[ { "id": "authors:mehe9-8p083", "collection": "authors", "collection_id": "mehe9-8p083", "cite_using_url": "https://authors.library.caltech.edu/records/mehe9-8p083", "type": "article", "title": "Searching for Planets Orbiting \u03f5 Eridani with JWST/NIRCam", "author": [ { "family_name": "Llop-Sayson", "given_name": "Jorge", "orcid": "0000-0002-3414-784X", "clpid": "Llop-Sayson-Jorge" }, { "family_name": "Beichman", "given_name": "Charles", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Bryden", "given_name": "Geoffrey", "orcid": "0000-0001-5966-837X", "clpid": "Bryden-Geoffrey" }, { "family_name": "Ygouf", "given_name": "Marie", "orcid": "0000-0001-7591-2731", "clpid": "Ygouf-M" }, { "family_name": "Gaspar", "given_name": "Andras", "orcid": "0000-0001-8612-3236" }, { "family_name": "Thompson", "given_name": "William", "orcid": "0000-0001-5684-4593" }, { "family_name": "Sanghi", "given_name": "Aniket", "orcid": "0000-0002-1838-4757", "clpid": "Sanghi-Aniket" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Greenbaum", "given_name": "Alexandra Z.", "orcid": "0000-0002-7162-8036", "clpid": "Greenbaum-Alexandra-Z" }, { "family_name": "Leisenring", "given_name": "Jarron", "orcid": "0000-0002-0834-6140" }, { "family_name": "Wolff", "given_name": "Schuyler", "orcid": "0000-0002-9977-8255" }, { "family_name": "Rieke", "given_name": "Marcia", "orcid": "0000-0002-7893-6170" }, { "family_name": "Rieke", "given_name": "George", "orcid": "0000-0003-2303-6519" } ], "abstract": "

We present observations of \u03f5 Eridani with the JWST/NIRCam coronagraph aimed at imaging planets orbiting within this system. In particular, these observations targeted (1) the Jupiter-like planet, first detected orbiting at 3.5 au with radial velocity observations, and (2) the planet postulated to be responsible for carving the edges of \u03f5 Eridani’s outer ring, expected to orbit at 40–50 au. However, no point sources were detected at a statistically significant level. We report new, improved upper limits at 4 μm: ∼1 × 10−6 contrast at 1″, and ∼2 × 10−8 beyond 5″. The latter contrast limit precludes Saturn-mass planets at separations >16 au given current models. We also report upper limits for \u03f5 Eridani’s disk emission at 4 μm. While the radial surface brightness profile shows no evidence of emission, we detect a 1σ surface brightness signal on the east side of the system, consistent with forward scattering emission expected for \u03f5 Eridani’s disk inclination. Finally, we evaluate the performance of the 3-roll observation strategy, which was first employed in these observations: the gains in contrast are modest, with 20%–30% improvements with respect to the conventional two-roll strategy.

", "doi": "10.3847/1538-3881/adf727", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2025-10", "series_number": "4", "volume": "170", "issue": "4", "pages": "229" }, { "id": "authors:g8206-gf406", "collection": "authors", "collection_id": "g8206-gf406", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200722-110124170", "type": "article", "title": "Two Directly Imaged, Wide-orbit Giant Planets around the Young, Solar Analog TYC 8998-760-1", "author": [ { "family_name": "Bohn", "given_name": "Alexander J.", "orcid": "0000-0003-1401-9952", "clpid": "Bohn-A-J" }, { "family_name": "Kenworthy", "given_name": "Matthew A.", "orcid": "0000-0002-7064-8270", "clpid": "Kenworthy-M-A" }, { "family_name": "Ginski", "given_name": "Christian", "clpid": "Ginski-C" }, { "family_name": "Rieder", "given_name": "Steven", "orcid": "0000-0003-3688-5798", "clpid": "Rieder-S" }, { "family_name": "Mamajek", "given_name": "Eric E.", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Pecaut", "given_name": "Mark J.", "orcid": "0000-0002-7859-1504", "clpid": "Pecaut-M-J" }, { "family_name": "Reggiani", "given_name": "Maddalena", "orcid": "0000-0003-2911-0898", "clpid": "Reggiani-M" }, { "family_name": "de Boer", "given_name": "Jozua", "clpid": "de-Boer-J" }, { "family_name": "Keller", "given_name": "Christoph U.", "orcid": "0000-0002-1368-841X", "clpid": "Keller-C-U" }, { "family_name": "Snik", "given_name": "Frans", "orcid": "0000-0003-1946-7009", "clpid": "Snik-F" }, { "family_name": "Southworth", "given_name": "John", "orcid": "0000-0002-3807-3198", "clpid": "Southworth-J" } ], "abstract": "Even though tens of directly imaged companions have been discovered in the past decades, the number of directly confirmed multiplanet systems is still small. Dynamical analysis of these systems imposes important constraints on formation mechanisms of these wide-orbit companions. As part of the Young Suns Exoplanet Survey we report the detection of a second planetary-mass companion around the 17 Myr-old, solar-type star TYC 8998-760-1 that is located in the Lower Centaurus Crux subgroup of the Scorpius\u2013Centaurus association. The companion has a projected physical separation of 320 au and several individual photometric measurements from 1.1 to 3.8 microns constrain a companion mass of 6 \u00b1 1 M_(Jup), which is equivalent to a mass ratio of q = 0.57 \u00b1 0.10% with respect to the primary. With the previously detected 14 \u00b1 3 M_(Jup) companion that is orbiting the primary at 160 au, TYC 8998-760-1 is the first directly imaged multiplanet system that is detected around a young, solar analog. We show that circular orbits are stable, but that mildly eccentric orbits for either/both components (e > 0.1) are chaotic on gigayear timescales, implying in situ formation or a very specific ejection by an unseen third companion. Due to the wide separations of the companions TYC 8998-760-1 is an excellent system for spectroscopic and photometric follow-up with space-based observatories such as the James Webb Space Telescope.", "doi": "10.3847/2041-8213/aba27e", "issn": "2041-8213", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2020-07-20", "series_number": "1", "volume": "898", "issue": "1", "pages": "Art. No. L16" }, { "id": "authors:p32nw-tds18", "collection": "authors", "collection_id": "p32nw-tds18", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200501-110445577", "type": "article", "title": "Keck/NIRC2 L'-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70", "author": [ { "family_name": "Wang", "given_name": "Jason J.", "orcid": "0000-0003-0774-6502", "clpid": "Wang-Jason-J" }, { "family_name": "Ginzburg", "given_name": "Sivan" }, { "family_name": "Ren", "given_name": "Bin", "orcid": "0000-0003-1698-9696", "clpid": "Ren-Bin" }, { "family_name": "Wallack", "given_name": "Nicole", "orcid": "0000-0003-0354-0187", "clpid": "Wallack-N-L" }, { "family_name": "Gao", "given_name": "Peter", "orcid": "0000-0002-8518-9601" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Bond", "given_name": "Charlotte Z." }, { "family_name": "Cetre", "given_name": "Sylvain" }, { "family_name": "Wizinowich", "given_name": "Peter", "orcid": "0000-0002-1646-442X" }, { "family_name": "De Rosa", "given_name": "Robert J.", "orcid": "0000-0002-4918-0247" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Liu", "given_name": "Michael C.", "orcid": "0000-0003-2232-7664" }, { "family_name": "Alvarez", "given_name": "Carlos" }, { "family_name": "Baranec", "given_name": "Christoph", "orcid": "0000-0002-1917-9157" }, { "family_name": "Choquet", "given_name": "\u00c9lodie", "orcid": "0000-0002-9173-0740" }, { "family_name": "Chun", "given_name": "Mark" }, { "family_name": "Delorme", "given_name": "Jacques-Robert", "clpid": "Delorme-J-R" }, { "family_name": "Duch\u00eane", "given_name": "Gaspard" }, { "family_name": "Ghez", "given_name": "Andrea M.", "orcid": "0000-0003-3230-5055" }, { "family_name": "Guyon", "given_name": "Olivier", "orcid": "0000-0002-1097-9908" }, { "family_name": "Hall", "given_name": "Donald N. B." }, { "family_name": "Jensen-Clem", "given_name": "Rebecca", "orcid": "0000-0003-0054-2953" }, { "family_name": "Jovanovic", "given_name": "Nemanja", "orcid": "0000-0001-5213-6207", "clpid": "Jovanovic-N" }, { "family_name": "Lilley", "given_name": "Scott" }, { "family_name": "M\u00e9nard", "given_name": "Fran\u00e7ois", "orcid": "0000-0002-1637-7393" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Millar-Blanchaer", "given_name": "Maxwell A.", "orcid": "0000-0001-6205-9233", "clpid": "Millar-Blanchaer-M-A" }, { "family_name": "Ngo", "given_name": "Henry", "orcid": "0000-0001-5172-4859" }, { "family_name": "Pinte", "given_name": "Christophe", "orcid": "0000-0001-5907-5179" }, { "family_name": "Ragland", "given_name": "Sam" }, { "family_name": "Wang", "given_name": "Ji", "orcid": "0000-0002-4361-8885" }, { "family_name": "Wetherell", "given_name": "Ed" }, { "family_name": "Williams", "given_name": "Jonathan P.", "orcid": "0000-0001-5058-695X" }, { "family_name": "Ygouf", "given_name": "Marie", "orcid": "0000-0001-7591-2731", "clpid": "Ygouf-M" }, { "family_name": "Zuckerman", "given_name": "Ben" }, { "family_name": "Matthews", "given_name": "Keith", "clpid": "Matthews-Keith-Astronomy" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" } ], "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.", "doi": "10.3847/1538-3881/ab8aef", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2020-06", "series_number": "6", "volume": "159", "issue": "6", "pages": "Art. No. 263" }, { "id": "authors:8279q-ysm77", "collection": "authors", "collection_id": "8279q-ysm77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191122-075655860", "type": "article", "title": "Near-Infrared Imaging of a Spiral in the CQ Tau Disk", "author": [ { "family_name": "Uyama", "given_name": "Taichi", "orcid": "0000-0002-6879-3030", "clpid": "Uyama-Taichi" }, { "family_name": "Muto", "given_name": "Takayuki" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Christiaens", "given_name": "Valentin", "orcid": "0000-0002-0101-8814" }, { "family_name": "Hashimoto", "given_name": "Jun", "orcid": "0000-0002-3053-3575" }, { "family_name": "Kudo", "given_name": "Tomoyuki", "orcid": "0000-0002-9294-1793" }, { "family_name": "Kuzuhara", "given_name": "Masayuki", "orcid": "0000-0002-4677-9182" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Beichman", "given_name": "Charles", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Absil", "given_name": "Olivier", "orcid": "0000-0002-4006-6237", "clpid": "Absil-Olivier" }, { "family_name": "Akiyama", "given_name": "Eiji", "orcid": "0000-0002-5082-8880" }, { "family_name": "Bae", "given_name": "Jaehan" }, { "family_name": "Bottom", "given_name": "Michael", "orcid": "0000-0003-1341-5531" }, { "family_name": "Choquet", "given_name": "\u00c9lodie", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Currie", "given_name": "Thayne", "orcid": "0000-0002-7405-3119" }, { "family_name": "Dong", "given_name": "Ruobing", "orcid": "0000-0001-9290-7846" }, { "family_name": "Follette", "given_name": "Katherine B.", "orcid": "0000-0002-7821-0695" }, { "family_name": "Fukagawa", "given_name": "Misato" }, { "family_name": "Guidi", "given_name": "Greta" }, { "family_name": "Huby", "given_name": "Elsa" }, { "family_name": "Kwon", "given_name": "Jungmi", "orcid": "0000-0003-2815-7774" }, { "family_name": "Mayama", "given_name": "Satoshi", "orcid": "0000-0002-3424-6266" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Reggiani", "given_name": "Maddalena", "orcid": "0000-0003-2911-0898" }, { "family_name": "Ricci", "given_name": "Luca" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" }, { "family_name": "Tamura", "given_name": "Motohide", "orcid": "0000-0002-6510-0681" }, { "family_name": "Testi", "given_name": "Leonardo", "orcid": "0000-0003-1859-3070" }, { "family_name": "Wallack", "given_name": "Nicole", "orcid": "0000-0003-0354-0187", "clpid": "Wallack-N-L" }, { "family_name": "Williams", "given_name": "Jonathan", "orcid": "0000-0001-5058-695X" }, { "family_name": "Zhu", "given_name": "Zhaohuan", "orcid": "0000-0003-3616-6822" } ], "abstract": "We present L'-band Keck/NIRC2 imaging and H-band Subaru/AO188+HiCIAO polarimetric observations of the CQ Tau disk with a new spiral arm. Apart from the spiral feature, our observations could not detect any companion candidates. We traced the spiral feature from the r\u00b2-scaled High-Contrast Coronographic Imager for Adaptive Optics (HiCIAO) polarimetric intensity image and the fitted result is used for forward modeling to reproduce the ADI-reduced NIRC2 image. We estimated the original surface brightness after throughput correction in the L' band to be ~126 mJy arcsec\u207b\u00b2 at most. We suggest that the grain temperature of the spiral may be heated up to ~200 K in order to explain both of the H- and L'-band results. The H-band emission at the location of the spiral originates from the scattering from the disk surface while both scattering and thermal emission may contribute to the L'-band emission. If the central star is only the light source of scattered light, the spiral emission at the L' band should be thermal emission. If an inner disk also acts as the light source, the scattered light and the thermal emission may equally contribute to the L'-band spiral structure.", "doi": "10.3847/1538-3881/ab7006", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2020-03", "series_number": "3", "volume": "159", "issue": "3", "pages": "Art. No. 118" }, { "id": "authors:mnkwr-49k53", "collection": "authors", "collection_id": "mnkwr-49k53", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200228-075427719", "type": "article", "title": "Young Suns Exoplanet Survey: Detection of a wide-orbit planetary-mass companion to a solar-type Sco-Cen member", "author": [ { "family_name": "Bohn", "given_name": "A. J.", "orcid": "0000-0003-1401-9952", "clpid": "Bohn-A-J" }, { "family_name": "Kenworthy", "given_name": "M. A.", "orcid": "0000-0002-7064-8270", "clpid": "Kenworthy-M-A" }, { "family_name": "Ginski", "given_name": "C.", "clpid": "Ginski-C" }, { "family_name": "Manara", "given_name": "C. F.", "orcid": "0000-0003-3562-262X", "clpid": "Manara-C-F" }, { "family_name": "Pecaut", "given_name": "M. J.", "clpid": "Pecaut-M-J" }, { "family_name": "de\u00a0Boer", "given_name": "J.", "clpid": "de-Boer-J" }, { "family_name": "Keller", "given_name": "C. U.", "clpid": "Keller-C-U" }, { "family_name": "Mamajek", "given_name": "E. E.", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Reggiani", "given_name": "M.", "orcid": "0000-0003-2911-0898", "clpid": "Reggiani-M" }, { "family_name": "Todorov", "given_name": "K. O.", "orcid": "0000-0002-9276-8118", "clpid": "Todorov-K-O" }, { "family_name": "Snik", "given_name": "F.", "clpid": "Snik-F" } ], "abstract": "The Young Suns Exoplanet Survey consists of a homogeneous sample of 70 young, solar-mass stars located in the Lower Centaurus-Crux subgroup of the Scorpius-Centaurus association with an average age of 15 \u00b1 3\u2009Myr. We report the detection of a co-moving companion around the K3IV star TYC 8998-760-1 (2MASSJ13251211\u20136456207) that is located at a distance of 94.6 \u00b1 0.3\u2009pc using SPHERE/IRDIS on the VLT. Spectroscopic observations with VLT/X-SHOOTER constrain the mass of the star to 1.00\u00b10.02M\u2299 and an age of 16.7\u00b11.4 Myr. The companion TYC 8998-760-1 b is detected at a projected separation of 1.71\u2033, which implies a projected physical separation of 162\u2009au. Photometric measurements ranging from Y to M band provide a mass estimate of 14\u00b13 M_(jup) by comparison to BT-Settl and AMES-dusty isochrones, corresponding to a mass ratio of q = 0.013 \u00b1 0.003 with respect to the primary. We rule out additional companions to TYC 8998-760-1 that are more massive than 12 M_(jup) and farther than 12\u2009au away from the host. Future polarimetric and spectroscopic observations of this system with ground and space based observatories will facilitate testing of formation and evolution scenarios shaping the architecture of the circumstellar environment around this 'young Sun'.", "doi": "10.1093/mnras/stz3462", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2020-02", "series_number": "1", "volume": "492", "issue": "1", "pages": "431-443" }, { "id": "authors:1pz11-k3p78", "collection": "authors", "collection_id": "1pz11-k3p78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190613-112836662", "type": "article", "title": "The Effect of Binarity on Circumstellar Disk Evolution", "author": [ { "family_name": "Barenfeld", "given_name": "Scott A.", "orcid": "0000-0001-5222-6851", "clpid": "Barenfeld-S-A" }, { "family_name": "Carpenter", "given_name": "John M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Rizzuto", "given_name": "Aaron C.", "orcid": "0000-0001-9982-1332", "clpid": "Rizzuto-A-C" }, { "family_name": "Kraus", "given_name": "Adam L.", "orcid": "0000-0001-9811-568X", "clpid": "Kraus-A-L" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Akeson", "given_name": "Rachel L.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Jensen", "given_name": "Eric L. N.", "orcid": "0000-0002-4625-7333", "clpid": "Jensen-E-L-N" }, { "family_name": "Hinkley", "given_name": "Sasha", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" } ], "abstract": "We present new results on how the presence of stellar companions affects disk evolution based on a study of the 5\u201311 Myr old Upper Scorpius OB Association. Of the 50 G0-M3 Upper Sco members with disks in our sample, only seven host a stellar companion within 2'' and brighter than K = 15, compared to 35 of 75 members without disks. This matches a trend seen in the 1\u20132 Myr old Taurus region, where systems with a stellar companion within 40 au have a lower fraction of infrared-identified disks than those without such companions, indicating shorter disk lifetimes in close multiple systems. However, the fractions of disk systems with a stellar companion within 40 au match in Upper Sco and Taurus. Additionally, we see no difference in the millimeter brightnesses of disks in Upper Sco systems with and without companions, in contrast to Taurus where systems with a companion within 300 au are significantly fainter than wider and single systems. These results suggest that the effects of stellar companions on disk lifetimes occur within the first 1\u20132 Myr of disk evolution, after which companions play little further role. By contrast, disks around single stars lose the millimeter-sized dust grains in their outer regions between ages of 1\u20132 Myr and 5\u201311 Myr. The end result of small dust disk sizes and faint millimeter luminosities is the same whether the disk has been truncated by a companion or has evolved through internal processes.", "doi": "10.3847/1538-4357/ab1e50", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2019-06-10", "series_number": "1", "volume": "878", "issue": "1", "pages": "Art. No. 45" }, { "id": "authors:2tm0h-asr65", "collection": "authors", "collection_id": "2tm0h-asr65", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190503-133931082", "type": "article", "title": "Discovery of a directly imaged disk in scattered light around the Sco-Cen member Wray 15-788", "author": [ { "family_name": "Bohn", "given_name": "A. J.", "orcid": "0000-0003-1401-9952", "clpid": "Bohn-A-J" }, { "family_name": "Kenworthy", "given_name": "M. A.", "orcid": "0000-0002-7064-8270", "clpid": "Kenworthy-M-A" }, { "family_name": "Ginski", "given_name": "C.", "clpid": "Ginski-C" }, { "family_name": "Benisty", "given_name": "M.", "orcid": "0000-0002-7695-7605", "clpid": "Benisty-M" }, { "family_name": "De Boer", "given_name": "J.", "clpid": "De-Boer-J" }, { "family_name": "Keller", "given_name": "C. U.", "clpid": "Keller-C-U" }, { "family_name": "Mamajek", "given_name": "E. E.", "orcid": "0000-0003-2008-1488", "clpid": "Mamajek-E-E" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Muro-Arena", "given_name": "G. A.", "clpid": "Muro-Arena-G-A" }, { "family_name": "Pecaut", "given_name": "M. J.", "clpid": "Pecaut-M-J" }, { "family_name": "Snik", "given_name": "F.", "clpid": "Snik-F" }, { "family_name": "Wolff", "given_name": "S. G.", "clpid": "Wolff-S-G" }, { "family_name": "Reggiani", "given_name": "M.", "orcid": "0000-0003-2911-0898", "clpid": "Reggiani-M" } ], "abstract": "Context. Protoplanetary disks are the birth environments of planetary systems. Therefore, the study of young, circumstellar environments is essential in understanding the processes taking place in planet formation and the evolution of planetary systems.\nAims. We detect and characterize circumstellar disks and potential companions around solar-type, pre-main sequence stars in the Scorpius-Centaurus association (Sco-Cen).\nMethods. As part of our ongoing survey we carried out high-contrast imaging with VLT/SPHERE/IRDIS to obtain polarized and total intensity images of the young (11_(\u22127)^(+16) Myr old) K3IV star Wray 15-788 within the Lower Centaurus Crux subgroup of Sco-Cen. For the total intensity images, we remove the stellar halo via an approach based on reference star differential imaging in combination with principal component analysis.\nResults. Both total intensity and polarimetric data resolve a disk around the young, solar-like Sco-Cen member Wray 15-788. Modeling of the stellar spectral energy distribution suggests that this is a protoplanetary disk at a transition stage. We detect a bright outer ring at a projected separation of ~370 mas (\u224856 au), hints of inner substructures at ~170 mas (\u224828 au), and a gap in between. Within a position angle range of only 60\u00b0 < \u03d5 < 240\u00b0, we are confident at the 5\u03c3 level that we detect actual scattered light flux from the outer ring of the disk; the remaining part is indistinguishable from background noise. For the detected part of the outer ring we determine a disk inclination of i = 21\u00b0 \u00b1 6\u00b0 and a position angle of \u03c6 = 76\u00b0 \u00b1 16\u00b0. Furthermore, we find that Wray 15-788 is part of a binary system with the A2V star HD 98363 at a separation of ~50\u2032\u2032 (\u22486900 au).\nConclusions. The detection of only half of the outer ring might be due to shadowing by a misaligned inner disk. A potential substellar companion can cause the misalignment of the inner structures and can be responsible for clearing the detected gap from scattering material. However, we cannot rule out the possibility of a non-detection due to our limited signal-to-noise ratio (S/N), combined with brightness azimuthal asymmetry. From our data we can exclude companions more massive than 10 M_(jup) within the gap at a separation of ~230 mas (\u224835 au). Additional data are required to characterize the disk's peculiar morphology and to set tighter constraints on the potential perturber's orbital parameters and mass.", "doi": "10.1051/0004-6361/201834523", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2019-04", "volume": "624", "pages": "Art. No. A87" }, { "id": "authors:crwjn-e5v50", "collection": "authors", "collection_id": "crwjn-e5v50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190214-105330131", "type": "article", "title": "Reference Star Differential Imaging of Close-in Companions and Circumstellar Disks with the NIRC2 Vortex Coronagraph at the W. M. Keck Observatory", "author": [ { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Ngo", "given_name": "Henry", "orcid": "0000-0001-5172-4859", "clpid": "Ngo-Henry-Hoang-Khoi-Exoplanets" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Absil", "given_name": "Olivier", "orcid": "0000-0002-4006-6237", "clpid": "Absil-Olivier" }, { "family_name": "Choquet", "given_name": "\u00c9lodie", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Cook", "given_name": "Therese", "clpid": "Cook-Therese" }, { "family_name": "Gomez Gonzalez", "given_name": "Carlos A.", "orcid": "0000-0003-2050-1710", "clpid": "G\u00f3mez-Gonz\u00e1lez-C-A" }, { "family_name": "Huby", "given_name": "Elsa", "clpid": "Huby-Elsa" }, { "family_name": "Matthews", "given_name": "Keith", "clpid": "Matthews-Keith-Astronomy" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Reggiani", "given_name": "Maddalena", "orcid": "0000-0003-2911-0898", "clpid": "Reggiani-M" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" }, { "family_name": "Wallack", "given_name": "Nicole", "orcid": "0000-0003-0354-0187", "clpid": "Wallack-N-L" }, { "family_name": "Xuan", "given_name": "W. Jerry", "orcid": "0000-0002-6618-1137", "clpid": "Xuan-Wenhao-Jerry" } ], "abstract": "Reference star differential imaging (RDI) is a powerful strategy for high-contrast imaging. Using example observations taken with the vortex coronagraph mode of Keck/NIRC2 in L' band, we demonstrate that RDI provides improved sensitivity to point sources at small angular separations compared to angular differential imaging (ADI). Applying RDI to images of the low-mass stellar companions HIP 79124 C (192 mas separation, \u0394L' = 4.01) and HIP 78233 B (141 mas separation, \u0394L' = 4.78), the latter a first imaging detection, increases the significance of their detections by up to a factor of 5 with respect to ADI. We compare methods for reference frame selection and find that pre-selection of frames improves detection significance of point sources by up to a factor of 3. In addition, we use observations of the circumstellar disks around MWC 758 and 2MASS J16042165\u22122130284 to show that RDI allows for accurate mapping of scattered light distributions without self-subtraction artifacts.", "doi": "10.3847/1538-3881/aafee2", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2019-03", "series_number": "3", "volume": "157", "issue": "3", "pages": "Art. No. 118" }, { "id": "authors:m8php-zz548", "collection": "authors", "collection_id": "m8php-zz548", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180817-160159509", "type": "article", "title": "An Excess of Jupiter Analogs in Super-Earth Systems", "author": [ { "family_name": "Bryan", "given_name": "Marta L.", "orcid": "0000-0002-6076-5967", "clpid": "Bryan-M-L" }, { "family_name": "Knutson", "given_name": "Heather A.", "orcid": "0000-0002-5375-4725", "clpid": "Knutson-H-A" }, { "family_name": "Lee", "given_name": "Eve J.", "orcid": "0000-0002-1228-9820", "clpid": "Lee-Eve-J" }, { "family_name": "Fulton", "given_name": "B. J.", "orcid": "0000-0003-3504-5316", "clpid": "Fulton-B-J" }, { "family_name": "Batygin", "given_name": "Konstantin", "orcid": "0000-0002-7094-7908", "clpid": "Batygin-K" }, { "family_name": "Ngo", "given_name": "Henry", "orcid": "0000-0001-5172-4859", "clpid": "Ngo-Henry-Hoang-Khoi-Exoplanets" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" } ], "abstract": "We use radial velocity (RV) observations to search for long-period gas giant companions in systems hosting inner super-Earth (1\u20134 R\u2295, 1\u201310 M\u2295) planets to constrain formation and migration scenarios for this population. We consistently refit published RV data sets for 65 stars and find nine systems with statistically significant trends indicating the presence of an outer companion. We combine these RV data with AO images to constrain the masses and semi-major axes of these companions. We quantify our sensitivity to the presence of long-period companions by fitting the sample with a power-law distribution and find an occurrence rate of 39% \u00b1 7% for companions 0.5\u201320 M_(Jup) and 1\u201320 au. Half of our systems were discovered by the transit method, and half were discovered by the RV method. While differences in the RV baselines and number of data points between the two samples lead to different sensitivities to distant companions, we find that occurrence rates of gas giant companions in each sample are consistent at the 0.5\u03c3 level. We compare the frequency of Jupiter analogs in these systems to the equivalent rate from field star surveys and find that Jupiter analogs are more common around stars hosting super-Earths. We conclude that the presence of outer gas giants does not suppress the formation of inner super-Earths, and that these two populations of planets instead appear to be correlated. We also find that the stellar metallicities of systems with gas giant companions are higher than those without companions, in agreement with the well-established metallicity correlation from RV surveys of field stars.", "doi": "10.3847/1538-3881/aaf57f", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2019-02", "series_number": "2", "volume": "157", "issue": "2", "pages": "Art. No. 52" }, { "id": "authors:4fgrs-68k96", "collection": "authors", "collection_id": "4fgrs-68k96", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190103-105531269", "type": "article", "title": "Deep Exploration of \u03f5 Eridani with Keck Ms-band Vortex Coronagraphy and Radial Velocities: Mass and Orbital Parameters of the Giant Exoplanet", "author": [ { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Hirsch", "given_name": "Lea", "orcid": "0000-0001-8058-7443", "clpid": "Hirsch-L-A" }, { "family_name": "Lee", "given_name": "Eve J.", "orcid": "0000-0002-1228-9820", "clpid": "Lee-Eve-J" }, { "family_name": "Ruffio", "given_name": "Jean-Baptiste", "orcid": "0000-0003-2233-4821", "clpid": "Ruffio-J-B" }, { "family_name": "Bottom", "given_name": "Michael", "orcid": "0000-0003-1341-5531", "clpid": "Bottom-M" }, { "family_name": "Fulton", "given_name": "Benjamin J.", "orcid": "0000-0003-3504-5316", "clpid": "Fulton-B-J" }, { "family_name": "Absil", "given_name": "Olivier", "orcid": "0000-0002-4006-6237", "clpid": "Absil-Olivier" }, { "family_name": "Beichman", "given_name": "Charles", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Bowler", "given_name": "Brendan", "orcid": "0000-0003-2649-2288", "clpid": "Bowler-B-P" }, { "family_name": "Bryan", "given_name": "Marta", "orcid": "0000-0002-6076-5967", "clpid": "Bryan-M-L" }, { "family_name": "Choquet", "given_name": "\u00c9lodie", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Ciardi", "given_name": "David", "orcid": "0000-0002-5741-3047", "clpid": "Ciardi-D-R" }, { "family_name": "Christiaens", "given_name": "Valentin", "orcid": "0000-0002-0101-8814", "clpid": "Christiaens-V" }, { "family_name": "Defr\u00e8re", "given_name": "Denis", "orcid": "0000-0003-3499-2506", "clpid": "Defr\u00e8re-D" }, { "family_name": "Gomez Gonzalez", "given_name": "Carlos Alberto", "orcid": "0000-0003-2050-1710", "clpid": "G\u00f3mez-Gonz\u00e1lez-C-A" }, { "family_name": "Howard", "given_name": "Andrew W.", "orcid": "0000-0001-8638-0320", "clpid": "Howard-A-W" }, { "family_name": "Huby", "given_name": "Elsa", "clpid": "Huby-Elsa" }, { "family_name": "Isaacson", "given_name": "Howard", "orcid": "0000-0002-0531-1073", "clpid": "Isaacson-H-T" }, { "family_name": "Jensen-Clem", "given_name": "Rebecca", "orcid": "0000-0003-0054-2953", "clpid": "Jensen-Clem-R-M" }, { "family_name": "Kosiarek", "given_name": "Molly", "orcid": "0000-0002-6115-4359", "clpid": "Kosiarek-M-R" }, { "family_name": "Marcy", "given_name": "Geoff", "orcid": "0000-0002-2909-0113", "clpid": "Marcy-G-W" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Petigura", "given_name": "Erik", "orcid": "0000-0003-0967-2893", "clpid": "Petigura-E-A" }, { "family_name": "Reggiani", "given_name": "Maddalena", "orcid": "0000-0003-2911-0898", "clpid": "Reggiani-M" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" }, { "family_name": "Sinukoff", "given_name": "Evan", "orcid": "0000-0002-5658-0601", "clpid": "Sinukoff-E" }, { "family_name": "Wang", "given_name": "Ji", "orcid": "0000-0002-4361-8885", "clpid": "Wang-Ji" }, { "family_name": "Weiss", "given_name": "Lauren", "orcid": "0000-0002-3725-3058", "clpid": "Weiss-L-M" }, { "family_name": "Ygouf", "given_name": "Marie", "orcid": "0000-0001-7591-2731", "clpid": "Ygouf-M" } ], "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.", "doi": "10.3847/1538-3881/aaef8a", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2019-01", "series_number": "1", "volume": "157", "issue": "1", "pages": "Art. No. 33" }, { "id": "authors:yvya2-c6174", "collection": "authors", "collection_id": "yvya2-c6174", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181115-095346090", "type": "article", "title": "Maximum Angular Separation Epochs for Exoplanet Imaging Observations", "author": [ { "family_name": "Kane", "given_name": "Stephen R.", "orcid": "0000-0002-7084-0529", "clpid": "Kane-S-R" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Turnbull", "given_name": "Margaret C.", "clpid": "Turnbull-M-C" } ], "abstract": "Direct imaging of exoplanets presents both significant challenges and significant gains. The advantages primarily lie in receiving emitted and, with future instruments, reflected photons at phase angles not accessible by other techniques, enabling the potential for atmospheric studies and the detection of rotation and surface features. The challenges are numerous and include coronagraph development and achieving the necessary contrast ratio. Here, we address the specific challenge of determining epochs of maximum angular separation for the star and planet. We compute orbital ephemerides for known transiting and radial velocity planets, taking Keplerian orbital elements into account. We provide analytical expressions for angular star\u2013planet separation as a function of the true anomaly, including the locations of minimum and maximum. These expressions are used to calculate uncertainties for maximum angular separation as a function of time for the known exoplanets, and we provide strategies for improving ephemerides with application to proposed and planned imaging missions.", "doi": "10.3847/1538-3881/aae981", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2018-12", "series_number": "6", "volume": "156", "issue": "6", "pages": "Art. No. 267" }, { "id": "authors:zswd2-8xd98", "collection": "authors", "collection_id": "zswd2-8xd98", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181220-092840342", "type": "article", "title": "Substellar and low-mass dwarf identification with near-infrared imaging space observatories", "author": [ { "family_name": "Holwerda", "given_name": "B. W.", "orcid": "0000-0002-4884-6756", "clpid": "Holwerda-B-W" }, { "family_name": "Bridge", "given_name": "J. S.", "clpid": "Bridge-J-S" }, { "family_name": "Ryan", "given_name": "R.", "clpid": "Ryan-R" }, { "family_name": "Kenworthy", "given_name": "M. A.", "orcid": "0000-0002-7064-8270", "clpid": "Kenworthy-M-A" }, { "family_name": "Pirzkal", "given_name": "N.", "orcid": "0000-0003-3382-5941", "clpid": "Pirzkal-Nor" }, { "family_name": "Andersen", "given_name": "M.", "clpid": "Andersen-M" }, { "family_name": "Wilkins", "given_name": "S.", "clpid": "Wilkins-S" }, { "family_name": "Smit", "given_name": "R.", "orcid": "0000-0001-8034-7802", "clpid": "Smit-Renske" }, { "family_name": "Bernard", "given_name": "S. R.", "clpid": "Bernard-S-R" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Steele", "given_name": "R.", "clpid": "Steele-R" }, { "family_name": "Bouwens", "given_name": "R. C.", "clpid": "Bouwens-R-C" } ], "abstract": "Aims. We aim to evaluate the near-infrared colors of brown dwarfs as observed with four major infrared imaging space observatories: the Hubble Space Telescope (HST), the James Webb Space Telescope (JWST), the Euclid mission, and the WFIRST telescope. \n\nMethods. We used the SPLAT SPEX/ISPEX spectroscopic library to map out the colors of the M-, L-, and T-type dwarfs. We have identified which color\u2013color combination is optimal for identifying broad type and which single color is optimal to then identify the subtype (e.g., T0-9). We evaluated each observatory separately as well as the narrow-field (HST and JWST) and wide-field (Euclid and WFIRST) combinations. \n\nResults. The Euclid filters perform equally well as HST wide filters in discriminating between broad types of brown dwarfs. WFIRST performs similarly well, despite a wider selection of filters. However, subtyping with any combination of Euclid and WFIRST observations remains uncertain due to the lack of medium, or narrow-band filters. We argue that a medium band added to the WFIRST filter selection would greatly improve its ability to preselect brown dwarfs its imaging surveys. \n\nConclusions. The HST filters used in high-redshift searches are close to optimal to identify broad stellar type. However, the addition of F127M to the commonly used broad filter sets would allow for unambiguous subtyping. An improvement over HST is one of two broad and medium filter combinations on JWST: pairing F140M with either F150W or F162M discriminates very well between subtypes.", "doi": "10.1051/0004-6361/201832838", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2018-12", "volume": "620", "pages": "Art. No. A132" }, { "id": "authors:7v2bn-psh58", "collection": "authors", "collection_id": "7v2bn-psh58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181023-090840047", "type": "article", "title": "A Deep Search for Planets in the Inner 15 au around Vega", "author": [ { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Nilsson", "given_name": "Ricky", "orcid": "0000-0002-5408-4954", "clpid": "Nilsson-R" }, { "family_name": "Aguilar", "given_name": "Jonathan", "orcid": "0000-0003-3184-0873", "clpid": "Aguilar-J" }, { "family_name": "Vasisht", "given_name": "Gautam", "orcid": "0000-0002-1871-6264", "clpid": "Vasisht-G" }, { "family_name": "Oppenheimer", "given_name": "Rebecca", "orcid": "0000-0001-7130-7681", "clpid": "Oppenheimer-Rebecca" }, { "family_name": "Su", "given_name": "Kate Y. L.", "orcid": "0000-0002-3532-5580", "clpid": "Su-Katherine-Y-L" }, { "family_name": "Cady", "given_name": "Eric", "orcid": "0000-0002-8789-2931", "clpid": "Cady-E" }, { "family_name": "Lockhart", "given_name": "Thomas", "clpid": "Lockhart-T-G" }, { "family_name": "Matthews", "given_name": "Christopher", "orcid": "0000-0002-7782-0272", "clpid": "Matthews-C" }, { "family_name": "Dekany", "given_name": "Richard", "clpid": "Dekany-Richard" }, { "family_name": "Leisenring", "given_name": "Jarron", "orcid": "0000-0002-0834-6140", "clpid": "Leisenring-J" }, { "family_name": "Ygouf", "given_name": "Marie", "orcid": "0000-0001-7591-2731", "clpid": "Ygouf-M" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Pueyo", "given_name": "Laurent", "orcid": "0000-0003-3818-408X", "clpid": "Pueyo-L" }, { "family_name": "Beichman", "given_name": "Charles", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" } ], "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.", "doi": "10.3847/1538-3881/aae14f", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2018-11", "series_number": "5", "volume": "156", "issue": "5", "pages": "Art. No. 214" }, { "id": "authors:vhchg-taa69", "collection": "authors", "collection_id": "vhchg-taa69", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181205-163501986", "type": "article", "title": "Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments", "author": [ { "family_name": "Matthews", "given_name": "Elisabeth", "clpid": "Matthews-E" }, { "family_name": "Hinkley", "given_name": "Sasha", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" }, { "family_name": "Vigan", "given_name": "Arthur", "orcid": "0000-0002-5902-7828", "clpid": "Vigan-A" }, { "family_name": "Kennedy", "given_name": "Grant", "orcid": "0000-0001-6831-7547", "clpid": "Kennedy-G" }, { "family_name": "Sutlieff", "given_name": "Ben", "clpid": "Sutlieff-B" }, { "family_name": "Wickenden", "given_name": "Dawn", "clpid": "Wickenden-D" }, { "family_name": "Treves", "given_name": "Sam", "clpid": "Treves-S-B" }, { "family_name": "David", "given_name": "Trevor", "orcid": "0000-0001-6534-6246", "clpid": "David-T-J" }, { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Morales", "given_name": "Farisa", "orcid": "0000-0001-9414-3851", "clpid": "Morales-F-Y" }, { "family_name": "Shannon", "given_name": "Andrew", "clpid": "Shannon-A" }, { "family_name": "Stapelfeldt", "given_name": "Karl", "orcid": "0000-0002-2805-7338", "clpid": "Stapelfeldt-K-R" } ], "abstract": "Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR\u20098799 and HD\u200995086 systems, and even the Solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disc, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high-contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical time-scales to clear debris. The typical dynamical lower limit is \u223c0.2M_J in this work, and in some cases exceeds 1M_J. Direct imaging data, meanwhile, are typically sensitive to planets down to \u223c3.6M_J at 1\u2009arcsec, and 1.7M_J in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers.", "doi": "10.1093/mnras/sty1778", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2018-10-21", "series_number": "2", "volume": "480", "issue": "2", "pages": "2757-2783" }, { "id": "authors:355ky-nvq88", "collection": "authors", "collection_id": "355ky-nvq88", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180726-075612565", "type": "article", "title": "High-contrast imaging of HD 163296 with the Keck/NIRC2 L\u2032-band vortex coronograph", "author": [ { "family_name": "Guidi", "given_name": "G.", "clpid": "Guidi-G-M" }, { "family_name": "Ruane", "given_name": "G.", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Williams", "given_name": "J. P.", "orcid": "0000-0001-5058-695X", "clpid": "Williams-J-P" }, { "family_name": "Mawet", "given_name": "D.", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Testi", "given_name": "L.", "orcid": "0000-0003-1859-3070", "clpid": "Testi-L" }, { "family_name": "Zurlo", "given_name": "A.", "orcid": "0000-0002-5903-8316", "clpid": "Zurlo-A" }, { "family_name": "Absil", "given_name": "O.", "orcid": "0000-0002-4006-6237", "clpid": "Absil-Olivier" }, { "family_name": "Bottom", "given_name": "M.", "orcid": "0000-0003-1341-5531", "clpid": "Bottom-M" }, { "family_name": "Choquet", "given_name": "\u00c9.", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Christiaens", "given_name": "V.", "orcid": "0000-0002-0101-8814", "clpid": "Christiaens-V" }, { "family_name": "Femen\u00eda-Castell\u00e1", "given_name": "B.", "clpid": "Femen\u00eda-Castell\u00e1-B" }, { "family_name": "Huby", "given_name": "E.", "clpid": "Huby-Elsa" }, { "family_name": "Isella", "given_name": "A.", "orcid": "0000-0001-8061-2207", "clpid": "Isella-A" }, { "family_name": "Kastner", "given_name": "J.", "orcid": "0000-0002-3138-8250", "clpid": "Kastner-J-H" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Reggiani", "given_name": "M.", "orcid": "0000-0003-2911-0898", "clpid": "Reggiani-M" }, { "family_name": "Riggs", "given_name": "A.", "clpid": "Riggs-A" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-E" }, { "family_name": "Wallack", "given_name": "N.", "orcid": "0000-0003-0354-0187", "clpid": "Wallack-N-L" } ], "abstract": "We present observations of the nearby (D\u223c100\u2009pc) Herbig star HD 163296 taken with the vortex coronograph at Keck/NIRC2 in the L\u2032 band (3.7 \u03bcm) to search for planetary mass companions in the ringed disc surrounding this pre-main-sequence star. The images reveal an arc-like region of scattered light from the disc surface layers that is likely associated with the first bright ring detected with ALMA in the \u03bb = 1.3\u2009mm dust continuum at \u223c65 au. We also detect a point-like source at \u223c0.5\u2009arcsec projected separation in the north-east direction, close to the inner edge of the second gap in the millimetre images. Comparing the point source photometry with the atmospheric emission models of non-accreting giant planets, we obtain a mass of 6\u20137 M_J for a putative protoplanet, assuming a system age of 5 Myr. Based on the contrast at a 95\u2009per\u2009cent level of completeness calculated on the emission-free regions of our images, we set upper limits for the masses of giant planets of 8\u201315 M_J, 4.5\u20136.5 M_J, and 2.5\u20134.0 M_J at the locations of the first, second, and third gap in the millimetre dust continuum, respectively. Further deep, high-resolution thermal IR imaging of the HD 163296 system are warranted to confirm the presence and nature of the point source and to better understand the structure of the dust disc.", "doi": "10.1093/mnras/sty1642", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2018-09-11", "series_number": "2", "volume": "479", "issue": "2", "pages": "1505-1513" }, { "id": "authors:m8pas-z2t50", "collection": "authors", "collection_id": "m8pas-z2t50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171012-145251179", "type": "article", "title": "A Direct Imaging Survey of Spitzer detected debris disks: Occurrence of giant planets in dusty systems", "author": [ { "family_name": "Meshkat", "given_name": "Tiffany", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Bryan", "given_name": "Marta L.", "orcid": "0000-0002-6076-5967", "clpid": "Bryan-M-L" }, { "family_name": "Hinkley", "given_name": "Sasha", "orcid": "0000-0001-8074-2562", "clpid": "Hinkley-S" }, { "family_name": "Bowler", "given_name": "Brendan P.", "orcid": "0000-0003-2649-2288", "clpid": "Bowler-B-P" }, { "family_name": "Stapelfeldt", "given_name": "Karl R.", "orcid": "0000-0002-2805-7338", "clpid": "Stapelfeldt-K-R" }, { "family_name": "Batygin", "given_name": "Konstantin", "orcid": "0000-0002-7094-7908", "clpid": "Batygin-K" }, { "family_name": "Padgett", "given_name": "Deborah", "orcid": "0000-0001-5334-5107", "clpid": "Padgett-D-L" }, { "family_name": "Morales", "given_name": "Farisa Y.", "orcid": "0000-0001-9414-3851", "clpid": "Morales-F-Y" }, { "family_name": "Serabyn", "given_name": "Eugene", "clpid": "Serabyn-E" }, { "family_name": "Christiaens", "given_name": "Valentin", "orcid": "0000-0002-0101-8814", "clpid": "Christiaens-V" }, { "family_name": "Brandt", "given_name": "Timothy D.", "orcid": "0000-0003-2630-8073", "clpid": "Brandt-T-D" }, { "family_name": "Wahhaj", "given_name": "Zahed", "orcid": "0000-0001-8269-324X", "clpid": "Wahhaj-Z" } ], "abstract": "We describe a joint high-contrast imaging survey for planets at the Keck and Very Large Telescope of the last large sample of debris disks identified by the Spitzer Space Telescope. No new substellar companions were discovered in our survey of 30 Spitzer-selected targets. We combine our observations with data from four published surveys to place constraints on the frequency of planets around 130 debris disk single stars, the largest sample to date. For a control sample, we assembled contrast curves from several published surveys targeting 277 stars that do not show infrared excesses. We assumed a double power-law distribution in mass and semimajor axis (SMA) of the form f(m, a) = cM^\u03b1a^\u03b2, where we adopted power-law values and logarithmically flat values for the mass and SMA of planets. We find that the frequency of giant planets with masses 5\u201320 M_(Jup) and separations 10\u20131000 au around stars with debris disks is 6.27% (68% confidence interval 3.68%\u20139.76%), compared to 0.73% (68% confidence interval 0.20%\u20131.80%) for the control sample of stars without disks. These distributions differ at the 88% confidence level, tentatively suggesting distinctness of these samples.", "doi": "10.3847/1538-3881/aa8e9a", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2017-12", "series_number": "6", "volume": "154", "issue": "6", "pages": "Art. No. 245" }, { "id": "authors:0nyqq-vcj43", "collection": "authors", "collection_id": "0nyqq-vcj43", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170728-084506248", "type": "article", "title": "Deep Imaging Search for Planets Forming in the TW Hya Protoplanetary Disk with the Keck/NIRC2 Vortex Coronagraph", "author": [ { "family_name": "Ruane", "given_name": "G.", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Mawet", "given_name": "D.", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Kastner", "given_name": "J.", "orcid": "0000-0002-3138-8250", "clpid": "Kastner-J-H" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Bottom", "given_name": "M.", "orcid": "0000-0003-1341-5531", "clpid": "Bottom-M" }, { "family_name": "Femen\u00eda Castell\u00e1", "given_name": "B.", "clpid": "Femen\u00eda-Castell\u00e1-B" }, { "family_name": "Absil", "given_name": "O.", "orcid": "0000-0002-4006-6237", "clpid": "Absil-Olivier" }, { "family_name": "Gomez Gonzalez", "given_name": "C.", "orcid": "0000-0003-2050-1710", "clpid": "G\u00f3mez-Gonz\u00e1lez-C-A" }, { "family_name": "Huby", "given_name": "E.", "clpid": "Huby-Elsa" }, { "family_name": "Zhu", "given_name": "Z.", "orcid": "0000-0003-3616-6822", "clpid": "Zhu-Zhaohuan" }, { "family_name": "Jenson-Clem", "given_name": "R.", "clpid": "Jenson-Clem-R" }, { "family_name": "Choquet", "given_name": "\u00c9.", "orcid": "0000-0002-9173-0740", "clpid": "Choquet-\u00c9lodie" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-E" } ], "abstract": "Distinct gap features in the nearest protoplanetary disk, TW Hya (distance of 59.5 \u00b1 0.9 pc), may be signposts of ongoing planet formation. We performed long-exposure thermal infrared coronagraphic imaging observations to search for accreting planets, especially within dust gaps previously detected in scattered light and submillimeter-wave thermal emission. Three nights of observations with the Keck/NIRC2 vortex coronagraph in L' (3.4\u20134.1 \u03bcm) did not reveal any statistically significant point sources. We thereby set strict upper limits on the masses of non-accreting planets. In the four most prominent disk gaps at 24, 41, 47, and 88 au, we obtain upper mass limits of 1.6\u20132.3, 1.1\u20131.6, 1.1\u20131.5, and 1.0\u20131.2 Jupiter masses (M_J), assuming an age range of 7\u201310 Myr for TW Hya. These limits correspond to the contrast at 95% completeness (true positive fraction of 0.95) with a 1% chance of a false positive within 1'' of the star. We also approximate an upper limit on the product of the planet mass and planetary accretion rate of M_pM \u227e 10^(-8) M^2_j yr^(-1) implying that any putative ~0.1 M J planet, which could be responsible for opening the 24 au gap, is presently accreting at rates insufficient to build up a Jupiter mass within TW Hya's pre-main-sequence lifetime.", "doi": "10.3847/1538-3881/aa7b81", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2017-08", "series_number": "2", "volume": "154", "issue": "2", "pages": "Art. No. 73" }, { "id": "authors:2jk7m-7qg37", "collection": "authors", "collection_id": "2jk7m-7qg37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150526-162428581", "type": "article", "title": "Confirmation of the Planet around HD 95086 by Direct Imaging", "author": [ { "family_name": "Rameau", "given_name": "J.", "orcid": "0000-0003-0029-0258", "clpid": "Rameau-J" }, { "family_name": "Chauvin", "given_name": "G.", "clpid": "Chauvin-G" }, { "family_name": "Lagrange", "given_name": "A.-M.", "clpid": "Lagrange-A-M" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Boccaletti", "given_name": "A.", "orcid": "0000-0001-9353-2724", "clpid": "Boccaletti-A" }, { "family_name": "Quanz", "given_name": "S. P.", "orcid": "0000-0003-3829-7412", "clpid": "Quanz-S-P" }, { "family_name": "Currie", "given_name": "T.", "orcid": "0000-0002-7405-3119", "clpid": "Currie-T" }, { "family_name": "Mawet", "given_name": "D.", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Girard", "given_name": "J. H.", "orcid": "0000-0001-8627-0404", "clpid": "Girard-J-H" }, { "family_name": "Bonnefoy", "given_name": "M.", "orcid": "0000-0001-5579-5339", "clpid": "Bonnefoy-M" }, { "family_name": "Kenworthy", "given_name": "M.", "orcid": "0000-0002-7064-8270", "clpid": "Kenworthy-M-A" } ], "abstract": "VLT/NaCo angular differential imaging at L' (3.8 \u03bcm) revealed a probable giant planet comoving with the young and early-type HD 95086, also known to harbor an extended debris disk. The discovery was based on the proper motion analysis of two datasets spanning 15 months. However, the second dataset suffered from bad atmospheric conditions, which limited the significance of the re-detection at the 3\u03c3 level. In this Letter, we report new VLT/NaCo observations of HD 95086 obtained on 2013 June 26 and 27 at L' to recover the planet candidate. We unambiguously re-detect the companion HD 95086 b with multiple independent pipelines at a signal-to-noise ratio greater than or equal to 5. Combined with previously reported measurements, our astrometry decisively shows that the planet is comoving with HD 95086 and inconsistent with a background object. With a revised mass of 5 \u00b1 2 Jupiter masses, estimated from its L' photometry and \"hot-start\" models at 17 \u00b1 4 Myr, HD 95086 b becomes a new benchmark for further physical and orbital characterization of young giant planets.", "doi": "10.1088/2041-8205/779/2/L26", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2013-12-20", "series_number": "2", "volume": "779", "issue": "2", "pages": "Art. No. L26" } ]