CARMENES: an overview six months after first light

Quirrenbach, A.; Amado, P. J.; Caballero, J. A.; Mundt, R.; Reiners, A.; Ribas, I.; Seifert, W.; Abril, Miguel; Aceituno, J.; Alonso-Floriano, F. J.; Anwand-Heerwart, H.; Azzaro, M.; Bauer, F. F.; Barrado, D.; Becerril, S.; Béjar, V. J. S.; Benítez, D.; Berdiñas, Z. M.; Brinkmöller, M.; Cárdenas, M. C.; Casal, E.; Claret, A.; Colomé, J.; Cortés-Contreras, M.; Czesla, S.; Doellinger, M. P.; Dreizler, S.; Feiz, C.; Fernández, M.; Ferro, I. M.; Fuhrmeister, B.; Galadí, D.; Gallardo, I.; Gálvez-Ortiz, M. C.; García-Piquer, Á.; Garrido, R.; Gesa, L.; Galera, V. Gómez; Hernández, J. I. González; Peinado, R. González; Grözinger, U.; Guàrdia, J.; Guenther, E. W.; Guindos, E. de; Hagen, H. J.; Hatzes, A. P.; Hauschildt, P. H.; Helmling, J.; Henning, Thomas; Hermann, Daniel; Arabí, R. Hernández; Castaño, L. Hernández; Hernando, F. Hernández; Herrero, E.; Huber, Armin; Huber, K. F.; Huke, P.; Jeffers, S. V.; Juan, E. de; Kaminski, A.; Kehr, M.; Kim, M.; Klein, Randolf; Klüter, J.; Kürster, M.; Lafarga, M.; Lara, L. M.; Lamert, A.; Laun, W.; Launhardt, R.; Lemke, Ulrike; Lenzen, R.; Llamas, María Concepción Castrillo; Fresno, M. López del; López‐Puertas, M.; López‐Santiago, J.; Salas, J. F. López; Madinabeitia, H. Magán; Mall, U.; Mandel, H.; Mancini, L.; Molina, Juan; Fernández, D.; Martín, E. L.; Mart́ın-Rúız, S.; Marvin, C. J.; Mathar, Richard J.; Mirabet, E.; Montes, D.; Morales, J. C.; Muñoz, Rafael Morales; Nagel, E.; Naranjo, V.; Nowak, G.; Πάλλη, Ε.; Panduro, J.; Passegger, V. M.; Pavlov, A.; Pedraz, S.; Pérez, Emilio Rodríguez; Pérez-Medialdea, D.; Perger, M.; Pluto, M.; Ramón, A.; Rebolo, R.; Redondo, Pablo Quinzá; Reffert, S.; Reinhart, S.; Rhode, P.; Rix, Hans─Walter; Rodler, F.; Rodrı́guez, E.; López, C.; Rohloff, R.-R.; Rosich, A.; Carrasco, M. Á. Sánchez; Sanz-Forcada, J.; Sarkis, P.; Sarmiento, L. F.; Schäfer, Sebastian; Schiller, J.; Schmidt, C.; Schmitt, J. H. M. M.; Schöfer, P.; Schweitzer, A.; Shulyak, D.; Solano, E.; Stahl, O.; Storz, Clemens; Tabernero, H. M.; Tala, M.; Tal-Or, L.; Ulbrich, R. G.; Veredas, G.; Linares, J. I. Vico; Vilardell, F.; Wagner, K.; Winkler, Johannes; Osorio, M. R. Zapatero; Zechmeister, M.; Eiff, M. Ammler‐von; Anglada-Escudé, G.; Burgo, C. del; García-Vargas, M. L.; Klutsch, A.; Lizon, J. L.; López‐Morales, Mercedes; Ofir, A.; Pérez-Calpena, A.; Perryman, M. A. C.; Sánchez-Blanco, E.; Strachan, J. B. P.; Stürmer, Julian; Suárez, J. C.; Trifonov, T.; Tulloch, Simon; Xu, Wei

doi:10.1117/12.2231880

Cited by 76 publications

(18 citation statements)

References 21 publications

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“…We are using these spectra for calibrating spectral indices and abundance determinations with features analysed at high spectral resolution, and will appear in forthcoming publications. In particular, seven of our M-dwarf companions (namely BX Cet, o 02 Eri C, HD 233153, BD-02 2198, ρ 01 Cnc B, θ Boo B, and HD 154363 B) have also been observed with the CARMENES spectrograph with very high SNR and spectral resolution (Quirrenbach et al 2016;Reiners et al 2018).…”

Section: Observations and Reductionmentioning

confidence: 85%

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Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics★

Montes

González-Peinado

Tabernero

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We investigated almost 500 stars distributed among 193 binary or multiple systems made of late-F, G-, or early-K primaries and late-K or M dwarf companion candidates. For all of them, we compiled or measured coordinates, J-band magnitudes, spectral types, distances, and proper motions. With these data, we established a sample of 192 physically bound systems. In parallel, we carried out observations with HERMES/Mercator and obtained highresolution spectra for the 192 primaries and five secondaries. We used these spectra and the automatic StePar code for deriving precise stellar atmospheric parameters: T eff , log g, ξ, and chemical abundances for 13 atomic species, including [Fe/H]. After computing Galactocentric space velocities for all the primary stars, we performed a kinematic analysis and classified them in different Galactic populations and stellar kinematic groups of very different ages, which match our own metallicity determinations and isochronal age estimations. In particular, we identified three systems in the halo and 33 systems in the young Local Association, Ursa Major and Castor moving groups, and IC 2391 and Hyades Superclusters. We finally studied the exoplanet-metallicity relation in our 193 primaries and made a list 13 M-dwarf companions with very high metallicity that can be the targets of new dedicated exoplanet surveys. All in all, our dataset will be of great help for future works on the accurate determination of metallicity of M dwarfs.

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Section: Observations and Reductionmentioning

confidence: 85%

“…This is also illsutrated by new spectrographs optimised for exoplanet searches around M dwarfs (e.g. CARMENES -Alonso-Floriano et al 2015a ;Quirrenbach et al 2016;Reiners et al 2018).…”

Section: Introductionmentioning

confidence: 89%

Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics★

Montes

González-Peinado

Tabernero

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…We observed two transits of KELT-9b on August 6 and September 21, 2017 with the CARMENES instrument 6 . CARMENES is a high-resolution (R ∼ 94 600 in the visual channel) spectrograph installed at the 3.5 m telescope of the Calar Alto Observatory.…”

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confidence: 99%

An extended hydrogen envelope of the extremely hot giant exoplanet KELT-9b

2018

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Giant exoplanets orbiting close to their host stars have high temperatures because of the immense stellar irradiation which they receive. The extreme energy input leads to the expansion of the atmosphere and the escape of neutral hydrogen 1 2 3 . A particularly intriguing case among the hot giant planets is KELT-9b -an exoplanet orbiting very close to an early A-type star with the highest temperature (∼ 4600 K at day-side) among all the exoplanets known so far 4 . The atmospheric composition and dynamic of such a unique planet have been unknown. Here we report the first detection of an extended hot hydrogen atmosphere around KELT-9b. The detection was achieved by measuring the atomic hydrogen absorption during transit with the Balmer H α line, which is unusually strong mainly due to the high level of extreme-ultraviolet radiation from the star. We detected a significant wavelength shift of the H α absorption which is mostly attributed to the planetary orbital motion 5 . The obtained transmission spectrum has a significant line contrast (1.15% extra absorption at the H α line centre). The observation implies that the effective radius at the H α line centre is ∼ 1.64 times the size of the planetary radius, indicating the planet has a largely extended hydrogen envelope close to the size of the Roche lobe ( 1.91 +0.22 −0.26 R planet ) and is probably undergoing dramatic atmosphere escape.We observed two transits of KELT-9b on August 6 and September 21, 2017 with the CARMENES instrument 6 . CARMENES is a high-resolution (R ∼ 94 600 in the visual channel) spectrograph installed at the 3.5 m telescope of the Calar Alto Observatory. Each of the observations lasted for ∼ 6 hours covering the 4 hours transit and 1 hour before and after transit.For each transit dataset, we firstly removed the telluric H 2 O lines at the H α wavelength range and then aligned all the spectra to the stellar rest frame. A reference spectrum was obtained by combining all the spectra observed during out-of-transit. This reference spectrum is regarded as the spectrum of the star and each observed spectrum was then divided by the reference spectrum to remove the stellar H α spectrum. In this way, we obtained planetary absorption spectra with telluric and stellar lines removed. We then binned the planetary absorption spectra from both nights with a 0.01 orbital phase step, i. e. the spectra within each 0.01 phase bin were averaged with the spectral 1 arXiv:1807.00869v1 [astro-ph.EP] 2 Jul 2018 signal-to-noise ratio (SNR) as weight.The obtained planetary absorption spectra are displayed in Fig.1a. The figure shows a black shadow during transit which is the result of the H α absorption. The absorption feature has a significant wavelength shift and this radial velocity (RV) change is mostly attributed to the planetary orbital motion. We modeled the planetary absorption feature assuming it has a Gaussian profile. The semi-amplitude of the planetary orbital motion(K planet ) was set as a free parameter in the model. We included an atmosphere wind speed (...

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“…[1][2][3] As such, a number of precise Doppler spectrographs are being developed to target this spectral region (λ = 0.9 − 2.5 µm), including systems that use adaptive optics to correct for atmospheric seeing. [4][5][6][7][8][9] At the same time, ever-increasing demands for wavelength coverage and spectral resolution require large format, two-dimensional arrays to offer sufficient pixels to sample dispersed starlight.…”

Section: Introductionmentioning

confidence: 99%

Assessing the suitability of H4RG near-infrared detectors for precise Doppler radial velocity measurements

Bechter

Crepp

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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At wavelengths longwards of the sensitivity of silicon, hybrid structured mercury-cadmium-telluride (HgCdTe) detectors show promise to enable extremely precise radial velocity (RV) measurements of late-type stars. The most advanced near infrared (NIR) detector commercially available is the HAWAII series (HxRG) of NIR detectors. While the quantum efficiency of such devices has been shown to be ≈ 90%, the noise characteristics of these devices, and how they relate to RV measurements, have yet to be quantified. We characterize the various noise sources generated by H4RG arrays using numerical simulations. We present recent results using our end-to-end spectrograph simulator in combination with the HxRG Noise Generator, which emulates the effects of read noise, parameterized by white noise, correlated and uncorrelated pink (1/f ) noise, alternating column noise, and picture frame noise. The effects of nonlinear pixel response, dark current, persistence, and interpixel capacitance (IPC) on RV precision are also considered. Our results have implications for RV error budgets and instrument noise floors that can be achieved with NIR Doppler spectrographs that utilize this kind of detector.

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CARMENES: an overview six months after first light

Cited by 76 publications

References 21 publications

Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics★

Calibrating the metallicity of M dwarfs in wide physical binaries with F-, G-, and K-primaries – I: High-resolution spectroscopy with HERMES: stellar parameters, abundances, and kinematics★

An extended hydrogen envelope of the extremely hot giant exoplanet KELT-9b

Assessing the suitability of H4RG near-infrared detectors for precise Doppler radial velocity measurements

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