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1. Early Release Science of the exoplanet WASP-39b with JWST NIRSpec PRISM

Author

Rustamkulov, Z., Sing, D. K., Mukherjee, S., May, E. M., Kirk, J., Schlawin, E., Line, M. R., Piaulet, C., Carter, A. L., Batalha, N. E., Goyal, J. M., López-Morales, M., Lothringer, J. D., MacDonald, R. J., Moran, S. E., Stevenson, K. B., Wakeford, H. R., Espinoza, N., Bean, J. L., Batalha, N. M., Benneke, B., Berta-Thompson, Z. K., Crossfield, I. J. M., Gao, P., Kreidberg, L., Powell, D. K., Cubillos, P. E., Gibson, N. P., Leconte, J., Molaverdikhani, K., Nikolov, N. K., Parmentier, V., Roy, P., Taylor, J., Turner, J. D., Wheatley, P. J., Aggarwal, K., Ahrer, E., Alam, M. K., Alderson, L., Allen, N. H., Banerjee, A., Barat, S., Barrado, D., Barstow, J. K., Bell, T. J., Blecic, J., Brande, J., Casewell, S., Changeat, Q., Chubb, K. L., Crouzet, N., Daylan, T., Decin, L., Désert, J., Mikal-Evans, T., Feinstein, A. D., Flagg, L., Fortney, J. J., Harrington, J., Heng, K., Hong, Y., Hu, R., Iro, N., Kataria, T., Kempton, E. M.-R., Krick, J., Lendl, M., Lillo-Box, J., Louca, A., Lustig-Yaeger, J., Mancini, L., Mansfield, M., Mayne, N. J., Miguel, Y., Morello, G., Ohno, K., Palle, E., Petit Dit De La Roche, D. J. M., Rackham, B. V., Radica, M., Ramos-Rosado, L., Redfield, S., Rogers, L. K., Shkolnik, E. L., Southworth, J., Teske, J., Tremblin, P., Tucker, G. S., Venot, O., Waalkes, W. C., Welbanks, L., Zhang, X., Zieba, S., University of St Andrews. School of Physics and Astronomy, Rustamkulov, Z. [0000-0003-4408-0463], Sing, D. K. [0000-0001-6050-7645], Line, M. R. [0000-0001-6247-8323], Piaulet, C. [0000-0002-2875-917X], Goyal, J. M. [0000-0002-8515-7204], López-Morales, M. [0000-0003-3204-8183], Lothringer, J. D. [0000-0003-3667-8633], Stevenson, K. B. [0000-0002-7352-7941], Wakeford, H. R. [0000-0003-4328-3867], Benneke, B. [0000-0001-5578-1498], Powell, D. K. [0000-0002-4250-0957], Gibson, N. P. [0000-0002-9308-2353], Molaverdikhani, K. [0000-0002-0502-0428], Nikolov, N. K. [0000-0002-6500-3574], Taylor, J. [0000-0003-4844-9838], Wheatley, P. J. [0000-0003-1452-2240], Aggarwal, K. [0000-0002-7004-8670], Ahrer, E. [0000-0003-0973-8426], Alderson, L. [0000-0001-8703-7751], Allen, N. H. [0000-0002-0832-710X], Banerjee, A. [0000-0002-9124-6537], Barrado, D. [0000-0002-5971-9242], Barstow, J. K. [0000-0003-3726-5419], Crouzet, N. [0000-0001-7866-8738], Daylan, T. [0000-0002-6939-9211], Decin, L. [0000-0002-5342-8612], Mikal-Evans, T. [0000-0001-5442-1300], Feinstein, A. D. [0000-0002-9464-8101], Harrington, J. [0000-0002-8955-8531], Hu, R. [0000-0003-2215-8485], Kempton, E. M.-R. [0000-0002-1337-9051], Lillo-Box, J. [0000-0003-3742-1987], Mancini, L. [0000-0002-9428-8732], Mansfield, M. [0000-0003-4241-7413], Mayne, N. J. [0000-0001-6707-4563], Morello, G. [0000-0002-4262-5661], Palle, E. [0000-0003-0987-1593], Petit dit de la Roche, D. J. M. [0000-0002-8963-3810], Redfield, S. [0000-0003-3786-3486], Southworth, J. [0000-0002-3807-3198], Tremblin, P. [0000-0001-6172-3403], Zhang, X. [0000-0002-8706-6963], Apollo - University of Cambridge Repository, Johns Hopkins University (JHU), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Imperial College London, Steward Observatory, University of Arizona, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Department of Physics [Montréal], McGill University = Université McGill [Montréal, Canada], NASA Ames Research Center (ARC), National Institute of Science Education and Research (NISER), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Utah Valley University (UVU), Department of Astronomy, University of Michigan, Carl Sagan Institute, Cornell University [New York], Lunar and Planetary Laboratory [Tucson] (LPL), H. H. Wills Physics Laboratory [Bristol], University of Bristol [Bristol], Space Telescope Science Institute (STSci), Department of Astronomy and Astrophysics [Chicago], University of Chicago, Department of Astrophysical and Planetary Sciences [Boulder], University of Colorado [Boulder], Department of Physics and Astronomy [Lawrence Kansas], University of Kansas [Lawrence] (KU), Earth and Planets Laboratory [Washington], Carnegie Institution for Science, Max Planck Institute for Astronomy (MPIA), INAF/Osservatorio Astronomico di Torino, Turin, Italy, Trinity College Dublin, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University Observatory Munich, Ludwig-Maximillians University Munich, Ludwig Maximilian University [Munich] (LMU), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, University of Warwick [Coventry], Indian Institute of Technology Indore (IITI), Observatories [Carnegie Institution], The Open University [Milton Keynes] (OU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Bay Area Environmental Research Institute (BAER), New York University [Abu Dhabi], NYU System (NYU), University of Leicester, European Space Agency (Baltimore) Space Telescope Science Institute (ESA), University of St Andrews [Scotland], Leiden Observatory [Leiden], Universiteit Leiden, Department of Physics, Princeton University (DPPU), Princeton University, Université Catholique de Louvain = Catholic University of Louvain (UCL), Max Planck Institute for Radio Astronomy, Department of Astronomy and Astrophysics [UCSC Santa Cruz], University of California (UC)-University of California (UC), Florida Space Institute [Orlando] (FSI), University of Central Florida [Orlando] (UCF), California Institute of Technology (CALTECH), Institut de recherches Arctiques Jean Malaurie (IRAM), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Paris-Saclay, Maison de la Simulation (MDLS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), National Aeronautics and Space Administration, NASA, Entomological Society of America, ESA, Space Telescope Science Institute, STScI, Heising-Simons Foundation, HSF, Canadian Space Agency, CSA, (JWST-ERS-01366, NAS 5-03127), Rustamkulov, Z [0000-0003-4408-0463], Sing, DK [0000-0001-6050-7645], Line, MR [0000-0001-6247-8323], Piaulet, C [0000-0002-2875-917X], Goyal, JM [0000-0002-8515-7204], López-Morales, M [0000-0003-3204-8183], Lothringer, JD [0000-0003-3667-8633], Stevenson, KB [0000-0002-7352-7941], Wakeford, HR [0000-0003-4328-3867], Benneke, B [0000-0001-5578-1498], Powell, DK [0000-0002-4250-0957], Gibson, NP [0000-0002-9308-2353], Molaverdikhani, K [0000-0002-0502-0428], Nikolov, NK [0000-0002-6500-3574], Taylor, J [0000-0003-4844-9838], Wheatley, PJ [0000-0003-1452-2240], Aggarwal, K [0000-0002-7004-8670], Ahrer, E [0000-0003-0973-8426], Alderson, L [0000-0001-8703-7751], Allen, NH [0000-0002-0832-710X], Banerjee, A [0000-0002-9124-6537], Barrado, D [0000-0002-5971-9242], Barstow, JK [0000-0003-3726-5419], Crouzet, N [0000-0001-7866-8738], Daylan, T [0000-0002-6939-9211], Decin, L [0000-0002-5342-8612], Mikal-Evans, T [0000-0001-5442-1300], Feinstein, AD [0000-0002-9464-8101], Harrington, J [0000-0002-8955-8531], Hu, R [0000-0003-2215-8485], Kempton, EM-R [0000-0002-1337-9051], Lillo-Box, J [0000-0003-3742-1987], Mancini, L [0000-0002-9428-8732], Mansfield, M [0000-0003-4241-7413], Mayne, NJ [0000-0001-6707-4563], Morello, G [0000-0002-4262-5661], Palle, E [0000-0003-0987-1593], Petit Dit de la Roche, DJM [0000-0002-8963-3810], Redfield, S [0000-0003-3786-3486], Southworth, J [0000-0002-3807-3198], Tremblin, P [0000-0001-6172-3403], and Zhang, X [0000-0002-8706-6963]

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), 141, MCC, Multidisciplinary, Settore FIS/05, 134, [SDV]Life Sciences [q-bio], 639/33/445/862, article, FOS: Physical sciences, 639/33/445/824, DAS, 639/33/34/862, 5109 Space Sciences, 140, QC Physics, Astrophysics - Solar and Stellar Astrophysics, QB Astronomy, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 51 Physical Sciences, Solar and Stellar Astrophysics (astro-ph.SR), QC, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Transmission spectroscopy of exoplanets has revealed signatures of water vapor, aerosols, and alkali metals in a few dozen exoplanet atmospheres. However, these previous inferences with the Hubble and Spitzer Space Telescopes were hindered by the observations' relatively narrow wavelength range and spectral resolving power, which precluded the unambiguous identification of other chemical species$-$in particular the primary carbon-bearing molecules. Here we report a broad-wavelength 0.5-5.5 $\mu$m atmospheric transmission spectrum of WASP-39 b, a 1200 K, roughly Saturn-mass, Jupiter-radius exoplanet, measured with JWST NIRSpec's PRISM mode as part of the JWST Transiting Exoplanet Community Early Release Science Team program. We robustly detect multiple chemical species at high significance, including Na (19$\sigma$), H$_2$O (33$\sigma$), CO$_2$ (28$\sigma$), and CO (7$\sigma$). The non-detection of CH$_4$, combined with a strong CO$_2$ feature, favours atmospheric models with a super-solar atmospheric metallicity. An unanticipated absorption feature at 4$\mu$m is best explained by SO$_2$ (2.7$\sigma$), which could be a tracer of atmospheric photochemistry. These observations demonstrate JWST's sensitivity to a rich diversity of exoplanet compositions and chemical processes., Comment: 41 pages, 4 main figures, 10 extended data figures, 4 tables. Under review in Nature

Published
2023

2. Hubble Space Telescope Transmission Spectroscopy for the Temperate Sub-Neptune TOI-270 d: A Possible Hydrogen-rich Atmosphere Containing Water Vapor

Author

Thomas Mikal-Evans, Nikku Madhusudhan, Jason Dittmann, Maximilian N. Günther, Luis Welbanks, Vincent Van Eylen, Ian J. M. Crossfield, Tansu Daylan, Laura Kreidberg, Mikal-Evans, T [0000-0001-5442-1300], Madhusudhan, N [0000-0002-4869-000X], Günther, MN [0000-0002-3164-9086], Welbanks, L [0000-0003-0156-4564], Daylan, T [0000-0002-6939-9211], Kreidberg, L [0000-0003-0514-1147], and Apollo - University of Cambridge Repository

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, 5101 Astronomical Sciences, FOS: Physical sciences, Astronomy and Astrophysics, 5109 Space Sciences, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

TOI-270d is a temperate sub-Neptune discovered by the Transiting Exoplanet Survey Satellite (TESS) around a bright (J=9.1mag) M3V host star. With an approximate radius of 2RE and equilibrium temperature of 350K, TOI-270d is one of the most promising small exoplanets for atmospheric characterisation using transit spectroscopy. Here we present a primary transit observation of TOI-270d made with the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) spectrograph across the 1.126-1.644 micron wavelength range, and a 95% credible upper limit of $8.2 \times 10^{-14}$ erg s$^{-1}$ cm$^{-2}$ A$^{-1}$ arcsec$^{-2}$ for the stellar Ly-alpha emission obtained using the Space Telescope Imaging Spectrograph (STIS). The transmission spectrum derived from the TESS and WFC3 data provides evidence for molecular absorption by a hydrogen-rich atmosphere at 4-sigma significance relative to a featureless spectrum. The strongest evidence for any individual absorber is obtained for H2O, which is favoured at 3-sigma significance. When retrieving on the WFC3 data alone and allowing for the possibility of a heterogeneous stellar brightness profile, the detection significance of H2O is reduced to 2.8-sigma. Further observations are therefore required to robustly determine the atmospheric composition of TOI-270d and assess the impact of stellar heterogeneity. If confirmed, our findings would make TOI-270d one of the smallest and coolest exoplanets to date with detected atmospheric spectral features., Comment: Accepted for publication in AAS journals on November 22, 2022 (received July 5, 2022; revised October 30, 2022)

Published
2023

3. HST PanCET program: non-detection of atmospheric escape in the warm Saturn-sized planet WASP-29 b

Author

David K. Sing, Hannah R. Wakeford, Mercedes López-Morales, Alfred Vidal-Madjar, Panayotis Lavvas, A. Lecavelier des Etangs, Gregory W. Henry, L. A. dos Santos, Thomas Mikal-Evans, Vincent Bourrier, David Ehrenreich, A. García Muñoz, Jorge Sanz-Forcada, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dos Santos, L. A. [0000-0002-2248-3838], Sanz Forcada, J. [0000-0002-1600-7835], López Morales, M. [0000-0003-3204-8183], Sing, D. K. [0000-0001-6050-7645], García Muñoz, A. [0000-0003-1756-4825], Henry, G. W. [0000-0003-4155-8513], Lecavelier des Etangs, A. [0000-0002-5637-5253], Mikal Evans, T. [0000-0001-5442-1300], Centre National D'Etudes Spatiales (CNES), European Research Council (ERC), and Agencia Estatal de Investigación (AEI)

Subjects
010504 meteorology & atmospheric sciences, Gas giant, kinematics and dynamics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, Planet, individual: Wasp-29 [Stars], Saturn, Kinematics and dynamics [ISM], 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, individual, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Atmospheric escape, atmospheres -ISM, Astronomy and Astrophysics, Stars, Exoplanet, Interstellar medium, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], chromospheres [Stars], atmospheres [Planets and satellites], chromospheres -planets and satellites, Astrophysics::Earth and Planetary Astrophysics, WASP-29 -stars, Astrophysics - Earth and Planetary Astrophysics
Abstract

(Abridged) Short-period gas giant exoplanets are susceptible to intense atmospheric escape due to their large scale heights and strong high-energy irradiation. This process is thought to occur ubiquitously, but to date we have only detected direct evidence of atmospheric escape in hot Jupiters and warm Neptunes. The paucity of cases for intermediate, Saturn-sized exoplanets at varying levels of irradiation precludes a detailed understanding of the underlying physics in atmospheric escape of hot gas giants. Our objectives here are to assess the high-energy environment of the warm ($T_\mathrm{eq} = 970$ K) Saturn WASP-29 b and search for signatures of atmospheric escape. We used far-ultraviolet (FUV) observations from the Hubble Space Telescope to analyze the flux time series of H I, C II, Si III, Si IV, and N V during the transit of WASP-29 b. At 3$\sigma$ confidence, we rule out any in-transit absorption of H Ilarger than 92% in the Lyman-$\alpha$ blue wing and 19% in the red wing. We found an in-transit flux decrease of $39\%^{+12\%}_{-11\%}$ in the ground-state C II emission line at 133.45 nm. But due to this signal being significantly present in only one visit, it is difficult to attribute a planetary or stellar origin for the ground-state C II signal. We place 3$\sigma$ absorption upper limits of 40%, 49% and 24% for Si III, Si IV, and for excited-state C II at 133.57 nm, respectively. Low activity levels and the faint X-ray luminosity suggest that WASP-29 is an old, inactive star. An energy-limited approximation combined with the reconstructed EUV spectrum of the host suggests that the planet is losing its atmosphere at a rate of $4 \times 10^9$ g s$^{-1}$. The non-detection at Lyman-$\alpha$ could be partly explained by a low fraction of escaping neutral hydrogen, or by the state of fast radiative blow-out we infer from the reconstructed stellar Lyman-$\alpha$ line., Comment: 10 pages, 8 figures, accepted for publication in Astronomy & Astrophysics. v2 with a few text changes for consistency

Published
2021

4. Evidence of a Clear Atmosphere for WASP-62b: the Only Known Transiting Gas Giant in the JWST Continuous Viewing Zone

Author

Drake Deming, Munazza K. Alam, Nikole K. Lewis, Ryan J. MacDonald, Mercedes Lopez-Morales, David K. Sing, Joanna K. Barstow, James Kirk, Hannah R. Wakeford, Jorge Sanz-Forcada, Jayesh M. Goyal, Lars A. Buchhave, Alexander D. Rathcke, Thomas Mikal-Evans, Nikolay Nikolov, Alam, M. K. [0000-0003-4157-832X], López Morales, M. [0000-0003-3204-8183], MacDonald, R. J. [0000-0003-4816-3469], Nikolov, N. [0000-0002-6500-3574], Kirk, J. [0000-0002-4207-6615], Goyal, J. M. [0000-0002-8515-7204], Sing, D. K. [0000-0001-6050-7645], Wakeford, H. R. [0000-0003-4328-3867], Rathcke, A. D. [0000-0002-4227-4953], Deming, D. L. [0000-0001-5727-4094], Sanz Forcada, J. [0000-0002-1600-7835], Lewis, N. K. [0000-0002-8507-1304], Barstow, J. K. [0000-0003-3726-5419], Mikal Evans, T. [0000-0001-5442-1300], Buchhave, L. A. [0000-0003-1605-5666], National Aeronautics and Space Administration (NASA), National Science Foundation (NSF), and Agencia Estatal de Investigación (AEI)

Subjects
010504 meteorology & atmospheric sciences, Infrared, Gas giant, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Atmosphere, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), James Webb Space Telescope, Giant planet, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Exoplanet, Exoplanets atmospheres, Exoplanet atmospheric composition, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Planetary atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract

Exoplanets with cloud-free, haze-free atmospheres at the pressures probed by transmission spectroscopy represent a valuable opportunity for detailed atmospheric characterization and precise chemical abundance constraints. We present the first optical to infrared (0.3-5 microns) transmission spectrum of the hot Jupiter WASP-62b, measured with Hubble/STIS and Spitzer/IRAC. The spectrum is characterized by a 5.1-sigma detection of Na I absorption at 0.59 microns, in which the pressure-broadened wings of the Na D-lines are observed from space for the first time. A spectral feature at 0.4 microns is tentatively attributed to SiH at 2.1-sigma confidence. Our retrieval analyses are consistent with a cloud-free atmosphere without significant contamination from stellar heterogeneities. We simulate James Webb Space Telescope (JWST) observations, for a combination of instrument modes, to assess the atmospheric characterization potential of WASP-62b. We demonstrate that JWST can conclusively detect Na, H2O, FeH, and SiH within the scope of its Early Release Science (ERS) program. As the only transiting giant planet currently known in the JWST Continuous Viewing Zone, WASP-62b could prove a benchmark giant exoplanet for detailed atmospheric characterization in the James Webb era., 14 pages, 5 figures, accepted for publication in ApJL

Published
2020

5. The Hubble Space Telescope PanCET Program: An Optical to Infrared Transmission Spectrum of HAT-P-32Ab

Author

Vincent Bourrier, David K. Sing, Mercedes Lopez-Morales, Hannah R. Wakeford, Jorge Sanz-Forcada, Gregory W. Henry, Antonio García Muñoz, Claire Baxter, Ofer Cohen, Panayotis Lavvas, Lars A. Buchhave, Joanna K. Barstow, Nikolay Nikolov, Munazza Alam, Thomas Mikal-Evans, Michael H. Williamson, Jean-Michel Desert, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Space Telescope Science Institute (STSci), Department of Physics [Baltimore], University of Maryland [Baltimore County] (UMBC), University of Maryland System-University of Maryland System, Center of Excellence in Information Systems, Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Berlin (TU), Alam, M. K. [0000-0003-4157-832X], López Morales, M. [0000-0003-3204-8183], Nikolov, N. [0000-0002-6500-3574], Sing, D. K. [0000-0001-6050-7645], Henry, G. W. [0000-0003-4155-8513], Baxter, C. [0000-0003-3438-843X], Désert, J. M. [0000-0002-0875-8401], Barstow, J. K. [0000-0003-3726-5419], Mikal Evans, T. [0000-0001-5442-1300], Bourrier, V. [0000-0002-9148-034X], Lavvas, P. [0000-0002-5360-3660], Wakeford, H. R. [0000-0003-4328-3867], Forcada, J. S. [0000-0002-1600-7835], Buchhave, L. A. [0000-0003-1605-5666], Cohen, O. [0000-0003-3721-0215], García Muñoz, A. [0000-0003-1756-4825], National Aeronautics & Space Administration (NASA), NAS 5-26555, HST GO programs, 14767 14260, Space Telescope Science Institute, HST-GO-14767, Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), European Research Council (ERC), and Low Energy Astrophysics (API, FNWI)

Subjects
010504 meteorology & atmospheric sciences, Infrared, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Hot Jupiters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Space Telescope Imaging Spectrograph, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Eclipse, Physics, planets and satellites: atmospheres, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], planets and satellites: individual (HAT-P-32Ab), Exoplanets, planets and satellites: composition, Astronomy and Astrophysics, Exoplanet, Photometry (astronomy), Exoplanet atmospheric composition, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Wide Field Camera 3, Exoplanet atmospheres
Abstract

We present a 0.3-5 μm transmission spectrum of the hot Jupiter HAT-P-32Ab observed with the Space Telescope Imaging Spectrograph and Wide Field Camera 3 instruments mounted on the Hubble Space Telescope, combined with Spitzer Infrared Array Camera photometry. The spectrum is composed of 51 spectrophotometric bins with widths ranging between 150 and 400 Å, measured to a median precision of 215 ppm. Comparisons of the observed transmission spectrum to a grid of 1D radiative-convective equilibrium models indicate the presence of clouds/hazes, consistent with previous transit observations and secondary eclipse measurements. To provide more robust constraints on the planet's atmospheric properties, we perform the first full optical to infrared retrieval analysis for this planet. The retrieved spectrum is consistent with a limb temperature of 1248+9292 K, a thick cloud deck, enhanced Rayleigh scattering, and ∼10× solar H2O abundance. We find log(Z/Z o˙) =2.41+0.06-0.07, and compare this measurement with the mass-metallicity relation derived for the solar system., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Published
2020

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