2007A&A...469..755M


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET08:50:15

2007A&A...469..755M - Astronomy and Astrophysics, volume 469, 755-770 (2007/7-2)

The multiplicity of exoplanet host stars. Spectroscopic confirmation of the companions GJ 3021B and HD 27442B, one new planet host triple-star system, and global statistics.

MUGRAUER M., NEUHAEUSER R. and MAZEH T.

Abstract (from CDS):

We present new results from our ongoing multiplicity study of exoplanet host stars and present a list of 29 confirmed planet host multiple-star systems. Furthermore, we discuss the properties of these stellar systems and compare the properties of exoplanets detected in these systems with those of planets orbiting single stars. We used direct imaging to search for wide stellar and substellar companions of exoplanet host stars. With infrared and/or optical spectroscopy, we determined the spectral properties of the newly-found co-moving companions. We obtained infrared H- and K-band spectra of the co-moving companion GJ3021B. The infrared spectra and the apparent H-band photometry of the companion is consistent with an M3-M5 dwarf at the distance of the exoplanet host star. HD40979AB is a wide planet host stellar system, with a separation of ∼6400AU. The companion to the exoplanet host star turned out to be a close stellar pair with a projected separation of ∼130AU, hence, this system is a new member of those rare planet host triple-star systems of which only three other systems are presently known. HD27442AB is a wide binary system listed in the Washington Double Star Catalogue, whose common proper motion was recently confirmed. This system is composed of the subgiant HD27442A hosting the exoplanet, and its faint companion HD27442B. The visible and infrared J-, H-, and KS-band photometry of HD27442B at the distance of the primary star shows that the companion is probably a white dwarf. Our multi-epochs SofI imaging observations confirm this result and even refine the suggested physical characteristics of HD27442B. This companion should be a relatively young, hot white dwarf with an effective temperature of ∼14400K, and cooling age of ∼220Myr. Finally, we could unambiguously confirm the white dwarf nature of HD27442B with follow-up optical and infrared spectroscopy. The spectra of the companion show Hydrogen absorption features of the Balmer, Paschen, and Bracket series. With its subgiant primary and the white-dwarf companion, the HD27442AB system is the most evolved planet host stellar system known today. The mass-period and eccentricity-period correlation of planets around single stars and those residing in multiple-star systems seem different for the short-period planets. The distribution functions of planet orbital elements (P, e) are identical, while the mass-distribution (msin (i)) exhibits one difference. While both planet populations exhibit a peak in their mass-distribution at about 1MJup, the frequency of more massive planets continually decreases in single-star systems, whereas the mass-distribution of planets residing in multiple-star systems exhibits a further peak at about 4MJup. This indicates that the mass-distributions of the two planet populations might differ in the intermediate mass-range between 2 and 6MJup.

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Journal keyword(s): planetary systems

Simbad objects: 56

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Number of rows : 56

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 142 PM* 00 06 19.17544 -49 04 30.6817   6.30 5.76     F7V 220 1
2 HD 1237 PM* 00 16 12.6791488703 -79 51 04.244738563 7.692 7.335 6.578     G8V 203 1
3 HD 1237b Pl 00 16 12.6791488703 -79 51 04.244738563           ~ 53 1
4 HD 1237B * 00 16 15.0173846445 -79 51 01.177169459           M4V 4 1
5 * ups And PM* 01 36 47.84216 +41 24 19.6443 4.70 4.64 4.10 3.64 3.35 F9V 900 1
6 HD 11964 PM* 01 57 09.6073695508 -10 14 32.731766141   7.25 6.42     G9VCN+1 158 1
7 HD 13445 PM* 02 10 25.9190575041 -50 49 25.467227759   6.945 6.117     K1.5V 421 1
8 * 79 Cet b Pl 02 35 19.9292617962 -03 33 38.170691640           ~ 47 1
9 * 79 Cet PM* 02 35 19.9292617962 -03 33 38.170691640   7.49 6.78     G2V 270 1
10 * 94 Cet PM* 03 12 46.4369076602 -01 11 45.949836281   5.631 5.070     F8.5V 412 1
11 * eps Ret b Pl 04 16 29.0292136 -59 18 07.761375           ~ 44 1
12 * eps Ret PM* 04 16 29.0292136 -59 18 07.761375 6.59 5.52 4.44 3.62 3.08 K2III 216 1
13 * eps Ret B WD* 04 16 30.0402559816 -59 17 57.185290440     12.5     DA3 21 1
14 HD 41004 ** 05 59 49.6473573887 -48 14 22.805780232   9.49 8.65     K1IV 156 1
15 BD+44 1351 ** 06 04 13.0202246416 +44 16 41.081491427   10.05 9.105 9.05   ~ 15 0
16 HD 40979 PM* 06 04 29.9429293369 +44 15 37.597677891       6.4   F8 140 1
17 HD 46375 PM* 06 33 12.6225933827 +05 27 46.527797938   8.70 7.84     K1IV 211 2
18 HD 48215 * 06 42 07.3134536154 -06 06 51.394830610   6.885 6.999     B5/7III 21 0
19 HD 50491 * 06 52 40.7075487485 -21 11 03.397762033   7.331 7.434     B4V 21 0
20 HD 75289 PM* 08 47 40.3895634256 -41 44 12.456269569 7.04 6.94 6.36     F9VFe+0.3 253 1
21 UCAC3 97-62778 PM* 08 47 42.2616260300 -41 44 07.440815787       15.95 13.50 ~ 8 0
22 * rho01 Cnc c Pl 08 52 35.8113282132 +28 19 50.956901366           ~ 127 1
23 * rho01 Cnc PM* 08 52 35.8113282132 +28 19 50.956901366 7.45 6.82   5.4   K0IV-V 993 1
24 * rho01 Cnc e Pl 08 52 35.8113282132 +28 19 50.956901366           ~ 429 1
25 HD 80606 PM* 09 22 37.5769478105 +50 36 13.434928660   9.78 9.00     G5 291 2
26 HD 89744 PM* 10 22 10.5623067078 +41 13 46.308754730       5.4   F7V 307 1
27 HD 89744b Pl 10 22 10.5623067078 +41 13 46.308754730           ~ 48 1
28 * 83 Leo A PM* 11 26 45.3217209044 +03 00 47.158549988 7.78 7.28 6.46 6.0   G9IV-V 212 0
29 * 83 Leo ** 11 26 45.8 +03 00 35 7.63 7.01 6.16     ~ 209 0
30 * 83 Leo B PM* 11 26 46.2784696716 +03 00 22.757061950 9.467 8.554 7.530 6.97 6.508 K3 175 1
31 * 83 Leo Bb Pl 11 26 46.2784696716 +03 00 22.757061950           ~ 32 1
32 HD 109749 PM* 12 37 16.3786075146 -40 48 43.624370244   8.864 8.208 8.96   G3V 78 1
33 HD 114762 SB* 13 12 19.7467346230 +17 31 01.611425890 7.78         F9VgF8mF4+M6?V 518 1
34 HD 114729 PM* 13 12 44.2594905817 -31 52 24.057468040   7.31 6.69     G0V 166 1
35 * tau Boo Ro* 13 47 15.74340 +17 27 24.8552 5.02 4.98 4.49 4.09 3.85 F7IV-V 899 1
36 HD 142022 PM* 16 10 15.0268591227 -84 13 53.813712139   8.47 7.69     G9IV-V 91 1
37 HD 142022b Pl 16 10 15.0268591227 -84 13 53.813712139           ~ 25 1
38 HD 178911B PM* 19 09 03.0984180671 +34 35 59.473294546   8.71   7.3   G5 117 1
39 HD 178911 SB* 19 09 04.3519341413 +34 36 01.242009328   7.37   6.3   G1V+K1V 124 0
40 * 16 Cyg A ** 19 41 48.9539315338 +50 31 30.218780803 6.79 6.59 5.95 5.50 5.17 G1.5Vb 689 1
41 * 16 Cyg B PM* 19 41 51.9731830550 +50 31 03.086127222 7.07 6.86 6.20 5.76 5.42 G3V 810 1
42 HD 188753 ** 19 54 58.3717655 +41 52 17.529759   8.22 7.44 6.9   G9V 127 1
43 HD 188753A SB* 19 54 58.4 +41 52 17   8.2 7.4     ~ 20 1
44 HD 188753B * 19 54 58.4 +41 52 17   8.4 8.72     ~ 21 0
45 HD 190360c Pl 20 03 37.4049065078 +29 53 48.495330996           ~ 44 1
46 HD 190360 PM* 20 03 37.4049065078 +29 53 48.495330996   6.44   5.2   G7IV-V 397 1
47 HD 195019 PM* 20 28 18.6366531368 +18 46 10.179936391 7.730     6.5   G1V 236 1
48 HD 196050 PM* 20 37 51.7098385539 -60 38 04.147300896   8.16 7.49   9.01 G3V 126 1
49 HD 213240 PM* 22 31 00.3665162994 -49 25 59.767492660   7.41 6.80     G0/1V 156 1
50 * 51 Peg b Pl 22 57 27.9804167474 +20 46 07.782240714           ~ 546 1
51 * psi01 Aqr PM* 23 15 53.4952540919 -09 05 15.841221338 6.37 5.36 4.25 3.46 2.90 K1-IIIFe-0.5 223 1
52 * gam Cep b Pl 23 39 20.9015326708 +77 37 56.505477975           ~ 67 1
53 * gam Cep SB* 23 39 20.9015326708 +77 37 56.505477975 5.190 4.250   2.6   K1III-IVCN1 558 1
54 HD 222582 PM* 23 41 51.5299950324 -05 59 08.731514665   8.34 7.69     G5V 204 2
55 HD 222582b Pl 23 41 51.5299950324 -05 59 08.731514665           ~ 45 1
56 NAME Hyades Moving Group MGr ~ ~           ~ 244 0

    Equat.    Gal    SGal    Ecl

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2021.03.01-08:50:15

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