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Upper limits on atmospheric abundances of KELT-11b and WASP-69b from a retrieval approach
(EDP Sciences, 2025-12-12) Lesjak, F.; Nortmann, L.; Cont, D. 1 Conti, D; Amado, P. J.; Azzaro, M.; Caballero, J. A.; Czesla, S.; Hatzes, Artie; Henning, T.; López Puertas, M.; Molaverdikhani, K.; Montes, D.; Orell-Miquel, Jaume; Pallé, E.; Peláez-Torres, A.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Sánchez López, A.; Schweitzer, A.; Yan, F.; Ministerio de Economía y Competitividad (MINECO); Deutsche Forschungsgemeinschaft (DFG); Agencia Estatal de Investigación (AEI); European Research Council (ERC)
Context. WASP-69 b and KELT-11 b are two low-density hot Jupiters, which are expected to show strong atmospheric features in their transmission spectra. Such features offer valuable insights into the chemical composition, thermal structure, and cloud properties of exoplanet atmospheres. High-resolution spectroscopic observations can be used to study the line-forming regions in exoplanet atmospheres and potentially detect signals despite the presence of clouds.
Aims. We aimed to detect various molecular species and constrain the chemical abundances and cloud deck pressures using high-resolution spectroscopy.
Methods. We observed multiple transits of these planets with CARMENES and applied the cross-correlation method to detect atmospheric signatures. Further, we used an injection-recovery approach and retrievals to place constraints on the atmospheric properties.
Results. We detected a tentative H2O signal for KELT-11 b but not for WASP-69 b, and searches for other molecules such as H2S and CH4 resulted in non-detections for both planets. By investigating the signal strength of injected synthetic models, we constrained which atmospheric abundances and cloud deck pressures are consistent with our cross-correlation results. In addition, we show that a retrieval-based approach leads to similar constraints of these parameters.
Molecular gas stratification and disturbed kinematics in the Seyfert galaxy MCG-05-23-16 revealed by JWST and ALMA
(EDP Sciences, 2025-01-15) Esparza Arredondo, D., S.; Ramos Almeida, Cristina; Audibert, A.; Pereira Santaella, Miguel; García Bernete, I.; García-Burillo, Santiago, S.; Shimizu, T.; Davies, R.; Hermosa Muñoz, Laura; Alonso-Herrero, Almudena; Combes, Francoise; Speranza, G.; Zhang, Lulu; Campbell, Stephanie; Bellocchi, Enrica; Bunker, Andrew J.; Díaz Santos, T.; García Lorenzo, B.; González Martín, O.; Hicks, Erin K. S.; Labiano, Alvaro; Levenson, Nancy A.; Ricci, C.; Rosario, D.; Hönig, Sebastian; Packham, Christopher, C.; Stalevski, Marko; Fuller, L.; Izumi, T.; López Rodríguez, Enrique, E.; Rigopoulou, Dimitra; Rouan, D.; Ward, Martin; European Research Council (ERC); Comunidad de Madrid; Agencia Estatal de Investigación (España); Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT); Space Telescope Science Institute (US); Hellenic Foundation for Research and Innovation; Agencia Nacional de Investigación y Desarrollo (Chile)
Understanding the processes that drive the morphology and kinematics of molecular gas in galaxies is crucial for comprehending star formation and, ultimately, galaxy evolution. Using data from the Galactic Activity, Torus and Outflow Survey (GATOS) obtained with the James Webb Space Telescope (JWST) and the archival data from the Atacama Large Millimeter/submillimeter Array (ALMA), we study the behavior of the warm molecular gas at temperatures of hundreds of Kelvin and the cold molecular gas at tens of Kelvin in the galaxy MCG−05−23−16, which hosts an active galactic nucleus (AGN). Hubble Space Telescope (HST) images of this spheroidal galaxy, classified in the optical as S0, show a dust lane resembling a nuclear spiral and a surrounding ring. These features are also detected in CO(2−1) and H2, and their morphologies and kinematics are consistent with rotation plus local inward gas motions along the kinematic minor axis in the presence of a nuclear bar. The H2 transitions 0-0 S(3), 0-0 S(4), and 0-0 S(5), which trace warmer and more excited gas, show more disrupted kinematics than 0-0 S(1) and 0-0 S(2), including clumps of high velocity dispersion (of up to ∼160 km s−1), in regions devoid of CO(2−1). The kinematics of one of these clumps, located ∼350 pc westward of the nucleus, are consistent with outflowing gas, possibly driven by localized star formation traced by polycyclic aromatic hydrocarbon emission at 11.3 μm. Overall, we observe a stratification of the molecular gas, with the colder gas located in the nuclear spiral, ring, and connecting arms, and most of the warmer gas with a higher velocity dispersion filling the inter-arm space. The compact jet, approximately 200 pc in size, detected with Very Large Array (VLA) observations, does not appear to significantly affect the distribution and kinematics of the molecular gas, possibly due to its limited intersection with the molecular gas disk.
