CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Quirrenbach, A.; Amado, P. J.; Ribas, I.; Reiners, A.; Caballero, J. A.; Seifert, W.; Aceituno, J.; Azzaro, M.; Baroch, D.; Barrado, D.; Bauer, F. F.; Becerril, S.; Béjar, V. J. S.; Benítez, D.; Brinkmöller, M.; Guillén, C. Cardona; Cifuentes, C.; Colomé, J.; Cortés-Contreras, M.; Czesla, S.; Dreizler, S.; Frölich, K.; Fuhrmeister, B.; Galadí-Enríquez, D.; Hernández, J. I. González; Peinado, R. González; Guenther, E. W.; Guindos, E. de; Hagen, Hans; Hatzes, A. P.; Hauschildt, P. H.; Helmling, J.; Henning, Th.; Herbort, Oliver; Castaño, L. Hernández; Herrero, E.; Hintz, D.; Jeffers, S. V.; Johnson, E. N.; Juan, E. de; Kaminski, A.; Klahr, Hubert; Kürster, M.; Lafarga, M.; Sairam, Lalitha; Lampón, M.; Lara, L. M.; Launhardt, R.; Fresno, M. López del; López‐Puertas, M.; Luque, R.; Mandel, H.; Marfil, E.; Martín, E. L.; Mart́ın-Rúız, S.; Mathar, Richard J.; Montes, D.; Morales, J. C.; Nagel, E.; Nortmann, L.; Nowak, G.; Πάλλη, Ε.; Passegger, V. M.; Pavlov, A.; Pedraz, S.; Pérez-Medialdea, D.; Perger, M.; Rebolo, R.; Reffert, S.; Rodrı́guez, E.; López, C.; Rosich, A.; Sabotta, S.; Sadegi, S.; Salz, M.; Sánchez-López, A.; Sanz-Forcada, J.; Sarkis, P.; Schäfer, Sebastian; Schiller, J.; Schmitt, J. H. M. M.; Schöfer, P.; Schweitzer, A.; Shulyak, D.; Solano, E.; Stahl, O.; Pinto, Marcelo Tala; Trifonov, T.; Osorio, M. R. Zapatero; Yan, F.; Zechmeister, M.; Abellán, F. J.; Abril, Miguel; Alonso-Floriano, F. J.; Eiff, M. Ammler‐von; Anglada-Escudé, G.; Anwand-Heerwart, H.; Arroyo-Torres, B.; Berdiñas, Z. M.; Bergondy, G.; Blümcke, M.; Burgo, C. del; Cano, J.; Carro, Joseph; Cárdenas, M. C.; Casal, E.; Claret, A.; Díez-Alonso, E.; Doellinger, M. P.; Dorda, R.; Feiz, C.; Fernández, M.; Ferro, I. M.; Gaisné, G.; Gallardo, I.; Gálvez-Ortiz, M. C.; García-Piquer, Á.; García-Vargas, María Luisa; Garrido, R.; Gesa, L.; Galera, V. Gómez; González-Álvarez, E.; González-Cuesta, L.; Grohnert, S.; Grözinger, U.; Guàrdia, J.; Guijarro, A.; Hedrosa, R. P.; Hermann, Daniel; Hermelo, I.; Arabí, R. Hernández; Hernando, F. Hernández; Hidalgo, D.; Holgado, G.; Huber, Armin; Huber, K. F.; Huke, P.; Kehr, M.; Kim, M.; Klein, Ralf; Klüter, J.; Klutsch, A.; Labarga, F.; Labiche, N.; Lamert, A.; Laun, W.; Lázaro, Francisco J.; Lemke, Ulrike; Lenzen, R.; Llamas, María Concepción Castrillo; Lizon, J. L.; Lodieu, N.; González, Marta; López‐Morales, Mercedes; Salas, J. F. López; López‐Santiago, J.; Madinabeitia, H. Magán; Mall, U.; Mancini, L.; Molina, Juan; Martínez-Rodríguez, Héctor; Fernández, D.; Marvin, C. J.; Mirabet, E.; Moreno-Raya, M. E.; Moya, A.; Mundt, R.; Naranjo, V.; Panduro, J.; Pascual, Juan Pablo; Pérez-Calpena, A.; Perryman, M. A. C.; Pluto, M.; Ramón, A.; Redondo, Pablo Quinzá; Reinhart, S.; Rhode, P.; Rix, Hans─Walter; Rodler, F.; Rohloff, R.-R.; Sánchez-Blanco, E.; Carrasco, M. Á. Sánchez; Sarmiento, L. F.; Schmidt, C.; Storz, Clemens; Strachan, J. B. P.; Stürmer, Julian; Suárez, J. C.; Tabernero, H. M.; Tal-Or, L.; Tulloch, Simon; Ulbrich, R. G.; Veredas, G.; Linares, J. L. Vico; Vidal-Dasilva, Manuela; Vilardell, F.; Wagner, K.; Winkler, Johannes; Wolthoff, V.; Xu, Wei; Zhao, Z. S.

doi:10.1117/12.2313689

Cited by 52 publications

(20 citation statements)

References 24 publications

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“…For any given MOOG-compliant EW input file comprised of a significant number of Fe i and Fe ii lines, StePar follows a Downhill Simplex minimisation algorithm (Press et al 2002) across the parameter space in order to find the stellar atmospheric parameters that best reproduce the observed EWs. The code takes T eff = 5777 K, log g = 4.44 dex, and ξ = 1.0 km s −1 as the initial input values.…”

Section: Steparmentioning

confidence: 99%

“…A full account of the key caveats of these two methods can be found in Jofré et al (2019) and Blanco-Cuaresma (2019). The advent of high-resolution near-infrared (NIR) spectrographs such as CARMENES (Quirrenbach et al 2018), SPIRou (Artigau et al 2014), GIANO (Origlia et al 2014;Oliva et al 2018), CRIRES+ (Hatzes & CRIRES+ Team 2017), IRD (Kotani et al 2014), HPF (Wright et al 2018), and NIRPS (Wildi et al 2017) allows us to revisit these techniques, originally applied in the optical, in order to assess the impact of the NIR wavelength range on stellar parameter computations. In this context, new observations of FGK-type stars carried out with CARMENES 1 , the double-channel spectrograph at the 3.5 m Calar Alto telescope open up a unique opportunity to test the reliability of such techniques on high-resolution and high signal-to-noise (S/N) ratio spectra in the optical and near-infrared windows.…”

Section: Introductionmentioning

confidence: 99%

“…The wavelength coverage provided by CARMENES, from 5 200Å up to 17 100Å, allowed us to substantially increase the number of Fe i and Fe ii lines subject to analysis with the EW method with respect to previous studies restricted to the optical window (Meléndez & Barbuy 2009;Jofré et al 2014). Furthermore, the high spectral resolution of CARMENES, which is R = 94 600 in the VIS channel and R = 80 400 in the NIR channel (Quirrenbach et al 2018), significantly improves both the line identification process and the EW measurements. Despite the availability of iron line lists optimised for the NIR region in the literature, the impact on stellar parameter determinations of FGK-type stars is still unknown, mostly due to the fact that such line lists have not as yet been systematically applied to significantly large samples covering a wide portion of the stellar parameter space.…”

Section: Introductionmentioning

confidence: 99%

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Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Marfil

Tabernero

Montes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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With the purpose of assessing classic spectroscopic methods on high-resolution and high signal-to-noise ratio spectra in the near-infrared wavelength region, we selected a sample of 65 F-, G-, and K-type stars observed with CARMENES, the new, ultrastable, double-channel spectrograph at the 3.5 m Calar Alto telescope. We computed their stellar atmospheric parameters (T eff , log g, ξ, and [Fe/H]) by means of the StePar code, a Python implementation of the equivalent width method that employs the 2017 version of the MOOG code and a grid of MARCS model atmospheres. We compiled four Fe i and Fe ii line lists suited to metal-rich dwarfs, metal-poor dwarfs, metal-rich giants, and metal-poor giants that cover the wavelength range from 5 300 to 17 100Å, thus substantially increasing the number of identified Fe i and Fe ii lines up to 653 and 23, respectively. We examined the impact of the near-infrared Fe i and Fe ii lines upon our parameter determinations after an exhaustive literature search, placing special emphasis on the 14 Gaia benchmark stars contained in our sample. Even though our parameter determinations remain in good agreement with the literature values, the increase in the number of Fe i and Fe ii lines when the near-infrared region is taken into account reveals a deeper T eff scale that might stem from a higher sensitivity of the near-infrared lines to T eff .

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Section: Steparmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Marfil

Tabernero

Montes

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Additionally, space-based surveys by the K2 (Howell et al 2014) and TESS (Ricker et al 2015) missions have significant increased the number of nearby M-dwarfs surveyed for transiting planets with small orbital periods. Ground-based radial velocity (RV) surveys using instruments such as HPF (Mahadevan et al 2012), SPIRou (Artigau et al 2014), and CARMENES (Quirrenbach et al 2018) also will target M-dwarfs to better characterize their exoplanet population, extending to larger orbital periods.…”

Section: Introductionmentioning

confidence: 99%

Occurrence Rates of Planets Orbiting FGK Stars: Combining Kepler DR25, Gaia DR2, and Bayesian Inference

et al. 2019

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We present robust planet occurrence rates for Kepler planet candidates around M stars for planet radii R p = 0.5 − 4 R ⊕ and orbital periods P = 0.5 − 256 days using the approximate Bayesian computation (ABC) technique. This work incorporates the final Kepler DR25 planet candidate catalog and data products and augment them with updated stellar properties using Gaia DR2 and 2MASS PSC. We analyze a clean sample of 1, 530 Kepler targets that host 89 associated planet candidates. These early M-dwarfs and late K-dwarfs were selected from cross-referenced targets using several photometric quality flags from Gaia DR2 and color-magnitude cuts using 2MASS magnitudes. We identify a habitable zone occurrence rate of f HZ = 0.38 +0.04 −0.05 for planets with 0.75 − 1.5 R ⊕ size. We caution that occurrence rate estimates for Kepler's M stars are sensitive to the choice of prior due to the small sample of target stars and planet candidates. For example, we find an occurrence rate of 8.9 +1.2 −0.9 or 4.8 +0.7 −0.6 planets per M-dwarf (integrating over R p = 0.5 − 4 R ⊕ and P = 0.5 − 256 days) for our two choices of prior. These occurrence rates are greater than those for FGK-dwarf target when compared at the same range of orbital periods, but similar to occurrence rates when computed as a function of equivalent stellar insolation. This suggests that stellar irradiance has a significant and possibly dominant role in planet formation processes regardless of spectral type. Combining our result with recent studies of exoplanet architectures indicates that most, and potentially all, early-M dwarfs harbor planetary systems.

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“…The CARMENES survey (Moreno-Raya et al 2018) has as a main objective to search for and classify low mass planets around ∼ 300 M dwarf stars (Reiners et al 2018). The survey's spectrograph has an RV accuracy of ∼ 1 ms −1 and has been used for the discovery of several planetary systems, including GJ4276.…”

Section: Introductionmentioning

confidence: 99%

Dynamical interactions in the planetary system GJ4276

Horrobin

Rein

2019

Monthly Notices of the Royal Astronomical Society

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GJ4276 is an M4.0 dwarf star with an inferred Neptune mass planet from radial velocity (RV) observations. We reanalyse the RV data for this system and focus on the possibility of a second, super earth mass, planet. We compute the timescale for fast resonant librations in the eccentricity to be ∼ 2 000 days. Given that the observations were taken over 700 days, we expect to see the effect of these librations in the observations. We perform a fully dynamical fit to test this hypothesis. Similar to previous results, we determine that the data could be fit by two planets in a 2:1 mean motion resonance. However, we also find solutions near the 5:4 mean motion resonance which are not present when planet-planet interactions are ignored. Using the MEGNO indicator, we analyze the stability of the system and find that our solutions lie in a stable region of parameter space. We also find that though out of resonance solutions are possible, the system favours a configuration which is in a first order mean motion resonance. The existence of mean motion resonances has important implications in many planet formation theories. Although we do not attempt to distinguish between the one and two planet models in this work, in either case, the predicted orbital parameters are interesting enough to merit further study. Future observations should be able to distinguish between the different scenarios within the next 5 years.

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CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Cited by 52 publications

References 24 publications

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra

Occurrence Rates of Planets Orbiting FGK Stars: Combining Kepler DR25, Gaia DR2, and Bayesian Inference

Dynamical interactions in the planetary system GJ4276

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