2011A&A...525A..95S


Query : 2011A&A...525A..95S

2011A&A...525A..95S - Astronomy and Astrophysics, volume 525A, 95-95 (2011/1-1)

Search for brown-dwarf companions of stars.

SAHLMANN J., SEGRANSAN D., QUELOZ D., UDRY S., SANTOS N.C., MARMIER M., MAYOR M., NAEF D., PEPE F. and ZUCKER S.

Abstract (from CDS):

The frequency of brown-dwarf companions in close orbit around Sun-like stars is low compared to the frequency of planetary and stellar companions. There is presently no comprehensive explanation of this lack of brown-dwarf companions. By combining the orbital solutions obtained from stellar radial-velocity curves and Hipparcos astrometric measurements, we attempt to determine the orbit inclinations and therefore the masses of the orbiting companions. By determining the masses of potential brown-dwarf companions, we improve our knowledge of the companion mass-function. The radial-velocity solutions revealing potential brown-dwarf companions are obtained for stars from the CORALIE and HARPS planet-search surveys or from the literature. The best Keplerian fit to our radial-velocity measurements is found using the Levenberg-Marquardt method. The spectroscopic elements of the radial-velocity solution constrain the fit to the intermediate astrometric data of the new Hipparcos reduction. The astrometric solution and the orbit inclination are found using non-linear χ2-minimisation on a two-parameter search grid. The statistical confidence of the adopted orbital solution is evaluated based on the distribution-free permutation test. The discovery of nine new brown-dwarf candidates orbiting stars in the CORALIE and HARPS radial-velocity surveys is reported. New CORALIE radial velocities yielding accurate orbits of six previously-known hosts of potential brown-dwarf companions are presented. Including the literature targets, 33 hosts of potential brown-dwarf companions are examined. Employing innovative methods, we use the new reduction of the Hipparcos data to fully characterise the astrometric orbits of six objects, revealing M-dwarf companions of masses between 90MJ and 0.52M. In addition, the masses of two companions can be restricted to the stellar domain. The companion to HD 137510 is found to be a brown dwarf. At 95% confidence, the companion of HD 190228 is also a brown dwarf. Twenty-three companions remain brown-dwarf candidates. On the basis of the CORALIE planet-search sample, we obtain an upper limit of 0.6% for the frequency of brown-dwarf companions around Sun-like stars. We find that the companion-mass distribution function increases toward the lower end of the brown-dwarf mass range, suggesting that we detect the high-mass tail of the planetary distribution. Our findings agree with the results of previous similar studies and confirm the pronounced paucity of brown-dwarf companions around Sun-like stars. They are affected by the Hipparcos astrometric precision and mission duration, which limits the minimum detectable companion mass, and some of the remaining candidates are probably brown-dwarf companions.

Abstract Copyright:

Journal keyword(s): binaries: spectroscopic - brown dwarfs - stars: low-mass - techniques: radial velocities - astrometry

VizieR on-line data: <Available at CDS (J/A+A/525/A95): stars.dat tables.dat>

Errata: + corrigendum vol. 565, p. C2 (2014)

Status at CDS : All or part of tables of objects will be ingested in SIMBAD with priority 1.

Simbad objects: 52

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Number of rows : 52
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 3277 SB* 00 35 34.2519910392 -39 44 46.656656448   8.18 7.44     G8V 52 0
2 HD 4747 SB* 00 49 26.7604733944 -23 12 44.868742449 8.244 7.927 7.155 6.732 6.344 G8/K0V 192 0
3 HD 13189 * 02 09 40.1723129208 +32 18 59.160568824   9.04 7.55     K1II-III 83 1
4 HD 17289 SB* 02 43 35.4775673808 -62 55 09.103440972   8.00 7.43     G0V 45 0
5 HD 18445 SB* 02 57 13.1880251976 -24 58 30.414869580   9.01 7.86     K2V 106 0
6 BD-04 782 SB* 04 15 09.5344264586 -04 25 06.381142715 11.755 10.561 9.332 8.591 7.953 K5V 58 0
7 HD 30501 SB* 04 45 38.5783009064 -50 04 27.122415732 9.054 8.474 7.588 7.105 6.676 K2V 103 0
8 HD 30339 SB* 04 49 33.3469509960 +53 21 56.555449056   8.80 8.21     F8 55 0
9 HD 33636 Pe* 05 11 46.4494089528 +04 24 12.742146936   7.64   6.6   G0V_CH-0.3 192 1
10 HD 38529b Pl 05 46 34.9131388488 +01 10 05.502949860           ~ 88 1
11 HD 38529c Pl 05 46 34.9131388488 +01 10 05.502949860           ~ 83 1
12 HD 38529 PM* 05 46 34.9131388488 +01 10 05.502949860       5.4   G8III/IV 352 2
13 HD 43848 SB* 06 16 31.3559942976 -40 31 54.827597100   9.57 8.64     K2IV 41 1
14 HD 43848b Pl 06 16 31.3559942976 -40 31 54.827597100           ~ 9 1
15 HD 52756 SB* 07 00 29.5974807720 -41 22 47.306259516   9.35 8.47     K2IV 43 0
16 HD 53680 SB* 07 03 50.2137045243 -43 33 41.408685706 11.01 9.882 8.686 7.949 7.327 K6V 76 0
17 HD 53706 PM* 07 03 58.9212523543 -43 36 40.873487765 7.978 7.632 6.851 6.427 6.013 K0.5V 142 0
18 HD 65430 SB* 07 59 33.9396570535 +20 50 38.143369909 9.004 8.494 7.649 7.195 6.776 K0V 114 1
19 HD 74014 SB* 08 41 18.5612367504 -04 48 32.185759032   8.33 7.57     K0III 73 0
20 HD 74842 ** 08 44 45.0018205930 -42 38 04.058486266 8.26 7.96 7.22     G8V 62 0
21 HD 89707 SB* 10 20 49.9823777315 -15 28 47.688646996   7.72 7.18     G2VFe-1.5CH-0.8 139 0
22 HD 91669 PM* 10 34 54.4257484776 -13 47 16.624536036   10.62 9.70     K0/1III 26 0
23 * 11 Com PM* 12 20 43.0257695904 +17 47 34.327512348   5.74 4.74     G8+IIIFe-1 164 1
24 HD 112758 ** 12 59 01.5612841731 -09 50 02.679322421 8.737 8.384 7.588 7.163 6.729 G9V 188 1
25 HD 119445 PM* 13 42 28.8064320072 +41 40 27.425956548   7.178 6.289     G6III 35 0
26 HD 131664 * 15 00 06.0800617968 -73 32 07.189532412   8.82 8.13     G3V 81 1
27 HD 137510b Pl? 15 25 53.2697518752 +19 28 50.545457724           ~ 13 0
28 HD 137510 PM* 15 25 53.2697518752 +19 28 50.545457724   6.872 6.241     G0IV-V 111 0
29 L 768-119 SB* 15 42 06.5402655256 -19 28 18.312134612 14.559 13.46 11.855 10.738 9.305 M3 83 0
30 HD 140913 SB* 15 45 07.4491027968 +28 28 11.738768232   8.664 8.053     G0V 104 0
31 HD 145849 SB* 16 11 48.0553638168 +36 25 30.341129808   6.981 5.615     K3III 54 0
32 HD 154697 SB* 17 07 14.4091213440 -02 52 00.994366380   8.57 7.82     G6V 44 0
33 HD 162020 * 17 50 38.3557484304 -40 19 06.072311784   10.11 9.12     K3V 152 1
34 HD 164427B PM* 18 04 41.0746481280 -59 12 08.092807812       12.12 10.20 ~ 10 0
35 HD 164427 SB* 18 04 42.5969086224 -59 12 34.469434044   7.50 6.89     G0+V 64 0
36 HD 167665 SB* 18 17 23.7587105112 -28 17 20.218638480   6.94 6.40     F9VFe-0.8CH-0.4 110 0
37 HD 168443b Pl 18 20 03.9332862096 -09 35 44.614653900           ~ 97 1
38 HD 168443c Pl 18 20 03.9332862096 -09 35 44.614653900           ~ 95 1
39 HD 168443 PM* 18 20 03.9332862096 -09 35 44.614653900   7.62 6.92     G6V 313 1
40 HD 174457 SB* 18 50 02.0580006528 +15 18 41.432514516       7.2   F8 60 0
41 * 59 Dra PM* 19 09 09.8814606288 +76 33 37.813819608   5.400 5.107     A7V 128 1
42 CoRoT-3b Pl 19 28 13.2642131544 +00 07 18.613986132           ~ 138 1
43 HD 190228 PM* 20 03 00.7726656864 +28 18 24.687065520   8.094 7.296     G5IV 169 1
44 HD 190228b Pl 20 03 00.7726656864 +28 18 24.687065520           ~ 45 1
45 HD 189310 SB* 20 13 16.4278229424 -82 01 41.316970620   9.36 8.45     K2V 38 0
46 HD 191760 PM* 20 13 26.7462823536 -46 12 03.708889200   8.91 8.25     G3IV/V 46 1
47 CD-40 14067 SB* 20 52 16.3988020128 -39 59 50.580427020   11.72 10.39     K6.5Vk: 25 0
48 HD 202206 PM* 21 14 57.7686051936 -20 47 21.161521320   8.79 8.07     G6V 235 1
49 HD 202206c Pl 21 14 57.7686051936 -20 47 21.161521320           ~ 45 1
50 HD 202206b Pl 21 14 57.7686051936 -20 47 21.161521320           ~ 57 1
51 HD 211847 SB* 22 20 55.7384451240 -41 25 48.384652332   9.27 8.62     G5V 38 0
52 HD 217580 SB* 23 01 51.5363732448 -03 50 55.402732729 9.199 8.428 7.464 6.934 6.482 K3V 103 0

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