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 (P_c=7030_–630⁺⁹⁷⁰d) Saturn-mass (m_csini=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 P_c=532.6_–2.5^+4.1 days, eccentricity e_c=0.342_–0.062^+0.050 and minimum mass m_csini=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

Full paper

View the references in ADS

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 - 2023	#notes
1	V* GX And	Er*	00 18 22.8849799680	+44 01 22.637951588		10.120		7.3		M2V	516	0
2	V* GQ And	Er*	00 18 25.8251408611	+44 01 38.092431857		12.84	11.04	10.3		M3.5V	273	0
3	G 268-38	PM*	00 44 59.3309137511	-15 16 17.542839990			14.150	13.801		M4.5	118	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	212	0
5	HD 232979	Er*	04 37 40.9304170763	+52 53 37.012960438		10.006	8.648	8.750		M0.5V	175	0
6	HD 285968	PM*	04 42 55.7750207949	+18 57 29.395947044	12.668	11.49	9.951	8.931	7.702	M2.5V	310	2
7	HD 285968b	Pl	04 42 55.7753203198	+18 57 29.394344631						~	43	1
8	Wolf 1539	PM*	04 52 05.7321216445	+06 28 35.588676189	14.791	13.568	12.018	10.854	9.334	M2V	150	1
9	HD 73526	PM*	08 37 16.4833548528	-41 19 08.790456324		9.69	9.00			G6V	185	2
10	HD 82943	PM*	09 34 50.7353072232	-12 07 46.369202196		7.17	6.53			F9VFe+0.5	454	2
11	Ross 1003	PM*	11 41 44.6358403057	+42 45 07.102117090		13.36	13.795	11.524	9.18	M4.0V	125	1
12	Ross 1003c	Pl	11 41 44.6360191016	+42 45 07.104818145						~	8	0
13	Ross 1003b	Pl	11 41 44.6360191016	+42 45 07.104818145						~	23	1
14	Ross 905	PM*	11 42 11.0933350978	+26 42 23.650782778		12.06	10.613	10.272	8.24	M3V	597	1
15	Ross 905b	Pl	11 42 11.0933874353	+26 42 23.658083337						~	742	1
16	HD 122303b	Pl	14 01 03.1881878880	-02 39 17.514921066						~	10	0
17	HD 122303	PM*	14 01 03.1882316643	-02 39 17.519814662	12.343	11.177	9.707	8.745	7.66	M0V	153	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	1210	0
19	BD-07 4003	BY*	15 19 26.8269387505	-07 43 20.189497466	13.403	11.76	10.560	9.461	8.911	M3V	605	2
20	BD-07 4003c	Pl	15 19 26.8271336166	-07 43 20.190958776						~	107	1
21	BD-07 4003f	Pl?	15 19 26.8271336166	-07 43 20.190958776						~	6	0
22	BD-07 4003e	Pl	15 19 26.8271336166	-07 43 20.190958776						~	74	1
23	BD-07 4003b	Pl	15 19 26.8271336166	-07 43 20.190958776						~	82	1
24	BD-07 4003d	Pl	15 19 26.8271336166	-07 43 20.190958776						~	147	1
25	G 202-48	PM*	16 25 24.6230388531	+54 18 14.765465640		11.78	10.07	9.66		M1.5V	193	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	297	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	206	1
28	LP 229-17	LM*	18 34 36.6521805504	+40 07 26.384102544				11.104		M4V	67	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	264	1
30	BD-15 6290c	Pl	22 53 16.7323107416	-14 15 49.303409936						~	187	1
31	BD-15 6290e	Pl	22 53 16.7323107416	-14 15 49.303409936						~	45	1
32	BD-15 6290b	Pl	22 53 16.7323107416	-14 15 49.303409936						~	240	1
33	BD-15 6290d	Pl	22 53 16.7323107416	-14 15 49.303409936						~	150	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	963	1
35	TRAPPIST-1	LM*	23 06 29.3684948589	-05 02 29.037301866			18.798	16.466	14.024	M7.5e	828	0

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