J/A+A/671/A50       GJ 1151 CARMENES and HARPS-N data       (Blanco-Pozo+, 2023)

The CARMENES search for exoplanets around M dwarfs. A long-period planet around GJ 1151 measured with CARMENES and HARPS-N data. Blanco-Pozo J., Perger M., Damasso M., Anglada Escude G., Ribas I., Baroch D., Caballero J.A., Cifuentes C., Jeffers S.V., Lafarga M., Kaminski A., Kaur S., Nagel E., Perdelwitz V., Perez-Torres M., Sozzetti A., Vigano D., Amado P.J., Andreuzzi G., Bejar V.J.S., Brown E.L., Del Sordo F., Dreizler S., Galadi-Enriquez D., Hatzes A.P., Kuerster M., Lanza A.F., Melis A., Molinari E., Montes D., Murgia M., Palle E., Pena-Monino L., Perrodin D., Pilia M., Poretti E., Quirrenbach A., Reiners A., Schweitzer A., Zapatero Osorio M.R., Zechmeister M. <Astron. Astrophys. 671, A50 (2023)> =2023A&A...671A..50B 2023A&A...671A..50B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, M-type ; Radial velocities ; Optical Keywords: stars: late-type stars - stars: individual: GJ 1151 - techniques: radial velocities - planets and satellites: detection - stars: activity Abstract: Detecting a planetary companion in a short-period orbit through radio emission from the interaction with its host star is a new prospect in exoplanet science. A tantalising signal was found by Vedantham et al. (2020NatAs...4..577V 2020NatAs...4..577V) close to the low-mass stellar system GJ 1151 using LOFAR observations. We studied spectroscopic time-series data of GJ 1151 to search for planetary companions and to investigate possible signatures of stellar magnetic activity and to find possible explanations for the radio signal. We used the combined radial velocities measured from spectra acquired with the CARMENES, HARPS-N, and HPF instruments, extracted activity indices from those spectra in order to mitigate the impact of stellar magnetic activity on the data, and analysed in detail Gaia astrometry, and all available photometric time series coming from the MEarth and ASAS-SN surveys. We found a M>10.6MEarth companion to GJ 1151 in a 390-d orbit at a separation of 0.57au. Evidence for a second modulation is also present and could be due to long-term magnetic variability, or a second (substellar) companion. The star shows episodes of elevated magnetic activity, one of which could be linked to the observed LOFAR radio emission. We show that it is highly unlikely that the detected GJ 1151 b, or any additional outer companion can be the source of the detected signal. We cannot firmly rule out the explanation given by Vedantham et al. (2020NatAs...4..577V 2020NatAs...4..577V), as we establish an upper limit of 1.2MEarth for the minimum mass of an undetected short-period planet that could be related to the radio emission. Description: HARPS-N and CARMENES spectroscopic observations of GJ 1151. Objects: -------------------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------------------- 11 50 57.72 +48 22 38.5 GJ 1151 = 2MASS J11505787+4822395 -------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablec1.dat 104 46 HARPS-N spectroscopic observations calculated with terra and racoon tablec2.dat 135 101 CARMENES spectroscopic observations calculated with serval and racoon -------------------------------------------------------------------------------- See also: J/A+A/649/L12 : GJ 1151 radial velocity curve (Perger+, 2021) Byte-by-byte Description of file: tablec1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 F11.3 d BJD Barycentric Julian date 13- 18 F6.3 m/s RV Radial velocity 20- 24 F5.3 m/s e_RV Radial velocity uncertainty 26- 30 F5.2 m2/s2 dLw Differential line width 32- 35 F4.2 m2/s2 e_dLw Differential line width uncertainty 37- 43 F7.2 --- CRX Chromatic index (in m/s/Np unit) 45- 50 F6.2 --- e_CRX Chromatic index uncertainty (in m/s/Np unit) 52- 58 F7.2 m/s FWHM Full width height maximum 60- 65 F6.2 m/s e_FWHM Full width height maximum uncertainty 67- 71 F5.2 m/s BIS ? Bisector Inverse Span 73- 77 F5.2 m/s e_BIS ? Bisector Inverse Span uncertainty 79- 84 F6.3 % CON Contrast velocities 86- 90 F5.3 % e_CON Contrast uncertainty 92- 96 F5.3 m/s Halpha H-alpha line 98-102 F5.3 m/s e_Halpha H-alpha line uncertainty 104 I1 --- Notes [1]? Note (1) -------------------------------------------------------------------------------- Note (1): Note as follows: 1 = problems with the calculation of the CCF by raccoon -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablec2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 F11.3 d BJD Barycentric Julian date (BJD) 13- 19 F7.3 m/s RV ? Radial velocity 21- 26 F6.3 m/s e_RV ? Radial velocity uncertainty 28- 33 F6.2 m2/s2 dLw Differential line width 35- 39 F5.2 m2/s2 e_dLw Differential line width uncertainty 41- 46 F6.2 --- CRX Chromatic index (in m/s/Np unit) 48- 52 F5.2 --- e_CRX Chromatic index uncertainty (in m/s/Np unit) 54- 60 F7.2 m/s FWHM Full width height maximum 62- 66 F5.2 m/s e_FWHM Full width height maximum uncertainty 68- 73 F6.2 m/s BIS Bisector Inverse Span 75- 79 F5.2 m/s e_BIS Bisector Inverse Span uncertainty 81- 86 F6.3 % CON Contrast velocities 88- 92 F5.3 % e_CON Contrast uncertainty 94- 99 F6.4 --- Halpha Hydrogen-alpha line 101-106 F6.4 --- e_Halpha Hydrogen-alpha line uncertainty 108-113 F6.4 --- CaIRT Calcium infrared triplet line 115-120 F6.4 --- e_CaIRT Calcium infrared triplet line uncertainty 122-127 F6.3 --- NaD Sodium doublet line 129-133 F5.3 --- e_NaD Sodium doublet line uncertainty 135 I1 --- Notes [1/3]? Notes (1) -------------------------------------------------------------------------------- Note (1): Notes as follows 1 = large RV uncertainty >5σ; RV not used in final fit 2 = outlier; RV not used in final fit 3 = outliers, large S/N, no RV calculation -------------------------------------------------------------------------------- Acknowledgements: Jordi Blanco-Pozo, blanco(at)ice.csic.es
(End) Patricia Vannier [CDS] 09-Jan-2023
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