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5 results on '"De Rosa, RJ"'

1. Constraining the nature of the PDS 70 protoplanets with VLTI/GRAVITY

Author

Wang, JJ, Vigan, A, Lacour, S, Nowak, M, Stolker, T, De Rosa, RJ, Ginzburg, S, Gao, P, Abuter, R, Amorim, A, Asensio-Torres, R, Bauböck, M, Benisty, M, Berger, JP, Beust, H, Beuzit, JL, Blunt, S, Boccaletti, A, Bohn, A, Bonnefoy, M, Bonnet, H, Brandner, W, Cantalloube, F, Caselli, P, Charnay, B, Chauvin, G, Choquet, E, Christiaens, V, Clénet, Y, Coudé Du Foresto, V, Cridland, A, De Zeeuw, PT, Dembet, R, Dexter, J, Drescher, A, Duvert, G, Eckart, A, Eisenhauer, F, Facchini, S, Gao, F, Garcia, P, Garcia Lopez, R, Gardner, T, Gendron, E, Genzel, R, Gillessen, S, Girard, J, Haubois, X, Heißel, G, Henning, T, Hinkley, S, Hippler, S, Horrobin, M, Houllé, M, Hubert, Z, Jiménez-Rosales, A, Jocou, L, Kammerer, J, Keppler, M, Kervella, P, Meyer, M, Kreidberg, L, Lagrange, AM, Lapeyrère, V, Le Bouquin, JB, Léna, P, Lutz, D, Maire, AL, Ménard, F, Mérand, A, Mollière, P, Monnier, JD, Mouillet, D, Müller, A, Nasedkin, E, Ott, T, Otten, GPPL, Paladini, C, Paumard, T, Perraut, K, Perrin, G, Pfuhl, O, Pueyo, L, Rameau, J, Rodet, L, Rodríguez-Coira, G, Rousset, G, Scheithauer, S, Shangguan, J, Shimizu, T, Stadler, J, Straub, O, Straubmeier, C, Sturm, E, Tacconi, LJ, Van Dishoeck, EF, Vincent, F, Von Fellenberg, SD, Ward-Duong, K, Widmann, F, Wang, JJ [0000-0003-0774-6502], Vigan, A [0000-0002-5902-7828], Lacour, S [0000-0002-6948-0263], Stolker, T [0000-0002-5823-3072], De Rosa, RJ [0000-0002-4918-0247], Gao, P [0000-0002-8518-9601], Asensio-Torres, R [0000-0003-2990-0726], Benisty, M [0000-0002-7695-7605], Beuzit, JL [0000-0002-7391-479X], Blunt, S [0000-0002-3199-2888], Bohn, A [0000-0003-1401-9952], Bonnefoy, M [0000-0001-5579-5339], Brandner, W [0000-0003-1939-6351], Caselli, P [0000-0003-1481-7911], Charnay, B [0000-0003-0977-6545], Choquet, E [0000-0002-9173-0740], Christiaens, V [0000-0002-0101-8814], Clénet, Y [0000-0002-8382-2020], De Zeeuw, PT [0000-0003-4175-3474], Dexter, J [0000-0003-3903-0373], Eckart, A [0000-0001-6049-3132], Facchini, S [0000-0003-4689-2684], Gao, F [0000-0002-2581-9114], Garcia Lopez, R [0000-0002-2144-0991], Gardner, T [0000-0002-3003-3183], Genzel, R [0000-0002-2767-9653], Gillessen, S [0000-0002-5708-0481], Girard, J [0000-0001-8627-0404], Henning, T [0000-0002-1493-300X], Hinkley, S [0000-0001-8074-2562], Hippler, S [0000-0002-3912-6108], Horrobin, M [0000-0001-5451-7847], Kervella, P [0000-0003-0626-1749], Meyer, M [0000-0003-1227-3084], Kreidberg, L [0000-0003-0514-1147], Le Bouquin, JB [0000-0002-0493-4674], Lutz, D [0000-0003-0291-9582], Maire, AL [0000-0002-2591-4138], Mérand, A [0000-0002-1637-7393], Monnier, JD [0000-0002-3380-3307], Ott, T [0000-0003-1572-0396], Paumard, T [0000-0003-0655-0452], Perrin, G [0000-0003-0680-0167], Rameau, J [0000-0003-0029-0258], Rodríguez-Coira, G [0000-0002-4177-6433], Shangguan, J [0000-0002-4569-9009], Shimizu, T [0000-0002-2125-4670], Straub, O [0000-0001-5755-0677], Straubmeier, C [0000-0002-0671-9302], Sturm, E [0000-0002-0018-3666], Tacconi, LJ [0000-0002-1485-9401], Van Dishoeck, EF [0000-0001-7591-1907], Vincent, F [0000-0002-3855-0708], Von Fellenberg, SD [0000-0002-9156-2249], Ward-Duong, K [0000-0002-4479-8291], and Apollo - University of Cambridge Repository

Subjects
Orbit determination, Exoplanet formation, Long baseline interferometry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Exoplanet atmospheres
Abstract

We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 $\mu$as precision astrometry of both PDS 70 b and c in two epochs, as well as spatially resolving the hot inner disk around the star. Rejecting unstable orbits, we found a nonzero eccentricity for PDS 70 b of $0.17 \pm 0.06$, a near-circular orbit for PDS 70 c, and an orbital configuration that is consistent with the planets migrating into a 2:1 mean motion resonance. Enforcing dynamical stability, we obtained a 95% upper limit on the mass of PDS 70 b of 10 $M_\textrm{Jup}$, while the mass of PDS 70 c was unconstrained. The GRAVITY K-band spectra rules out pure blackbody models for the photospheres of both planets. Instead, the models with the most support from the data are planetary atmospheres that are dusty, but the nature of the dust is unclear. Any circumplanetary dust around these planets is not well constrained by the planets' 1-5 $\mu$m spectral energy distributions (SEDs) and requires longer wavelength data to probe with SED analysis. However with VLTI/GRAVITY, we made the first observations of a circumplanetary environment with sub-au spatial resolution, placing an upper limit of 0.3~au on the size of a bright disk around PDS 70 b.

Published
2022
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2. Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager

Author

Macintosh, B, Graham, JR, Barman, T, De Rosa, RJ, Konopacky, Q, Marley, MS, Marois, C, Nielsen, EL, Pueyo, L, Rajan, A, Rameau, J, Saumon, D, Wang, JJ, Patience, J, Ammons, M, Arriaga, P, Artigau, E, Beckwith, S, Brewster, J, Bruzzone, S, Bulger, J, Burningham, B, Burrows, AS, Chen, C, Chiang, E, Chilcote, JK, Dawson, RI, Dong, R, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, B, Goodsell, S, Greenbaum, AZ, Hibon, P, Hinkley, S, Cotton, TH, Hung, LW, Ingraham, P, Johnson-Groh, M, Kalas, P, Lafreniere, D, Larkin, JE, Lee, J, Line, M, Long, D, Maire, J, Marchis, F, Matthews, BC, Max, CE, Metchev, S, Millar-Blanchaer, MA, Mittal, T, Morley, CV, Morzinski, KM, Murray-Clay, R, Oppenheimer, R, Palmer, DW, Patel, R, Perrin, MD, Poyneer, LA, Rafikov, RR, Rantakyrö, FT, Rice, EL, Rojo, P, Rudy, AR, Ruffio, JB, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, and Vasisht, G

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric compositions and luminosities, which are influenced by their formation mechanisms. Using the Gemini Planet Imager, we discovered a planet orbiting the ∼20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water-vapor absorption. Modeling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 × 10-6and an effective temperature of 600 to 750 kelvin. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-accretion process that may have formed Jupiter.

Published
2015
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3. The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system (vol 576, pg A133, 2015)

Author

Maire, A-L, Skemer, AJ, Hinz, PM, Desidera, S, Esposito, S, Gratton, R, Marzari, F, Skrutskie, MF, Biller, BA, Defrere, D, Bailey, VP, Leisenring, JM, Apai, D, Bonnefoy, M, Brandner, W, Buenzli, E, Claudi, RU, Close, LM, Crepp, JR, De Rosa, RJ, Eisner, JA, Fortney, JJ, Henning, T, Hofmann, K-H, Kopytova, TG, Males, JR, Mesa, D, Morzinski, KM, Oza, A, Patience, J, Pinna, E, Rajan, A, Schertl, D, Schlieder, JE, Su, KYL, Vaz, A, Ward-Duong, K, Weigelt, G, and Woodward, CE

Subjects
individual: HR 8799 [stars], high angular resolution [techniques], data analysis [methods], adaptive optics [instrumentation], Astronomy & Astrophysics, errata, addenda, planetary systems, addenda, errata, Astronomical and Space Sciences
Published
2015
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4. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au

Author

Nielsen, EL, De Rosa, RJ, Macintosh, B, Wang, JJ, Ruffio, JB, Chiang, E, Marley, MS, Saumon, D, Savransky, D, Mark Ammons, S, Bailey, VP, Barman, T, Blain, C, Bulger, J, Burrows, A, Chilcote, J, Cotten, T, Czekala, I, Doyon, R, Duchene, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, BL, Goodsell, SJ, Graham, Greenbaum, AZ, Hibon, P, Hinkley, S, Hirsch, LA, Hom, J, Hung, LW, Ilene Dawson, R, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Lee, EJ, Lin, JW, Maire, J, Marchis, F, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rafikov, RR, Rajan, A, Rameau, J, Rantakyrö, FT, Ren, B, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Tallis, M, Thomas, S, Ward-Duong, K, and Wolff, S

Subjects
planets and satellites: detection, 13. Climate action, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, instrumentation: adaptive optics, planetary systems, Astrophysics::Galaxy Astrophysics
Abstract

We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey (GPIES). This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semi-major axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M $>$ 1.5 $M_\odot$ more likely to host planets with masses between 2-13 M$_{\rm Jup}$ and semi-major axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semi-major axis (a) for planet populations around high-mass stars (M $>$ 1.5M$_\odot$) of the form $\frac{d^2 N}{dm da} \propto m^\alpha a^\beta$, finding $\alpha$ = -2.4 $\pm$ 0.8 and $\beta$ = -2.0 $\pm$ 0.5, and an integrated occurrence rate of $9^{+5}_{-4}$% between 5-13 M$_{\rm Jup}$ and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8$^{+0.8}_{-0.5}$% of stars hosting a brown dwarf companion between 13-80 M$_{\rm Jup}$ and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semi-major axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semi-major axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the RV method, our results are consistent with a peak in occurrence of giant planets between ~1-10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.

5. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics From 10-100 AU

Author

Eric L. Nielsen, Robert J. De Rosa, Bruce Macintosh, Jason J. Wang, Jean-Baptiste Ruffio, Eugene Chiang, Mark S. Marley, Didier Saumon, Dmitry Savransky, S. Mark Ammons, Vanessa P. Bailey, Travis Barman, Célia Blain, Joanna Bulger, Adam Burrows, Jeffrey Chilcote, Tara Cotten, Ian Czekala, Rene Doyon, Gaspard Duchêne, Thomas M. Esposito, Daniel Fabrycky, Michael P. Fitzgerald, Katherine B. Follette, Jonathan J. Fortney, Benjamin L. Gerard, Stephen J. Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Sasha Hinkley, Lea A. Hirsch, Justin Hom, Li-Wei Hung, Rebekah Ilene Dawson, Patrick Ingraham, Paul Kalas, Quinn Konopacky, James E. Larkin, Eve J. Lee, Jonathan W. Lin, Jérôme Maire, Franck Marchis, Christian Marois, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Katie M. Morzinski, Rebecca Oppenheimer, David Palmer, Jennifer Patience, Marshall Perrin, Lisa Poyneer, Laurent Pueyo, Roman R. Rafikov, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Adam C. Schneider, Anand Sivaramakrishnan, Inseok Song, Remi Soummer, Melisa Tallis, Sandrine Thomas, Kimberly Ward-Duong, Schuyler Wolff, Nielsen, EL [0000-0001-6975-9056], De Rosa, RJ [0000-0002-4918-0247], Macintosh, B [0000-0003-1212-7538], Wang, JJ [0000-0003-0774-6502], Ruffio, JB [0000-0003-2233-4821], Chiang, E [0000-0002-6246-2310], Marley, MS [0000-0002-5251-2943], Saumon, D [0000-0001-6800-3505], Savransky, D [0000-0002-8711-7206], Mark Ammons, S [0000-0001-5172-7902], Bailey, VP [0000-0002-5407-2806], Barman, T [0000-0002-7129-3002], Bulger, J [0000-0003-4641-2003], Burrows, A [0000-0002-3099-5024], Chilcote, J [0000-0001-6305-7272], Cotten, T [0000-0003-0156-3019], Czekala, I [0000-0002-1483-8811], Esposito, TM [0000-0002-0792-3719], Fabrycky, D [0000-0003-3750-0183], Fitzgerald, MP [0000-0002-0176-8973], Follette, KB [0000-0002-7821-0695], Fortney, JJ [0000-0002-9843-4354], Gerard, BL [0000-0003-3978-9195], Goodsell, SJ [0000-0002-4144-5116], Greenbaum, AZ [0000-0002-7162-8036], Hibon, P [0000-0003-3726-5494], Hinkley, S [0000-0001-8074-2562], Hung, LW [0000-0003-1498-6088], Ilene Dawson, R [0000-0001-9677-1296], Ingraham, P [0000-0003-3715-8138], Konopacky, Q [0000-0002-9936-6285], Larkin, JE [0000-0001-7687-3965], Lee, EJ [0000-0002-1228-9820], Marchis, F [0000-0001-7016-7277], Marois, C [0000-0002-4164-4182], Metchev, S [0000-0003-3050-8203], Millar-Blanchaer, MA [0000-0001-6205-9233], Morzinski, KM [0000-0002-1384-0063], Oppenheimer, R [0000-0001-7130-7681], Perrin, M [0000-0002-3191-8151], Rafikov, RR [0000-0002-0012-1609], Rajan, A [0000-0002-9246-5467], Rameau, J [0000-0003-0029-0258], Rantakyrö, FT [0000-0002-9667-2244], Ren, B [0000-0003-1698-9696], Schneider, AC [0000-0002-6294-5937], Sivaramakrishnan, A [0000-0003-1251-4124], Song, I [0000-0002-5815-7372], Soummer, R [0000-0003-2753-2819], Tallis, M [0000-0002-5917-6524], Thomas, S [0000-0002-9121-3436], Ward-Duong, K [0000-0002-4479-8291], Wolff, S [0000-0002-9977-8255], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, Stellar mass, detection [planets and satellites], Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, adaptive optics [instrumentation], Astronomy & Astrophysics, instrumentation: adaptive optics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Mass distribution, Giant planet, Astronomy and Astrophysics, Exoplanet, Stars, 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astronomical and Space Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey (GPIES). This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semi-major axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M $>$ 1.5 $M_\odot$ more likely to host planets with masses between 2-13 M$_{\rm Jup}$ and semi-major axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semi-major axis (a) for planet populations around high-mass stars (M $>$ 1.5M$_\odot$) of the form $\frac{d^2 N}{dm da} \propto m^\alpha a^\beta$, finding $\alpha$ = -2.4 $\pm$ 0.8 and $\beta$ = -2.0 $\pm$ 0.5, and an integrated occurrence rate of $9^{+5}_{-4}$% between 5-13 M$_{\rm Jup}$ and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with 0.8$^{+0.8}_{-0.5}$% of stars hosting a brown dwarf companion between 13-80 M$_{\rm Jup}$ and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semi-major axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semi-major axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the RV method, our results are consistent with a peak in occurrence of giant planets between ~1-10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability., Comment: 52 pages, 18 figures. AJ in press

Published
2019

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