2013A&A...559A..83L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:17:11

2013A&A...559A..83L - Astronomy and Astrophysics, volume 559A, 83-83 (2013/11-1)

Planets around stars in young nearby associations. Radial velocity searches: a feasibility study and first results.

LAGRANGE A.-M., MEUNIER N., CHAUVIN G., STERZIK M., GALLAND F., LO CURTO G., RAMEAU J. and SOSNOWSKA D.

Abstract (from CDS):

Stars in young nearby associations are the only targets that allow giant planet searches in the near future, at all separations by coupling indirect techniques, such as radial velocity (RV) and deep imaging. These stars are first priority targets for the forthcoming planet imagers on eight- to ten-metre class telescopes. Young stars rotate more rapidly and are more active than their older counterparts. Both effects can limit the ability to detect planets using RV. We wish to explore the planet detection abilities of a representative sample of stars in close and young associations with RV data and to explore the complementarity between this technique and direct imaging. We observed 26 such targets with spectral types from A to K and ages from 8 to 300Myr with HARPS. We computed the detection limits with two methods, in particular, a method we have recently developed that takes the frequency distribution of the RV variations into account. We also attempted to improve the detection limits in a few cases by correcting for the stellar activity. Our A-type stars RV show high-frequency variations due to pulsations, while our F-K stars clearly show activity with more or less complex patterns. For F-K stars, the RV jitter and vsini rapidly decrease with star age. The data allow us to search for planets with periods typically ranging from 1 day to 100 days, and up to more than 500 days in a few cases. Within the present detection limits, no planet was found in our sample. For the bulk of our F-K stars, the detection limits fall to sub-Jupiter masses. We show that these limits can be significantly improved by correcting even partially for stellar activity, down to a few Neptune masses for the least active stars. The detection limits on A-type stars can be significantly improved, down to a few Jupiter-mass planets, provided an appropriate observing strategy. We finally show the tremendous potential of coupling RV and adaptive-optics deep imaging results. The RV technique allows the detection of planets lighter than Jupiter, reaching a few Neptune masses around young stars aged typically 30Myr or more. Detection limits increase at younger ages, but (sub-)Jupiter mass planets are still detectable. In the next few years, using complementary techniques will allow a full exploration of the Jupiter-mass planets' content of many of these stars.

Abstract Copyright:

Journal keyword(s): techniques: radial velocities - techniques: high angular resolution - planets and satellites: detection

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME THA As* 00 00 -62.0           ~ 340 0
2 HD 987 Ro* 00 13 53.0105874824 -74 41 17.851248731   9.48 8.724   7.933 G8V 79 0
3 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2654 0
4 V* AB Dor TT* 05 28 44.8916324761 -65 26 55.289846904 8.259 7.856 6.999 6.496 5.993 K0V 931 0
5 V* UY Pic RS* 05 36 56.8530716709 -47 57 52.884166166   8.77 7.676   6.699 K0V 111 0
6 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1654 1
7 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 339 1
8 HD 42270 Ro* 05 53 29.3170612989 -81 56 53.185140942   9.85 9.154   8.185 K0V 30 0
9 HD 45270 PM* 06 22 30.9412022189 -60 13 07.143258224 7.186 7.11 6.508   5.87 G1V 101 0
10 BD+20 1790 BY* 07 23 43.5892690689 +20 24 58.654590844   11.08 10.001 9.43 8.522 K5e 75 0
11 HD 61005 PM* 07 35 47.4624262763 -32 12 14.042600581   8.96 8.22     G8Vk 171 0
12 * 30 Mon PM* 08 25 39.6320108 -03 54 23.117820 3.85 3.88 3.90 3.87 3.92 A0Va 257 0
13 * 29 Cnc * 08 28 37.3395946659 +14 12 38.971903176   6.136 5.948     A5V 49 0
14 HD 90905 PM* 10 29 42.2300405874 +01 29 28.039591756       6.5   G1V 71 0
15 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
16 NAME TW Hya Association As* 11 01.9 -34 42           ~ 819 0
17 HD 102458 Y*O 11 47 24.5436617458 -49 53 03.018055867   9.70 9.07   8.40 G4V 79 0
18 HD 105690 Ro* 12 10 06.4713164686 -49 10 50.656895587   8.86 8.199   7.414 G5V 46 0
19 HD 109536 PM* 12 35 45.5323383923 -41 01 19.021555705   5.342 5.114     A7V 66 0
20 V* NY Aps BY* 15 12 23.4362962400 -75 15 15.642843358   10.23 9.378   8.512 G9V 36 0
21 HD 141493 * 15 49 56.7374312432 -15 58 16.280561430   10.422 9.498     G8III/IV 4 0
22 HD 141593 * 15 50 28.6926574074 -17 20 55.605012083   9.72 8.04     M1III 10 0
23 V* NZ Lup BY* 15 53 27.2914974411 -42 16 00.711812290   8.48 7.975   7.213 G2 73 0
24 * d Sco PM* 16 18 17.9001656 -28 36 50.476788   4.804 4.782     A1Va 147 0
25 HD 172555 PM* 18 45 26.9004853 -64 52 16.539796   4.967 4.767     A7V 234 0
26 V* PZ Tel BY* 18 53 05.8733807460 -50 10 49.901380086   9.22 8.342   7.464 G9IV 286 0
27 * rho Tel PM* 19 06 19.9556991283 -52 20 27.288013018   5.700 5.174     F6V 68 0
28 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 225 0
29 HD 183414 PM* 19 35 09.7191296886 -69 58 32.098743191   8.538 7.891     G3V 42 0
30 HD 188288 * 19 54 08.4088692380 +07 12 49.157737207   10.52 9.43     K0 2 0
31 HD 188828 * 19 58 25.9025474185 -37 04 11.332547144   10.36 8.89     K2III 3 0
32 * eps Pav PM* 20 00 35.5555788 -72 54 37.819779   3.927 3.940     A0Va 111 0
33 V* BO Mic BY* 20 47 44.9892114361 -36 35 40.819135413   10.39 9.337   8.216 K3V(e) 165 0
34 HD 207575 PM* 21 52 09.7248951966 -62 03 08.508117999   7.72 7.23     F6V 63 0
35 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1115 3
36 HD 217343 PM* 23 00 19.2872945687 -26 09 13.506860661   8.12 7.48   6.75 G5V 94 0
37 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 896 0
38 HD 224228 PM* 23 56 10.6732720614 -39 03 08.409993692 9.977 9.21 8.225 7.669 7.194 K2V 67 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-18:17:11

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