2018A&A...618A.142B


Query : 2018A&A...618A.142B

2018A&A...618A.142B - Astronomy and Astrophysics, volume 618A, 142-142 (2018/1-0)

Radial velocity follow-up of GJ1132 with HARPS. A precise mass for planet b and the discovery of a second planet.

BONFILS X., ALMENARA J.-M., CLOUTIER R., WUNSCHE A., ASTUDILLO-DEFRU N., BERTA-THOMPSON Z., BOUCHY F., CHARBONNEAU D., DELFOSSE X., DIAZ R.F., DITTMANN J., DOYON R., FORVEILLE T., IRWIN J., LOVIS C., MAYOR M., MENOU K., MURGAS F., NEWTON E., PEPE F., SANTOS N.C. and UDRY S.

Abstract (from CDS):

The source GJ1132 is a nearby red dwarf known to host a transiting Earth-size planet. After its initial detection, we pursued an intense follow-up with the HARPS velocimeter. We now confirm the detection of GJ1132b with radial velocities alone. We refined its orbital parameters, and in particular, its mass (mb=1.66+±0.23M), density (ρb=6.3±1.3g/cm3), and eccentricity (eb<0.22; 95%). We also detected at least one more planet in the system. GJ1132c is a super-Earth with period Pc=8.93±0.01-days and minimum mass mcsinic=2.64±0.44M. Receiving about 1.9 times more flux than Earth in our solar system, its equilibrium temperature is that of a temperate planet (Teq=230-300K for albedos A=0.75-0.00), which places GJ1132c near the inner edge of the so-called habitable zone. Despite an a priori favorable orientation for the system, Spitzer observations reject most transit configurations, leaving a posterior probability <1% that GJ1132c transits. GJ1132(d) is a third signal with period Pd=177±5days attributed to either a planet candidate with minimum mass mdsinid=8.4–2.5+1.7M or stellar activity. Its Doppler signal is the most powerful in our HARPS time series but appears on a timescale where either the stellar rotation or a magnetic cycle are viable alternatives to the planet hypothesis. On the one hand, the period is different than that measured for the stellar rotation (∼125days), and a Bayesian statistical analysis we performed with a Markov chain Monte Carlo and Gaussian processes demonstrates that the signal is better described by a Keplerian function than by correlated noise. On the other hand, periodograms of spectral indices sensitive to stellar activity show power excess at similar periods to that of this third signal, and radial velocity shifts induced by stellar activity can also match a Keplerian function. We, therefore, prefer to leave the status of GJ1132(d) undecided.

Abstract Copyright: © ESO 2018

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

VizieR on-line data: <Available at CDS (J/A+A/618/A142): table3.dat>

Simbad objects: 8

goto Full paper

goto View the references in ADS

Number of rows : 8
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 NAME L 320-124b Pl 10 14 51.7783473599 -47 09 24.189733387           ~ 109 0
2 NAME L 320-124c Pl 10 14 51.7783473599 -47 09 24.189733387           ~ 10 0
3 L 320-124 PM* 10 14 51.7783473599 -47 09 24.189733387       13.067   M4 84 0
4 Kepler-177b Pl 19 04 11.3086849436 +45 03 11.549711498           ~ 26 0
5 Kepler-60b Pl 19 15 50.6983559226 +42 15 54.050526895           ~ 34 1
6 Kepler-11f Pl 19 48 27.6228219845 +41 54 32.902654079           ~ 117 1
7 Kepler-11b Pl 19 48 27.6228219845 +41 54 32.902654079           ~ 133 1
8 * 51 Peg b Pl 22 57 27.9804167474 +20 46 07.782240714           ~ 571 1

To bookmark this query, right click on this link: simbad:objects in 2018A&A...618A.142B and select 'bookmark this link' or equivalent in the popup menu


2021.09.18-00:14:00

© Université de Strasbourg/CNRS

    • Contact