2012A&A...545A..87M


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.27CET11:48:45

2012A&A...545A..87M - Astronomy and Astrophysics, volume 545A, 87-87 (2012/9-1)

Comparison of different exoplanet mass detection limit methods using a sample of main-sequence intermediate-type stars.

MEUNIER N., LAGRANGE A.-M. and DE BONDT K.

Abstract (from CDS):

The radial velocity (RV) technique is a powerful tool for detecting extrasolar planets and deriving mass detection limits that are useful for constraining planet pulsations and formation models. Detection limit methods must take into account the temporal distribution of power of various origins in the stellar signal. These methods must also be able to be applied to large samples of stellar RV time series We describe new methods for providing detection limits. We compute the detection limits for a sample of ten main-sequence stars, which are of G-F-A type, in general active, and/or with detected planets and various properties. We use them to compare the performances of these methods with those of two other methods used in the litterature. We obtained detection limits in the 2-1000-day period range for ten stars. Two of the proposed methods, based on the correlation between periodograms and the power in the periodogram of the RV time series in specific period ranges, are robust and represent a significant improvement compared to a method based on the root mean square of the RV signal. We conclude that two of the new methods (correlation-based method and local power analysis, i.e. LPA, method) provide robust detection limits, which are better than those provided by methods that do not take into account the temporal sampling.

Abstract Copyright:

Journal keyword(s): techniques: radial velocities - planetary systems - stars: early-type - stars: general

Simbad objects: 11

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Number of rows : 11

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 10180 * 01 37 53.5773715933 -60 30 41.485438420   7.95 7.32     G1V 156 2
2 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1686 1
3 HD 60532 PM* 07 34 03.1802404179 -22 17 45.838378187 5.02 4.94 4.39     F6IV-V 203 1
4 HD 105690 Ro* 12 10 06.4713164686 -49 10 50.656895587   8.86 8.199   7.414 G5V 48 0
5 * 38 Vir ** 12 53 11.1564265214 -03 33 11.148154533   6.61 6.11     F6V 78 0
6 * iot Cen PM* 13 20 35.8128156095 -36 42 44.296492410 2.77 2.76 2.73 2.68 2.69 kA1.5hA3mA3Va 194 0
7 * iot Vir PM* 14 16 00.8695049 -06 00 01.963348 4.64 4.60 4.08     F7III 338 0
8 HD 172555 PM* 18 45 26.9004853 -64 52 16.539796   4.967 4.767     A7V 240 0
9 HD 199260 PM* 20 56 47.3303687041 -26 17 46.969399809   6.20 5.70     F6V 101 0
10 * tau PsA PM* 22 10 08.7803395485 -32 32 54.275502381   5.40 4.92     F6V 135 0
11 HD 219482 PM* 23 16 57.6873978547 -62 00 04.318777045   6.146 5.647     F6V 105 0

    Equat.    Gal    SGal    Ecl

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