TY - JOUR
T1 - The hubble PanCET program
T2 - A metal-rich atmosphere for the inflated hot jupiter HAT-P-41b
AU - Sheppard, Kyle B.
AU - Welbanks, Luis
AU - Mandell, Avi M.
AU - Madhusudhan, Nikku
AU - Nikolov, Nikolay
AU - Deming, Drake
AU - Henry, Gregory W.
AU - Williamson, Michael H.
AU - Sing, David K.
AU - López-Morales, Mercedes
AU - Ih, Jegug
AU - Sanz-Forcada, Jorge
AU - Lavvas, Panayotis
AU - Ballester, Gilda E.
AU - Evans, Thomas M.
AU - Muñoz, Antonio García
AU - dos Santos, Leonardo A.
N1 - Funding Information:
The authors are grateful to Michael Zhang and Yayaati Chachan for many helpful discussions about PLATON. We thank Daniel Thorngren for providing the interior modeling metallicity constraint, as well as Daniel Kitzmann for providing the refractive indices of the Mie scattering condensates. We thank Eliza Kempton for productive conversations. This work is based on observations from the Hubble Space Telescope, operated by AURA, Inc. on behalf of NASA/ESA. This work also includes observations made with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. K. B. S. acknowledges support from CRESST, as well as funding from HST grant HST-GO-14767. A. M. M. acknowledges support from HST grant HST-GO-14260, and the GSFC Sellers Exoplanet Environments Collaboration (SEEC), which is funded in part by the NASA Planetary Science Division's Internal Scientist Funding Model. J. S. F. acknowledges support from the Spanish State Research Agency project AYA2016-79425-C3-2-P. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https:// www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Software: IRAF (Tody 1986, 1993), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007), nestle (https://github.com/kbarbary/ nestle), BATMAN (Kreidberg 2015), Kapetyn (Terlouw & Vogelaar 2015), Corner.py (Foreman-Mackey 2016), AstroPy (Astropy Collaboration et al. 2018), PLATON (Zhang et al. 2019), Dynesty (Higson et al. 2019), NumPy (Harris et al. 2020), Pandas (The Pandas development Team 2020).
Funding Information:
The authors are grateful to Michael Zhang and Yayaati Chachan for many helpful discussions about PLATON. We thank Daniel Thorngren for providing the interior modeling metallicity constraint, as well as Daniel Kitzmann for providing the refractive indices of the Mie scattering condensates. We thank Eliza Kempton for productive conversations. This work is based on observations from the Hubble Space Telescope, operated by AURA, Inc. on behalf of NASA/ESA. This work also includes observations made with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. K. B. S. acknowledges support from CRESST, as well as funding from HST grant HST-GO-14767. A. M. M. acknowledges support from HST grant HST-GO-14260, and the GSFC Sellers Exoplanet Environments Collaboration (SEEC), which is funded in part by the NASA Planetary Science Divisionʼs Internal Scientist Funding Model. J. S. F. acknowledges support from the Spanish State Research Agency project AYA2016-79425-C3-2-P. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https:// www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
Publisher Copyright:
© 2021. The American Astronomical Society. All rights reserved.
PY - 2021/1/6
Y1 - 2021/1/6
N2 - 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 log10 Z Z☉ = 1.46-+0.680.53 log10 Z Z☉ = 2.33-+0.250.23, respectively); this is driven by a 4.9σ detection of H2O as well as evidence of gas and 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 (log10 Z Z☉ < 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.
AB - 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 log10 Z Z☉ = 1.46-+0.680.53 log10 Z Z☉ = 2.33-+0.250.23, respectively); this is driven by a 4.9σ detection of H2O as well as evidence of gas and 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 (log10 Z Z☉ < 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.
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U2 - 10.3847/1538-3881/abc8f4
DO - 10.3847/1538-3881/abc8f4
M3 - Article
AN - SCOPUS:85099194643
SN - 0004-6256
VL - 161
JO - Astronomical Journal
JF - Astronomical Journal
IS - 2
M1 - 51
ER -