systems, which are in other regions of the association. Based on kinematic evidence from Gaia, stellar rotation periods from TESS, and spectroscopy, these three objects are also approximately 40 million years (Myr) old. More specifically, we find that Kepler-1643 is 46\u207a\u2079\u208b\u2087 Myr old, based on its membership in a dense sub-cluster of the complex called RSG-5. KOI-7368 and KOI-7913 are 36\u207a\u00b9\u2070\u208b\u2088 Myr old, and are in a diffuse region that we call CH-2. Based on the transit shapes and high resolution imaging, all three objects are most likely planets, with false positive probabilities of 6 \u00d7 10\u207b\u2079, 4 \u00d7 10\u207b\u00b3, and 1 \u00d7 10\u207b\u2074 for Kepler-1643, KOI-7368, and KOI-7913 respectively. These planets demonstrate that mini-Neptunes with sizes of approximately 2 Earth radii exist at ages of 40 million years.", "doi": "10.48550/arXiv.2205.01112", "publisher": "arXiv", "publication_date": "2022-05-02" }, { "id": "authors:navaw-vkk84", "collection": "authors", "collection_id": "navaw-vkk84", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220517-214301863", "type": "monograph", "title": "Measuring Optical Extinction Towards Young Stellar Objects Using Diffuse Interstellar Bands", "author": [ { "family_name": "Carvalho", "given_name": "Adolfo", "orcid": "0000-0002-9540-853X", "clpid": "Carvalho-Adolfo-S" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" } ], "abstract": "Line-of-sight extinction estimates to well-studied young T Tauri and Herbig Ae/Be stars are based on many different measurements and analysis methods. This has resulted in wide scatter among the published A_V values for the same star. In this work, we discuss the challenges in measuring extinction to actively accreting and especially outbursting young stellar objects (YSOs), and explore a method not previously applied to young stars, utilizing diffuse interstellar bands (DIBs). In early-type stars, narrow correlations exist between DIB equivalent widths and the column density of interstellar material, and therefore the line-of-sight extinction. Here, we measure equivalent widths of the 5780 \u00c5 and 6614 \u00c5 DIB features in a sample of actively accreting YSOs, and apply established DIB--reddening calibrations to derive reddening, and subsequently extinction. We also compare the DIBs-inferred optical line-of-sight extinction values with previous extinction estimates for our sample stars.", "doi": "10.48550/arXiv.2204.06061", "publisher": "arXiv", "publication_date": "2022-04-12" }, { "id": "authors:9n1qk-w2317", "collection": "authors", "collection_id": "9n1qk-w2317", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220517-214248373", "type": "monograph", "title": "Accretion Variability as a Guide to Stellar Mass Assembly", "author": [ { "family_name": "Fischer", "given_name": "William J.", "orcid": "0000-0002-3747-2496", "clpid": "Fischer-William-J" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Herczeg", "given_name": "Gregory J.", "orcid": "0000-0002-7154-6065", "clpid": "Herczeg-Gregory-J" }, { "family_name": "Johnstone", "given_name": "Doug", "orcid": "0000-0002-6773-459X", "clpid": "Johnstone-Doug" }, { "family_name": "K\u00f3sp\u00e1l", "given_name": "\u00c1gnes", "clpid": "K\u00f3sp\u00e1l-\u00c1gnes" }, { "family_name": "Dunham", "given_name": "Michael M.", "orcid": "0000-0003-0749-9505", "clpid": "Dunham-Michael-M" } ], "abstract": "Variable accretion in young stellar objects reveals itself photometrically and spectroscopically over a continuum of timescales and amplitudes. Most dramatic are the large outbursts (e.g., FU Ori, V1647 Ori, and EX Lup type events), but more frequent are the less coherent, smaller burst-like variations in accretion rate. Improving our understanding of time-variable accretion directly addresses the fundamental question of how stars gain their masses. We review variability phenomena, as characterized from observations across the wavelength spectrum, and how those observations probe underlying physical conditions. The diversity of observed lightcurves and spectra at optical and infrared wavelengths defies a simple classification of outbursts and bursts into well-defined categories. Mid-infrared and sub-millimeter wavelengths are sensitive to lower-temperature phenomena, and it is currently unclear if observed flux variations probe similar or distinct physics relative to the shorter wavelengths. We highlight unresolved issues and emphasize the value of spectroscopy, multiwavelength studies, and ultimately patience in using variable accretion to understand stellar mass assembly.", "doi": "10.48550/arXiv.2203.11257", "publisher": "arXiv", "publication_date": "2022-03-21" }, { "id": "authors:3da81-qr804", "collection": "authors", "collection_id": "3da81-qr804", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220517-214244996", "type": "monograph", "title": "The Effect of Molecular Cloud Properties on the Kinematics of Stars Formed in the Trifid Region", "author": [ { "family_name": "Kuhns", "given_name": "Michael A.", "orcid": "0000-0002-0631-7514", "clpid": "Kuhn-Michael-A" }, { "family_name": "Hillenbrand", "given_name": "Lynne A.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Feigelson", "given_name": "Eric D.", "orcid": "0000-0002-5077-6734", "clpid": "Feigelson-Eric-D" }, { "family_name": "Fowler", "given_name": "Ian", "orcid": "0000-0002-4958-8648", "clpid": "Fowler-Ian" }, { "family_name": "Getman", "given_name": "Konstantin V.", "orcid": "0000-0002-6137-8280", "clpid": "Getman-Konstantin-V" }, { "family_name": "Broos", "given_name": "Patrick S.", "orcid": "0000-0002-7872-2025", "clpid": "Broos-Patrick-S" }, { "family_name": "Povich", "given_name": "Matthew S.", "orcid": "0000-0001-9062-3583", "clpid": "Povich-Matthew-S" }, { "family_name": "Gromadzki", "given_name": "Mariusz", "orcid": "0000-0002-1650-1518", "clpid": "Gromadzki-Mariusz" } ], "abstract": "The dynamical states of molecular clouds may affect the properties of the stars they form. In the vicinity of the Trifid Nebula (d = 1180 \u00b1 25 pc), the main star cluster (Trifid Main) lies within an expanding section of the molecular cloud; however, ~0.3 deg to the north (Trifid North), the cloud's velocity structure is more tranquil. We acquired a Chandra X-ray observation to identify pre-main-sequence stars in Trifid North, complementing a previous observation of Trifid Main. In Trifid North, we identified 51 candidate pre-main-sequence stars, of which 13 are high-confidence Trifid members based on Gaia EDR3 parallaxes and proper motions. We also re-analyzed membership of Trifid Main and separated out multiple background stellar associations. Trifid North represents a stellar population ~10% as rich as Trifid Main that formed in a separate part of the cloud. The 1D stellar velocity dispersion in Trifid North (0.6 \u00b1 0.2 km/s) is three times lower than in Trifid Main (1.9 \u00b1 0.2 km/s). Furthermore, in Trifid Main, proper motions indicate that the portion of the star cluster superimposed on the optical nebula is expanding. Expansion of the HII region around the O-star HD 164492A, and the resulting gas expulsion, can explain both the motions of the stars and gas in Trifid Main. Contrary to previous studies, we find no evidence that a cloud-cloud collision triggered star formation in the region.", "doi": "10.48550/arXiv.2203.07382", "publisher": "arXiv", "publication_date": "2022-03-14" }, { "id": "authors:t21jf-jyk53", "collection": "authors", "collection_id": "t21jf-jyk53", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220411-225157319", "type": "monograph", "title": "Illuminating Galaxy Evolution at Cosmic Noon with ISCEA: the Infrared Satellite for Cosmic Evolution Astrophysics", "author": [ { "family_name": "Wang", "given_name": "Yun", "orcid": "0000-0002-4749-2984", "clpid": "Wang-Yun" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-Lee" }, { "family_name": "Benson", "given_name": "Andrew", "orcid": "0000-0001-5501-6008", "clpid": "Benson-Andrew-J" }, { "family_name": "Daddi", "given_name": "Emanuele", "orcid": "0000-0002-3331-9590", "clpid": "Daddi-Emanuele" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-Andreas-L" }, { "family_name": "Gonzalez", "given_name": "Anthony", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-Anthony-H" }, { "family_name": "Papovich", "given_name": "Casey", "orcid": "0000-0001-7503-8482", "clpid": "Papovich-Casey-J" }, { "family_name": "Ninkov", "given_name": "Zoran", "clpid": "Ninkov-Zoran" }, { "family_name": "Robberto", "given_name": "Massimo", "orcid": "0000-0002-9573-3199", "clpid": "Robberto-Massimo" }, { "family_name": "Rose", "given_name": "Randall J.", "clpid": "Rose-Randall-J" }, { "family_name": "Rose", "given_name": "Thomas", "clpid": "Rose-Thomas" }, { "family_name": "Scarlata", "given_name": "Claudia", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-Claudia-M" }, { "family_name": "Stanford", "given_name": "S. A.", "orcid": "0000-0003-0122-0841", "clpid": "Stanford-Specncer-A" }, { "family_name": "Veach", "given_name": "Todd", "clpid": "Veach-Todd" }, { "family_name": "Zhai", "given_name": "Zhongxu", "orcid": "0000-0001-7984-5476", "clpid": "Zhai-Zhongxu" }, { "family_name": "Benson", "given_name": "Bradford", "orcid": "0000-0002-5108-6823", "clpid": "Benson-Bradford-A" }, { "family_name": "Bleem", "given_name": "L. E.", "orcid": "0000-0001-7665-5079", "clpid": "Bleem-Lindsey-E" }, { "family_name": "Davis", "given_name": "Michael W.", "clpid": "Davis-Michael-W" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" } ], "abstract": "ISCEA (Infrared Satellite for Cosmic Evolution Astrophysics) is a small astrophysics mission whose Science Goal is to discover how galaxies evolved in the cosmic web of dark matter at cosmic noon. Its Science Objective is to determine the history of star formation and its quenching in galaxies as a function of local density and stellar mass when the Universe was 3-5 Gyrs old (1.2 < z < 2.1). ISCEA is designed to test the Science Hypothesis that during the period of cosmic noon, at 1.7 < z < 2.1, environmental quenching is the dominant quenching mechanism for typical galaxies not only in clusters and groups, but also in the extended cosmic web surrounding these structures. ISCEA meets its Science Objective by making a 10% shot noise measurement of star formation rate down to 6 M_\u2299\u2002 yr\u207b\u00b9 using H-\u03b1 out to a radius > 10 Mpc in each of 50 protocluster (cluster and cosmic web) fields at 1.2 < z < 2.1. ISCEA measures the star formation quenching factor in those fields, and galaxy kinematics with a precision < 50 km s\u207b\u00b9 to deduce the 3D spatial distribution in each field. ISCEA will transform our understanding of galaxy evolution at cosmic noon. \n\nISCEA is a small satellite observatory with a 30 cm equivalent diameter aperture telescope with a FoV of 0.32 deg\u00b2, and a multi-object spectrograph with a digital micro-mirror device (DMD) as its programmable slit mask. ISCEA will obtain spectra of 1000 galaxies simultaneously at an effective resolving power of R = 1000, with 2.8\" x 2.8\" slits, over the NIR wavelength range of 1.1 to 2.0 \u00b5m, a regime not accessible from the ground without large gaps in coverage. ISCEA will achieve a pointing accuracy of \u2264 2\" FWHM over 200s. ISCEA will be launched into a Low Earth Orbit, with a prime mission of 2.5 years. ISCEA's space-qualification of DMDs opens a new window for spectroscopy from space, enabling revolutionary advances in astrophysics.", "doi": "10.48550/arXiv.2112.02387", "publisher": "arXiv", "publication_date": "2021-12-04" }, { "id": "authors:6acr1-why17", "collection": "authors", "collection_id": "6acr1-why17", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190620-155138416", "type": "monograph", "title": "Directly Imaging Rocky Planets from the Ground", "author": [ { "family_name": "Mazin", "given_name": "B.", "clpid": "Mazin-B-A" }, { "family_name": "Artigau", "given_name": "\u00c9." }, { "family_name": "Bailey", "given_name": "V.", "orcid": "0000-0002-5407-2806", "clpid": "Bailey-V-P" }, { "family_name": "Baranec", "given_name": "C." }, { "family_name": "Beichman", "given_name": "C.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Benneke", "given_name": "B." }, { "family_name": "Birkby", "given_name": "J." }, { "family_name": "Brandt", "given_name": "T." }, { "family_name": "Chilcote", "given_name": "J." }, { "family_name": "Chun", "given_name": "M." }, { "family_name": "Close", "given_name": "L." }, { "family_name": "Currie", "given_name": "T." }, { "family_name": "Crossfield", "given_name": "I." }, { "family_name": "Dekany", "given_name": "R.", "clpid": "Dekany-Richard" }, { "family_name": "Delorme", "given_name": "J. R.", "clpid": "Delorme-J-R" }, { "family_name": "Dong", "given_name": "C." }, { "family_name": "Dong", "given_name": "R." }, { "family_name": "Doyon", "given_name": "R." }, { "family_name": "Dressing", "given_name": "C." }, { "family_name": "Fitzgerald", "given_name": "M." }, { "family_name": "Fortney", "given_name": "J." }, { "family_name": "Frazin", "given_name": "R." }, { "family_name": "Gaidos", "given_name": "E." }, { "family_name": "Guyon", "given_name": "O." }, { "family_name": "Hashimoto", "given_name": "J." }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Howard", "given_name": "A.", "orcid": "0000-0001-8638-0320", "clpid": "Howard-A-W" }, { "family_name": "Jensen-Clem", "given_name": "R." }, { "family_name": "Jovanovic", "given_name": "N.", "clpid": "Jovanovic-N" }, { "family_name": "Kotani", "given_name": "T." }, { "family_name": "Kawahara", "given_name": "H." }, { "family_name": "Konopacky", "given_name": "Q." }, { "family_name": "Knutson", "given_name": "H.", "orcid": "0000-0002-5375-4725", "clpid": "Knutson-H-A" }, { "family_name": "Liu", "given_name": "M." }, { "family_name": "Lu", "given_name": "J." }, { "family_name": "Lozi", "given_name": "J." }, { "family_name": "Macintosh", "given_name": "B." }, { "family_name": "Males", "given_name": "J." }, { "family_name": "Marley", "given_name": "M." }, { "family_name": "Marois", "given_name": "C." }, { "family_name": "Mawet", "given_name": "D.", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Meeker", "given_name": "S.", "clpid": "Meeker-S-R" }, { "family_name": "Millar-Blanchaer", "given_name": "M.", "orcid": "0000-0001-6205-9233", "clpid": "Millar-Blanchaer-M-A" }, { "family_name": "Mondal", "given_name": "S." }, { "family_name": "Bose", "given_name": "S. N." }, { "family_name": "Murakami", "given_name": "N." }, { "family_name": "Murray-Clay", "given_name": "R." }, { "family_name": "Narita", "given_name": "N." }, { "family_name": "Pyo", "given_name": "T. S." }, { "family_name": "Roberts", "given_name": "L.", "orcid": "0000-0003-3892-2900", "clpid": "Roberts-L-C-Jr" }, { "family_name": "Ruane", "given_name": "G.", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Serabyn", "given_name": "G.", "clpid": "Serabyn-G" }, { "family_name": "Shields", "given_name": "A." }, { "family_name": "Skemer", "given_name": "A." }, { "family_name": "Simard", "given_name": "L." }, { "family_name": "Stelter", "given_name": "D." }, { "family_name": "Tamura", "given_name": "M." }, { "family_name": "Troy", "given_name": "M.", "clpid": "Troy-M" }, { "family_name": "Vasisht", "given_name": "G.", "orcid": "0000-0002-1871-6264" }, { "family_name": "Wallace", "given_name": "J. K.", "clpid": "Wallace-J-Kent" }, { "family_name": "Wang", "given_name": "J." }, { "family_name": "Wang", "given_name": "J.", "orcid": "0000-0002-4361-8885", "clpid": "Wang-Ji" }, { "family_name": "Wright", "given_name": "S." } ], "abstract": "Over the past three decades instruments on the ground and in space have discovered thousands of planets outside the solar system. These observations have given rise to an astonishingly detailed picture of the demographics of short-period planets, but are incomplete at longer periods where both the sensitivity of transit surveys and radial velocity signals plummet. Even more glaring is that the spectra of planets discovered with these indirect methods are either inaccessible (radial velocity detections) or only available for a small subclass of transiting planets with thick, clear atmospheres. Direct detection can be used to discover and characterize the atmospheres of planets at intermediate and wide separations, including non-transiting exoplanets. Today, a small number of exoplanets have been directly imaged, but they represent only a rare class of young, self-luminous super-Jovian-mass objects orbiting tens to hundreds of AU from their host stars. Atmospheric characterization of planets in the <5 AU regime, where radial velocity (RV) surveys have revealed an abundance of other worlds, is technically feasible with 30-m class apertures in combination with an advanced AO system, coronagraph, and suite of spectrometers and imagers. There is a vast range of unexplored science accessible through astrometry, photometry, and spectroscopy of rocky planets, ice giants, and gas giants. In this white paper we will focus on one of the most ambitious science goals --- detecting for the first time habitable-zone rocky (<1.6 R_Earth) exoplanets in reflected light around nearby M-dwarfs", "doi": "10.48550/arXiv.1905.04275", "publisher": "arXiv", "publication_date": "2019-05-10" }, { "id": "authors:ts3gk-d8y56", "collection": "authors", "collection_id": "ts3gk-d8y56", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180914-101943065", "type": "monograph", "title": "Science Impacts of the SPHEREx All-Sky Optical to Near-Infrared Spectral Survey: Report of a Community Workshop Examining Extragalactic, Galactic, Stellar and Planetary Science", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-D" }, { "family_name": "Werner", "given_name": "Michael", "clpid": "Werner-M-W" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bull", "given_name": "Philip", "clpid": "Bull-P" }, { "family_name": "Crill", "given_name": "Brendan", "orcid": "0000-0002-4650-8518", "clpid": "Crill-B-P" }, { "family_name": "de Putter", "given_name": "Roland", "clpid": "de-Putter-R" }, { "family_name": "Eifler", "given_name": "Tim", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" }, { "family_name": "Korngut", "given_name": "Phillip", "clpid": "Korngut-P-M" }, { "family_name": "Nguyen", "given_name": "Hien", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" } ], "abstract": "SPHEREx is a proposed SMEX mission selected for Phase A. SPHEREx will carry out the first all-sky spectral survey and provide for every 6.2\" pixel a spectra between 0.75 and 4.18 \u03bcm [with R\u223c41.4] and 4.18 and 5.00 \u03bcm [with R\u223c135]. The SPHEREx team has proposed three specific science investigations to be carried out with this unique data set: cosmic inflation, interstellar and circumstellar ices, and the extra-galactic background light. It is readily apparent, however, that many other questions in astrophysics and planetary sciences could be addressed with the SPHEREx data. The SPHEREx team convened a community workshop in February 2016, with the intent of enlisting the aid of a larger group of scientists in defining these questions. This paper summarizes the rich and varied menu of investigations that was laid out. It includes studies of the composition of main belt and Trojan/Greek asteroids; mapping the zodiacal light with unprecedented spatial and spectral resolution; identifying and studying very low-metallicity stars; improving stellar parameters in order to better characterize transiting exoplanets; studying aliphatic and aromatic carbon-bearing molecules in the interstellar medium; mapping star formation rates in nearby galaxies; determining the redshift of clusters of galaxies; identifying high redshift quasars over the full sky; and providing a NIR spectrum for most eROSITA X-ray sources. All of these investigations, and others not listed here, can be carried out with the nominal all-sky spectra to be produced by SPHEREx. In addition, the workshop defined enhanced data products and user tools which would facilitate some of these scientific studies. Finally, the workshop noted the high degrees of synergy between SPHEREx and a number of other current or forthcoming programs, including JWST, WFIRST, Euclid, GAIA, K2/Kepler, TESS, eROSITA and LSST.", "doi": "10.48550/arXiv.1606.07039", "publication_date": "2016-06-22" }, { "id": "authors:haa3c-fxs78", "collection": "authors", "collection_id": "haa3c-fxs78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-110407615", "type": "monograph", "title": "Wide-Field InfraRed Survey Telescope WFIRST Final Report", "author": [ { "family_name": "Green", "given_name": "J.", "clpid": "Green-J" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Helou", "given_name": "G.", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Cutri", "given_name": "R.", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" } ], "abstract": "In December 2010, NASA created a Science Definition Team (SDT) for WFIRST, the Wide Field Infra-Red Survey Telescope, recommended by the Astro 2010 Decadal Survey as the highest priority for a large space mission. The SDT was chartered to work with the WFIRST Project Office at GSFC and the Program Office at JPL to produce a Design Reference Mission (DRM) for WFIRST. Part of the original charge was to produce an interim design reference mission by mid-2011. That document was delivered to NASA and widely circulated within the astronomical community. In late 2011 the Astrophysics Division augmented its original charge, asking for two design reference missions. The first of these, DRM1, was to be a finalized version of the interim DRM, reducing overall mission costs where possible. The second of these, DRM2, was to identify and eliminate capabilities that overlapped with those of NASA's James Webb Space Telescope (henceforth JWST), ESA's Euclid mission, and the NSF's ground-based Large Synoptic Survey Telescope (henceforth LSST), and again to reduce overall mission cost, while staying faithful to NWNH. This report presents both DRM1 and DRM2.", "doi": "10.48550/arXiv.1208.4012", "publisher": "NASA", "publication_date": "2012-08-20" } ]