Bibcode
Reiners, A.; Zechmeister, M.; Caballero, J. A.; Ribas, I.; Morales, J. C.; Jeffers, S. V.; Schöfer, P.; Tal-Or, L.; Quirrenbach, A.; Amado, P. J.; Kaminski, A.; Seifert, W.; Abril, M.; Aceituno, J.; Alonso-Floriano, F. J.; Ammler-von Eiff, M.; Antona, R.; Anglada-Escudé, G.; Anwand-Heerwart, H.; Arroyo-Torres, B.; Azzaro, M.; Baroch, D.; Barrado, D.; Bauer, F. F.; Becerril, S.; Béjar, V. J. S.; Benítez, D.; Berdinas˜, Z. M.; Bergond, G.; Blümcke, M.; Brinkmöller, M.; del Burgo, C.; Cano, J.; Cárdenas Vázquez, M. C.; Casal, E.; Cifuentes, C.; Claret, A.; Colomé, J.; Cortés-Contreras, M.; Czesla, S.; Díez-Alonso, E.; Dreizler, S.; Feiz, C.; Fernández, M.; Ferro, I. M.; Fuhrmeister, B.; Galadí-Enríquez, D.; Garcia-Piquer, A.; García Vargas, M. L.; Gesa, L.; Galera, V. Gómez; González Hernández, J. I.; González-Peinado, R.; Grözinger, U.; Grohnert, S.; Guàrdia, J.; Guenther, E. W.; Guijarro, A.; Guindos, E. de; Gutiérrez-Soto, J.; Hagen, H.-J.; Hatzes, A. P.; Hauschildt, P. H.; Hedrosa, R. P.; Helmling, J.; Henning, Th.; Hermelo, I.; Hernández Arabí, R.; Hernández Castaño, L.; Hernández Hernando, F.; Herrero, E.; Huber, A.; Huke, P.; Johnson, E. N.; Juan, E. de; Kim, M.; Klein, R.; Klüter, J.; Klutsch, A.; Kürster, M.; Lafarga, M.; Lamert, A.; Lampón, M.; Lara, L. M.; Laun, W.; Lemke, U.; Lenzen, R.; Launhardt, R.; López del Fresno, M.; López-González, J.; López-Puertas, M.; López Salas, J. F.; López-Santiago, J.; Luque, R.; Magán Madinabeitia, H.; Mall, U.; Mancini, L.; Mandel, H.; Marfil, E.; Marín Molina, J. A. et al.
Bibliographical reference
Astronomy and Astrophysics, Volume 612, id.A49, 63 pp.
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4
2018
Journal
Citations
213
Refereed citations
188
Description
The CARMENES radial velocity (RV) survey is observing 324 M dwarfs to
search for any orbiting planets. In this paper, we present the survey
sample by publishing one CARMENES spectrum for each M dwarf. These
spectra cover the wavelength range 520-1710 nm at a resolution of at
least R >80 000, and we measure its RV, Hα emission, and
projected rotation velocity. We present an atlas of high-resolution
M-dwarf spectra and compare the spectra to atmospheric models. To
quantify the RV precision that can be achieved in low-mass stars over
the CARMENES wavelength range, we analyze our empirical information on
the RV precision from more than 6500 observations. We compare our
high-resolution M-dwarf spectra to atmospheric models where we determine
the spectroscopic RV information content, Q, and signal-to-noise ratio.
We find that for all M-type dwarfs, the highest RV precision can be
reached in the wavelength range 700-900 nm. Observations at longer
wavelengths are equally precise only at the very latest spectral types
(M8 and M9). We demonstrate that in this spectroscopic range, the large
amount of absorption features compensates for the intrinsic faintness of
an M7 star. To reach an RV precision of 1 m s-1 in very low
mass M dwarfs at longer wavelengths likely requires the use of a 10 m
class telescope. For spectral types M6 and earlier, the combination of a
red visual and a near-infrared spectrograph is ideal to search for
low-mass planets and to distinguish between planets and stellar
variability. At a 4 m class telescope, an instrument like CARMENES has
the potential to push the RV precision well below the typical jitter
level of 3-4 m s-1.
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