J/A+A/625/A17 SOPHIE data of Gliese 411 (Diaz+, 2019)
The SOPHIE search for northern extrasolar planets.
XIV. A temperate (Teq ∼ 300 K) super-earth around the nearby star Gliese 411.
Diaz R.F., Delfosse X., Hobson M.J., Boisse I., Astudillo-Defru N.,
Bonfils X., Henry G.W., Arnold L., Bouchy F., Bourrier V., Brugger B.,
Dalal S., Deleuil M., Demangeon O., Dolon F., Dumusque X., Forveille T.,
Hara N., Hebrard G., Kiefer F., Lopez T., Mignon L., Moreau F., Mousis O.,
Moutou C., Pepe F., Perruchot S., Richaud Y., Santerne A., Santos N.C.,
Sottile R., Stalport M., Segransan D., Udry S., Unger N., Wilson P.A.
<Astron. Astrophys. 625, A17 (2019)>
=2019A&A...625A..17D 2019A&A...625A..17D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, M-type ; Exoplanets ;
Radial velocities ; Spectroscopy
Keywords: planetary systems - techniques: radial velocities -
stars: low-mass - stars: individual: Gl 411
Abstract:
Periodic radial velocity variations in the nearby M-dwarf star Gl 411
are reported, based on measurements with the SOPHIE spectrograph.
Current data do not allow us to distinguish between a 12.95-day period
and its one-day alias at 1.08-days, but favour the former slightly.
The velocity variation has an amplitude of 1.6m/s, making this the
lowest-amplitude signal detected with SOPHIE up to now. We have
performed a detailed analysis of the significance of the signal and
its origin, including extensive simulations with both uncorrelated and
correlated noise, representing the signal induced by stellar activity.
The signal is significantly detected, and the results from all tests
point to its planetary origin. Additionally, the presence of an
additional acceleration in the velocity time series is suggested by
the current data. On the other hand, a previously reported signal with
a period of 9.9 days, detected in HIRES velocities of this star, is
not recovered in the SOPHIE data. An independent analysis of the HIRES
dataset also fails to unveil the 9.9-day signal. If the 12.95-day
period is the real one, the amplitude of the signal detected with
SOPHIE implies the presence of a planet, called Gl 411 b, with a
minimum mass of around three Earth masses, orbiting its star at a
distance of 0.079AU. The planet receives about 3.5 times the
insolation received by Earth, which implies an equilibrium temperature
between 256 and 350K, and makes it too hot to be in the habitable
zone. At a distance of only 2.5pc, Gl 411 b, is the third closest
low-mass planet detected to date. Its proximity to Earth will permit
probing its atmosphere with a combination of high-contrast imaging and
high-dispersion spectroscopy in the next decade.
Description:
Observations of Gliese 411 obtained with the SOPHIE spectrograph,
mounted on the 1.93-m telescope at the Observatoire de Haute-Provence,
obtained over XXX days. The 155 visits used for the analysis in the
article are listed. For each visit, the BJD (col. 1), measured radial
velocity (col. 2) and associated error (photon noise + calibration
noise) (col. 3), full width at half maximum (FWHM; col. 4) of the
cross-correlation function (CCF) and bisector velocity span (col. 5)
are given, together with the spectroscopic indexes used as activity
proxies, based on the Hα line flux (col. 6) and the Ca II H&K
lines (col. 7). Finally, column 7 presents the zero-point offset of
the instrument, measured on a series of constant stars, interpolated
to the time of the observation.
Objects:
------------------------------------------------------
RA (2000) DE Designation(s)
------------------------------------------------------
11 03 20.19 +35 58 11.6 Gliese 411 = HD 95735
------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 62 155 SOPHIE observations of Gliese 411
--------------------------------------------------------------------------------
See also:
J/A+A/505/853 : HD16760 radial velocity curve (Bouchy+, 2009)
J/A+A/513/A69 : HD9446 radial velocity curve (Hebrard+, 2010)
J/A+A/523/A88 : A Jupiter-mass companion around HD 109246 (Boisse+, 2010)
J/A+A/538/A113 : RV of eight stars (Diaz+ 2012)
J/A+A/545/A55 : RV of 5 stars (Boisse+, 2012)
J/A+A/563/A22 : RV of 3 new hot Jupiters (Moutou+, 2014)
J/A+A/585/A46 : RV of 5 stars (Bouchy+, 2016)
J/A+A/588/A144 : RV of 15 targets (Wilson+, 2016)
J/A+A/588/A145 : RV of 8 stars with giant planets (Hebrard+, 2016)
J/A+A/601/A9 : HD17674, HD29021, and HD42012 radial velocities (Rey+, 2017)
J/A+A/618/A103 : Gl617A and Gl96 radial velocity curves (Hobson+, 2018)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 F14.6 --- BJD Barycentric Julian Date of observation
16- 23 F8.4 km/s RV Radial velocity
25- 30 F6.4 km/s e_RV Uncertainty in radial velocity
32- 36 F5.3 km/s FWHM FWHM of cross-correlation function
38- 42 F5.2 m/s BIS Bisector velocity span of CCF
44- 48 F5.3 --- IHa Activity proxy based on Hα line flux
50- 55 F6.3 --- logRHK ?=- Activity proxy based on CaII H & K
line fluxes (1)
57- 62 F6.3 m/s zpoint Instrument zero-point offset
--------------------------------------------------------------------------------
Note (1): Measurements of spectra obtained using the Fabry-Perot etalon
as simultaneous wavelength reference are missing due to incomplete
background correction.
--------------------------------------------------------------------------------
Acknowledgements:
Rodrigo Diaz, rodrigo(at)iafe.uba.ar
References:
Bouchy et al., Paper I 2009A&A...505..853B 2009A&A...505..853B, Cat. J/A+A/505/853
Hebrard et al., Paper II 2010A&A...513A..69H 2010A&A...513A..69H, Cat. J/A+A/513/A69
Boisse et al., Paper III 2010A&A...523A..88B 2010A&A...523A..88B, Cat. J/A+A/535/A88
Diaz et al., Paper IV 2012A&A...538A.113D 2012A&A...538A.113D, Cat. J/A+A/538/A113
Boisse et al., Paper V 2012A&A...545A..55B 2012A&A...545A..55B, Cat. J/A+A/545/A55
Moutou et al., Paper VI 2014A&A...563A..22M 2014A&A...563A..22M, Cat. J/A+A/563/A22
Courcol et al., Paper VII 2015A&A...581A..38C 2015A&A...581A..38C
Bouchy et al., Paper VIII 2016A&A...585A..46B 2016A&A...585A..46B, Cat. J/A+A/585/A46
Wilson et al., Paper IX 2016A&A...588A.144W 2016A&A...588A.144W, Cat. J/A+A/588/A144
Hebrard et al., Paper X 2016A&A...588A.145H 2016A&A...588A.145H, Cat. J/A+A/588/A145
Diaz et al., Paper XI 2016A&A...591A.146D 2016A&A...591A.146D
Rey et al., Paper XII 2017A&A...601A...9R 2017A&A...601A...9R, Cat. J/A+A/601/A9
Hobson et al., Paper XIII 2018A&A...618A.103H 2018A&A...618A.103H, Cat. J/A+A/618/A03
(End) Rodrigo Diaz [IAFE, Argentina], Patricia Vannier [CDS] 23-Apr-2019