2022A&A...666A.187D


Query : 2022A&A...666A.187D

2022A&A...666A.187D - Astronomy and Astrophysics, volume 666A, 187 (2022/10-1)

A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514 A super-Earth on an eccentric orbit moving in and out of the habitable zone,.

DAMASSO M., PERGER M., ALMENARA J.M., NARDIELLO D., PEREZ-TORRES M., SOZZETTI A., HARA N.C., QUIRRENBACH A., BONFILS X., ZAPATERO OSORIO M.R., ASTUDILLO-DEFRU N., GONZALEZ HERNANDEZ J.I., SUAREZ MASCARENO A., AMADO P.J., FORVEILLE T., LILLO-BOX J., ALIBERT Y., CABALLERO J.A., CIFUENTES C., DELFOSSE X., FIGUEIRA P., GALADI-ENRIQUEZ D., HATZES A.P., HENNING T., KAMINSKI A., MAYOR M., MURGAS F., MONTES D., PINAMONTI M., REINERS A., RIBAS I., BEJAR V.J.S., SCHWEITZER A. and ZECHMEISTER M.

Abstract (from CDS):


Context. Statistical analyses based on Kepler data show that most of the early-type M dwarfs host multi-planet systems consisting of Earth- to sub-Neptune-sized planets with orbital periods of up to ∼250 days, and that at least one such planet is likely located within the habitable zone. M dwarfs are therefore primary targets to search for potentially habitable planets in the solar neighbourhood.
Aims. We investigated the presence of planetary companions around the nearby (7.6 pc) and bright (V = 9 mag) early-type M dwarf Gl 514, analysing 540 radial velocities collected over nearly 25 yr with the HIRES, HARPS, and CARMENES spectrographs.
Methods. The data are affected by time-correlated signals at the level of 2-3 m s–1 due to stellar activity, which we filtered out, testing three different models based on Gaussian process regression. As a sanity cross-check, we repeated the analyses using HARPS radial velocities extracted with three different algorithms. We used HIRES radial velocities and Hipparcos-Gaia astrometry to put constraints on the presence of long-period companions, and we analysed TESS photometric data.
Results. We find strong evidence that Gl 514 hosts a super-Earth on a likely eccentric orbit, residing in the conservative habitable zone for nearly 34% of its orbital period. The planet Gl 514b has minimum mass mb sin ib = 5.2 ± 0.9 M, orbital period Pb = 140.43 ± 0.41 days, and eccentricity eb = 0.45–0.14+0.15. No evidence for transits is found in the TESS light curve. There is no evidence for a longer period companion in the radial velocities and, based on astrometry, we can rule out a ∼0.2 MJup planet at a distance of ∼3-10 astronomical units, and massive giant planets and brown dwarfs out to several tens of astronomical units. We discuss the possible presence of a second low-mass companion at a shorter distance from the host than Gl 514 b.
Conclusions. Gl 514 b represents an interesting science case for studying the habitability of planets on eccentric orbits. We advocate for additional spectroscopic follow-up to get more accurate and precise planetary parameters. Further follow-up is also needed to investigate the presence of additional planetary signals of less than 1 m s–1.

Abstract Copyright: © M. Damasso et al. 2022

Journal keyword(s): techniques: radial velocities - techniques: photometric - planetary systems - stars: activity - stars: individual: Gl 514

VizieR on-line data: <Available at CDS (J/A+A/666/A187): tablea1.dat tablea2.dat tablea3.dat tablea4.dat tablea5.dat>

Simbad objects: 25

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Number of rows : 25
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 HD 1326 Er* 00 18 22.8849799680 +44 01 22.637951588   10.120   7.3   M2V 544 0
2 NAME G 268-38b Pl 00 44 59.3309137511 -15 16 17.542839990           ~ 180 0
3 NAME L 229-91c Pl 04 09 15.6683376139 -53 22 25.290024815           ~ 24 1
4 HD 42581c Pl 06 10 34.6149358167 -21 51 52.656352926           ~ 13 0
5 NAME L 678-39d Pl 09 36 01.6372169407 -21 39 38.877606712           ~ 22 0
6 K2-3 PM* 11 29 20.3917077216 -01 27 17.281697868   13.52 12.17 11.88   M1V 75 0
7 K2-3d Pl 11 29 20.3917077216 -01 27 17.281697868           ~ 51 0
8 K2-18b Pl 11 30 14.5177445592 +07 35 18.255348492           ~ 165 0
9 BD+11 2576 PM* 13 29 59.7858994351 +10 22 37.784532575 11.728 10.524 9.029 8.07 7.013 M1.0V 260 0
10 GJ 514 b Pl? 13 29 59.7858994351 +10 22 37.784532575           ~ 9 0
11 NAME Proxima d Pl? 14 29 42.9461331854 -62 40 46.164680672           ~ 9 0
12 NAME Proxima Centauri b Pl 14 29 42.9461331854 -62 40 46.164680672           ~ 370 0
13 BD+11 3149 PM* 17 16 00.6368683489 +11 03 27.615757436 13.521 12.338 10.828 9.858 8.767 M1V 73 0
14 CD-44 11909b Pl 17 37 03.6654566674 -44 19 09.166492972           ~ 16 0
15 BD+18 3421 PM* 17 37 53.3468417549 +18 35 30.164096453 12.315 11.109 9.577 8.599 7.525 M1.5V 213 0
16 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 14463 0
17 Kepler-705b Pl 19 18 02.0398062000 +41 48 43.568864100           ~ 40 0
18 KOI-4427.01 Pl? 19 40 28.1364460440 +39 16 26.756274612           ~ 20 0
19 KOI-2418.01 Pl 19 49 56.8076265768 +46 59 48.103495728           ~ 49 0
20 Kepler-186f Pl 19 54 36.6535147488 +43 57 18.025920324           ~ 84 0
21 HD 204961c Pl 21 33 33.9751191976 -49 00 32.399427028           ~ 29 0
22 TRAPPIST-1g Pl 23 06 29.3684948589 -05 02 29.037301866           ~ 196 0
23 TRAPPIST-1e Pl 23 06 29.3684948589 -05 02 29.037301866           ~ 289 0
24 TRAPPIST-1f Pl 23 06 29.3684948589 -05 02 29.037301866           ~ 233 0
25 TRAPPIST-1d Pl 23 06 29.3684948589 -05 02 29.037301866           ~ 215 0

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