@misc{reiners2017carmenes,
  abstract = {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--1710nm at a resolution of at least $R > 80,000$, and we
measure its RV, H$\alpha$ 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--900nm. 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 1ms$^{-1}$ in very low mass M dwarfs at longer wavelengths likely requires
the use of a 10m 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 4m class telescope, an instrument like CARMENES has the
potential to push the RV precision well below the typical jitter level of
3-4ms$^{-1}$.},
  added-at = {2017-11-20T19:39:43.000+0100},
  author = {Reiners, A. and Zechmeister, M. and Caballero, J. A. and Ribas, I. and Morales, J. C. and Jeffers, S. V. and Schöfer, P. and Tal-Or, L. and Quirrenbach, A. and Amado, P. J. and Kaminski, A. and Seifert, W. and Abril, M. and Aceituno, J. and Alonso-Floriano, F. J. and Eiff, M. Ammler-von and Antona, R. and Anglada-Escudé, G. and Anwand-Heerwart, H. and Arroyo-Torres, B. and Azzaro, M. and Baroch, D. and Barrado, D. and Bauer, F. F. and Becerril, S. and Béjar, V. J. S. and Benítez, D. and Berdiñas, Z. M. and Bergond, G. and Blümcke, M. and Brinkmöller, M. and del Burgo, C. and Cano, J. and Vázquez, M. C. Cárdenas and Casal, E. and Cifuentes, C. and Claret, A. and Colomé, J. and Cortés-Contreras, M. and Czesla, S. and Díez-Alonso, E. and Dreizler, S. and Feiz, C. and Fernández, M. and Ferro, I. M. and Fuhrmeister, B. and Galadí-Enríquez, D. and Garcia-Piquer, A. and Vargas, M. L. García and Gesa, L. and Gómez, V. and Galera and Hernández, J. I. González and González-Peinado, R. and Grözinger, U. and Grohnert, S. and Guàrdia, J. and Guenther, E. W. and Guijarro, A. and de Guindos, E. and Gutiérrez-Soto, J. and Hagen, H. J. and Hatzes, A. P. and Hauschildt, P. H. and Hedrosa, R. P. and Helmling, J. and Henning, Th. and Hermelo, I. and Arabí, R. Hernández and Castaño, L. Hernández and Hernando, F. Hernández and Herrero, E. and Huber, A. and Huke, P. and Johnson, E. and de Juan, E. and Kim, M. and Klein, R. and Klüter, J. and Klutsch, A. and Kürster, M. and Lafarga, M. and Lamert, A. and Lampón, M. and Lara, L. M. and Laun, W. and Lemke, U. and Lenzen, R. and Launhardt, R. and del Fresno, M. López and López-González, J. and López-Puertas, M. and Salas, J. F. López and López-Santiago, J. and Luque, R. and Madinabeitia, H. Magán and Mall, U. and Mancini, L. and Mandel, H. and Marfil, E. and Molina, J. A. Marín and Maroto, D. and Fernández and Martín, E. L. and Martín-Ruiz, S. and Marvin, C. J. and Mathar, R. J. and Mirabet, E. and Montes, D. and Moreno-Raya, M. E. and Moya, A. and Mundt, R. and Nagel, E. and Naranjo, V. and Nortmann, L. and Nowak, G. and Ofir, A. and Oreiro, R. and Pallé, E. and Panduro, J. and Pascual, J. and Passegger, V. M. and Pavlov, A. and Pedraz, S. and Pérez-Calpena, A. and Medialdea, D. Pérez and Perger, M. and Perryman, M. A. C. and Pluto, M. and Rabaza, O. and Ramón, A. and Rebolo, R. and Redondo, P. and Reffert, S. and Reinhart, S. and Rhode, P. and Rix, H. W. and Rodler, F. and Rodríguez, E. and Rodríguez-López, C. and Trinidad, A. Rodríguez and Rohloff, R. R. and Rosich, A. and Sadegi, S. and Sánchez-Blanco, E. and Carrasco, M. A. Sánchez and Sánchez-López, A. and Sanz-Forcada, J. and Sarkis, P. and Sarmiento, L. F. and Schäfer, S. and Schmitt, J. H. M. M. and Schiller, J. and Schweitzer, A. and Solano, E. and Stahl, O. and Strachan, J. B. P. and Stürmer, J. and Suárez, J. C. and Tabernero, H. M. and Tala, M. and Trifonov, T. and Tulloch, S. M. and Ulbrich, R. G. and Veredas, G. and Linares, J. I. Vico and Vilardell, F. and Wagner, K. and Winkler, J. and Wolthoff, V. and Xu, W. and Yan, F. and Osorio, M. R. Zapatero},
  biburl = {http://www.bibsonomy.org/bibtex/292656324489fa380bdb0bb38c00486eb/superjenwinters},
  description = {The CARMENES search for exoplanets around M dwarfs: High-resolution
  optical and near-infrared spectroscopy of 324 survey stars},
  interhash = {659eddba860d48a570c7a8ca924c261a},
  intrahash = {92656324489fa380bdb0bb38c00486eb},
  keywords = {multiplicity mdwarf nearby exoplanet},
  note = {cite arxiv:1711.06576Comment: accepted for publication in A&A, 13 pages plus 40 pages spectral  atlas, first 10 atlas pages are reduced in quality to fit arXiv size limit;  one CARMENES spectrum for each of the 324 stars is published in electronic  format at http://carmenes.cab.inta-csic.es/},
  timestamp = {2017-11-20T19:39:43.000+0100},
  title = {The CARMENES search for exoplanets around M dwarfs: High-resolution
  optical and near-infrared spectroscopy of 324 survey stars},
  url = {http://arxiv.org/abs/1711.06576},
  year = 2017
}

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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--900nm. 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 1ms$^{-1}$ in very low mass M dwarfs at longer wavelengths likely requires the use of a 10m class telescope. 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CARMENES search for exoplanets around M dwarfs: High-resolution optical and near-infrared spectroscopy of 324 survey stars","interhash":"659eddba860d48a570c7a8ca924c261a","intrahash":"92656324489fa380bdb0bb38c00486eb","keywords":"multiplicity mdwarf nearby exoplanet","note":"cite arxiv:1711.06576Comment: accepted for publication in A&A, 13 pages plus 40 pages spectral atlas, first 10 atlas pages are reduced in quality to fit arXiv size limit; one CARMENES spectrum for each of the 324 stars is published in electronic format at http://carmenes.cab.inta-csic.es/","timestamp":"2017-11-20T19:39:43.000+0100","title":"The CARMENES search for exoplanets around M dwarfs: High-resolution optical and near-infrared spectroscopy of 324 survey stars","url":"http://arxiv.org/abs/1711.06576","year":"2017","bibtex":"@misc{reiners2017carmenes,\n abstract = {The CARMENES radial velocity (RV) survey is observing 324 M dwarfs to search\r\nfor any orbiting planets. In this paper, we present the survey sample by\r\npublishing one CARMENES spectrum for each M dwarf. These spectra cover the\r\nwavelength range 520--1710nm at a resolution of at least $R > 80,000$, and we\r\nmeasure its RV, H$\\alpha$ emission, and projected rotation velocity. We present\r\nan atlas of high-resolution M-dwarf spectra and compare the spectra to\r\natmospheric models. To quantify the RV precision that can be achieved in\r\nlow-mass stars over the CARMENES wavelength range, we analyze our empirical\r\ninformation on the RV precision from more than 6500 observations. We compare\r\nour high-resolution M-dwarf spectra to atmospheric models where we determine\r\nthe spectroscopic RV information content, $Q$, and signal-to-noise ratio. We\r\nfind that for all M-type dwarfs, the highest RV precision can be reached in the\r\nwavelength range 700--900nm. Observations at longer wavelengths are equally\r\nprecise only at the very latest spectral types (M8 and M9). We demonstrate that\r\nin this spectroscopic range, the large amount of absorption features\r\ncompensates for the intrinsic faintness of an M7 star. To reach an RV precision\r\nof 1ms$^{-1}$ in very low mass M dwarfs at longer wavelengths likely requires\r\nthe use of a 10m class telescope. For spectral types M6 and earlier, the\r\ncombination of a red visual and a near-infrared spectrograph is ideal to search\r\nfor low-mass planets and to distinguish between planets and stellar\r\nvariability. At a 4m class telescope, an instrument like CARMENES has the\r\npotential to push the RV precision well below the typical jitter level of\r\n3-4ms$^{-1}$.},\n added-at = {2017-11-20T19:39:43.000+0100},\n author = {Reiners, A. and Zechmeister, M. and Caballero, J. A. and Ribas, I. and Morales, J. C. and Jeffers, S. V. and Schöfer, P. and Tal-Or, L. and Quirrenbach, A. and Amado, P. J. and Kaminski, A. and Seifert, W. and Abril, M. and Aceituno, J. and Alonso-Floriano, F. J. and Eiff, M. Ammler-von and Antona, R. and Anglada-Escudé, G. and Anwand-Heerwart, H. and Arroyo-Torres, B. and Azzaro, M. and Baroch, D. and Barrado, D. and Bauer, F. F. and Becerril, S. and Béjar, V. J. S. and Benítez, D. and Berdiñas, Z. M. and Bergond, G. and Blümcke, M. and Brinkmöller, M. and del Burgo, C. and Cano, J. and Vázquez, M. C. Cárdenas and Casal, E. and Cifuentes, C. and Claret, A. and Colomé, J. and Cortés-Contreras, M. and Czesla, S. and Díez-Alonso, E. and Dreizler, S. and Feiz, C. and Fernández, M. and Ferro, I. M. and Fuhrmeister, B. and Galadí-Enríquez, D. and Garcia-Piquer, A. and Vargas, M. L. García and Gesa, L. and Gómez, V. and Galera and Hernández, J. I. González and González-Peinado, R. and Grözinger, U. and Grohnert, S. and Guàrdia, J. and Guenther, E. W. and Guijarro, A. and de Guindos, E. and Gutiérrez-Soto, J. and Hagen, H. J. and Hatzes, A. P. and Hauschildt, P. H. and Hedrosa, R. P. and Helmling, J. and Henning, Th. and Hermelo, I. and Arabí, R. Hernández and Castaño, L. Hernández and Hernando, F. Hernández and Herrero, E. and Huber, A. and Huke, P. and Johnson, E. and de Juan, E. and Kim, M. and Klein, R. and Klüter, J. and Klutsch, A. and Kürster, M. and Lafarga, M. and Lamert, A. and Lampón, M. and Lara, L. M. and Laun, W. and Lemke, U. and Lenzen, R. and Launhardt, R. and del Fresno, M. López and López-González, J. and López-Puertas, M. and Salas, J. F. López and López-Santiago, J. and Luque, R. and Madinabeitia, H. Magán and Mall, U. and Mancini, L. and Mandel, H. and Marfil, E. and Molina, J. A. Marín and Maroto, D. and Fernández and Martín, E. L. and Martín-Ruiz, S. and Marvin, C. J. and Mathar, R. J. and Mirabet, E. and Montes, D. and Moreno-Raya, M. E. and Moya, A. and Mundt, R. and Nagel, E. and Naranjo, V. and Nortmann, L. and Nowak, G. and Ofir, A. and Oreiro, R. and Pallé, E. and Panduro, J. and Pascual, J. and Passegger, V. M. and Pavlov, A. and Pedraz, S. and Pérez-Calpena, A. and Medialdea, D. Pérez and Perger, M. and Perryman, M. A. C. and Pluto, M. and Rabaza, O. and Ramón, A. and Rebolo, R. and Redondo, P. and Reffert, S. and Reinhart, S. and Rhode, P. and Rix, H. W. and Rodler, F. and Rodríguez, E. and Rodríguez-López, C. and Trinidad, A. Rodríguez and Rohloff, R. R. and Rosich, A. and Sadegi, S. and Sánchez-Blanco, E. and Carrasco, M. A. Sánchez and Sánchez-López, A. and Sanz-Forcada, J. and Sarkis, P. and Sarmiento, L. F. and Schäfer, S. and Schmitt, J. H. M. M. and Schiller, J. and Schweitzer, A. and Solano, E. and Stahl, O. and Strachan, J. B. P. and Stürmer, J. and Suárez, J. C. and Tabernero, H. M. and Tala, M. and Trifonov, T. and Tulloch, S. M. and Ulbrich, R. G. and Veredas, G. and Linares, J. I. Vico and Vilardell, F. and Wagner, K. and Winkler, J. and Wolthoff, V. and Xu, W. and Yan, F. and Osorio, M. R. Zapatero},\n biburl = {http://www.bibsonomy.org/bibtex/292656324489fa380bdb0bb38c00486eb/superjenwinters},\n description = {The CARMENES search for exoplanets around M dwarfs: High-resolution\r\n optical and near-infrared spectroscopy of 324 survey stars},\n interhash = {659eddba860d48a570c7a8ca924c261a},\n intrahash = {92656324489fa380bdb0bb38c00486eb},\n keywords = {multiplicity mdwarf nearby exoplanet},\n note = {cite arxiv:1711.06576Comment: accepted for publication in A&A, 13 pages plus 40 pages spectral atlas, first 10 atlas pages are reduced in quality to fit arXiv size limit; one CARMENES spectrum for each of the 324 stars is published in electronic format at http://carmenes.cab.inta-csic.es/},\n timestamp = {2017-11-20T19:39:43.000+0100},\n title = {The CARMENES search for exoplanets around M dwarfs: High-resolution\r\n optical and near-infrared spectroscopy of 324 survey stars},\n url = {http://arxiv.org/abs/1711.06576},\n year = 2017\n}\n\n","author_short":["Reiners, A.","Zechmeister, M.","Caballero, J. 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