J/A+A/646/A159 Radial velocity measurements of 51 Peg (Scandariato+, 2021)
The GAPS Programme at TNG. XXIX. No detection of reflected light from 51 Peg b
using optical high-resolution spectroscopy.
Scandariato G., Borsa F., Sicilia D., Malavolta L., Biazzo K., Bonomo A.S.,
Bruno G., Claudi R., Covino E., Di Marcantonio P., Esposito M.,
Frustagli G., Lanza A.F., Maldonado J., Maggio A., Mancini L., Micela G.,
Nardiello D., Rainer M., Singh V., Sozzetti A., Affer L., Benatti S.,
Bignamini A., Biliotti V., Capuzzo-Dolcetta R., Carleo I., Cosentino R.,
Damasso M., Desidera S., Garcia de Gurtubai A., Ghedina A., Giacobbe P.,
Giani E., Harutyunyan A., Hernandez N., Hernandez Diaz M., Knapic C.,
Leto G., Fiorenzano A.F.Martinez, E.Molinari, Nascimbeni V., Pagano I.,
Pedani M., Piotto G., Poretti E., Stoev H.
<Astron. Astrophys. 646, A159 (2021)>
=2021A&A...646A.159S 2021A&A...646A.159S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type ; Exoplanets ; Radial velocities ; Spectroscopy
Keywords: techniques: spectroscopic - planets and satellites: atmospheres -
planets and satellites: detection -
planets and satellites: gaseous planets -
planets and satellites: individual: 51 Peg b
Abstract:
The analysis of exoplanetary atmospheres by means of high-resolution
spectroscopy is an expanding research field which provides information
o n chemical composition, thermal structure, atmospheric dynamics and
orbital velocity of exoplanets. In this work, we aim at the detection
of the light reflected by the exoplanet 51 Peg b employing optical
high-resolution spectroscopy. To detect the light reflected by the
planetary dayside we use optical HARPS and HARPS-N spectra taken near
the superior conjunction of the planet, when the flux contrast between
the planet and the star is maximum. To search for the weak planetary
signal, we cross-correlate the observed spectra with a high S/N
stellar spectrum. We homogeneously analyze the available datasets and
derive a 10-5 upper limit on the planet-to-star flux contrast in the
optical. The upper limit on the planet-to-star flux contrast of 10-5
translates into a low albedo of the planetary atmosphere
(Ag∼0.05-0.15 for an assumed planetary radius in the range
1.5-0.9RJup, as estimated from the planet's mass).
Description:
We collected high-cadence spectroscopy of the star 51 Peg (G2.5V,
V=5.46mag, K=3.91mag) in two nights of observations, respectively
before and after the superior conjunction of the planet 51 Peg b. We
used the high-resolution spectrograph HARPS-N mounted at the TNG
observatory, Roque de Los Muchachos, Spain.
The observations aim at the extraction of the reflected light from the
planet. To this purpose we needed the best and most up-to-date
ephemeris of the planet. We thus measured the radial velocity of the
star using the same collected spectra, and complemented them with the
compilation of radial velocities by Birkby et al. (2017, Cat.
J/AJ/153/138) and with recent spectroscopic observations publicly
available in the literature. These data span observing dates from 1994
September 15 to 2018 September 2, resulting in 1259 radial velocity
measurements over 24 years.
Objects:
-----------------------------------------------------------
RA (2000) DE Designation(s) (Period)
-----------------------------------------------------------
22 57 27.98 +20 46 07.8 51 Peg = HR 8729 (P=4.230784)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 68 1259 Stellar radial velocity measurements of
51 Peg from multiple observatories
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See also:
J/A+A/414/351 : ELODIE survey for northern extrasolar planets (Naef+, 2004)
J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006)
J/ApJS/210/5 : The twenty-five year Lick planet search (Fischer+, 2014)
J/A+A/576/A134 : Radial velocities of 51 Peg (Martins+, 2015)
J/AJ/153/138 : Radial velocity curve of 51 Peg (Birkby+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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3- 16 F14.8 d BJD Barycentric Julian Date (BJD-2400000)
(BJD_TDB) (1)
23- 33 F11.4 m/s RV ? Radial velocity
(for ELODIE and HARPS data) (2)
36- 43 F8.4 m/s RVr ? Relative radial velocity
(for LICK and HIRES data) (2)
52- 57 F6.3 m/s e_RV Uncertainty in RV
62- 68 A7 --- Set Dataset identifier (3)
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Note (1): Barycentric Dynamical Time.
Note (2): The RV measurements labeled as 'HARPS' and 'HARPS-N' are obtained
using the data reduction pipeline of the corresponding instruments. All the
other RV measurements are extracted from (Birkby et al., 2017,
Cat. J/AJ/153/138.
Note (3): The identifiers define the instrumental setup for the observations
as follows:
ELODIE = The ELODIE spectrograph at Observatoire Haute Provence
Lick6 = Hamilton spectrograph at the Lick Observatory, number 6 in the
Lick dataset names denote the dewar associated with each upgrade
to the Hamilton spectrograph
Lick8 = Hamilton spectrograph at the Lick Observatory, number 8 in the
Lick dataset names denote the dewar associated with each upgrade
to the Hamilton spectrograph
Lick13 = Hamilton spectrograph at the Lick Observatory, number 13 in the
Lick dataset names denote the dewar associated with each upgrade
to the Hamilton spectrograph
HIRES = High Resolution Echelle Spectrometer (HIRES) at the Keck Observatory
HARPS = High Accuracy Radial velocity Planet Searcher at the ESO-3.6m
telescope
HARPS-N = High Accuracy Radial velocity Planet Searcher for the Northern
hemisphere at the TNG telescope
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Acknowledgements:
Gaetano Scandariato, gaetano.scandariato(at)inaf.it
References:
Covino et al., Paper I 2013A&A...554A..28C 2013A&A...554A..28C, Cat. J/A+A/554/A28
Desidera et al., Paper II 2013A&A...554A..29D 2013A&A...554A..29D
Esposito et al., Paper III 2014A&A...564L..13E 2014A&A...564L..13E
Desidera et al., Paper IV 2014A&A...567L...6D 2014A&A...567L...6D
Damasso et al., Paper V 2015A&A...575A.111D 2015A&A...575A.111D, Cat. J/A+A/575/A111
Sozzetti et al., Paper VI 2015A&A...575L..15S 2015A&A...575L..15S, Cat. J/A+A/575/L15
Borsa et al., Paper VII 2015A&A...578A..64B 2015A&A...578A..64B, Cat. J/A+A/578/A64
Mancini et al., Paper VIII 2015A&A...579A.136M 2015A&A...579A.136M, Cat. J/A+A/579/A136
Damasso et al., Paper IX 2015A&A...581L...6D 2015A&A...581L...6D
Biazzo et al., Paper X 2015A&A...583A.135B 2015A&A...583A.135B, Cat. J/A+A/583/A135
Malavolta et al., Paper XI 2016A&A...588A.118M 2016A&A...588A.118M, Cat. J/A+A/588/A118
Benatti et al., Paper XII 2017A&A...599A..90B 2017A&A...599A..90B, Cat. J/A+A/599/A90
Esposito et al., Paper XIII 2017A&A...601A..53E 2017A&A...601A..53E
Bonomo et al., Paper XIV 2017A&A...602A.107B 2017A&A...602A.107B, Cat. J/A+A/602/A107
Gonzalez-Alvarez et al., Paper XV 2017A&A...606A..51G 2017A&A...606A..51G
Mancini et al., Paper XVI 2018A&A...613A..41M 2018A&A...613A..41M, Cat. J/A+A/613/A41
Lanza et al., Paper XVII 2018A&A...616A.155L 2018A&A...616A.155L, Cat. J/A+A/616/A155
Barbato et al., Paper XVIII 2019A&A...621A.110B 2019A&A...621A.110B, Cat. J/A+A/621/A110
Borsa et al., Paper XIX 2019A&A...631A..34B 2019A&A...631A..34B, Cat. J/A+A/631/A34
Pino et al., Paper XX 2020ApJ...894L..27P 2020ApJ...894L..27P
Carleo et al., Paper XXI 2020A&A...638A...5C 2020A&A...638A...5C, Cat. J/A+A/638/A5
Guilluy et al., Paper XXII 2020A&A...639A..49G 2020A&A...639A..49G
Benatti et al., Paper XXIII 2020A&A...639A..50B 2020A&A...639A..50B, Cat. J/A+A/639/A50
Barbato et al., Paper XXIV 2020A&A...641A..68B 2020A&A...641A..68B
Baratella et al., Paper XXV 2020A&A...640A.123B 2020A&A...640A.123B
Di Maio et al., Paper XXVI 2020A&A...642A..53D 2020A&A...642A..53D
Damasso et al., Paper XXVII 2020A&A...642A.133D 2020A&A...642A.133D, Cat. J/A+A/642/A133
Carleo et al., Paper XXVIII 2021A&A...645A..71C 2021A&A...645A..71C
(End) Patricia Vannier [CDS] 25-Dec-2020