CARMENES instrument overview

Quirrenbach, A.; Amado, P. J.; Caballero, J. A.; Mundt, R.; Reiners, A.; Ribas, I.; Seifert, W.; Abril, Miguel; Aceituno, J.; Alonso-Floriano, F. J.; Eiff, M. Ammler‐von; Jimenez, R.; Anwand-Heerwart, H.; Azzaro, M.; Bauer, F. F.; Barrado, D.; Becerril, S.; Béjar, V. J. S.; Benítez, D.; Berdiñas, Z. M.; Cárdenas, M. C.; Casal, E.; Claret, A.; Colomé, J.; Cortés-Contreras, M.; Czesla, S.; Doellinger, M. P.; Dreizler, S.; Feiz, C.; Fernández, M.; Galadí, D.; Gálvez-Ortiz, M. C.; García-Piquer, Á.; García-Vargas, M. L.; Garrido, R.; Gesa, L.; Galera, V. Gómez; Álvarez, E. González; Hernández, J. I. González; Grözinger, U.; Guàrdia, J.; Guenther, E. W.; Guindos, E. de; Gutiérrez‐Soto, J.; Hagen, Hans; Hatzes, A. P.; Hauschildt, P. H.; Helmling, J.; Henning, Thomas; Hermann, Daniel; Castaño, L. Hernández; Herrero, E.; Hidalgo, D.; Holgado, G.; Huber, Armin; Huber, K. F.; Jeffers, S. V.; Joergens, V.; Juan, E. de; Kehr, M.; Klein, Ralf; Kürster, M.; Lamert, A.; Lalitha, S.; Laun, W.; Lemke, Ulrike; Lenzen, R.; Fresno, M. López del; Martí, Belén López; López‐Santiago, J.; Mall, U.; Mandel, H.; Martín, E. L.; Mart́ın-Rúız, S.; Martínez-Rodríguez, Héctor; Marvin, C. J.; Mathar, Richard J.; Mirabet, E.; Montes, D.; Muñoz, Rafael Morales; Moya, A.; Naranjo, Vianac; Ofir, A.; Oreiro, R.; Πάλλη, Ε.; Panduro, J.; Passegger, V. M.; Pérez-Calpena, A.; Medialdea, D. Pérez; Perger, M.; Pluto, M.; Ramón, A.; Rebolo, R.; Redondo, Pablo Quinzá; Reffert, S.; Reinhardt, S.; Rhode, P.; Rix, H. W.; Rodler, F.; Rodrı́guez, E.; Rodríguez‐López, C.; Rodríguez-Pérez, E.; Rohloff, R. R.; Rosich, A.; Sánchez-Blanco, E.; Carrasco, M. Á. Sánchez; Sanz-Forcada, J.; Sarmiento, L. F.; Schäfer, Sebastian; Schiller, J.; Schmidt, C.; Schmitt, J. H. M. M.; Solano, E.; Stahl, O.; Storz, Clemens; Stürmer, Julian; Suárez, J. C.; Ulbrich, R. G.; Veredas, G.; Wagner, K.; Winkler, Johannes; Osorio, M. R. Zapatero; Zechmeister, M.; Paco, F. J. Abellán de; Anglada-Escudé, G.; Burgo, C. del; Klutsch, A.; Lizon, J. L.; López‐Morales, Mercedes; Morales, J. C.; Perryman, M. A. C.; Tulloch, Simon; Xu, Wei

doi:10.1117/12.2056453

Cited by 154 publications

(32 citation statements)

References 15 publications

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“…Firstly, the current TESS mission will provide many exoplanet candidates orbiting bright enough stars for characterisation with this method. Secondly, a wealth of high-resolution observations is expected with the commissioning of CRIRES+ at the VLT (Follert et al 2014) as well as other high throughput instruments such as CARMENES (Quirrenbach et al 2014). The use of smaller telescopes with high throughput spectrographs such as GI-ANO has been shown to prove fruitful in HRS exoplanet spectroscopy (Brogi et al 2018;Guilluy et al 2019).…”

Section: High-resolution Parametersmentioning

confidence: 99%

HyDRA-H: Simultaneous Hybrid Retrieval of Exoplanetary Emission Spectra

Gandhi

Madhusudhan

Hawker

et al. 2019

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High-resolution Doppler spectroscopy has been used to detect several chemical species in exoplanetary atmospheres. Such detections have traditionally relied on cross correlation of observed spectra against spectral model templates, an approach that is successful for detecting chemical species but not optimised for constraining abundances. Recent work has explored ways to perform atmospheric retrievals on high-resolution spectra (HRS) and combine them with retrievals routinely performed for low-resolution spectra (LRS) by developing a mapping from the cross correlation function to a likelihood metric. We build upon previous studies and report HyDRA-H, a hybrid retrieval code for simultaneous analysis of low-and high-resolution thermal emission spectra of exoplanets in a fully Bayesian approach. We demonstrate HyDRA-H on the hot Jupiter HD 209458b as a case study. We validate our HRS retrieval capability by confirming previous results and report a simultaneous hybrid retrieval using both HRS and LRS data. The LRS data span the HST WFC3 (1.1-1.7 µm) and Spitzer photometry (IRAC 3.6-8µm) bands, while the HRS data were obtained with CRIRES on VLT at 2.3 µm. The constraints on the composition and temperature profiles for the hybrid retrieval are more stringent than retrievals with either LRS or HRS datasets individually. We retrieve abundances of log(H 2 O) = −4.11 +0.91 −0.30 and log(CO) = −2.16 +0.99 −0.47 , and C/O = 0.99 +0.01 −0.02 , consistent with previous works. We constrain the photospheric temperature to be 1498 +216 −57 K, consistent with the equilibrium temperature. Our results demonstrate the significant advantages of hybrid retrievals by combining strengths of both HRS and LRS observations which probe complementary aspects of exoplanetary atmospheres.

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Section: High-resolution Parametersmentioning

confidence: 99%

HyDRA-H: Simultaneous Hybrid Retrieval of Exoplanetary Emission Spectra

Gandhi

Madhusudhan

Hawker

et al. 2019

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“…Another complication is that an active host star shows variability in Hα, making it harder to disentangle signatures from the star and from the planetary atmosphere (Cauley et al 2017). Recently, escaping atmospheres were detected using the metastable helium triplet at ∼ 10830Å (Nortmann et al 2018;Allart et al 2019;Alonso-Floriano et al 2019), opening up new possibilities for probing planetary atmospheres with ground-based instrumentation in the infrared, such as with CARMENES (Quirrenbach et al 2014) and SpIRou (Cloutier et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Evolution of atmospheric escape in close-in giant planets and their associated Ly α and H α transit predictions

Allan

Vidotto

2019

Monthly Notices of the Royal Astronomical Society

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Strong atmospheric escape has been detected in several close-in exoplanets. As these planets consist mostly of hydrogen, observations in hydrogen lines, such as Lyα and Hα, are powerful diagnostics of escape. Here, we simulate the evolution of atmospheric escape of close-in giant planets and calculate their associated Lyα and Hα transits. We use a one-dimensional hydrodynamic escape model to compute physical properties of the atmosphere and a ray-tracing technique to simulate spectroscopic transits. We consider giant (0.3 and 1M jup ) planets orbiting a solar-like star at 0.045au, evolving from 10 to 5000 Myr. We find that younger giants show higher rates of escape, owing to a favourable combination of higher irradiation fluxes and weaker gravities. Less massive planets show higher escape rates (10 10 -10 13 g/s) than those more massive (10 9 -10 12 g/s) over their evolution. We estimate that the 1-M jup planet would lose at most 1% of its initial mass due to escape, while the 0.3-M jup planet, could lose up to 20%. This supports the idea that the Neptunian desert has been formed due to significant mass loss in low-gravity planets. At younger ages, we find that the mid-transit Lyα line is saturated at line centre, while Hα exhibits transit depths of at most 3 -4% in excess of their geometric transit. While at older ages, Lyα absorption is still significant (and possibly saturated for the lower mass planet), the Hα absorption nearly disappears. This is because the extended atmosphere of neutral hydrogen becomes predominantly in the ground state after ∼ 1.2 Gyr.

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“…Super-Earths can be found with either high-precision RV observations or space-based transit searches. Such high-precision RV surveys include those being undertaken currently with HARPS (e.g., Díaz et al 2016), HARPS-N (M15), APF (Vogt et al 2014), and CHIRON (Tokovinin et al 2013), and in the near future with MINERVA (Swift et al 2015), CARMENES (Quirrenbach et al 2014), ESPRESSO (Mégevand et al 2014), and SPIRou (Artigau et al 2014). The major upcoming space-based transit survey is that of TESS (Ricker et al 2015).…”

Section: Introductionmentioning

confidence: 99%

A 12-Year Activity Cycle for the Nearby Planet Host Star Hd 219134

Johnson

Endl

Cochran

et al. 2016

ApJ

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The nearby (6.5 pc) star HD 219134 was recently shown by Motalebi et al. and Vogt et al. to host several planets, the innermost of which is transiting. We present 27 years of radial velocity (RV) observations of this star from the McDonald Observatory Planet Search program, and 19 years of stellar activity data. We detect a long-period activity cycle measured in the Ca II S HK index, with a period of 4230±100 days (11.7 years), very similar to the 11 year solar activity cycle. Although the period of the Saturn-mass planet HD 219134 h is close to half that of the activity cycle, we argue that it is not an artifact due to stellar activity. We also find a significant periodicity in the S HK data due to stellar rotation with a period of 22.8 days. This is identical to the period of planet f identified by Vogt et al., suggesting that this RV signal might be caused by rotational modulation of stellar activity rather than a planet. Analysis of our RVs allows us to detect the long-period planet HD 219134 h and the transiting super-Earth HD 219134 b. Finally, we use our long time baseline to constrain the presence of longer period planets in the system, excluding to s 1 objects with

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CARMENES instrument overview

Cited by 154 publications

References 15 publications

HyDRA-H: Simultaneous Hybrid Retrieval of Exoplanetary Emission Spectra

HyDRA-H: Simultaneous Hybrid Retrieval of Exoplanetary Emission Spectra

Evolution of atmospheric escape in close-in giant planets and their associated Ly α and H α transit predictions

A 12-Year Activity Cycle for the Nearby Planet Host Star Hd 219134

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