J/A+A/684/A83 Wolf 327b RV and spectral line activity indices (Murgas+, 2024)
Wolf 327b:
A new member of the pack of ultra-short-period super-Earths around M dwarfs.
Murgas F., Palle E., Orell-Miquel J., Carleo I., Pena-Monino L.,
Perez-Torres M., Watkins C.N., Jeffers S.V., Azzaro M., Barkaoui K.,
Belinski A.A., Caballero J.A., Charbonneau D., Cheryasov D.V., Ciardi D.R.,
Collins K.A., Cortes-Contreras M., de Leon J., Duque-Arribas C., Enoc G.,
Esparza-Borges E., Fukui A., Geraldia-Gonzalez S., Gilbert E.A.,
Hatzes A.P., Hayashi Y., Henning T., Herrero E., Jenkins J.M., Lillo-Box J.,
Lodieu N., Lund M.B., Luque R., Montes D., Nagel E., Narita N.,
Parviainen H., Polanski A.S., Reffert S., Schlecker M., Schoefer P.,
Schwarz R.P., Schweitzer A., Seager S., Stassun K.G., Tabernero H.M.,
Terada Y., Twicken J.D., Vanaverbeke S., Winn J.N., Zambelli R., Amado P.J.,
Quirrenbach A., Reiners A., Ribas I.
<Astron. Astrophys. 684, A83 (2024)>
=2024A&A...684A..83M 2024A&A...684A..83M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets; Spectroscopy ;
Radial velocities
Keywords: techniques: photometric - techniques: radial velocities -
planets and satellites: detection -
planets and satellites: terrestrial planets -
stars: individual: Wolf 327 - stars: late-type
Abstract:
Planets with orbital periods shorter than 1 day are rare and have
formation histories that are not completely understood. Small (R_p < 2
R_earth) ultra-short-period (USP) planets are highly irradiated,
probably have rocky compositions with high bulk densities, and are
often found in multi-planet systems. Additionally, USP planets found
around small stars are excellent candidates for characterization using
present-day instrumentation. Of the current full sample of
approximately 5500 confirmed exoplanets, only 130 are USP planets and
around 40 have mass and radius measurements. Wolf 327 (TOI-5747) is an
M dwarf (Rstar=0.406±0.015R☉, Mstar=0.405±0.019M☉,
Teff=3542±70K, and V=13mag) located at a distance d=28.5pc. NASA's
planet hunter satellite, TESS, detected transits in this star with a
period of 0.573d (13.7h) and with a transit depth of 818ppm.
Ground-based follow-up photometry, high resolution imaging, and radial
velocity (RV) measurements taken with the CARMENES spectrograph
confirm the presence of this new USP planet. Wolf 327b is a
super-Earth with a radius of Rp=1.24±0.06R⊕ and a mass of
Mp=2.53±0.46M⊕, yielding a bulk density of
7.24±1.66g/cm3 and thus suggesting a rocky composition. Owing to
its close proximity to its host star (a=0.01au), Wolf 327b has an
equilibrium temperature of 996±22K. This planet has a mass and
radius similar to K2-229b, a planet with an inferred Mercury-like
internal composition. Planet interior models suggest that Wolf 327b
has a large iron core, a small rocky mantle, and a negligible (if any)
H/He atmosphere.
Description:
Radial velocity and activity indices of Wolf 327 taken with CARMENES.
Spectroscopic data reduced with SERVAL.
Objects:
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RA (2000) DE Designation(s)
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09 53 30.90 +35 34 16.7 Wolf 327 = TIC 4918918
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 55 22 CARMENES (VIS channel) radial velocity
measurements computed with SERVAL, instrumental
drift, and nightly zero point correction
tablea2.dat 108 22 SERVAL spectral line activity indices
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 F14.6 d BJD Barycentric Julian date (TDB)
16- 21 F6.3 m/s RV Radial velocity (VIS channel)
24- 28 F5.3 m/s e_RV Radial velocity error (VIS channel)
30- 36 F7.3 m/s Drift Instrumental drift (VIS channel)
38- 42 F5.3 m/s e_Drift Instrumental drift error (VIS channel)
44- 49 F6.3 m/s zpt Instrumental zero point correction (VIS channel)
51- 55 F5.3 m/s e_zpt Instrumental zero point correction error
(VIS channel)
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 14 F14.6 d BJD Barycentric julian date (TBD)
16- 20 F5.1 m/s CRX Chromatic index (in m/s/Np)
22- 25 F4.1 m/s e_CRX Chromatic index uncertainty (in m/s/Np)
27- 31 F5.1 m2/s2 dLW Differential line width
33- 36 F4.1 m2/s2 e_dLW Differential line width uncertainty
38- 42 F5.3 --- Halpha Hα index
44- 48 F5.3 --- e_Halpha Hα index uncertainty
50- 54 F5.3 --- NaD1 Na D1 index
56- 60 F5.3 --- e_NaD1 Na D1 index uncertainty
62- 66 F5.3 --- NaD2 Na D2 index
68- 72 F5.3 --- e_NaD2 Na D2 index uncertainty
74- 78 F5.3 --- CaIRT1 Ca IRT 1 index
80- 84 F5.3 --- e_CaIRT1 Ca IRT 1 index uncertainty
86- 90 F5.3 --- CaIRT2 Ca IRT 2 index
92- 96 F5.3 --- e_CaIRT2 Ca IRT 2 index uncertainty
98-102 F5.3 --- CaIRT3 Ca IRT 3 index
104-108 F5.3 --- e_CaIRT3 Ca IRT 3 index uncertainty
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Acknowledgements:
Felipe Murgas, fmurgas(at)iac.es, CARMENES Consortium
(End) Felipe Murgas [IAC, Spain], Patricia Vannier [CDS] 31-Jan-2024