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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. HST hot Jupiter Transmission Spectral Survey: A detection of Na and strong optical absorption in HAT-P-1b

Author

Nikolov, N., Sing, D. K., Pont, F., Burrows, A. S., Fortney, J. J., Ballester, G. E., Evans, T. M., Huitson, C. M., Wakeford, H. R., Wilson, P. A., Aigrain, S., Deming, D., Gibson, N. P., Henry, G. W., Knutson, H., Etangs, A. Lecavelier des, Showman, A. P., Vidal-Madjar, A., and Zahnle, K.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present an optical to near-infrared transmission spectrum of the hot Jupiter HAT-P-1b, based on HST observations, covering the spectral regime from 0.29 to 1.027{\mu}m with STIS, which is coupled with a recent WFC3 transit (1.087 to 1.687{\mu}m). We derive refined physical parameters of the HAT-P-1 system, including an improved orbital ephemeris. The transmission spectrum shows a strong absorption signature shortward of 0.55{\mu}m, with a strong blueward slope into the near-ultraviolet. We detect atmospheric sodium absorption at a 3.3{\sigma} significance level, but find no evidence for the potassium feature. The red data implies a marginally flat spectrum with a tentative absorption enhancement at wavelength longer than ~0.85{\mu}m. The STIS and WFC3 spectra differ significantly in absolute radius level (4.3 +/- 1.6 pressure scale heights), implying strong optical absorption in the atmosphere of HAT-P-1b. The optical to near-infrared difference cannot be explained by stellar activity, as simulta- neous stellar activity monitoring of the G0V HAT-P-1b host star and its identical companion show no significant activity that could explain the result. We compare the complete STIS and WFC3 transmission spectrum with theoretical atmospheric mod- els which include haze, sodium and an extra optical absorber. We find that both an optical absorber and a super-solar sodium to water abundance ratio might be a sce- nario explaining the HAT-P-1b observations. Our results suggest that strong optical absorbers may be a dominant atmospheric feature in some hot Jupiter exoplanets.

Published
2013
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3. 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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