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Ahrer, E.M.; Alderson, L.; Batalha, N.M.; Batalha, N.E.; Bean, J.L.; Beatty, T.G.; Bell, T.J.; Benneke, B.; Berta-Thompson, Z.K.; Carter, A.L.; Crossfield, I.J.M.; Espinoza, N.; Feinstein, A.D.; Fortney, J.J.; Gibson, N.P.; Goyal, J.M.; Kempton, E.M.R.; Kirk, J.; Kreidberg, L.; Lopez-Morales, M.; Line, M.R.; Lothringer, J.D.; Moran, S.E.; Mukherjee, S.; Ohno, K.; Parmentier, V.; Piaulet, C.; Rustamkulov, Z.; Schlawin, E.; Sing, D.K.; Stevenson, K.B.; Wakeford, H.R.; Allen, N.H.; Birkmann, S.M.; Brande, J.; Crouzet, N.; Cubillos, P.E.; Damiano, M.; Desert, J.M.; Gao, P.; Harrington, J.; Hu, R.Y.; Kendrew, S.; Knutson, H.A.; Lagage, P.O.; Leconte, J.; Lendl, M.; MacDonald, R.J.; May, E.M.; Miguel, Y.; Molaverdikhani, K.; Moses, J.I.; Murray, C.A.; Nehring, M.; Nikolov, N.K.; de la Roche, D.J.M.P.D.; Radica, M.; Roy, P.A.; Stassun, K.G.; Taylor, J.; Waalkes, W.C.; Wachiraphan, P.; Welbanks, L.; Wheatley, P.J.; Aggarwal, K.; Alam, M.K.; Banerjee, A.; Barstow, J.K.; Blecic, J.; Casewell, S.L.; Changeat, Q.; Chubb, K.L.; Colon, K.D.; Coulombe, L.P.; Daylan, T.; De Val-Borro, M.; Decin, L.; Dos Santos, L.A.; Flagg, L.; France, K.; Fu, G.W.; Munoz, A.G.; Gizis, J.E.; Glidden, A.; Grant, D.; Heng, K.; Henning, T.; Hong, Y.C.; Inglis, J.; Iro, N.; Kataria, T.; Komacek, T.D.; Krick, J.E.; Lee, E.K.H.; Lewis, N.K.; Lillo-Box, J.; Lustig-Yaeger, J.; Mancini, L.; Mandell, A.M.; Mansfield, M.; Marley, M.S.; Mikal-Evans, T.; Morello, G.; Nixon, M.C.; Ceballos, K.O.; Piette, A.A.A.; Powell, D.; Rackham, B.V.; Ramos-Rosado, L.; Rauscher, E.; Redfield, S.; Rogers, L.K.; Roman, M.T.; Roudier, G.M.; Scarsdale, N.; Shkolnik, E.L.; Southworth, J.; Spake, J.J.; Steinrueck, M.E.; Tan, X.Y.; Teske, J.K.; Tremblin, P.; Tsai, S.M.; Tucker, G.S.; Turner, J.D.; Valenti, J.A.; Venot, O.; Waldmann, I.P.; Wallack, N.L.; Zhang, X.; Zieba, S. |
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Identification of carbon dioxide in an exoplanet atmosphere |
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2023 |
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Nature |
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Nature |
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Early Access |
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GIANT PLANETS; BROWN DWARFS; LINE LISTS; H2O; SKY |
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Carbon dioxide (CO2) is a key chemical species that is found in a wide range of planetary atmospheres. In the context of exoplanets, CO2 is an indicator of the metal enrichment (that is, elements heavier than helium, also called 'metallicity')(1-3), and thus the formation processes of the primary atmospheres of hot gas giants(4-6). It is also one of the most promising species to detect in the secondary atmospheres of terrestrial exoplanets(7-9). Previous photometric measurements of transiting planets with the Spitzer Space Telescope have given hints of the presence of CO2, but have not yielded definitive detections owing to the lack of unambiguous spectroscopic identification(10-12). Here we present the detection of CO2 in the atmosphere of the gas giant exoplanet WASP-39b from transmission spectroscopy observations obtained with JWST as part of the Early Release Science programme(13,14). The data used in this study span 3.0-5.5micrometres in wavelength and show a prominent CO2 absorption feature at 4.3micrometres (26-sigma significance). The overall spectrum is well matched by one-dimensional, ten-times solar metallicity models that assume radiative-convective-thermochemical equilibrium and have moderate cloud opacity. These models predict that the atmosphere should have water, carbon monoxide and hydrogen sulfide in addition to CO2, but little methane. Furthermore, we also tentatively detect a small absorption feature near 4.0micrometres that is not reproduced by these models. |
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0028-0836 |
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WOS:000927885000001 |
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UAI @ alexi.delcanto @ |
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1760 |
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Allen, N.H.; Espinoza, N.; Jordan, A.; Lopez-Morales, M.; Apai, D.; Rackham, B.V.; Kirk, J.; Osip, D.J.; Weaver, I.C.; McGruder, C.; Ceballos, K.O.; Reggiani, H.; Brahm, R.; Rodler, F.; Lewis, N.K.; Fraine, J. |
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ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b |
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2022 |
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Astronomical Journal |
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Astron. J. |
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164 |
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4 |
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153 |
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BAYESIAN-INFERENCE; EXOPLANET; SKY; ATMOSPHERES; EFFICIENT; TOOL; CHEMISTRY; ASTROPY |
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We present a precise ground-based optical transmission spectrum of the hot Saturn HATS-5b (T (eq) = 1025 K), obtained as part of the ACCESS survey with the IMACS multi-object spectrograph mounted on the Magellan Baade Telescope. Our spectra cover the 0.5-0.9 mu m region and are the product of five individual transits observed between 2014 and 2018. We introduce the usage of additional second-order light in our analyses, which allows us to extract an “extra” transit light curve, improving the overall precision of our combined transit spectrum. We find that the favored atmospheric model for this transmission spectrum is a solar-metallicity atmosphere with subsolar C/O, whose features are dominated by H2O and with a depleted abundance of Na and K. If confirmed, this would point to a “clear” atmosphere at the pressure levels probed by transmission spectroscopy for HATS-5b. Our best-fit atmospheric model predicts a rich near-IR spectrum, which makes this exoplanet an excellent target for future follow-up observations with the James Webb Space Telescope, both to confirm this H2O detection and to superbly constrain the atmosphere's parameters. |
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0004-6256 |
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WOS:000856537200001 |
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UAI @ alexi.delcanto @ |
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1650 |
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McGruder, C.D.; Lopez-Morales, M.; Kirk, J.; Espinoza, N.; Rackham, B.V.; Alam, M.K.; Allen, N.; Nikolov, N.; Weaver, I.C.; Ceballos, K.O.; Osip, D.J.; Apai, D.; Jordan, A.; Fortney, J.J. |
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ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques |
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2022 |
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Astronomical Journal |
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Astron. J. |
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164 |
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4 |
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134 |
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OPTICAL-TRANSMISSION SPECTRUM; CA-II H; RAYLEIGH-SCATTERING; BAYESIAN-INFERENCE; PANCET PROGRAM; K-EMISSION; LRG-BEASTS; EXOPLANET; HUBBLE; MODEL |
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One of the strongest Na I features was observed in WASP-96b. To confirm this novel detection, we provide a new 475-825 nm transmission spectrum obtained with Magellan/IMACS, which indeed confirms the presence of a broad sodium absorption feature. We find the same result when reanalyzing the 400-825 nm VLT/FORS2 data. We also utilize synthetic data to test the effectiveness of two common detrending techniques: (1) a Gaussian processes (GP) routine, and (2) common-mode correction followed by polynomial correction (CMC+Poly). We find that both methods poorly reproduce the absolute transit depths but maintain their true spectral shape. This emphasizes the importance of fitting for offsets when combining spectra from different sources or epochs. Additionally, we find that, for our data sets, both methods give consistent results, but CMC+Poly is more accurate and precise. We combine the Magellan/IMACS and VLT/FORS2 spectra with literature 800-1644 nm HST/ WFC3 spectra, yielding a global spectrum from 400 to 1644 nm. We used the PLATON and Exoretrievals retrieval codes to interpret this spectrum, and find that both yield relatively deeper pressures where the atmosphere is optically thick at log-pressures between 1.3(-1.1)(+1.0) and 0.29(-)(2.02)(+1.86) bars, respectively. Exoretrievals finds solar to supersolar Na I and H2O log-mixing ratios of -5.4(-1.9)(+2.0) and -4.5(-2.0)(+2.0), respectively, while PLATON finds an overall metallicity of log(10) (Z/Z(circle dot)) = -0.49(-0.37)(+1.0) dex. Therefore, our findings are in agreement with the literature and support the inference that the terminator of WASP-96b has few aerosols obscuring prominent features in the optical to near-infrared (near-IR) spectrum. |
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0004-6256 |
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WOS:000852038000001 |
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UAI @ alexi.delcanto @ |
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1649 |
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