2013A&A...552A..78Z


Query : 2013A&A...552A..78Z

2013A&A...552A..78Z - Astronomy and Astrophysics, volume 552A, 78-78 (2013/4-1)

The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars.

ZECHMEISTER M., KUERSTER M., ENDL M., LO CURTO G., HARTMAN H., NILSSON H., HENNING T., HATZES A.P. and COCHRAN W.D.

Abstract (from CDS):

In 1992 we began a precision radial velocity survey for planets around solar-like stars with the Coude Echelle Spectrograph and the Long Camera (CES LC) at the 1.4m telescope in La Silla (Chile) resulting in the discovery of the planet ι Hor b. We have continued the survey with the upgraded CES Very Long Camera (VLC) and the HARPS spectrographs, both at the 3.6m telescope, until 2007. In this paper we present additional radial velocities for 31 stars of the original sample with higher precision. The observations cover a time span of up to 15 years and permit a search for Jupiter analogues.The survey was carried out with three different instruments/instrument configurations using the iodine absorption cell and the ThAr methods for wavelength calibration. We combine the data sets and perform a joint analysis for variability, trends, and periodicities. We compute Keplerian orbits for companions and detection limits in case of non-detections. Moreover, the HARPS radial velocities are analysed for correlations with activity indicators (CaII H&K and cross-correlation function shape).We achieve a long-term RV precision of 15m/s (CES+LC, 1992-1998), 9m/s (CES+VLC, 1999-2006), and 2.8m/s (HARPS, 2003-2009, including archive data), respectively. This enables us to confirm the known planetary signals in ι Hor and HR 506 as well as the three known planets around HR 3259. A steady RV trend for ε Ind A can be explained by a planetary companion and calls for direct imaging campaigns. On the other hand, we find previously reported trends to be smaller for β Hyi and not present for α Men. The candidate planet ε Eri b was not detected despite our better precision. Also the planet announced for HR 4523 cannot be confirmed. Long-term trends in several of our stars are compatible with known stellar companions. We provide a spectroscopic orbital solution for the binary HR 2400 and refined solutions for the planets around HR 506 and ι Hor. For some other stars the variations could be attributed to stellar activity, as e.g. the magnetic cycle in the case of HR 8323.The occurrence of two Jupiter-mass planets in our sample is in line with the estimate of 10% for the frequency of giant planets with periods smaller than 10yr around solar-like stars. We have not detected a Jupiter analogue, while the detections limits for circular orbits indicate at 5AU a sensitivity for minimum mass of at least 1MJup (2MJup) for 13% (61%) of the stars.

Abstract Copyright:

Journal keyword(s): stars: general - planetary systems - techniques: radial velocities - methods: data analysis

VizieR on-line data: <Available at CDS (J/A+A/552/A78): stars.dat lc/* vlc/* harps/*>

Simbad objects: 54

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Number of rows : 54
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 * zet Tuc PM* 00 20 04.2586334956 -64 52 29.257190108 4.82 4.80 4.23 3.73 3.40 F9.5V 362 0
2 * bet Hyi PM* 00 25 45.07036 -77 15 15.2860 3.52 3.41 2.79 2.28 1.94 G0V 576 0
3 HD 4391 EB* 00 45 45.5929295136 -47 33 07.142647212   6.418 5.794     G3V 106 0
4 * nu. Phe PM* 01 15 11.1214282378 -45 31 53.992580679 5.65 5.54 4.96 4.47 4.11 F9VFe+0.4 244 0
5 HD 9562 PM* 01 33 42.8357181696 -07 01 31.238801760 6.61 6.40 5.76     G1V 250 0
6 * q01 Eri PM* 01 42 29.3145176952 -53 44 26.991453264   6.05 5.52     F9V 296 1
7 * tau Cet PM* 01 44 04.0831371922 -15 56 14.927607677 4.43 4.22 3.50 2.88 2.41 G8V 1172 1
8 * kap For PM* 02 22 32.5904688744 -23 49 00.479863128   5.802 5.198   4.51 G0V 257 0
9 HD 16160 PM* 02 36 04.9013368983 +06 53 12.383654295   6.81   5.2   K3V 513 1
10 * iot Hor b Pl 02 42 33.4664838826 -50 48 01.056222150           ~ 43 1
11 * iot Hor PM* 02 42 33.4666679022 -50 48 01.055138166   5.97 5.40     F8V 366 1
12 * alf For B PM* 03 12 04.1990698698 -28 59 13.010512475   7.19 7.19     G7V 15 0
13 * alf For ** 03 12 04.5273570 -28 59 15.433684 4.41 4.36 3.85 3.39 3.08 F6V+G7V 258 0
14 * zet01 Ret PM* 03 17 46.1634549490 -62 34 31.152456644 6.24 6.18 5.54 5.00 4.66 G2.5VHdel1 284 0
15 * zet02 Ret ** 03 18 12.8188824117 -62 30 22.904711032   5.814 5.228     G1V 346 0
16 * eps Eri BY* 03 32 55.8444911587 -09 27 29.739493865 5.19 4.61 3.73 3.00 2.54 K2V 1806 1
17 * eps Eri b Pl 03 32 55.8449634 -09 27 29.731165           ~ 121 1
18 * del Eri * 03 43 14.9005379551 -09 45 48.210955899 5.13 4.46 3.54 2.82 2.32 K0+IV 574 0
19 * alf Men B * 06 10 13.7640981192 -74 45 12.002891832           M3.5 4 0
20 * alf Men PM* 06 10 14.4725823672 -74 45 10.958331816   5.798 5.069     G7V 260 0
21 HD 46569 PM* 06 31 18.3309320376 -51 49 33.456173988   6.102 5.573     F8VFe-0.4 54 0
22 HD 53705 PM* 07 03 57.3152216292 -43 36 28.925859669   5.94 5.28 5.05 4.71 G1.5V 184 0
23 HD 53706 PM* 07 03 58.9212523543 -43 36 40.873487765 7.978 7.632 6.851 6.427 6.013 K0.5V 135 0
24 HD 69830 PM* 08 18 23.9469682407 -12 37 55.817187530   6.74 5.95     G8:V 494 1
25 * k01 Vel ** 09 14 57.1711337256 -37 36 08.745702300   6.676 5.850     K0/1III+A3/7 20 0
26 CD-31 9113 PM* 11 35 26.9477670462 -32 32 23.884215079 12.508 11.322 9.813 8.821 7.664 M2V 141 1
27 HD 102365 PM* 11 46 31.0725331317 -40 30 01.285867174 5.65 5.55 4.88 4.35 3.97 G2V 310 1
28 HD 102365B PM* 11 46 32.6898754106 -40 29 47.604751207     15.43     M4V 19 0
29 HD 114613 PM* 13 12 03.1842958709 -37 48 10.879928463 5.86 5.55 4.85 4.28 3.92 G3V 181 0
30 NAME Proxima Centauri Er* 14 29 42.9461331854 -62 40 46.164680672 14.21 12.95 11.13 9.45 7.41 M5.5Ve 1136 0
31 * alf Cen ** 14 39 29.71993 -60 49 55.9990   0.4 -0.1     G2V+K1V 889 0
32 * alf Cen B PM* 14 39 35.06311 -60 50 15.0992 2.89 2.21 1.33     K1V 963 1
33 * alf Cen A SB* 14 39 36.49400 -60 50 02.3737 0.96 0.72 0.01     G2V 1206 0
34 GJ 570 D BD* 14 57 14.96256 -21 21 47.7504           T8 205 1
35 HD 131977 BY* 14 57 28.0007918772 -21 24 55.727265310 7.89 6.83 5.72 4.74 4.19 K4V 466 0
36 HD 150706b Pl 16 31 17.5833539505 +79 47 23.199471923           ~ 35 1
37 HD 154345b Pl 17 02 36.4039047898 +47 04 54.762678953           ~ 41 1
38 2MASS J17184972-4638190 * 17 18 49.7240325912 -46 38 19.090762944   15.03 13.65 13.24   M6.5V 4 0
39 UCAC2 11845260 * 17 18 55.0977240120 -46 37 38.754138396     14.0 14.36 13.33 M7V 5 0
40 * 41 Ara B PM* 17 19 02.9687982578 -46 38 13.108096647   10.10 8.69     M0VpCa-3Cr-1 30 0
41 * 41 Ara PM* 17 19 03.8375517433 -46 38 10.440417011 6.66 6.28 5.48 4.76 4.30 G9V 184 0
42 NAME Barnard's star BY* 17 57 48.4984700685 +04 41 36.113879676 12.497 11.24 9.511 8.298 6.741 M4V 742 2
43 HD 172051 ** 18 38 53.4010594968 -21 03 06.750986472   6.518 5.860     G6V 187 1
44 * b Aql PM* 19 24 58.1999714302 +11 56 39.888480530 6.35 5.93   4.7   G7IVHdel1 469 0
45 HD 191408 PM* 20 11 11.9387690214 -36 06 04.351725607   5.44 5.32     K2.5V 252 1
46 HD 191408B PM* 20 11 12.2 -36 06 09           M3.5 225 1
47 * phi02 Pav PM* 20 40 02.6374808954 -60 32 56.018592211   5.63 5.121     G0VFe-0.8CH-0.5 168 1
48 HD 207129 PM* 21 48 15.7511634187 -47 18 13.017893348   6.18 5.58     G2V 309 0
49 * eps Ind PM* 22 03 21.6536261624 -56 47 09.522795714   5.75 4.69     K5V 507 0
50 * eps Ind B BD* 22 04 10.5951812451 -56 46 58.239102418     24.12 20.8 15.60 T1V+T6V 143 2
51 HD 211415 PM* 22 18 15.6133953371 -53 37 37.466806476   5.98 5.39 6.52   G0V 179 0
52 * 51 Peg b Pl 22 57 27.9804167474 +20 46 07.782240714           ~ 593 1
53 HD 220096 * 23 21 15.4989573624 -26 59 12.365460132   6.470 5.656     G5IV 77 0
54 HD 222155b Pl 23 38 00.3072118024 +48 59 47.486499625           ~ 13 1

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2022.07.05-07:43:18

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