Examinando por Autor "Deming, D. L."

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Acceso Abierto
Evidence of a Clear Atmosphere for WASP-62b: The Only Known Transiting Gas Giant in the JWST Continuous Viewing Zone
(IOP Science Publishing, 2021-01-11) Alam, M. K.; López Morales, M.; MacDonald, R. J.; Nikolov, N.; Kirk, J.; Goyal, J. M.; Sing, D. K.; Wakeford, H. R.; Rathcke, A. D.; Deming, D. L.; Sanz Forcada, J.; Lewis, N. K.; Barstow, J. K.; Mikal Evans, T.; Buchhave, L. A.; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); Agencia Estatal de Investigación (AEI); 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]
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 μm) transmission spectrum of the hot Jupiter WASP-62b, measured with Hubble/STIS and Spitzer/IRAC. The spectrum is characterized by a 5.1σ detection of Na i absorption at 0.59 μm, 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 μm is tentatively attributed to SiH at 2.1σ 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, NH3, CO, CO2, CH4, 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.
Acceso Abierto
The Hubble PanCET Program: A Metal-rich Atmosphere for the Inflated Hot Jupiter HAT-P-41b
(IOP Science Publishing, 2021-01-06) Sheppard, K. B.; Welbanks, L.; Mandell, A. M.; Madhusudhan, N.; Nikolov, N.; Deming, D. L.; Henry, G. W.; Williamson, M. H.; Sing, D. K.; López Morales, M.; Ih, J.; Sanz Forcada, J.; Lavvas, P.; Ballester, G. E.; Evans, T. M.; García Muñoz, Antonio; Dos Santos, L. A.; National Aeronautics and Space Administration (NASA); Sheppard, K. B. [0000-0003-4552-9541]; Welbanks, L. [0000-0003-0156-4564]; Mandell, A. M. [0000-0002-8119-3355]; Madhusudhan, M. [0000-0002-4869-000X]; Nikolov, N. [0000-0002-6500-3574]; Deming, D. [0000-0001-5727-4094]; Sing, D. K. [0000-0001-6050-7645]; Henry, G. W. [0000-0003-4155-8513]; López Morales, M. [0000-0003-3204-8183]; Ih, J. [0000-0003-2775-653X]; Sanz Forcada, J. [0000-0002-1600-7835]; Lavvas, P. [0000-0002-5360-3660]; Evans, T. M. [0000-0001-5442-1300]; García Muñoz, A. [0000-0003-1756-4825]; Dos Santos, L. A. [0000-0002-2248-3838]
We present a comprehensive analysis of the 0.3–5 μm transit spectrum for the inflated hot Jupiter HAT-P-41b. The planet was observed in transit with Hubble STIS and WFC3 as part of the Hubble Panchromatic Comparative Exoplanet Treasury (PanCET) program, and we combine those data with warm Spitzer transit observations. We extract transit depths from each of the data sets, presenting the STIS transit spectrum (0.29–0.93 μm) for the first time. We retrieve the transit spectrum both with a free-chemistry retrieval suite (AURA) and a complementary chemical equilibrium retrieval suite (PLATON) to constrain the atmospheric properties at the day–night terminator. Both methods provide an excellent fit to the observed spectrum. Both AURA and PLATON retrieve a metal-rich atmosphere for almost all model assumptions (most likely O/H ratio of ${\mathrm{log}}_{10}Z/{Z}_{\odot }={1.46}_{-0.68}^{+0.53}$ and ${\mathrm{log}}_{10}Z/{Z}_{\odot }={2.33}_{-0.25}^{+0.23}$, respectively); this is driven by a 4.9σ detection of H2O as well as evidence of gas absorption in the optical (>2.7σ detection) due to Na, AlO, and/or VO/TiO, though no individual species is strongly detected. Both retrievals determine the transit spectrum to be consistent with a clear atmosphere, with no evidence of haze or high-altitude clouds. Interior modeling constraints on the maximum atmospheric metallicity (${\mathrm{log}}_{10}Z/{Z}_{\odot }\lt 1.7$) favor the AURA results. The inferred elemental oxygen abundance suggests that HAT-P-41b has one of the most metal-rich atmospheres of any hot Jupiters known to date. Overall, the inferred high metallicity and high inflation make HAT-P-41b an interesting test case for planet formation theories.