J/A+A/676/A90 Exoplanet-host stars vsini (Rainer+, 2023)
The GAPS programme at TNG. XLIV. Projected rotational velocities of
273 exoplanet-host stars observed with HARPS-N.
Rainer M., Desidera S., Borsa F., Barbato D., Biazzo K., Bonomo A.,
Gratton R., Messina S., Scandariato G., Affer L., Benatti S.,
Carleo I., Cabona L., Covino E., Lanza A.F., Ligi R., Maldonado J.,
Mancini L., Nardiello D., Sicilia D., Sozzetti A., Bignamini A.,
Cosentino R., Knapic C., Martinez Fiorenzano A.F., Molinari E.,
Pedani M., Poretti E.
<Astron. Astrophys. 676, A90 (2023)>
=2023A&A...676A..90R 2023A&A...676A..90R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Spectroscopy ;
Rotational velocities
Keywords: planetary systems - techniques: spectroscopic - stars: rotation
Abstract:
The leading spectrographs used for exoplanets' search and
characterization offer online data reduction softwares (DRS) that yield,
as an ancillary result, the full-width at half-maximum (FWHM) of the
cross-correlation function (CCF) that is used to estimate the radial
velocity of the host star. The FWHM also contains information on the
stellar projected rotational velocity veqsini*, if appropriately
calibrated.
We wanted to establish a simple relationship to derive the
veqsini* directly from the FWHM computed by the HARPS-N DRS in the
case of slow-rotating solar-like stars. This may also help to recover
the stellar inclination i*, which in turn affects the exoplanets'
parameters.
We selected stars with an inclination of the spin axis compatible with
90 deg by looking at exoplanetary transiting systems with known small
sky-projected obliquity: for these calibrators, we can presume that
veqsini* is equal to stellar equatorial velocity veq. We derived
their rotational periods from photometric and spectroscopic time
series and their radii from the spectral energy distribution (SED)
fitting. This allowed us to recover their veq, which could be compared
to the FWHM values of the CCFs obtained both with G2 and K5
spectral-type masks.
We obtained an empirical relation for each mask: this can be used to
derive veqsini* directly fromFWHMvalues for slow rotators
(FWHM<20km/s). We applied our relations to 273 exoplanet-host stars
observed with HARPS-N, obtaining homogeneous veqsini*
measurements. When possible, we compared our results with the
literature ones to confirm the reliability of our work. We were also
able to recover or constrain i* for 12 objects with no prior
veqsini* estimation.
We provide two simple empirical relations to directly convert the
HARPS-N FWHM obtained with the G2 and K5 mask to a veqsini* value.
We tested our results on a statistically significant sample, and we
found a good agreement with literature values found with more
sophisticated methods for stars with logg>3.5. We also tried our
relation on HARPS and SOPHIE data, and we conclude that it can be used
as it is also on FWHM derived by HARPS DRS with the G2 and K5 mask,
and it may be adapted to the SOPHIE data as long as the spectra are
taken in high-resolution mode.
Description:
Projected rotational velocities (vsini) of 273 exoplanet-host stars
observed with the high-resolution echelle spectrograph HARPS-N at the
Telescopio Nazionale Galileo (TNG). The vsini were computed using an
empirical relation that directly converts the FWHM obtained with the
HARPS-N DRS using the G2 and K5 mask to a vsini value.
Tabulated data include the name of the objects, the spectral type, the
mask used by the HARPS-N DRS during the reduction (either G2 or K5),
the FWHM value as computed by the HARPS-N DRS, the computed vsini, the
error on the vsini, the vsini value found in literature (if any), the
error on the literature vsini, the reference for the literature vsini.
The last 3 columns are given for comparison sake.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 110 273 Exoplanet-host stars vsini
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Object name
25- 31 A7 --- SpType Spectral Type
36- 37 A2 --- Mask Mask used by HARPS-N DRS
40- 44 F5.2 km/s FWHM FWHM computed by HARPS-N DRS
47- 51 F5.2 km/s vsini Computed vsini
54- 57 F4.2 km/s e_vsini Error on the computed vsini
60 A1 --- l_vsinil Limit flag on vsinil
61- 65 F5.2 km/s vsinil ?=- Literature vsini (if any)
68- 72 F5.3 km/s e_vsinil ?=- Error on the literature vsini (if any)
78- 90 A13 --- Aut Reference for the literature vsini
(first author name)
92-110 A19 --- BibCode Reference for the literature vsini
(BibCode)
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Acknowledgements:
Monica Rainer, monica.rainer(at)inaf.it
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(End) Patricia Vannier [CDS] 10-Jul-2023