Search

Your search keyword '"planets and satellites: individual: hd 209458 b"' showing total 16 results
Start Over Descriptor "planets and satellites: individual: hd 209458 b"
16 results on '"planets and satellites: individual: hd 209458 b"'

1. Four HD 209458 b transits through CRIRES+: Detection of H2O and non-detections of C2H2, CH4, and HCN.

Author

Blain, D., Landman, R., Mollière, P., and Dittmann, J.

Subjects
*NATURAL satellite atmospheres, *PLANETARY atmospheres, *PLANETARY systems, *CROSS correlation, *EXTRASOLAR planets
Abstract

Context. HD 209458 b is one of the most studied exoplanets to date. Despite this, atmospheric characterisation studies yielded inconsistent species detections and abundances. Values reported for the C/O ratio range from ≈0.1 to 1.0. Of particular interest is the simultaneous detection of H2O and HCN reported by some studies using high-resolution ground-based observations, which would require the atmospheric C/O ratio to be fine-tuned to a narrow interval around 1. HCN has however not been detected from recent space-based observations. Aims. We aim to provide an independent study of HD 209458 b's atmosphere with high-resolution observations, in order to infer the presence of several species, including H2O and HCN. Methods. We observed four primary transits of HD 209458 b at a high resolution (ℛ ≈ 92000) with CRIRES+ in the near infrared (band H, 1.431243–1.837253 μm). After reducing the data with pycrires, we prepared the data using the SysRem algorithm and performed a cross-correlation (CCF) analysis of the transmission spectra. We also compared the results with those obtained from simulated datasets constructed by combining the Exo-REM self-consistent model with the petitRADTRANS package. Results. Combining the four transits, we detect H2O with a signal-to-noise CCF metric of 8.7σ. This corresponds to a signal emitted at Kp = 151.3−23.4+31.1 km s−1 and blueshifted by −6−2+1 km s−1, consistent with what is expected for HD 209458 b. We do not detect any other species among C2H2, CH4, CO, CO2, H2S, HCN, and NH3. Comparing this with our simulated datasets, this result is consistent with a C/O ratio of 0.1 and an opaque cloud top pressure of 50 Pa, at a 3 times solar metallicity. This would also be consistent with recent JWST observations. However, none of the simulated results obtained with a bulk C/O ratio of 0.8, a value suggested by previous studies using GIANO-B and CRIRES, are consistent with our observations. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

2. The dark days are overcast: iron-bearing clouds on HD 209458 b and WASP-43 b can explain low-dayside albedos.

Author

Chubb, K L, Samra, D, Helling, Ch, Carone, L, and Stam, D M

Subjects
*CLIMATE change models, *NATURAL satellites, *GENERAL circulation model, *HOT Jupiters, *ATMOSPHERE of Jupiter
Abstract

We simulate the geometric albedo spectra of hot Jupiter exoplanets HD 209458 b and WASP-43 b, based on global climate model post-processed with kinetic cloud models. We predict WASP-43 b to be cloudy throughout its dayside, while HD 209458 b has a clear upper atmosphere around the hot subsolar point, largely due to the inclusion of strong optical absorbers TiO and VO in the general circulation model for the latter causes a temperature inversion. In both cases our models find low-geometric albedos – 0.026 for WASP-43 b and 0.028 for HD 209458 b when averaged over the CHaracterizing ExOPlanet Satellite bandpass of |$\sim$| 0.35–1.1  μ m – indicating dark daysides, similar to the low albedos measured by observations. We demonstrate the strong impact of clouds that contain Fe-bearing species on the modelled geometric albedos; without Fe-bearing species forming in the clouds, the albedos of both planets would be much higher (0.518 for WASP-43 b, 1.37 for HD 209458 b). We conclude that a cloudy upper or mid-to-lower atmosphere that contains strongly absorbing Fe-bearing aerosol species, is an alternative to a cloud-free atmosphere in explaining the low-dayside albedos of hot Jupiter atmospheres such as HD 209458 b and WASP-43 b. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

3. Sulfur chemistry in the atmospheres of warm and hot Jupiters.

Author

Hobbs, Richard, Rimmer, Paul B, Shorttle, Oliver, and Madhusudhan, Nikku

Subjects
*HOT Jupiters, *ATMOSPHERE of Jupiter, *SULFUR, *CHEMICAL kinetics, *ATMOSPHERIC models
Abstract

We present and validate a new network of atmospheric thermochemical and photochemical sulfur reactions. We use a 1D chemical kinetics model to investigate these reactions as part of a broader HCNO chemical network in a series of hot and warm Jupiters. We find that temperatures approaching |$1400\, \mathrm{K}$| are favourable for the production of H2S and HS around |$\mathrm{10^{-3}\, bar}$| at mixing ratios of around 10−5, an atmospheric level where detection by transit spectroscopy may be possible. At |$\mathrm{10^{-3}\, bar}$| and at lower temperatures, down to |$1000\, \mathrm{K}$|⁠ , mixing ratios of S2 can be up to 10−5, at the expense of H2S and HS, which are depleted down to a mixing ratio of 10−7. We also investigate how the inclusion of sulfur can manifest in an atmosphere indirectly, by its effect on the abundance of non-sulfur-bearing species. We find that in a model of the atmosphere of HD 209458 b, the inclusion of sulfur can lower the abundance of NH3, CH4, and HCN by up to two orders of magnitude around |$\mathrm{10^{-3}\, bar}$|⁠. In the atmosphere of the warm Jupiter 51 Eri b, we additionally find the inclusion of sulfur depletes the peak abundance of CO2 by a factor of 5, qualitatively consistent with prior models. We note that many of the reactions used in the network have poorly determined rate constants, especially at higher temperatures. To obtain an accurate idea of the impact of sulfur chemistry in hot and warm Jupiter atmospheres, experimental measurements of these reaction rates must take place. [ABSTRACT FROM AUTHOR]

Published
2021
Full Text
View/download PDF

4. Discriminating between hazy and clear hot-Jupiter atmospheres with CARMENES.

Author

Sánchez-López, A., López-Puertas, M., Snellen, I. A. G., Nagel, E., Bauer, F. F., Pallé, E., Tal-Or, L., Amado, P. J., Caballero, J. A., Czesla, S., Nortmann, L., Reiners, A., Ribas, I., Quirrenbach, A., Aceituno, J., Béjar, V. J. S., Casasayas-Barris, N., Henning, Th., Molaverdikhani, K., and Montes, D.

Subjects
*HOT Jupiters, *SPECTROGRAPHS, *RAYLEIGH scattering, *SPACE telescopes, *ATMOSPHERE, *ASTRONOMICAL transits
Abstract

Context. Relatively large radii of some hot Jupiters observed in the ultraviolet and blue-optical are generally interpreted to be due to Rayleigh scattering by high-altitude haze particles. However, the haze composition and its production mechanisms are not fully understood, and observational information is still limited. Aims. We aim to study the presence of hazes in the atmospheres of HD 209458 b and HD 189733 b with high spectral resolution spectra by analysing the strength of water vapour cross-correlation signals across the red optical and near-infrared wavelength ranges. Methods. A total of seven transits of the two planets were observed with the CARMENES spectrograph at the 3.5 m Calar Alto telescope. Their Doppler-shifted signals were disentangled from the telluric and stellar contributions using the detrending algorithm SYSREM. The residual spectra were subsequently cross-correlated with water vapour templates at 0.70–0.96 μm to measure the strength of the water vapour absorption bands. Results. The optical water vapour bands were detected at 5.2σ in HD 209458 b in one transit, whereas no evidence of them was found in four transits of HD 189733 b. Therefore, the relative strength of the optical water bands compared to those in the near-infrared were found to be larger in HD 209458 b than in HD 189733 b. Conclusions. We interpret the non-detection of optical water bands in the transmission spectra of HD 189733 b, compared to the detection in HD 209458 b, to be due to the presence of high-altitude hazes in the former planet, which are largely absent in the latter. This is consistent with previous measurements with the Hubble Space Telescope. We show that currently available CARMENES observations of hot Jupiters can be used to investigate the presence of haze extinction in their atmospheres. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

5. He Iλ 10 830 Å in the transmission spectrum of HD209458 b.

Author

Alonso-Floriano, F. J., Snellen, I. A. G., Czesla, S., Bauer, F. F., Salz, M., Lampón, M., Lara, L. M., Nagel, E., López-Puertas, M., Nortmann, L., Sánchez-López, A., Sanz-Forcada, J., Caballero, J. A., Reiners, A., Ribas, I., Quirrenbach, A., Amado, P. J., Aceituno, J., Anglada-Escudé, G., and Béjar, V. J. S.

Subjects
*ASTRONOMICAL transits, *PLANETARY atmospheres, *HOT Jupiters, *MAGNETOTELLURICS, *EXTENDED X-ray absorption fine structure, *PLANETARY systems
Abstract

Context. Recently, the He I triplet at 10 830 Å was rediscovered as an excellent probe of the extended and possibly evaporating atmospheres of close-in transiting planets. This has already resulted in detections of this triplet in the atmospheres of a handful of planets, both from space and from the ground. However, while a strong signal is expected for the hot Jupiter HD 209458 b, only upper limits have been obtained so far. Aims. Our goal is to measure the helium excess absorption from HD 209458 b and assess the extended atmosphere of the planet and possible evaporation. Methods. We obtained new high-resolution spectral transit time-series of HD 209458 b using CARMENES at the 3.5 m Calar Alto telescope, targeting the He I triplet at 10 830 Å at a spectral resolving power of 80 400. The observed spectra were corrected for stellar absorption lines using out-of-transit data, for telluric absorption using the MOLECFIT software, and for the sky emission lines using simultaneous sky measurements through a second fibre. Results. We detect He I absorption at a level of 0.91 ± 0.10% (9 σ) at mid-transit. The absorption follows the radial velocity change of the planet during transit, unambiguously identifying the planet as the source of the absorption. The core of the absorption exhibits a net blueshift of 1.8 ± 1.3 km s−1. Possible low-level excess absorption is seen further blueward from the main absorption near the centre of the transit, which could be caused by an extended tail. However, this needs to be confirmed. Conclusions. Our results further support a close relation between the strength of planetary absorption in the helium triplet lines and the level of ionising, stellar X-ray, and extreme-UV irradiation. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

6. CHEOPS geometric albedo of the hot Jupiter HD 209458 b

Author

Brandeker, Alexis, Heng, K., Lendl, M., Patel, Jayshil Ashokkumar, Morris, B. M., Broeg, C., Guterman, P., Beck, M., Maxted, P. F. L., Demangeon, O., Delrez, L., Demory, B-O, Kitzmann, D., Santos, N. C., Singh, V, Alibert, Y., Alonso, R., Anglada, G., Barczy, T., Barrado y Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Bruno, G., Cabrera, J., Charnoz, S., Collier Cameron, A., van Damme, C. Corral, Csizmadia, Sz, Davies, M. B., Deleuil, M., Deline, A., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Guedel, M., Hoyer, S., Isaak, K. G., Kiss, L., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Luntzer, A., Magrin, D., Nascimbeni, V, Olofsson, Göran, Ottensamer, R., Pagano, I, Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I, Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, G. M., Thomas, N., Udry, S., Van Grootel, V., Walton, N., Wolter, D., Brandeker, Alexis, Heng, K., Lendl, M., Patel, Jayshil Ashokkumar, Morris, B. M., Broeg, C., Guterman, P., Beck, M., Maxted, P. F. L., Demangeon, O., Delrez, L., Demory, B-O, Kitzmann, D., Santos, N. C., Singh, V, Alibert, Y., Alonso, R., Anglada, G., Barczy, T., Barrado y Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Bruno, G., Cabrera, J., Charnoz, S., Collier Cameron, A., van Damme, C. Corral, Csizmadia, Sz, Davies, M. B., Deleuil, M., Deline, A., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Guedel, M., Hoyer, S., Isaak, K. G., Kiss, L., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Luntzer, A., Magrin, D., Nascimbeni, V, Olofsson, Göran, Ottensamer, R., Pagano, I, Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I, Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, G. M., Thomas, N., Udry, S., Van Grootel, V., Walton, N., and Wolter, D.

Abstract

We report the detection of the secondary eclipse of the hot Jupiter HD 209458 b in optical/visible light using the CHEOPS space telescope. Our measurement of 20.4−3.3+3.2 parts per million translates into a geometric albedo of Ag = 0.096 ± 0.016. The previously estimated dayside temperature of about 1500 K implies that our geometric albedo measurement consists predominantly of reflected starlight and is largely uncontaminated by thermal emission. This makes the present result one of the most robust measurements of Ag for any exoplanet. Our calculations of the bandpass-integrated geometric albedo demonstrate that the measured value of Ag is consistent with a cloud-free atmosphere, where starlight is reflected via Rayleigh scattering by hydrogen molecules, and the water and sodium abundances are consistent with stellar metallicity. We predict that the bandpass-integrated TESS geometric albedo is too faint to detect and that a phase curve of HD 209458 b observed by CHEOPS would have a distinct shape associated with Rayleigh scattering if the atmosphere is indeed cloud free.

Published
2022
Full Text
View/download PDF

7. CHEOPS geometric albedo of the hot Jupiter HD 209458 b

Author

Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Brandeker, Alexis, Anglada-Escudé, Guillem, Barrado y Navascués, David, Ribas, Ignasi, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Brandeker, Alexis, Anglada-Escudé, Guillem, Barrado y Navascués, David, and Ribas, Ignasi

Abstract

We report the detection of the secondary eclipse of the hot Jupiter HD 209458 b in optical/visible light using the CHEOPS space telescope. Our measurement of 20.4−3.3+3.2 parts per million translates into a geometric albedo of Ag = 0.096 ± 0.016. The previously estimated dayside temperature of about 1500 K implies that our geometric albedo measurement consists predominantly of reflected starlight and is largely uncontaminated by thermal emission. This makes the present result one of the most robust measurements of Ag for any exoplanet. Our calculations of the bandpass-integrated geometric albedo demonstrate that the measured value of Ag is consistent with a cloud-free atmosphere, where starlight is reflected via Rayleigh scattering by hydrogen molecules, and the water and sodium abundances are consistent with stellar metallicity. We predict that the bandpass-integrated TESS geometric albedo is too faint to detect and that a phase curve of HD 209458 b observed by CHEOPS would have a distinct shape associated with Rayleigh scattering if the atmosphere is indeed cloud free.

Published
2022

8. CHEOPS geometric albedo of the hot Jupiter HD 209458 b

Author

Brandeker, A., Heng, K., Lendl, M., Patel, J. A., Morris, B. M., Broeg, C., Guterman, P., Beck, M., Maxted, P. F. L., Demangeon, O., Delrez, L., Demory, B.-O., Kitzmann, D., Santos, N. C., Singh, V., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Barrado y Navascues, D., Barros, S. C. C., Baumjohann, W., Beck, T., Benz, W., Billot, N., Bonfils, X., Bruno, G., Cabrera, J., Charnoz, S., Collier Cameron, A., Corral van Damme, C., Csizmadia, Sz., Davies, M. B., Deleuil, M., Deline, A., Ehrenreich, D., Erikson, A., Farinato, J., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Hoyer, S., Isaak, K. G., Kiss, L., Laskar, J., Lecavelier des Etangs, A., Lovis, C., Luntzer, A., Magrin, D., Nascimbeni, V., Olofsson, G., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Sousa, S. G., Steller, M., Szabó, G. M., Thomas, N., Udry, S., Van Grootel, V., Walton, N., Wolter, D., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, Planetary systems, Planets, Planets and satellites: Atmospheres, Satellites: Individual: HD 209458 b, Techniques: Photometric, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, FOS: Physical sciences, planets and satellites: individual: HD 209458 b, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 620 Engineering, techniques: photometric, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 570 Life sciences, biology, Astrophysics::Earth and Planetary Astrophysics, 610 Medicine & health, planetary systems, Astrophysics::Galaxy Astrophysics, QB, photometric, planets and satellites: individual: HD 209458 b [techniques], Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the detection of the secondary eclipse of the hot Jupiter HD 209458b in optical/visible light using the CHEOPS space telescope. Our measurement of 20.4 +/- 3.3 ppm translates into a geometric albedo of A_g = 0.096 +/- 0.016. The previously estimated dayside temperature of about 1500 K implies that our geometric albedo measurement consists predominantly of reflected starlight and is largely uncontaminated by thermal emission. This makes the present result one of the most robust measurements of A_g for any exoplanet. Our calculations of the bandpass-integrated geometric albedo demonstrate that the measured value of A_g is consistent with a cloud-free atmosphere, where starlight is reflected via Rayleigh scattering by hydrogen molecules, and the water and sodium abundances are consistent with stellar metallicity. We predict that the bandpass-integrated TESS geometric albedo is too faint to detect and that a phase curve of HD 209458b observed by CHEOPS would have a distinct shape associated with Rayleigh scattering if the atmosphere is indeed cloud free., Comment: 9 pages, accepted by A&A Letters

Published
2022

9. Sulfur chemistry in the atmospheres of warm and hot Jupiters

Author

Paul B. Rimmer, Richard Hobbs, Oliver Shorttle, Nikku Madhusudhan, Shorttle, Oliver [0000-0002-8713-1446], Nikku, Madhusudhan [0000-0002-4869-000X], and Apollo - University of Cambridge Repository

Subjects
010504 meteorology & atmospheric sciences, chemistry.chemical_element, Thermodynamics, FOS: Physical sciences, planets and satellites: individual: HD 209458 b, 01 natural sciences, Reaction rate, Atmosphere, Jupiter, Physics - Chemical Physics, 0103 physical sciences, Hot Jupiter, Mixing ratio, planets and satellites: individual: 51 Eri b, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Chemical Physics (physics.chem-ph), planets and satellites: atmospheres, planets and satellites: composition, Astronomy and Astrophysics, Sulfur, planets and satellites: gaseous planets, chemistry, Space and Planetary Science, Production (computer science), Bar (unit), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present and validate a new network of atmospheric thermo-chemical and photo-chemical sulfur reactions. We use a 1-D chemical kinetics model to investigate these reactions as part of a broader HCNO chemical network in a series of hot and warm Jupiters. We find that temperatures approaching $1400\,\mathrm{K}$ are favourable for the production of H2S and HS around $\mathrm{10^{-3}\,bar}$, the atmospheric level where detection by transit spectroscopy may be possible, leading to mixing ratios of around $10^{-6}$. At lower temperatures, down to $1000\,\mathrm{K}$, the abundance of S2 can be up to a mixing ratio of $10^{-5}$ at the same pressure, at the expense of H2S and HS, which are depleted down to a mixing ratio of $10^{-6}$. We also investigate how the inclusion of sulfur can manifest in an atmosphere indirectly, by its effect on the abundance of non-sulfur-bearing species. We find that in a model of the atmosphere of HD 209458 b, the inclusion of sulfur can lower the abundance of NH3, CH4 and HCN by up to two orders of magnitude around $\mathrm{10^{-3}\,bar}$. In the atmosphere of the warm Jupiter 51 Eri b, we additionally find the inclusion of sulphur depletes the peak abundance of CO2 by a factor of five, qualitatively consistent with prior models. We note that many of the reactions used in the network have poorly determined rates, especially at higher temperatures. To obtain a truly accurate idea of the impact of sulfur chemistry in hot and warm Jupiter atmospheres, new measurements of these reaction rates must take place., Comment: 17 pages, 9 Figures

Published
2021
Full Text
View/download PDF

10. Evidence of energy-, recombination-, and photon-limited escape regimes in giant planet H/He atmospheres

Author

Pedro J. Amado, Manuel López-Puertas, Luisa Lara, Jose A. Caballero, Enric Palle, M. Salz, Jorge Sanz-Forcada, Ignasi Ribas, Th. Henning, Ansgar Reiners, Lisa Nortmann, Andreas Quirrenbach, D. Montes, M. Lampón, S. Czesla, A. Sánchez-López, Karan Molaverdikhani, European Commission, European Research Council, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía , SEV-2017-0709, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Canarias, SEV-2015-0548, Lampón, M. [0000-0002-0183-7158], López Puertas, M. [0000-0003-2941-7734], Sánchez López, A. [0000-0002-0516-7956], Lara, L. M. [0000-0002-7184-920X], Sanz Forcada, J. [0000-0002-1600-7835], Molaverdikhani, K. [0000-0002-0502-0428], Caballero, J. A. [0000-0002-7349-1387], Nortmann, L. [0000-0001-8419-8760], Amado, P. J. [0000-0001-8012-3788], Montes, D. [0000-0002-7779-238X], Ribas, I. [0000-0002-6689-0312], Consejo Superior de Investigaciones Científicas (CSIC), Junta de Andalucía, European Regional Development Fund (ERDF), Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), Generalitat de Catalunya, and European Research Council (ERC)

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, chemistry.chemical_element, Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Planets and satellites: atmospheres, Absorption (electromagnetic radiation), Planets and satellites: individual: GJ 3470 b, 010303 astronomy & astrophysics, Helium, 0105 earth and related environmental sciences, Hydrodynamic escape, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Advection, individual: HD 209458 b [Planets and satellites], individual: HD 189733 b [Planets and satellites], Giant planet, Astronomy and Astrophysics, Planets and satellites: individual: HD 189733 b, Exoplanet, Planets and satellites: gaseous planets, Planets and satellites: individual: HD 209458 b, Astronomía, gaseous planets [Planets and satellites], chemistry, individual: GJ 3470 b [Planets and satellites], 13. Climate action, Space and Planetary Science, atmospheres [Planets and satellites], Planetary mass, Recombination, Astrophysics - Earth and Planetary Astrophysics
Abstract

Hydrodynamic escape is the most efficient atmospheric mechanism of planetary mass loss and has a large impact on planetary evolution. Three hydrodynamic escape regimes have been identified theoretically: energy-limited, recombination-limited, and photon-limited. However, no evidence of these regimes had been reported until now. Here, we report evidence of these three regimes via an analysis of a helium I triplet at 10 830 Å and Lyα absorption involving a 1D hydrodynamic model that allows us to estimate hydrogen recombination and advection rates. In particular, we show that HD 209458 b is in the energy-limited regime, HD 189733 b is in the recombination-limited regime, and GJ 3470 b is in the photon-limited regime. These exoplanets can be considered as benchmark cases for their respective regimes. © ESO 2021., CARMENES is an instrument for the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisica de Andalucia (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Cientificas (CSIC), the Ministerio de Economia y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the MINECO, the Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme and Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the ERDF through projects ESP2016-76076-R, ESP2017-87143-R, BES-2015-074542, PID2019-110689RB-I00/AEI/10.13039/501100011033, PGC2018-099425-B-I00, PID2019-109522GB-C51/2/3/4, PGC2018-098153-B-C33, AYA2016-79425-C3-1/2/3-P, ESP2016-80435-C2-1-R, and the Centre of Excellence "Severo Ochoa" and "Maria de Maeztu" awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM-2017-0737), and the Generalitat de Catalunya/CERCA programme. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 832428. A.S.L. acknowledges funding from the European Research Council under the European Union's Horizon 2020 research and innovation program under grant agreement No 694513.

Published
2021

11. Modelling the He i triplet absorption at 10 830 A in the atmosphere of HD 209458 b

Author

Enric Palle, Ignasi Ribas, Jose A. Caballero, Lisa Nortmann, Andreas Quirrenbach, F. J. Alonso-Floriano, S. Czesla, Karan Molaverdikhani, M. Salz, Manuel López-Puertas, Jorge Sanz-Forcada, L. M. Lara, M. Lampón, Ansgar Reiners, F. F. Bauer, A. Sánchez-López, Evangelos Nagel, D. Montes, Pedro J. Amado, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), Junta de Andalucía, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, German Research Foundation, Consejo Superior de Investigaciones Científicas (España), Max Planck Society, Lampón, M. [0000-0002-0183-7158], López Puertas, M. [0000-0003-2941-7734], Lara, L. M. [0000-0002-7184-920X], Sánchez López, A. [0000-0002-0516-7956], Molaverdikhani, K. [0000-0002-0502-0428], Caballero, J. A. [0000-0002-7349-1387], Bauer, F. F. [0000-0003-1212-5225], Pallé, E. [0000-0003-0987-1593], Montes, D. [0000-0002-7779-238X], Nagel, E. [0000-0002-4019-3631], Ribas, I. [0000-0002-6689-0312], Amado, P. J. [0000-0002-8388-6040], Ministerio de Ciencia e Innovación (MICINN), European Commission (EC), and Consejo Superior de Investigaciones Científicas (CSIC)

Subjects
Astrofísica, Satellites: gaseous planets, Absorption spectroscopy, Population, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, Atmosphere, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Planets and satellites: atmospheres, Triplet state, 010306 general physics, education, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Physics, education.field_of_study, individual: HD 209458 b [Planets and satellites], Astronomy and Astrophysics, Planets and satellites: gaseous planets, Planets and satellites: individual: HD 209458 b, Astronomía, gaseous planets [Planets and satellites], Space and Planetary Science, Physics::Accelerator Physics, atmospheres [Planets and satellites], Atomic physics, Thermosphere, gaseous planets [Satellites]
Abstract

arXiv:2003.04872v2, [Context]: HD 209458 b is an exoplanet with an upper atmosphere undergoing blow-off escape that has mainly been studied using measurements of the Lyα absorption. Recently, high-resolution measurements of absorption in the He I triplet line at 10 830 Å of several exoplanets (including HD 209458 b) have been reported, creating a new opportunity to probe escaping atmospheres., [Aims]: We aim to better understand the atmospheric regions of HD 209458 b from where the escape originates., [Methods]: We developed a 1D hydrodynamic model with spherical symmetry for the HD 209458 b thermosphere coupled with a non-local thermodynamic model for the population of the He I triplet state. In addition, we performed high-resolution radiative transfer calculations of synthetic spectra for the helium triplet lines and compared them with the measured absorption spectrum in order to retrieve information about the atmospheric parameters., [Results]: We find that the measured spectrum constrains the [H]/[H+] transition altitude occurring in the range of 1.2 RP–1.9 RP. Hydrogen is almost fully ionised at altitudes above 2.9 RP. We also find that the X-ray and extreme ultraviolet absorption takes place at effective radii from 1.16 to 1.30 RP, and that the He I triplet peak density occurs at altitudes from 1.04 to 1.60 RP. Additionally, the averaged mean molecular weight is confined to the 0.61–0.73 g mole−1 interval, and the thermospheric H/He ratio should be larger than 90/10, and most likely approximately 98/2. We also provide a one-to-one relationship between mass-loss rate and temperature. Based on the energy-limited escape approach and assuming heating efficiencies of 0.1–0.2, we find a mass-loss rate in the range of (0.42–1.00) ×1011 g s−1 and a corresponding temperature range of 7125–8125 K., [Conclusions]: The analysis of the measured He I triplet absorption spectrum significantly constrains the thermospheric structure of HD 209458 b and advances our knowledge of its escaping atmosphere., IAA authors acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa" award SEV-2017-0709. CARMENES is an instrument for the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA, Almería, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Científicas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max- Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Königstuhl, Institut de Ciències de l’Espai, Insitut für Astrophysik Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano-Alemán), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-Württemberg and Niedersachsen, and by the Junta de Andalucía. We acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia, Innovación y Universidades, funds through projects: ESP2016–76076–R, ESP2017-87143-R, BES–2015–074542, BES– 2015–073500, PGC2018-098153-B-C31, AYA2016-79425-C3-1/2/3-P.

Published
2020

12. Discriminating between hazy and clear hot-Jupiter atmospheres with CARMENES

Author

Manuel López-Puertas, M. R. Zapatero Osorio, Lev Tal-Or, Mathias Zechmeister, Enric Palle, Víctor J. S. Béjar, Karan Molaverdikhani, Th. Henning, Lisa Nortmann, Andreas Quirrenbach, S. Czesla, J. Aceituno, P. J. Amado, Ansgar Reiners, F. F. Bauer, A. Sánchez-López, M. Stangret, J. A. Caballero, Ignas Snellen, Núria Casasayas-Barris, Evangelos Nagel, D. Montes, Ignasi Ribas, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, German Research Foundation, Klaus Tschira Foundation, Junta de Andalucía, Consejo Superior de Investigaciones Científicas (España), Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Pallé, E. [0000-0003-0987-1593], Sánchez López, A. [0000-0002-0516-7956], Nagel, E. [0000-0002-4019-3631], Montes, D. [0000-0002-7779-238X], Molaverdikhani, K. [0000-0002-0502-0428], López Puertas, M. [0000-0003-2941-7734], Snellen, I. A. G. [0000-0003-1624-3667], European Research Council (ERC), Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), Ministerio de Ciencia e Innovación (MICINN), European Union through FEDER/ERF, FICTS-2011-02, European Science Foundation (ESF), German Research Foundation (DFG), FOR2544, and European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, Extinction (astronomy), FOS: Physical sciences, Astrophysics, planetary systems [Infrared], 01 natural sciences, Spectral line, spectroscopic [Techniques], law.invention, Telescope, Infrared: planetary systems, Planet, law, 0103 physical sciences, Hot Jupiter, Planets and satellites: atmospheres, Transit (astronomy), Spectral resolution, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, individual: HD 189733 b [Planets and satellites], individual: HD 209458 b [Planets and satellites], Astronomy and Astrophysics, Planets and satellites: individual: HD 189733 b, Planets and satellites: individual: HD 209458 b, Astronomía, 13. Climate action, Space and Planetary Science, atmospheres [Planets and satellites], Water vapor, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Relatively large radii of some hot Jupiters observed in the ultraviolet and blue-optical are generally interpreted to be due to Rayleigh scattering by high-altitude haze particles. However, the haze composition and its production mechanisms are not fully understood, and observational information is still limited. Aims. We aim to study the presence of hazes in the atmospheres of HD 209458 b and HD 189733 b with high spectral resolution spectra by analysing the strength of water vapour cross-correlation signals across the red optical and near-infrared wavelength ranges. Methods. A total of seven transits of the two planets were observed with the CARMENES spectrograph at the 3.5 m Calar Alto telescope. Their Doppler-shifted signals were disentangled from the telluric and stellar contributions using the detrending algorithm SYSREM. The residual spectra were subsequently cross-correlated with water vapour templates at 0.70-0.96 μm to measure the strength of the water vapour absorption bands. Results. The optical water vapour bands were detected at 5.2σ in HD 209458 b in one transit, whereas no evidence of them was found in four transits of HD 189733 b. Therefore, the relative strength of the optical water bands compared to those in the near-infrared were found to be larger in HD 209458 b than in HD 189733 b. Conclusions. We interpret the non-detection of optical water bands in the transmission spectra of HD 189733 b, compared to the detection in HD 209458 b, to be due to the presence of high-altitude hazes in the former planet, which are largely absent in the latter. This is consistent with previous measurements with the Hubble Space Telescope. We show that currently available CARMENES observations of hot Jupiters can be used to investigate the presence of haze extinction in their atmospheres. © 2020 ESO., A.S.L. and I.S. acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program under grant agreement no. 694513. CARMENES is an instrument for the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA, Almería, Spain). CARMENES is funded by the German Max-PlanckGesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Científicas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Königstuhl, Institut de Ciències de l’Espai, Insitut für Astrophysik Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano-Alemán), with additional contributions by the Spanish Ministerios de Ciencia e Innovación and of Economía y Competitividad, the Fondo Europeo de Desarrollo Regional (FEDER/ERF), the Agencia estatal de investigación, the Fondo Social Europeo under grants AYA2011-30 147-C03-01, -02 and -03, AYA2012- 39612-C03-01, ESP2013-48391-C4-1-R, ESP2014-54062-R, ESP 2016-76076- R, ESP2016-80435-C2-2-R, ESP2017- 87143-R, PGC2018-098153-B-C31, BES-2015-073500 and BES- 2015-074542, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-Württemberg and Niedersachsen, and by the Junta de Andalucía. IAA authors acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award SEV-2017-0709. Based on observations collected at the Centro Astronómico Hispano-Alemán (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Cientííficas (IAA-CSIC). We thank the anonymous referee for the very useful comments

Published
2020

13. Water vapor detection in the transmission spectra of HD 209458 b with the CARMENES NIR channel

Author

Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Universidad Autónoma de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Israel Science Foundation, Sánchez-López, A., Alonso-Floriano, F. Javier, López-Puertas, Manuel, Snellen, Ignas A. G., Funke, Bernd, Nagel, Evangelos, Bauer, Florian Franz, Amado, Pedro J., Caballero, J. A., Czesla, S., Nortmann, L., Pallé, Enric, Salz, M., Reiners, Ansgar, Ribas, Ignasi, Quirrenbach, Andreas, Anglada-Escudé, Guillem, Béjar, Victor J. S., Casasayas-Barris, N., Galadí-Enriquez, D., Henning, Thomas, Kaminski, Adrian, Kürster, M., Lampón, M., Lara, Luisa María, Montes, D., Morales, Juan Carlos, Stangret, M., Tal-Or, L., Sanz-Forcada, J., Schmitt, Jürgen H. M. M., Zapatero Osorio, María Rosa, Zechmeister, Mathias, Guenther, E. W., Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Universidad Autónoma de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Israel Science Foundation, Sánchez-López, A., Alonso-Floriano, F. Javier, López-Puertas, Manuel, Snellen, Ignas A. G., Funke, Bernd, Nagel, Evangelos, Bauer, Florian Franz, Amado, Pedro J., Caballero, J. A., Czesla, S., Nortmann, L., Pallé, Enric, Salz, M., Reiners, Ansgar, Ribas, Ignasi, Quirrenbach, Andreas, Anglada-Escudé, Guillem, Béjar, Victor J. S., Casasayas-Barris, N., Galadí-Enriquez, D., Henning, Thomas, Kaminski, Adrian, Kürster, M., Lampón, M., Lara, Luisa María, Montes, D., Morales, Juan Carlos, Stangret, M., Tal-Or, L., Sanz-Forcada, J., Schmitt, Jürgen H. M. M., Zapatero Osorio, María Rosa, Zechmeister, Mathias, and Guenther, E. W.

Abstract

Aims: We aim at detecting water vapor in the atmosphere of the hot Jupiter HD 209458 b and perform a multi-band study in the near infrared with CARMENES. Methods: The water vapor absorption lines from the atmosphere of the planet are Doppler-shifted due to the large change in its radial velocity during transit. This shift is of the order of tens of km s-1, whilst the Earth's telluric and the stellar lines can be considered quasi-static. We took advantage of this shift to remove the telluric and stellar lines using SYSREM, which performs a principal component analysis including proper error propagation. The residual spectra contain the signal from thousands of planetary molecular lines well below the noise level. We retrieve the information from those lines by cross-correlating the residual spectra with models of the atmospheric absorption of the planet. Results: We find a cross-correlation signal with a signal-to-noise ratio (S/N) of 6.4, revealing H2O in HD 209458 b. We obtain a net blueshift of the signal of -5.2 -1.3+2.6 km s-1 that, despite the large error bars, is a firm indication of day- to night-side winds at the terminator of this hot Jupiter. Additionally, we performed a multi-band study for the detection of H2O individually from the three near infrared bands covered by CARMENES. We detect H2O from its 0.96-1.06 ¿m band with a S/N of 5.8, and also find hints of a detection from the 1.06-1.26 ¿m band, with a low S/N of 2.8. No clear planetary signal is found from the 1.26-1.62 ¿m band. Conclusions: Our significant H2O signal at 0.96-1.06 ¿m in HD 209458 b represents the first detection of H2O from this band individually, the bluest one to date. The unfavorable observational conditions might be the reason for the inconclusive detection from the stronger 1.15 and 1.4 ¿m bands. H2O is detected from the 0.96-1.06 ¿m band in HD 209458 b, but hardly in HD 189733 b, which supports a stronger aerosol extinction in the latter, in line with previous studies. Future d

Published
2019

14. He I lambda 10 830 angstrom in the transmission spectrum of HD 209458 b

Author

Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), Comunidad de Madrid, Junta de Andalucía, Alonso-Floriano, F. Javier, Snellen, Ignas A. G., Czesla, S., Bauer, Florian Franz, Salz, M., Lampón, M., Lara, Luisa María, Nagel, Evangelos, López-Puertas, Manuel, Nortmann, L., Sánchez-López, A., Sanz-Forcada, J., Caballero, J. A., Reiners, Ansgar, Ribas, Ignasi, Quirrenbach, Andreas, Amado, Pedro J., Aceituno, Jesús, Anglada-Escudé, Guillem, Béjar, Victor J. S., Hatzes, Artie P., Henning, Thomas, Kaminski, Adrian, Kürster, M., Labarga, F., Montes, D., Pallé, Enric, Schmitt, Jürgen H. M. M., Zapatero Osorio, María Rosa, Brinkmöller, M., Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), Comunidad de Madrid, Junta de Andalucía, Alonso-Floriano, F. Javier, Snellen, Ignas A. G., Czesla, S., Bauer, Florian Franz, Salz, M., Lampón, M., Lara, Luisa María, Nagel, Evangelos, López-Puertas, Manuel, Nortmann, L., Sánchez-López, A., Sanz-Forcada, J., Caballero, J. A., Reiners, Ansgar, Ribas, Ignasi, Quirrenbach, Andreas, Amado, Pedro J., Aceituno, Jesús, Anglada-Escudé, Guillem, Béjar, Victor J. S., Hatzes, Artie P., Henning, Thomas, Kaminski, Adrian, Kürster, M., Labarga, F., Montes, D., Pallé, Enric, Schmitt, Jürgen H. M. M., Zapatero Osorio, María Rosa, and Brinkmöller, M.

Abstract

Recently, the He I triplet at 10 830 Å was rediscovered as an excellent probe of the extended and possibly evaporating atmospheres of close-in transiting planets. This has already resulted in detections of this triplet in the atmospheres of a handful of planets, both from space and from the ground. However, while a strong signal is expected for the hot Jupiter HD 209458 b, only upper limits have been obtained so far. Aims: Our goal is to measure the helium excess absorption from HD 209458 b and assess the extended atmosphere of the planet and possible evaporation. Methods: We obtained new high-resolution spectral transit time-series of HD 209458 b using CARMENES at the 3.5 m Calar Alto telescope, targeting the He I triplet at 10 830 Å at a spectral resolving power of 80 400. The observed spectra were corrected for stellar absorption lines using out-of-transit data, for telluric absorption using the MOLECFIT software, and for the sky emission lines using simultaneous sky measurements through a second fibre. Results: We detect He I absorption at a level of 0.91 ± 0.10% (9 ¿) at mid-transit. The absorption follows the radial velocity change of the planet during transit, unambiguously identifying the planet as the source of the absorption. The core of the absorption exhibits a net blueshift of 1.8 ± 1.3 km s-1. Possible low-level excess absorption is seen further blueward from the main absorption near the centre of the transit, which could be caused by an extended tail. However, this needs to be confirmed. Conclusions: Our results further support a close relation between the strength of planetary absorption in the helium triplet lines and the level of ionising, stellar X-ray, and extreme-UV irradiation.© ESO 2019

Published
2019

15. Water vapor detection in the transmission spectra of HD 209458 b with the CARMENES NIR channel

Author

Jorge Sanz-Forcada, Núria Casasayas-Barris, Enric Palle, S. Czesla, Víctor J. S. Béjar, Ignasi Ribas, A. Kaminski, Jürgen H. M. M. Schmitt, Bernd Funke, A. Sánchez-López, D. Galadí-Enríquez, M. Stangret, M. Salz, Luisa Lara, Evangelos Nagel, Ansgar Reiners, Martin Kürster, F. F. Bauer, Ignas Snellen, Mathias Zechmeister, Guillem Anglada-Escudé, E. W. Guenther, F. J. Alonso-Floriano, Lev Tal-Or, Pedro J. Amado, Juan Carlos Morales, M. Lampón, D. Montes, Manuel López-Puertas, M. R. Zapatero Osorio, Jose A. Caballero, Th. Henning, Lisa Nortmann, Andreas Quirrenbach, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Universidad Autónoma de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Israel Science Foundation, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Sánchez López, A. [0000-0002-0516-7956], Alonso Floriano, F. J. [0000-0003-1202-5734], Snellen, I. [0000-0003-1624-3667], Zapatero Osorio, M. R. [0000-0001-5664-2852], Ministerio de Ciencia e Innovación (MICINN), Israel Science Foundation (ISF), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), Science Foundation grant, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, Max-Planck-Gesellschaft (MPG), European Commission (EC), Ministerium für Wissenschaft, Forschung und Kunst Baden-Württemberg (MWK), Deutsche Forschungsgemeinschaft (DFG), Universidad Complutense de Madrid (UCM), and Universidad Autónoma de Madrid (UAM)

Subjects
Astrofísica, individual: HD 209458b [Planets and satellites], 010504 meteorology & atmospheric sciences, planets and satellites: individual: hd 209458 b, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, planets and satellites, atmospheres, individual, HD 209458 b, techniques, spectroscopic, infrared, planetary systems, Atmosphere, Planet, 0103 physical sciences, Hot Jupiter, infrared: planetary systems, planetary systems [infrared], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, planets and satellites: atmospheres, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Near-infrared spectroscopy, Astronomy and Astrophysics, atmospheres [planets and satellites], Blueshift, Radial velocity, 13. Climate action, Space and Planetary Science, individual: hd 209458 b [planets and satellites], spectroscopic [techniques], techniques: spectroscopic, Water vapor, Astrophysics - Earth and Planetary Astrophysics
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Aims: We aim at detecting water vapor in the atmosphere of the hot Jupiter HD 209458 b and perform a multi-band study in the near infrared with CARMENES. Methods: The water vapor absorption lines from the atmosphere of the planet are Doppler-shifted due to the large change in its radial velocity during transit. This shift is of the order of tens of km s-1, whilst the Earth's telluric and the stellar lines can be considered quasi-static. We took advantage of this shift to remove the telluric and stellar lines using SYSREM, which performs a principal component analysis including proper error propagation. The residual spectra contain the signal from thousands of planetary molecular lines well below the noise level. We retrieve the information from those lines by cross-correlating the residual spectra with models of the atmospheric absorption of the planet. Results: We find a cross-correlation signal with a signal-to-noise ratio (S/N) of 6.4, revealing H2O in HD 209458 b. We obtain a net blueshift of the signal of -5.2 -1.3+2.6 km s-1 that, despite the large error bars, is a firm indication of day- to night-side winds at the terminator of this hot Jupiter. Additionally, we performed a multi-band study for the detection of H2O individually from the three near infrared bands covered by CARMENES. We detect H2O from its 0.96-1.06 ¿m band with a S/N of 5.8, and also find hints of a detection from the 1.06-1.26 ¿m band, with a low S/N of 2.8. No clear planetary signal is found from the 1.26-1.62 ¿m band. Conclusions: Our significant H2O signal at 0.96-1.06 ¿m in HD 209458 b represents the first detection of H2O from this band individually, the bluest one to date. The unfavorable observational conditions might be the reason for the inconclusive detection from the stronger 1.15 and 1.4 ¿m bands. H2O is detected from the 0.96-1.06 ¿m band in HD 209458 b, but hardly in HD 189733 b, which supports a stronger aerosol extinction in the latter, in line with previous studies. Future data gathered at more stable conditions and with larger S/N at both optical and near-infrared wavelengths could help to characterize the presence of aerosols in HD 209458 b and other planets.© A. Sánchez-López et al. 2019, CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through European Regional Fund (FEDER/ERF), the Spanish Ministry of Economy and Competitiveness, the state of Baden-Wurttemberg, the German Science Foundation (DFG), and the Junta de Andalucia, with additional contributions by the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia, and the Observatorio de Calar Alto). Financial support was also provided by the Universidad Complutense de Madrid, the Comunidad Autonoma de Madrid, the Spanish Ministerios de Ciencia e Innovacion and of Economia y Competitividad, the Fondo Europeo de Desarrollo Regional (FEDER/ERF), the Agencia estatal de investigacion, and the Fondo Social Europeo under grants AYA2011-30 147-C03-01, -02, and -03, AYA2012-39612-C03-01, ESP2013-48391-C4-1-R, ESP2014-54062-R, ESP 2016-76076-R, ESP2016-80435-C2-2-R, ESP2017-87143-R, BES-2015-073500, and BES-2015-074542. IAA authors acknowledge financial support from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award SEV-2017-0709. L.T.-O. acknowledges support from the Israel Science Foundation (grant No. 848/16). Based on observations collected at the Observatorio de Calar Alto. We thank the anonymous referee for their insightful comments, which contributed to improve the quality of the manuscript.

Published
2019

16. He I lambda 10 830 angstrom in the transmission spectrum of HD 209458 b

Author

Alonso-Floriano, F. Javier, Snellen, Ignas A. G., Czesla, S., Bauer, FF, Salz, M., Lampón, M., Lara, Luisa María, Nagel, E., López-Puertas, Manuel, Nortmann, L., Sánchez-López, A., Sanz-Forcada, J., Caballero, J. A., Reiners, A., Ribas, I., Quirrenbach, A., Amado, Pedro J., Aceituno, Jesús, Anglada, Guillem, Béjar, V.J.S., Hatzes, A. P., Henning, Thomas, Kaminski, Adrian, Kürster, M., Labarga, F., Montes, D., Pallé, E., Schmitt, Jürgen H. M. M., Zapatero Osorio, María Rosa, Brinkmöller, M., Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), Comunidad de Madrid, and Junta de Andalucía

Subjects
planets and satellites: atmospheres, individual: hd 209458 b [planets and satellites], planets and satellites: individual: hd 209458 b, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, atmospheres [planets and satellites], planetary systems [infrared], infrared: planetary systems, Astrophysics::Galaxy Astrophysics, techniques: spectroscopic
Abstract

Recently, the He I triplet at 10 830 Å was rediscovered as an excellent probe of the extended and possibly evaporating atmospheres of close-in transiting planets. This has already resulted in detections of this triplet in the atmospheres of a handful of planets, both from space and from the ground. However, while a strong signal is expected for the hot Jupiter HD 209458 b, only upper limits have been obtained so far. Aims: Our goal is to measure the helium excess absorption from HD 209458 b and assess the extended atmosphere of the planet and possible evaporation. Methods: We obtained new high-resolution spectral transit time-series of HD 209458 b using CARMENES at the 3.5 m Calar Alto telescope, targeting the He I triplet at 10 830 Å at a spectral resolving power of 80 400. The observed spectra were corrected for stellar absorption lines using out-of-transit data, for telluric absorption using the MOLECFIT software, and for the sky emission lines using simultaneous sky measurements through a second fibre. Results: We detect He I absorption at a level of 0.91 ± 0.10% (9 ¿) at mid-transit. The absorption follows the radial velocity change of the planet during transit, unambiguously identifying the planet as the source of the absorption. The core of the absorption exhibits a net blueshift of 1.8 ± 1.3 km s-1. Possible low-level excess absorption is seen further blueward from the main absorption near the centre of the transit, which could be caused by an extended tail. However, this needs to be confirmed. Conclusions: Our results further support a close relation between the strength of planetary absorption in the helium triplet lines and the level of ionising, stellar X-ray, and extreme-UV irradiation.© ESO 2019, We thank P. Molliere and A. Wyttenbach for the nice scientific discussions during the preparation of this publication. F.J.A.-F. and I.S. acknowledge funding from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation programme under grant agreement No 694 513. CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium (MaxPlanck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG Research Unit FOR2544 >Blue Planets around Red Stars>, the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. Financial support was also provided by the Universidad Complutense de Madrid, the Comunidad Autonoma de Madrid, the Spanish Ministerios de Ciencia e Innovacion and of Economia y Competitividad, the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> and Science & Technology Facility Council Consolidated, and the Fondo Social Europeo. The corresponding funding grants are: ESP2014-54 362-P, ESP2014-54 062-R, AYA2015-69 350-C3-2-P, BES-2015-074542, AYA2016-79 425-C3-1/2/3-P, ESP2016-76 076-R, ESP2017-87 143-R, SEV-2017-0709, ST/P000592/1. Based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia. We thank the anonymous referee for their insightful comments, which contributed to improve the quality of the manuscript.

Published
2019

Catalog

Books, media, physical & digital resources
See catalog results