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},
"title": "Searching for Planets Orbiting Fomalhaut with JWST/NIRCam",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Space and Planetary Science; Astronomy and Astrophysics",
"note": "
© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
\n
\n\nThis work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-03127 for JWST. These observations are associated with program #1193. NIRCam development and use at the University of Arizona is supported through NASA contract NAS5-02105. A team at JPL's MicroDevices Laboratory designed and manufactured the coronagraph masks used in these observations. Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). We are grateful for support from NASA through the JWST NIRCam project through contract No. NAS5-02105 (M. Rieke, University of Arizona, PI). The High Performance Computing resources used in this investigation were provided by funding from the JPL Information and Technology Solutions Directorate. The work of A.G., G.R., S.W., and K.S. is partially supported by NASA grants NNX13AD82G and 1255094. D.J. is supported by NRC Canada and by an NSERC Discovery Grant. We thank Dr. Paul Kalas for the discussions about the HST observations of Fomalhaut. The authors would like to thank the staff of the Space Telescope Science Institute, especially Crystal Mannfolk for her help in preparing the APT files, William Balmer, Jens Kammerer, and Julien Girard for providing valuable hints about the early stages of pipeline processing.
\n\nJWST - James Webb Space Telescope
\n\nastropy (Astropy Collaboration et al. 2013, 2018, 2022), jwst (Bushouse et al. 2023), NIRCoS (Kammerer et al. 2022), pyNRC (J. Leisenring 2023 in preparation), pyKLIP (Wang et al. 2015), species (Stolker et al. 2020), WebbPSF (Perrin et al. 2014), WebbPSF_ext (J. Leisenring 2023 in preparation)
",
"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
",
"date": "2024-01",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "167",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "26",
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},
{
"grant_number": "80NM0018D0004"
},
{
"grant_number": "NX13AD82G"
},
{
"grant_number": "1255094"
},
{},
{}
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"author_list": "Ygouf, Marie; Beichman, Charles A.; et el."
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{
"id": "Uyama-Taichi",
"name": {
"family": "Uyama",
"given": "Taichi"
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{
"name": {
"family": "Currie",
"given": "Thayne"
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"orcid": "0000-0002-7405-3119"
},
{
"name": {
"family": "Christiaens",
"given": "Valentin"
},
"orcid": "0000-0002-0101-8814"
},
{
"name": {
"family": "Bae",
"given": "Jaehan"
}
},
{
"name": {
"family": "Muto",
"given": "Takayuki"
}
},
{
"name": {
"family": "Takahashi",
"given": "Sanemichi Z."
},
"orcid": "0000-0003-3038-364X"
},
{
"name": {
"family": "Tazaki",
"given": "Ryo"
}
},
{
"id": "Ygouf-M",
"name": {
"family": "Ygouf",
"given": "Marie"
},
"orcid": "0000-0001-7591-2731"
},
{
"name": {
"family": "Kasdin",
"given": "Jeremy N."
}
},
{
"name": {
"family": "Groff",
"given": "Tyler"
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"orcid": "0000-0001-5978-3247"
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{
"name": {
"family": "Brandt",
"given": "Timothy D."
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"orcid": "0000-0003-2630-8073"
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{
"name": {
"family": "Chilcote",
"given": "Jeffrey"
},
"orcid": "0000-0001-6305-7272"
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{
"name": {
"family": "Hayashi",
"given": "Masahiko"
}
},
{
"name": {
"family": "McElwain",
"given": "Michael W."
},
"orcid": "0000-0003-0241-8956"
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{
"name": {
"family": "Guyon",
"given": "Olivier"
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"orcid": "0000-0002-1097-9908"
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"family": "Lozi",
"given": "Julien"
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"family": "Jovanovic",
"given": "Nemanja"
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"family": "Martinache",
"given": "Frantz"
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"name": {
"family": "Kudo",
"given": "Tomoyuki"
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{
"name": {
"family": "Tamura",
"given": "Motohide"
},
"orcid": "0000-0002-6510-0681"
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{
"name": {
"family": "Akiyama",
"given": "Eiji"
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"orcid": "0000-0002-5082-8880"
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"name": {
"family": "Beichman",
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"name": {
"family": "Grady",
"given": "Carol A."
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{
"name": {
"family": "Knapp",
"given": "Gillian R."
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"name": {
"family": "Kwon",
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"family": "Sitko",
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"family": "Takami",
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{
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"family": "Wagner",
"given": "Kevin R."
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"family": "Wisniewski",
"given": "John P."
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"family": "Yang",
"given": "Yi"
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},
"title": "SCExAO/CHARIS High-Contrast Imaging of Spirals and Darkening Features in the HD 34700 A Protoplanetary Disk",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "Coronagraphic imaging, Protoplanetary disks",
"note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 June 1; revised 2020 July 22; accepted 2020 July 22; published 2020 September 9. \n\nThe authors would like to thank the anonymous referees for their constructive comments and suggestions to improve the quality of the paper. We thank John Monnier for authorization to use GPI-PDI images originally presented in Monnier et al. (2019). The authors are grateful to Gijs Mulders for helpful comments. This research is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatories of Japan. This research has made use of NASA's Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018). \n\nT.U. acknowledges JSPS overseas research fellowship. T.C. is funded by a NASA Senior Postdoctoral Fellowship. J.W. acknowledges funding support from the NASA XRP program via grants 80NSSC20K0252 and NNX17AF88G. S.T. is supported by JSPS KAKENHI Grant-in-Aid for Early-Career Scientists No. 19K14764. M.T. is supported by MEXT/JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. E.A. is supported by MEXT/JSPS KAKENHI grant No. 17K05399. The development of SCExAO was supported by JSPS (Grant-in-Aid for Research #23340051, #26220704 & #23103002), Astrobiology Center of NINS, Japan, the Mt Cuba Foundation, and the director's contingency fund at Subaru Telescope. CHARIS was developed under the support by the Grant-in-Aid for Scientific Research on Innovative Areas #2302. \n\nThe authors wish to acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nPublished - Uyama_2020_ApJ_900_135.pdf
Submitted - 2007.11655.pdf
",
"abstract": "We present Subaru/SCExAO+Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) broadband (JHK-band) integral field spectroscopy of HD 34700 A. CHARIS data recover HD 34700 A's disk ring and confirm multiple spirals discovered by Monnier et al. We set limits on substellar companions of ~12 M_(Jup) at 0.\"3 (in the ring gap) and ~5 M_(Jup) at 0.\"75 (outside the ring). The data reveal darkening effects on the ring and spiral, although we do not identify the origin of each feature such as shadows or physical features related to the outer spirals. Geometric albedos converted from the surface brightness suggest a greater scale height and/or prominently abundant submicron dust at position angles between ~45\u00b0 and 90\u00b0. Spiral fitting resulted in very large pitch angles (~30\u00b0\u201350\u00b0); a stellar flyby of HD 34700 B or infall from a possible envelope is perhaps a reasonable scenario to explain the large pitch angles.",
"date": "2020-09-10",
"date_type": "published",
"publication": "Astrophysical Journal",
"volume": "900",
"number": "2",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 135",
"id_number": "CaltechAUTHORS:20200817-123125126",
"issn": "1538-4357",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200817-123125126",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA Senior Postdoctoral Fellowship"
},
{
"agency": "NASA",
"grant_number": "80NSSC20K0252"
},
{
"agency": "NASA",
"grant_number": "NNX17AF88G"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "19K14764"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "18H05442"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "15H02063"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "22000005"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "17K05399"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "23340051"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "26220704"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "23103002"
},
{
"agency": "National Institutes of Natural Sciences (NINS)"
},
{
"agency": "Mt. Cuba Astronomical Foundation"
},
{
"agency": "Subaru Telescope"
},
{
"agency": "Japan Society for the Promotion of Science (JSPS)",
"grant_number": "2302"
}
]
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},
"title": "Paving the Way to Future Missions: the Roman Space Telescope Coronagraph Technology Demonstration",
"ispublished": "unpub",
"full_text_status": "public",
"note": "Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \u00a9 2020 California Institute of Technology. Government sponsorship acknowledged.\n\nSubmitted - 2008.05624.pdf
",
"abstract": "This document summarizes how far the Nancy Grace Roman Space Telescope Coronagraph Instrument (Roman CGI) will go toward demonstrating high-contrast imaging and spectroscopic requirements for potential future exoplanet direct imaging missions, illustrated by the HabEx and LUVOIR concepts. The assessment is made for two levels of assumed CGI performance: (i) current best estimate (CBE) as of August 2020, based on laboratory results and realistic end-to-end simulations with JPL-standard Model Uncertainty Factors (MUFs); (ii) CGI design specifications inherited from Phase B requirements. We find that the predicted performance (CBE) of many CGI subsystems compares favorably with the needs of future missions, despite providing more modest point source detection limits than future missions. This is essentially due to the challenging pupil of the Roman Space Telescope; this pupil pushes the coronagraph masks sensitivities to misalignments to be commensurate with future missions. In particular, CGI will demonstrate active low-order wavefront control and photon counting capabilities at levels of performance either higher than, or comparable to, the needs of future missions.",
"date": "2020-08-17",
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"title": "Keck/NIRC2 L'-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70",
"ispublished": "pub",
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"keywords": "Exoplanet formation; Exoplanet atmospheres; Orbit determination; Exoplanet dynamics; Coronagraphic imaging",
"note": "\u00a9 2020 The American Astronomical Society.\n\nReceived 2020 March 13; revised 2020 April 10; accepted 2020 April 17; published 2020 May 18.\n\nWe thank Trevor David for helpful discussion and the referees for their helpful suggestions for the paper. J.J.W., S.G., and P.G. are supported by the Heising-Simons Foundation 51 Pegasi b postdoctoral fellowship. The Keck infrared pyramid wave front sensor was developed with support from the National Science Foundation under grant Nos. AST-1611623 and AST-1106391, as well as the Heising Simons Foundation under the Keck Planet Imager and Characterizer project. This research is partially supported by NASA ROSES XRP, award 80NSSC19K0294. F.M. acknowledges funding from ANR of France under contract ANR-16-CE31-0013. Part of the computations presented here were conducted on the Caltech High Performance Cluster, partially supported by a grant from the Gordon and Betty Moore Foundation. This project has received funding from the European Research Council (ERC) under the European Union's Seventh Framework Program (grant agreement 337569, VORTEX) and under the European Union's Horizon 2020 research and innovation programme (grant agreement 819155, EPIC). The research was supported by the Wallonia-Brussels Federation (grant for Concerted Research Actions). Data presented in this work were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nFacility: Keck II (NIRC2). -\n\nSoftware: pyKLIP (Wang et al. 2015), orbitize! (Blunt et al. 2020), DebrisDiskFM (Ren et al. 2019), emcee (Foreman-Mackey et al. 2013), ptemcee (Vousden et al. 2016), MCFOST (Pinte et al. 2006, 2009).\n\nPublished - Wang_2020_AJ_159_263.pdf
Submitted - 2004.09597.pdf
",
"abstract": "We present L'-band imaging of the PDS 70 planetary system with Keck/NIRC2 using the new infrared pyramid wave front sensor. We detected both PDS 70 b and c in our images, as well as the front rim of the circumstellar disk. After subtracting off a model of the disk, we measured the astrometry and photometry of both planets. Placing priors based on the dynamics of the system, we estimated PDS 70 b to have a semimajor axis of 20\u207a\u00b3\u208b\u2084 au and PDS 70 c to have a semimajor axis of 34\u207a\u00b9\u00b2\u208b\u2086 au (95% credible interval). We fit the spectral energy distribution (SED) of both planets. For PDS 70 b, we were able to place better constraints on the red half of its SED than previous studies and inferred the radius of the photosphere to be 2\u20133 R_(Jup). The SED of PDS 70 c is less well constrained, with a range of total luminosities spanning an order of magnitude. With our inferred radii and luminosities, we used evolutionary models of accreting protoplanets to derive a mass of PDS 70 b between 2 and 4 M_(Jup) and a mean mass accretion rate between 3 \u00d7 10\u207b\u2077 and 8 \u00d7 10\u207b\u2077 M_(Jup)/yr. For PDS 70 c, we computed a mass between 1 and 3 M_(Jup) and mean mass accretion rate between 1 \u00d7 10\u207b\u2077 and 5 \u00d7 10\u207b\u2077 M_(Jup) /yr. The mass accretion rates imply dust accretion timescales short enough to hide strong molecular absorption features in both planets' SEDs.",
"date": "2020-06",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "159",
"number": "6",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 263",
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"issn": "1538-3881",
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"agency": "Heising-Simons Foundation",
"grant_number": "51 Pegasi b Fellowship"
},
{
"agency": "NSF",
"grant_number": "AST-1611623"
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"agency": "Agence Nationale pour la Recherche (ANR)",
"grant_number": "ANR-16-CE31-0013"
},
{
"agency": "Gordon and Betty Moore Foundation"
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{
"agency": "European Research Council (ERC)",
"grant_number": "337569"
},
{
"agency": "European Research Council (ERC)",
"grant_number": "819155"
},
{
"agency": "Wallonia-Brussels Federation"
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{
"agency": "W. M. Keck Foundation"
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"title": "Searching for Planets Orbiting \u03b1 Cen A with the James Webb Space Telescope",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "infrared: planetary systems \u2013 planetary systems \u2013 planets and satellites: detection \u2013 space vehicles: instruments",
"note": "\u00a9 2019. The Astronomical Society of the Pacific. \n\nReceived 2019 August 25; accepted 2019 October 14; published 2019 December 12. \n\nSome of the research described in this publication was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Copyright 2019 California Inst of Technology. All rights reserved.\n\nPublished - Beichman_2020_PASP_132_015002.pdf
Accepted Version - 1910.09709.pdf
",
"abstract": "\u03b1 Centauri A is the closest solar-type star to the Sun and offers an excellent opportunity to detect the thermal emission of a mature planet heated by its host star. The MIRI coronagraph on JWST can search the 1-3 AU (1\"-2\") region around \u03b1 Cen A which is predicted to be stable within the \u03b1 Cen AB system. We demonstrate that with reasonable performance of the telescope and instrument, a 20 hr program combining on-target and reference star observations at 15.5 um could detect thermal emission from planets as small as ~5 R\u2295. Multiple visits every 3-6 months would increase the geometrical completeness, provide astrometric confirmation of detected sources, and push the radius limit down to ~3 R\u2295. An exozodiacal cloud only a few times brighter than our own should also be detectable, although a sufficiently bright cloud might obscure any planet present in the system. While current precision radial velocity (PRV) observations set a limit of 50-100 M\u2295 at 1-3 AU for planets orbiting \u03b1 Cen A, there is a broad range of exoplanet radii up to 10 RE consistent with these mass limits. A carefully planned observing sequence along with state-of-the-art post-processing analysis could reject the light from \u03b1 Cen A at the level of ~10\u207b\u2075 at 1\"-2\" and minimize the influence of \u03b1 Cen B located 7-8\" away in the 2022-2023 timeframe. These space-based observations would complement on-going imaging experiments at shorter wavelengths as well as PRV and astrometric experiments to detect planets dynamically. Planetary demographics suggest that the likelihood of directly imaging a planet whose mass and orbit are consistent with present PRV limits is small, ~5%, and possibly lower if the presence of a binary companion further reduces occurrence rates. However, at a distance of just 1.34 pc, \u03b1 Cen A is our closest sibling star and certainly merits close scrutiny.",
"date": "2020-01",
"date_type": "published",
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"volume": "132",
"number": "1007",
"publisher": "Astronomical Society of the Pacific",
"pagerange": "Art. No. 015002",
"id_number": "CaltechAUTHORS:20191121-152416477",
"issn": "0004-6280",
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"title": "The Potential of Exozodiacal Disks Observations with the WFIRST Coronagraph Instrument",
"ispublished": "unpub",
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"note": "Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nSubmitted - 1909.02161.pdf
",
"abstract": "The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) will be the first high-performance stellar coronagraph using active wavefront control for deep starlight suppression in space, providing unprecedented levels of contrast, spatial resolution, and sensitivity for astronomical observations in the optical. One science case enabled by the CGI will be taking images and(R~50)spectra of faint interplanetary dust structures present in the habitable zone of nearby sunlike stars (~10 pc) and within the snow-line of more distant ones(~20pc), down to dust density levels commensurate with that of the solar system zodiacal cloud. Reaching contrast levels below~10-7 for the first time, CGI will cross an important threshold in debris disks physics, accessing disks with low enough optical depths that their structure is dominated by transport phenomena than collisions. Hence, CGI results will be crucial for determining how exozodiacal dust grains are produced and transported in low-density disks around mature stars. Additionally, CGI will be able to measure the brightness level and constrain the degree of asymmetry of exozodiacal clouds around individual nearby sunlike stars in the optical, at the ~10x solar zodiacal emission level. This information will be extremely valuable for optimizing the observational strategy of possible future exo-Earth direct imaging missions, especially those planning to operate at optical wavelengths, such as Habitable Exoplanet Observatory (HabEx) and the Large Ultraviolet/Optical/Infrared Surveyor (LUVOIR).",
"date": "2019-10-02",
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"doi": "10.48550/arXiv.1909.02161",
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"author_list": "Mennesson, Bertrand; Akeson, R.; et el."
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"title": "An Exo-Kuiper Belt with an Extended Halo around HD 191089 in Scattered Light",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "protoplanetary disks \u2013 radiative transfer \u2013 stars: imaging \u2013 stars: individual (HD 191089) \u2013 techniques: image processing",
"note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2018 December 14; revised 2019 July 18; accepted 2019 July 18; published 2019 September 4. \n\nWe appreciate the suggestions from the anonymous referee that significantly improved this paper. B.R. is thankful for the useful discussions with Xinyu Lu and the comments from Kevin Schlaufman that improved the paper. E.C. acknowledges support from NASA through Hubble Fellowship grant HST-HF2-51355 awarded by STScI, operated by AURA, Inc., under contract NAS5-26555 and support from HST-AR-12652 for research carried out at the Jet Propulsion Laboratory, California Institute of Technology. T.E. was supported in part by NASA grants NNX15AD95G/NEXSS, NNX15AC89G, and NSF AST-1518332. C.P. acknowledges funding from the Australian Research Council via FT170100040 and DP180104235. G.D. acknowledges support from NSF grants NNX15AD95G/NEXSS, AST-1413718, and AST-1616479. This research has made use of data reprocessed as part of the ALICE program, which was supported by NASA through grants HST-AR-12652 (PI: R. Soummer), HST-GO-11136 (PI: D. Golimowski), HST-GO-13855 (PI: \u00c9. Choquet), and HST-GO-13331 (PI: L. Pueyo) and STScI Director's Discretionary Research funds and was conducted at STScI, which is operated by AURA under NASA contract NAS5-26555. The input images to ALICE processing are from the recalibrated NICMOS data products produced by the Legacy Archive project, \"A Legacy Archive PSF Library And Circumstellar Environments (LAPLACE) Investigation\" (HST-AR-11279; PI: G. Schneider). Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States); National Research Council (Canada); CONICYT (Chile); Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina); Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil); and Korea Astronomy and Space Science Institute (Republic of Korea). This research project (or part of this research project) was conducted using computational resources (and/or scientific computing services) at the Maryland Advanced Research Computing Center (MARCC). \n\nFacilities: HST (NICMOS - , STIS) - , Gemini:South (Gemini Planet Imager). - \n\nSoftware: corner.py (Foreman-Mackey 2016), DebrisDiskFM (Ren & Perrin 2018), Debris Ring Analyzer (Stark et al. 2014), emcee (version 3.0rc1; Foreman-Mackey et al. 2013), MCFOST (Pinte et al. 2006, 2009), nmf_imaging (Ren 2018), pysynphot (STScI Development Team 2013).\n\nPublished - Ren_2019_ApJ_882_64.pdf
Accepted Version - 1908.00006.pdf
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"abstract": "We have obtained Hubble Space Telescope STIS and NICMOS and Gemini/GPI scattered-light images of the HD 191089 debris disk. We identify two spatial components: a ring resembling the Kuiper Belt in radial extent (FWHM ~ 25 au, centered at ~46 au) and a halo extending to ~640 au. We find that the halo is significantly bluer than the ring, consistent with the scenario that the ring serves as the \"birth ring\" for the smaller dust in the halo. We measure the scattering phase functions in the 30\u00b0\u2013150\u00b0 scattering-angle range and find that the halo dust is more forward- and backward-scattering than the ring dust. We measure a surface density power-law index of \u22120.68 \u00b1 0.04 for the halo, which indicates the slowdown of the radial outward motion of the dust. Using radiative transfer modeling, we attempt to simultaneously reproduce the (visible) total and (near-infrared) polarized intensity images of the birth ring. Our modeling leads to mutually inconsistent results, indicating that more complex models, such as the inclusion of more realistic aggregate particles, are needed.",
"date": "2019-09-01",
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"publication": "Astrophysical Journal",
"volume": "882",
"number": "1",
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"title": "Key Technologies for the Wide Field Infrared Survey Telescope Coronagraph Instrument",
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"note": "\u00a9 2018 California Institute of Technology. Government sponsorship acknowledged. The work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The decision to implement the WFIRST mission will not be finalized until NASA's completion of the National Environmental Policy Act (NEPA) process. This document is being made available for information purposes only. \n\nThis whitepaper was submitted to the Exoplanet Science Strategy call in March 2018 and is presented here without modification. An updated version of Fig. 2 and associated detailed description can be found in ref (21).\n\nSubmitted - 1901.04050.pdf
",
"abstract": "The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) is a high-contrast imager and integral field spectrograph that will enable the study of exoplanets and circumstellar disks at visible wavelengths. Ground-based high-contrast instrumentation has fundamentally limited performance at small working angles, even under optimistic assumptions for 30m-class telescopes. There is a strong scientific driver for better performance, particularly at visible wavelengths. Future flagship mission concepts aim to image Earth analogues with visible light flux ratios of more than 10^10. CGI is a critical intermediate step toward that goal, with a predicted 10^8-9 flux ratio capability in the visible. CGI achieves this through improvements over current ground and space systems in several areas: (i) Hardware: space-qualified (TRL9) deformable mirrors, detectors, and coronagraphs, (ii) Algorithms: wavefront sensing and control; post-processing of integral field spectrograph, polarimetric, and extended object data, and (iii) Validation of telescope and instrument models at high accuracy and precision. This white paper, submitted to the 2018 NAS Exoplanet Science Strategy call, describes the status of key CGI technologies and presents ways in which performance is likely to evolve as the CGI design matures.",
"date": "2019-06-27",
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"title": "Cold Debris Disks as Strategic Targets for the 2020s",
"ispublished": "unpub",
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"note": "Submitted - 1906.02129.pdf
",
"abstract": "Cold debris disks (T<200 K) are analogues to the dust in the Solar System's Kuiper belt--dust generated from the evaporation and collision of minor bodies perturbed by planets, our Sun, and the local interstellar medium. Scattered light from debris disks acts as both a signpost for unseen planets as well as a source of contamination for directly imaging terrestrial planets, but many details of these disks are poorly understood. We lay out a critical observational path for the study of nearby debris disks that focuses on defining an empirical relationship between scattered light and thermal emission from a disk, probing the dynamics and properties of debris disks, and directly determining the influence of planets on disks. \nWe endorse the findings and recommendations published in the National Academy reports on Exoplanet Science Strategy and Astrobiology Strategy for the Search for Life in the Universe. This white paper extends and complements the material presented therein with a focus on debris disks around nearby stars. Separate complementary papers are being submitted regarding the inner warm regions of debris disks (Mennesson et al.), the modeling of debris disk evolution (Gaspar et al.), studies of dust properties (Chen et al.), and thermal emission from disks (Su et al.).",
"date": "2019-06-21",
"date_type": "published",
"publisher": "arXiv",
"id_number": "CaltechAUTHORS:20190621-081621109",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190621-081621109",
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"doi": "10.48550/arXiv.1906.02129",
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"title": "Deep Exploration of \u03f5 Eridani with Keck Ms-band Vortex Coronagraphy and Radial Velocities: Mass and Orbital Parameters of the Giant Exoplanet",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "planet\u2013disk interactions; planets and satellites: dynamical evolution and stability; planets and satellites: gaseous planets; planetary systems; techniques: high angular resolution; techniques: radial velocities",
"note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2018 May 1; revised 2018 October 16; accepted 2018 October 29; published 2019 January 3. \n\nThe authors would like to acknowledge the contributions and useful comments from Prof. Debra Fischer and Prof. James Graham. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work was partially performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. (C) 2017. All rights reserved. E.C. acknowledges support from NASA through Hubble Fellowship grant HF2-51355 awarded by STScI, which is operated by AURA, Inc. for NASA under contract NAS5-26555. We also acknowledge support from NASA/NExSS through grant no. NNX15AD95G. \n\nSoftware: RadVel (Fulton et al. 2018), emcee (Foreman-Mackey et al. 2013), VIP (Gomez Gonzalez et al. 2017), PyKLIP (Wang et al. 2015).\n\nPublished - Mawet_2019_AJ_157_33.pdf
Accepted Version - 1810.03794.pdf
",
"abstract": "We present the most sensitive direct imaging and radial velocity (RV) exploration of epsilon Eridani to date. epsilon Eridani is an adolescent planetary system, reminiscent of the early solar system. It is surrounded by a prominent and complex debris disk that is likely stirred by one or several gas giant exoplanets. The discovery of the RV signature of a giant exoplanet was announced 15 yr ago, but has met with scrutiny due to possible confusion with stellar noise. We confirm the planet with a new compilation and analysis of precise RV data spanning 30 yr, and combine it with upper limits from our direct imaging search, the most sensitive ever performed. The deep images were taken in the Ms band (4.7 \u03bcm) with the vortex coronagraph recently installed in W.M. Keck Observatory's infrared camera NIRC2, which opens a sensitive window for planet searches around nearby adolescent systems. The RV data and direct imaging upper limit maps were combined in an innovative joint Bayesian analysis, providing new constraints on the mass and orbital parameters of the elusive planet. epsilon Eridani b has a mass of 0.78_(-0.12)^(+0.38} M_(Jup) and is orbiting epsilon Eridani at about 3.48 \u00b1 0.02 au with a period of 7.37 \u00b1 0.07 yr. The eccentricity of epsilon Eridani b's orbit is 0.07_(-0.05)^(+0.06), an order of magnitude smaller than early estimates and consistent with a circular orbit. We discuss our findings from the standpoint of planet\u2013disk interactions and prospects for future detection and characterization with the James Webb Space Telescope.",
"date": "2019-01",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "157",
"number": "1",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 33",
"id_number": "CaltechAUTHORS:20190103-105531269",
"issn": "1538-3881",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190103-105531269",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
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{
"agency": "W. M. Keck Foundation"
},
{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "NASA Hubble Fellowship",
"grant_number": "HF2-51355"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "NASA",
"grant_number": "NNX15AD95G"
},
{
"agency": "Fonds de la Recherche Scientifique (FNRS)"
},
{
"agency": "Miller Institute for Basic Research in Science"
},
{
"agency": "NSF Graduate Research Fellowship"
},
{
"agency": "NSF Astronomy and Astrophysics Fellowship"
}
]
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},
"title": "Discovery of a Transiting Adolescent Sub-Neptune Exoplanet with K2",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "open clusters and associations: individual (Cas-Tau) \u2013 planetary systems \u2013 planets and satellites:\nindividual (EPIC 247267267 b) \u2013 planets and satellites: gaseous planets \u2013 planets and satellites: physical evolution \u2013 stars: low-mass",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 January 19; revised 2018 October 27; accepted 2018 November 4; published 2018 December 6. \n\nThis research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We thank the anonymous referee for comments which improved this manuscript. T.J.D. and E.E.M. acknowledge support from the Jet Propulsion Laboratory Exoplanetary Science Initiative. M.B. acknowledges support from the North Carolina Space Grant Consortium. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership of the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS 143, 23. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nFacilities: FLWO:1.5 m (TRES) - , Keck:I (HIRES) - KECK I Telescope, Keck:II (NIRC2) - KECK II Telescope, Kepler - The Kepler Mission, PS1 - Panoramic Survey Telescope and Rapid Response System Telescope #1 (Pan-STARRS), Shane (ShARCS) - Lick Observatory's 3m Shane Telescope. \n\nSoftware: emcee (Foreman-Mackey et al. 2013), forecaster (Chen & Kipping 2017b), isoclassify (Huber et al. 2017), k2sc (Aigrain et al. 2016), k2sff (Vanderburg & Johnson 2014), pytransit (Parviainen 2015), radvel (Fulton et al. 2018), vespa (Morton 2015).\n\nPublished - David_2018_AJ_156_302.pdf
Submitted - 1801.07320.pdf
",
"abstract": "The role of stellar age in the measured properties and occurrence rates of exoplanets is not well understood. This is in part due to a paucity of known young planets and the uncertainties in age-dating for most exoplanet host stars. Exoplanets with well-constrained ages, particularly those which are young, are useful as benchmarks for studies aiming to constrain the evolutionary timescales relevant for planets. Such timescales may concern orbital migration, gravitational contraction, or atmospheric photoevaporation, among other mechanisms. Here we report the discovery of an adolescent transiting sub-Neptune from K2 photometry of the low-mass star EPIC 247267267. From multiple age indicators, we estimate the age of the star to be 120 Myr, with a 68% confidence interval of 100\u2013760 Myr. The size of EPIC 247267267 b (R P = 2.8 \u00b1 0.1 R\u2295) combined with its youth make it an intriguing case study for photoevaporation models, which predict enhanced atmospheric mass loss during early evolutionary stages.",
"date": "2018-12",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "156",
"number": "6",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 302",
"id_number": "CaltechAUTHORS:20180817-160130573",
"issn": "1538-3881",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180817-160130573",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
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{
"agency": "NASA/JPL/Caltech"
},
{
"agency": "North Carolina Space Grant Consortium"
},
{
"agency": "NASA Sagan Fellowship"
},
{
"agency": "NASA",
"grant_number": "NAS5-26555"
},
{
"agency": "NASA",
"grant_number": "NNX09AF08G"
},
{
"agency": "W. M. Keck Foundation"
},
{
"agency": "Institute for Astronomy"
},
{
"agency": "University of Hawaii"
},
{
"agency": "Pan-STARRS Project Office"
},
{
"agency": "Max-Planck-Society"
},
{
"agency": "Max Planck Institute for Astronomy (MPIA)"
},
{
"agency": "Max Planck Institute for Extraterrestrial Physics"
},
{
"agency": "NASA",
"grant_number": "NNX08AR22G"
},
{
"agency": "NSF",
"grant_number": "AST-1238877"
},
{
"agency": "Gordon and Betty Moore Foundation"
},
{
"agency": "Gaia Multilateral Agreement"
}
]
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"name": {
"family": "Ygouf",
"given": "Marie"
},
"orcid": "0000-0001-7591-2731"
},
{
"id": "Mawet-D",
"name": {
"family": "Mawet",
"given": "Dimitri"
},
"orcid": "0000-0002-8895-4735"
},
{
"id": "Pueyo-L",
"name": {
"family": "Pueyo",
"given": "Laurent"
},
"orcid": "0000-0003-3818-408X"
},
{
"id": "Beichman-C-A",
"name": {
"family": "Beichman",
"given": "Charles"
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},
"title": "A Deep Search for Planets in the Inner 15 au around Vega",
"ispublished": "pub",
"full_text_status": "public",
"keywords": "circumstellar matter \u2013 planets and satellites: detection \u2013 stars: individual (Vega) \u2013 techniques: high angular resolution",
"note": "\u00a9 2018 The American Astronomical Society. \n\nReceived 2018 June 11; revised 2018 September 5; accepted 2018 September 11; published 2018 October 18. \n\nWe thank the anonymous referee for their helpful suggestions that improved this paper. We thank the Palomar mountain crew, especially Bruce Baker, Mike Doyle, Carolyn Heffner, John Henning, Greg van Idsinga, Steve Kunsman, Dan McKenna, Jean Mueller, Kajsa Peffer, Paul Nied, Joel Pearman, Kevin Rykoski, Carolyn Heffner, Jamey Eriksen, and Pam Thompson. We thank AAron Veicht for his contributions to the data acquisition during the observations. K.Y.L.S. acknowledges the partial support from the NASA grant NNX15AI86G. G.V. acknowledges the JPL Research & Technology Program and the NASA XRP grant 399131.02.07.02.66.\n\nPublished - Meshkat_2018_AJ_156_214.pdf
Accepted Version - 1809.06941.pdf
",
"abstract": "We present the results of a deep high-contrast imaging search for planets around Vega. Vega is an ideal target for high-contrast imaging because it is bright, nearby, and young with a face-on two-belt debris disk that may be shaped by unseen planets. We obtained J- and H-band data on Vega with the coronagraphic integral-field spectrograph Project 1640 (P1640) at Palomar Observatory. Two nights of data were obtained in 2016, in poor seeing conditions, and two additional nights in more favorable conditions in 2017. In total, we obtained 5.5 hours of integration time on Vega in moderate to good seeing conditions (<1farcs5). We did not detect any low-mass companions in this system. Our data present the most sensitive contrast limits around Vega at very small separations (2\u201315 au) thus far, allowing us to place new constraints on the companions that may be sculpting the Vega system. In addition to new constraints, as the deepest data obtained with P1640, these observations form the final legacy of the now decommissioned instrument.",
"date": "2018-11",
"date_type": "published",
"publication": "Astronomical Journal",
"volume": "156",
"number": "5",
"publisher": "American Astronomical Society",
"pagerange": "Art. No. 214",
"id_number": "CaltechAUTHORS:20181023-090840047",
"issn": "1538-3881",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181023-090840047",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "NASA",
"grant_number": "NNX15AI86G"
},
{
"agency": "JPL Research and Technology Development Fund"
},
{
"agency": "NASA",
"grant_number": "399131.02.07.02.66"
}
]
},
"local_group": {
"items": [
{
"id": "Infrared-Processing-and-Analysis-Center-(IPAC)"
},
{
"id": "Astronomy-Department"
}
]
},
"doi": "10.3847/1538-3881/aae14f",
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"author_list": "Meshkat, Tiffany; Nilsson, Ricky; et el."
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"id": "Ruane-G-J",
"name": {
"family": "Ruane",
"given": "G."
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"id": "Jovanovic-N",
"name": {
"family": "Jovanovic",
"given": "N."
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},
"title": "Review of high-contrast imaging systems for current and future ground- and space-based telescopes I: coronagraph design methods and optical performance metrics",
"ispublished": "unpub",
"full_text_status": "public",
"keywords": "High contrast imaging, instrumentation, exoplanets, direct detection, coronagraphs",
"note": "\u00a9 2018 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nThe authors would like to acknowledge the Lorentz Center for hosting and to a large extent funding the Optimal Optical Coronagraph workshop held September 25-29, 2017 at the Lorentz Center in Leiden, the Netherlands. Additional funding for the workshop was provided by the European Research Council under ERG Starting Grant agreement 678194 (FALCONER) granted to Frans Snik. This formed the platform where this work was carried out. G. Ruane is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1602444.\n\nPublished - 106982S.pdf
",
"abstract": "The Optimal Optical Coronagraph (OOC) Workshop at the Lorentz Center in September 2017 in Leiden, the Netherlands gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this first installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of design methods and optical performance metrics developed for coronagraph instruments. The design and optimization of coronagraphs for future telescopes has progressed rapidly over the past several years in the context of space mission studies for Exo-C, WFIRST, HabEx, and LUVOIR as well as ground-based telescopes. Design tools have been developed at several institutions to optimize a variety of coronagraph mask types. We aim to give a broad overview of the approaches used, examples of their utility, and provide the optimization tools to the community. Though it is clear that the basic function of coronagraphs is to suppress starlight while maintaining light from off-axis sources, our community lacks a general set of standard performance metrics that apply to both detecting and characterizing exoplanets. The attendees of the OOC workshop agreed that it would benefit our community to clearly define quantities for comparing the performance of coronagraph designs and systems. Therefore, we also present a set of metrics that may be applied to theoretical designs, testbeds, and deployed instruments. We show how these quantities may be used to easily relate the basic properties of the optical instrument to the detection significance of the given point source in the presence of realistic noise.",
"date": "2018-08-21",
"date_type": "published",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_pub": "Bellingham, WA",
"pagerange": "Art. No. 106982S",
"id_number": "CaltechAUTHORS:20181204-071738445",
"isbn": "9781510619494",
"book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181204-071738445",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "678194"
},
{
"agency": "NSF Astronomy and Astrophysics Fellowship",
"grant_number": "AST-1602444"
}
]
},
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"items": [
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"id": "Lystrup-M",
"name": {
"family": "Lystrup",
"given": "Makenzie"
}
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"id": "MacEwen-H-A",
"name": {
"family": "MacEwen",
"given": "Howard A."
}
},
{
"id": "Fazio-G-G",
"name": {
"family": "Fazio",
"given": "Giovanni G."
}
},
{
"id": "Batalha-N-M",
"name": {
"family": "Batalha",
"given": "Natalie"
}
},
{
"id": "Siegler-N",
"name": {
"family": "Siegler",
"given": "Nicholas"
}
},
{
"id": "Tong-Edward-C",
"name": {
"family": "Tong",
"given": "Edward C."
}
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"doi": "10.1117/12.2312948",
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"author_list": "Ruane, G.; Jovanovic, N.; et el."
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"items": [
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"id": "Snik-F",
"name": {
"family": "Snik",
"given": "Frans"
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"id": "Jovanovic-N",
"name": {
"family": "Jovanovic",
"given": "Nemanja"
}
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{
"id": "Ruane-G-J",
"name": {
"family": "Ruane",
"given": "Garreth"
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"orcid": "0000-0003-4769-1665"
},
{
"id": "Ygouf-M",
"name": {
"family": "Ygouf",
"given": "Marie"
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},
"title": "Review of high-contrast imaging systems for current and future ground-based and space-based telescopes III: technology opportunities and pathways",
"ispublished": "unpub",
"full_text_status": "public",
"keywords": "High contrast imaging, Exoplanets, Technology",
"note": "\u00a9 2018 Society of Photo-optical Instrumentation Engineers (SPIE). \n\nThe authors would like to acknowledge the Lorentz Center for hosting and to a large extend funding the Optimal Optical Coronagraph workshop in Leiden 2017. Additional funding for the workshop was provided by the European Research Council under ERC Starting Grant agreement 678194 (FALCONER) granted to Frans Snik. This formed the platform where this work was carried out.\n\nPublished - 107062L.pdf
Submitted - 1807.07100.pdf
",
"abstract": "The Optimal Optical CoronagraphWorkshop at the Lorentz Center in September 2017 in Leiden, the Netherlands gathered a diverse group of 30 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. This contribution is the final part of a series of three papers summarizing the outcomes of the workshop, and presents an overview of novel optical technologies and systems that are implemented or considered for high-contrast imaging instruments on both ground-based and space telescopes. The overall objective of high contrast instruments is to provide direct observations and characterizations of exoplanets at contrast levels as extreme as 10^(-10). We list shortcomings of current technologies, and identify opportunities and development paths for new technologies that enable quantum leaps in performance. Specifically, we discuss the design and manufacturing of key components like advanced deformable mirrors and coronagraphic optics, and their amalgamation in \"adaptive coronagraph\" systems. Moreover, we discuss highly integrated system designs that combine contrast-enhancing techniques and characterization techniques (like high-resolution spectroscopy) while minimizing the overall complexity. Finally, we explore extreme implementations using all-photonics solutions for ground-based telescopes and dedicated huge apertures for space telescopes.",
"date": "2018-07-10",
"date_type": "published",
"publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)",
"place_of_pub": "Bellingham, WA",
"pagerange": "Art. No. 107062L",
"id_number": "CaltechAUTHORS:20181129-144758627",
"isbn": "9781510619654",
"book_title": "Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation III",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181129-144758627",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
{
"agency": "European Research Council (ERC)",
"grant_number": "678194"
}
]
},
"local_group": {
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"items": [
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"id": "Navarro-R",
"name": {
"family": "Navarro",
"given": "Ram\u00f3n"
}
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{
"id": "Geyl-R",
"name": {
"family": "Geyl",
"given": "Roland"
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"doi": "10.1117/12.2313957",
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"datestamp": "2023-08-19 10:22:22",
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"items": [
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"id": "Jovanovic-N",
"name": {
"family": "Jovanovic",
"given": "Nemanja"
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{
"id": "Ruane-G-J",
"name": {
"family": "Ruane",
"given": "Garreth"
},
"orcid": "0000-0003-4769-1665"
},
{
"id": "Ygouf-M",
"name": {
"family": "Ygouf",
"given": "Marie"
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"orcid": "0000-0001-7591-2731"
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},
"title": "Review of high-contrast imaging systems for current and future ground-based and space-based telescopes: Part II. Common path wavefront sensing/control and coherent differential imaging",
"ispublished": "unpub",
"full_text_status": "public",
"keywords": "Wavefront sensing, common path wavefront sensing, coherent differential imaging, high contrast imaging, exoplanets",
"note": "\u00a9 2018 Society of Photo-Optical Instrumentation Engineers. \n\nThe authors would like to acknowledge the Lorentz Center for hosting and to a large extend funding the Optimal Optical Coronagraph workshop in Leiden 2017. Additional funding for the workshop was provided by the European Research Council under ERC Starting Grant agreement 678194 (FALCONER) granted to Frans Snik. This formed the platform where this work was carried out.\n\nPublished - 107031U.pdf
Submitted - 1807.07043.pdf
",
"abstract": "The Optimal Optical Coronagraph (OOC) Workshop held at the Lorentz Center in September 2017 in Leiden, the Netherlands, gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this second installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of common path wavefront sensing/control and Coherent Differential Imaging techniques, highlight the latest results, and expose their relative strengths and weaknesses. We layout critical milestones for the field with the aim of enhancing future ground/space based high contrast imaging platforms. Techniques like these will help to bridge the daunting contrast gap required to image a terrestrial planet in the zone where it can retain liquid water, in reflected light around a G type star from space.",
"date": "2018-07-10",
"date_type": "published",
"publisher": "Society of Photo-Optical Instrumentation Engineers",
"place_of_pub": "Bellingham, WA",
"pagerange": "Art. No. 107031U",
"id_number": "CaltechAUTHORS:20181203-104212029",
"isbn": "9781510619593",
"book_title": "Adaptive Optics Systems VI",
"official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181203-104212029",
"rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.",
"funders": {
"items": [
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"agency": "European Research Council (ERC)",
"grant_number": "678194"
}
]
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"id": "Close-L-M",
"name": {
"family": "Close",
"given": "Laird M."
}
},
{
"id": "Schreiber-L",
"name": {
"family": "Schreiber",
"given": "Laura"
}
},
{
"id": "Schmidt-D",
"name": {
"family": "Schmidt",
"given": "Dirk"
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"doi": "10.1117/12.2314260",
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