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

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 spectroph...

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Detalhes bibliográficos
Autores: Alam, M. K., López Morales, M., Nikolov, N., Sing, D. K., Henry, G. W., Baxter, C., Désert, J. M., Barstow, J. K., Mikal Evans, T., Bourrier, V., Lavvas, P., Wakeford, H. R., Williamson, M. H., Sanz-Forcada, Jorge, Buchhave, L. A., Cohen, O., García Muñoz, Antonio
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2020
País:España
Recursos:Instituto Nacional de Técnica Aeroespacial (INTA)
Repositorio:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial
OAI Identifier:oai:digital.inta.es:20.500.12666/405
Acesso em linha:https://iopscience.iop.org/article/10.3847/1538-3881/ab96cb
http://hdl.handle.net/20.500.12666/405
https://doi.org/10.3847/1538-3881/ab96cb
Access Level:acceso abierto
Palavra-chave:Exoplanet atmospheres
Exoplanet atmospheric composition
Exoplanets
Hot Jupiters
Descrição
Resumo: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 ${1248}_{-92}^{+92}$ K, a thick cloud deck, enhanced Rayleigh scattering, and ~10× solar H2O abundance. We find log(Z/Z⊙) = ${2.41}_{-0.07}^{+0.06}$, and compare this measurement with the mass–metallicity relation derived for the solar system.

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