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J/A+A/612/A49      324 CARMENES M dwarfs velocities            (Reiners+, 2018)

The CARMENES search for exoplanets around M dwarfs. High-resolution optical and near-infrared spectroscopy of 324 survey stars. Reiners A., Zechmeister M., Caballero J.A., Ribas I., Morales J.C., Jeffers S.V., Schofer 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-Escude G., Anwand-Heerwart H., Arroyo-Torres B., Azzaro M., Baroch D., Barrado D., Bauer F.F., Becerril S., Bejar V.J.S., Benitez D., Berdinas Z.M., Bergond G., Blumcke M., Brinkmoller M., Del Burgo C., Cano J., Cardenas Vazquez M.C., Casal E., Cifuentes C., Claret A., Colome J., Cortes-Contreras M., Czesla S., Diez-Alonso E., Dreizler S., Feiz C., Fernandez M., Ferro I.M., Fuhrmeister B., Galadi-Enriquez D., Garcia-Piquer A., Garcia Vargas M.L., Gesa L., Gomez Galera V., Gonzalez Hernandez J.I., Gonzalez-Peinado R., Grozinger U., Grohnert S., Guardia J., Guenther E.W., Guijarro A., De Guindos E., Gutierrez-Soto J., Hagen H.-J., Hatzes A.P., Hauschildt P.H., Hedrosa R.P., Helmling J., Henning T., Hermelo I., Hernandez Arabi R., Hernandez Castano L., Hernandez Hernando F., Herrero E., Huber A., Huke P., Johnson E.N., De Juan E., Kim M., Klein R., Kluter J., Klutsch A., Kurster M., Lafarga M., Lamert A., Lampon M., Lara L.M., Laun W., Lemke U., Lenzen R., Launhardt R., Lopez Del Fresno M., Lopez-Gonzalez J., Lopez-Puertas M., Lopez Salas J.F., Lopez-Santiago J., Luque R., Magan Madinabeitia H., Mall U., Mancini L., Mandel H., Marfil E., Marin Molina J.A., Maroto Fernandez D., Martin E.L., Martin-Ruiz S., Marvin C.J., Mathar R.J., Mirabet E., Montes D., Moreno-Raya M.E., Moya A., Mundt R., Nagel E., Naranjo V., Nortmann L., Nowak G., Ofir A., Oreiro R., Palle E., Panduro J., Pascual J., Passegger V.M., Pavlov A., Pedraz S., Perez-Calpena A., Perez Medialdea D., Perger M., Perryman M.A.C., Pluto M., Rabaza O., Ramon A., Rebolo R., Redondo P., Reffert S., Reinhart S., Rhode P., Rix H.-W., Rodler F., Rodriguez E., Rodriguez-Lopez C., Rodriguez Trinidad A., Rohloff R.-R., Rosich A., Sadegi S., Sanchez-Blanco E., Sanchez Carrasco M.A., Sanchez-Lopez A., Sanz-Forcada J., Sarkis P., Sarmiento L.F., Schafer S., Schmitt J.H.M.M., Schiller J., Schweitzer A., Solano E., Stahl O., Strachan J.B.P., Sturmer J., Suarez J.C., Tabernero H.M., Tala M., Trifonov T., Tulloch S.M., Ulbrich R.G., Veredas G., Vico Linares J.I., Vilardell F., Wagner K., Winkler J., Wolthoff V., Xu W., Yan F., Zapatero Osorio M.R. <Astron. Astrophys., 612, A49 (2018)> =2018A&A...612A..49R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Stars, dwarfs ; Radial velocities ; Rotational velocities Keywords: atlases - catalogs - stars: rotation - stars: late-type - stars: low-mass - infrared: stars 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>80000, 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 700-900nm. 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 1m/s 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 3-4m/s. Description: As part of the GTO agreement, we provide early access to one CARMENES spectrum for each of our sample targets (Table B.1). They can be downloaded from the CARMENES GTO Data Archive (Caballero et al., 2016, in Observatory Operations: Strategies, Processes, and Systems VI, Proc. SPIE, 9910, 99100E) (http://carmenes.cab.inta-csic.es) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tableb1.dat 128 324 Basic data of the CARMENES GTO sample
See also: J/A+A/577/A128 : CARMENES input catalogue of M dwarfs. I (Alonso-Floriano+, 2015) J/A+A/597/A47 : CARMENES input catalogue of M dwarfs II (Cortes-Contreras+ 2017) J/A+A/609/A117 : CARMENES radial velocity curves of 7 M-dwarf (Trifonov+, 2018) J/A+A/609/L5 : HD147379 b velocity curve (Reiners+, 2018) J/A+A/614/A122 : Radial-velocity of CARMENES M dwarfs (Tal-Or+, 2018) Byte-by-byte Description of file: tableb1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Sequential number 5- 15 A11 --- ID ID (JHHMMm+DDmA) 17- 22 A6 --- GJ GJ name 24- 46 A23 --- Name Name 48- 51 A4 --- SpType MK spectral type 53- 57 F5.2 mag Jmag J magnitude 59- 62 F4.2 Msun Mass Mass 64- 71 F8.3 km/s RV Radial velocity 73- 78 F6.2 d Per ? Period 80- 84 F5.2 d e_Per ? rms uncertainty on Per 86- 91 A6 --- r_Per Period reference (1) 93 A1 --- l_vsini Limit flag on vsini 94- 97 F4.1 km/s vsini Rotational velocity 99-102 F4.1 km/s e_vsini ? rms uncertainty on vsini 104 A1 --- l_Pvsini Limit flag on Pvsini 105-109 F5.2 d Pvsini Period from vsini 111-115 F5.2 d e_Pvsini ? rms uncertainty on Pvsini 116-117 A2 --- l_i [≤ ] Limit flag on i 118-119 I2 deg i ? Inclination 121-122 I2 deg e_i ? rms uncertainty on i 124-128 F5.2 [-] logLHa/Lbol ? Hα to bolometric luminosity ratio
Note (1): References as follows Irw11 = Irwin et al. (2011ApJ...727...56I) New16a = Newton et al. (2016, Cat. J/ApJ/821/93) SM16a = Suarez Mascareno et al. (2016A&A...595A..12S) Kira12 = Kiraga (2012, Cat. J/AcA/62/67) KS07 = Kiraga & Stepien (2007AcA....57..149K) HM15 = Houdebine & Mullan (2015ApJ...801..106H) Chu74 = Chugainov (1974IzKry..52....3C) FH00 = Fekel & Henry (2000AJ....120.3265F) Har11 = Hartman et al. (2011, Cat. J/AJ/141/166) WF11 = Wang & Ford (2011MNRAS.418.1822W) West15 = West et al. (2015, Cat. J/ApJ/812/3) SM15 = Suarez Mascareno et al. (2015MNRAS.452.2745S) Nor07 = Norton et al. (2007, Cat. J/A+A/467/785) Ba83 = Baliunas et al. (1983ApJ...275..752B) Kor10 = Korhonen et al. (2010AN....331..772K) Tes04 = Testa et al. (2004ApJ...617..508T) KS13 = Kiraga & Stepien (2013, Cat. J/AcA/63/53)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Jun-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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