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:
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RA (2000) DE Designation(s)
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11 50 57.72 +48 22 38.5 GJ 1151 = 2MASS J11505787+4822395
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File Summary:
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FileName Lrecl Records Explanations
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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
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See also:
J/A+A/649/L12 : GJ 1151 radial velocity curve (Perger+, 2021)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): Note as follows:
1 = problems with the calculation of the CCF by raccoon
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Byte-by-byte Description of file: tablec2.dat
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Bytes Format Units Label Explanations
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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)
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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
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Acknowledgements:
Jordi Blanco-Pozo, blanco(at)ice.csic.es
(End) Patricia Vannier [CDS] 09-Jan-2023