2018A&A...609A.117T

Query : 2018A&A...609A.117T

2018A&A...609A.117T - Astronomy and Astrophysics, volume 609A, 117-117 (2018/1-1)

The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems.

TRIFONOV T., KURSTER M., ZECHMEISTER M., TAL-OR L., CABALLERO J.A., QUIRRENBACH A., AMADO P.J., RIBAS I., REINERS A., REFFERT S., DREIZLER S., HATZES A.P., KAMINSKI A., LAUNHARDT R., HENNING T., MONTES D., BEJAR V.J.S., MUNDT R., PAVLOV A., SCHMITT J.H.M.M., SEIFERT W., MORALES J.C., NOWAK G., JEFFERS S.V., RODRIGUEZ-LOPEZ C., DEL BURGO C., ANGLADA-ESCUDE G., LOPEZ-SANTIAGO J., MATHAR R.J., AMMLER-VON EIFF M., GUENTHER E.W., BARRADO D., GONZALEZ HERNANDEZ J.I., MANCINI L., STURMER J., ABRIL M., ACEITUNO J., ALONSO-FLORIANO F.J., ANTONA R., ANWAND-HEERWART H., ARROYO-TORRES B., AZZARO M., BAROCH D., BAUER F.F., BECERRIL S., BENITEZ D., BERDINAS Z.M., BERGOND G., BLUMCKE M., BRINKMOLLER M., CANO J., CARDENAS VAZQUEZ M.C., CASAL E., CIFUENTES C., CLARET A., COLOME J., CORTES-CONTRERAS M., CZESLA S., DIEZ-ALONSO E., 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-PEINADO R., GROZINGER U., GROHNERT S., GUARDIA J., GUIJARRO A., DE GUINDOS E., GUTIERREZ-SOTO J., HAGEN H.-J., HAUSCHILDT P.H., HEDROSA R.P., HELMLING J., HERMELO I., HERNANDEZ ARABI R., HERNANDEZ CASTANO L., HERNANDEZ HERNANDO F., HERRERO E., HUBER A., HUKE P., JOHNSON E., DE JUAN E., KIM M., KLEIN R., KLUTER J., KLUTSCH A., LAFARGA M., LAMPON M., LARA L.M., LAUN W., LEMKE U., LENZEN R., LOPEZ DEL FRESNO M., LOPEZ-GONZALEZ M.J., LOPEZ-PUERTAS M., LOPEZ SALAS J.F., LUQUE R., MAGAN MADINABEITIA H., MALL U., MANDEL H., MARFIL E., MARIN MOLINA J.A., MAROTO FERNANDEZ D., MARTIN E.L., MARTIN-RUIZ S., MARVIN C.J., MIRABET E., MOYA A., MORENO-RAYA M.E., NAGEL E., NARANJO V., NORTMANN L., OFIR A., OREIRO R., PALLE E., PANDURO J., PASCUAL J., PASSEGGER V.M., PEDRAZ S., PEREZ-CALPENA A., PEREZ MEDIALDEA D., PERGER M., PERRYMAN M.A.C., PLUTO M., RABAZA O., RAMON A., REBOLO R., REDONDO P., REINHARDT S., RHODE P., RIX H.-W., RODLER F., RODRIGUEZ E., 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., SCHILLER J., SCHOFER P., SCHWEITZER A., SOLANO E., STAHL O., STRACHAN J.B.P., SUAREZ J.C., TABERNERO H.M., TALA M., TULLOCH S.M., VEREDAS G., VICO LINARES J.I., VILARDELL F., WAGNER K., WINKLER J., WOLTHOFF V., XU W., YAN F. and ZAPATERO OSORIO M.R.

Abstract (from CDS):

Context. The main goal of the CARMENES survey is to find Earth-mass planets around nearby M-dwarf stars. Seven M dwarfs included in the CARMENES sample had been observed before with HIRES and HARPS and either were reported to have one short period planetary companion (GJ 15 A, GJ 176, GJ 436, GJ 536 and GJ 1148) or are multiple planetary systems (GJ 581 and GJ 876).
Aims. We aim to report new precise optical radial velocity measurements for these planet hosts and test the overall capabilities of CARMENES.
Methods. We combined our CARMENES precise Doppler measurements with those available from HIRES and HARPS and derived new orbital parameters for the systems. Bona-fide single planet systems were fitted with a Keplerian model. The multiple planet systems were analyzed using a self-consistent dynamical model and their best fit orbits were tested for long-term stability.
Results. We confirm or provide supportive arguments for planets around all the investigated stars except for GJ 15 A, for which we find that the post-discovery HIRES data and our CARMENES data do not show a signal at 11.4 days. Although we cannot confirm the super-Earth planet GJ 15 Ab, we show evidence for a possible long-period (Pc=7030–630+970d) Saturn-mass (mcsini=51.8–5.8+5.5M⊕) planet around GJ 15 A. In addition, based on our CARMENES and HIRES data we discover a second planet around GJ 1148, for which we estimate a period Pc=532.6–2.5+4.1 days, eccentricity ec=0.342–0.062+0.050 and minimum mass mcsini=68.1–2.2+4.9M⊕.
Conclusions. The CARMENES optical radial velocities have similar precision and overall scatter when compared to the Doppler measurements conducted with HARPS and HIRES. We conclude that CARMENES is an instrument that is up to the challenge of discovering rocky planets around low-mass stars.

Abstract Copyright: © ESO, 2018

Journal keyword(s): planetary systems - stars: late-type - stars: low-mass - planets and satellites: dynamical evolution and stability

VizieR on-line data: <Available at CDS (J/A+A/609/A117): table1.dat gj1148.dat gj15a.dat gj176.dat gj436.dat gj536.dat gj581.dat gj876.dat>

Simbad objects: 35

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Number of rows : 35
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 HD 1326 Er* 00 18 22.8849799680 +44 01 22.637951588   10.120   7.3   M2V 542 0
2 HD 1326B Er* 00 18 25.8251408611 +44 01 38.092431857   12.84 11.04 10.3   M3.5V 286 0
3 G 268-38 PM* 00 44 59.3309137511 -15 16 17.542839990     14.150 13.801   M4.5V 141 0
4 V* VX Ari Er* 02 44 15.5097410539 +25 31 24.114854200 13.363 12.141 10.563 9.49 8.115 dM3 220 0
5 HD 232979 Er* 04 37 40.9304170763 +52 53 37.012960438   10.006 8.648 8.750   M0.5V 181 0
6 HD 285968b Pl 04 42 55.7750207949 +18 57 29.395947044           ~ 47 1
7 HD 285968 PM* 04 42 55.7750207949 +18 57 29.395947044 12.668 11.49 9.951 8.931 7.702 M2.5V 335 2
8 Wolf 1539 PM* 04 52 05.7321216445 +06 28 35.588676189 14.791 13.568 12.018 10.854 9.334 M2V 158 1
9 HD 73526 PM* 08 37 16.4833548528 -41 19 08.790456324   9.69 9.00     G6V 190 2
10 HD 82943 PM* 09 34 50.7353072232 -12 07 46.369202196   7.17 6.53     F9VFe+0.5 470 2
11 Ross 1003c Pl 11 41 44.6358403057 +42 45 07.102117090           ~ 10 0
12 Ross 1003 PM* 11 41 44.6358403057 +42 45 07.102117090   13.36 13.795 11.524 9.18 M4.0V 139 1
13 Ross 1003b Pl 11 41 44.6358403057 +42 45 07.102117090           ~ 29 1
14 Ross 905b Pl 11 42 11.0933350978 +26 42 23.650782778           ~ 810 1
15 Ross 905 PM* 11 42 11.0933350978 +26 42 23.650782778   12.06 10.613 10.272 8.24 M3V 645 1
16 HD 122303 PM* 14 01 03.1882316643 -02 39 17.519814662 12.343 11.177 9.707 8.745 7.66 M0V 163 0
17 HD 122303b Pl 14 01 03.1882316643 -02 39 17.519814662           ~ 11 0
18 NAME Proxima Centauri Er* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1299 0
19 BD-07 4003f Pl? 15 19 26.8269387505 -07 43 20.189497466           ~ 7 0
20 BD-07 4003 BY* 15 19 26.8269387505 -07 43 20.189497466 13.403 11.76 10.560 9.461 8.911 M3V 641 2
21 BD-07 4003c Pl 15 19 26.8269387505 -07 43 20.189497466           ~ 115 1
22 BD-07 4003e Pl 15 19 26.8269387505 -07 43 20.189497466           ~ 79 1
23 BD-07 4003d Pl 15 19 26.8269387505 -07 43 20.189497466           ~ 152 1
24 BD-07 4003b Pl 15 19 26.8269387505 -07 43 20.189497466           ~ 88 1
25 G 202-48 PM* 16 25 24.6230388531 +54 18 14.765465640   11.78 10.07 9.66   M1.5V 207 0
26 BD-12 4523 BY* 16 30 18.0583947383 -12 39 45.321217732 12.829 11.638 10.072 8.917 7.421 M3V 315 0
27 BD+25 3173 PM* 16 58 08.8496107083 +25 44 38.974052855 12.342 11.139 9.655 8.685 7.602 M2V 224 1
28 LP 229-17 LM* 18 34 36.6521805504 +40 07 26.384102544       11.104   M4V 77 0
29 BD-05 5715 PM* 22 09 40.3443137051 -04 38 26.650757960 13.006 11.868 10.366 9.279 7.877 M3.5V 286 1
30 BD-15 6290b Pl 22 53 16.7325836486 -14 15 49.304052185           ~ 253 1
31 BD-15 6290d Pl 22 53 16.7325836486 -14 15 49.304052185           ~ 157 1
32 BD-15 6290e Pl 22 53 16.7325836486 -14 15 49.304052185           ~ 50 1
33 BD-15 6290c Pl 22 53 16.7325836486 -14 15 49.304052185           ~ 195 1
34 BD-15 6290 BY* 22 53 16.7325836486 -14 15 49.304052185 12.928 11.749 10.192 9.013 7.462 M3.5V 1013 1
35 TRAPPIST-1 LM* 23 06 29.3684948589 -05 02 29.037301866     18.798 16.466 14.024 M7.5e 995 0

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