2017A&A...599A..57B


Query : 2017A&A...599A..57B

2017A&A...599A..57B - Astronomy and Astrophysics, volume 599A, 57-57 (2017/3-1)

Extrasolar planets and brown dwarfs around AF-type stars. IX. The HARPS southern sample.

BORGNIET S., LAGRANGE A.-M., MEUNIER N. and GALLAND F.

Abstract (from CDS):

Context. Massive, main-sequence (MS) AF-type stars have so far remained unexplored in past radial velocities (RV) surveys due to their small number of spectral lines and high rotational velocities that prevent the classic RV computation method.
Aims. Our aim is to search for giant planets (GPs) around AF MS stars, to get primary statistical information on their occurrence rate and to compare the results with evolved stars and lower-mass MS stars.
Methods. We used the HARPS spectrograph located on the 3.6m telescope at ESO La Silla Observatory to observe 108 AF MS stars with B-V in the range -0.04 to 0.58 and masses in the range 1.1 to 3.6M. We used our SAFIR software developed to compute the RV and other spectroscopic observables of these early-type stars. We characterized the detected companions as well as the intrinsic stellar variability. We computed the detection limits and used them as well as the detected companions to derive the first estimates of the close-in brown dwarf (BD) and GP frequencies around AF stars.
Results. We report the detection of a mpsini=4.51MJup planetary companion with an ∼826-day period to the F6V dwarf HD 111998. We also present new data on the two-planet system around the F6IV-V dwarf HD 60532. We also report the detections of 14 binaries with long-term RV trends and/or high-amplitude RV variations combined to a flat RV-bisector span diagram. We constrain the minimal masses and semi-major axes of these companions and check that these constraints are compatible with the stellar companions previously detected by direct imaging or astrometry for six of these targets. We get detection limits deep into the planetary domain with 70% of our targets showing detection limits between 0.1 and 10MJup at all orbital periods in the 1- to 103-day range. We derive BD (13≤mpsini≤80MJup) occurrence rates in the 1- to 103-day period range of 2–2+5% and 2.6–2.6+6.7% for stars with M* in the ranges 1.1 to 1.5 and 1.5 to 3M, respectively. As for Jupiter-mass companions (1≤mpsini≤13MJup), we get occurrence rates in the 1- to 103-day period range of 4–0.9+5.9% and 6.3–6.3+15.9% respectively for the same M* ranges. When considering the same Jupiter-mass companions but periods in the 1- to 100-day range only, we get occurrence rates of 2–2+5.2% and 3.9–3.9+9.9%. Given the present error bars, these results do not show a significant difference from companion frequencies derived in the same domains for solar-like MS stars.

Abstract Copyright: © ESO, 2017

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

Simbad objects: 28

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Number of rows : 28
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 NAME THA As* 00 00 -62.0           ~ 467 0
2 HD 15082 EB* 02 26 51.0582618096 +37 33 01.736482032   8.41 8.14     kA5hA8mF4 198 1
3 HD 25457 TT* 04 02 36.7442719512 -00 16 08.119921152   5.88 5.38     F7V 265 0
4 Cl Melotte 25 OpC 04 29 47.3 +16 56 53           ~ 3071 0
5 * bet Cae PM* 04 42 03.4822983552 -37 08 39.588865224   5.42 5.05     F3IV 97 0
6 HD 49095 PM* 06 45 22.9403936275 -31 47 37.133210127   6.396 5.916     F6.5V 85 0
7 HD 60532c Pl 07 34 03.1805638968 -22 17 45.843172440           ~ 25 1
8 HD 60532 PM* 07 34 03.1805638968 -22 17 45.843172440 5.02 4.94 4.39     F6IV-V 223 1
9 HD 60532b Pl 07 34 03.1805638968 -22 17 45.843172440           ~ 25 1
10 * B Car SB* 08 09 00.6369168474 -61 18 08.545898653   5.163 4.742     F6VFe-0.8CH-0.4 163 0
11 OGLE2-TR L9 * 11 07 55.1808382920 -61 08 46.537684260       14.60   F3 35 1
12 * iot Crt PM* 11 38 40.0180807728 -13 12 06.981257088   5.97 5.48     F6.5V 80 0
13 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 439 2
14 * 38 Vir b Pl 12 53 11.1567755256 -03 33 11.151261180           ~ 6 0
15 * 38 Vir ** 12 53 11.1567755256 -03 33 11.151261180   6.61 6.11     F6V 95 0
16 HD 113337 PM* 13 01 46.9268934864 +63 36 36.795618540       5.8   F6V 112 1
17 * iot Vir PM* 14 16 00.8682760805 -06 00 01.969483331 4.64 4.60 4.08     F7III 357 0
18 HD 125276 PM* 14 19 00.8956927577 -25 48 55.529829905   6.36 5.87     F9VFe-1.5CH-0.7 100 0
19 * mu. Ser ** 15 49 37.20696 -03 25 48.7358 3.39 3.49 3.53 3.54 3.59 B9.5III 113 0
20 * 26 Oph ** 17 00 09.5293323528 -24 59 20.901756372   6.117 5.731     F3V 57 0
21 CoRoT-11 EB* 18 42 44.9499236256 +05 56 15.652972716   13.73 12.939     F6V 52 1
22 HD 196385 PM* 20 37 52.2290682144 -25 06 33.177581820   6.684 6.377     A9V 55 0
23 * 29 Vul PM* 20 38 31.3388452704 +21 12 04.185221724 4.73 4.80 4.82 4.79 4.83 A0Va(_sh) 130 0
24 * 16 Del ** 20 55 38.5698407208 +12 34 06.877431480 5.740 5.650 5.540     A5V 43 0
25 * del Aqr PM* 22 54 39.0062577912 -15 49 14.950434720 3.41 3.33 3.28 3.21 3.17 A3Vp 159 0
26 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1135 0
27 HD 223011 PM* 23 46 01.2562482888 -40 10 57.236437668   6.503 6.302     A7III/IV 51 0
28 * eta Tuc ** 23 57 35.0786487048 -64 17 53.627347464   5.046 4.989     A1V 86 0

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