J/A+A/700/A11 Proxima spectroscopy and photometry (Suarez Mascareno+, 2025)
Diving into the planetary system of Proxima with NIRPS.
Breaking the metre per second barrier in the infrared.
Suarez Mascareno A., Artigau E., Mignon L., Delfosse X., Cook N.J.,
Bouchy F., Doyon R., Gonzalez Hernandez J.I., Vandal T., de Castro Leao I.,
Stefanov A.K., Faria J., Cadieux C., Lamontagne P., Baron F., Barros S.C.C.,
Benneke B., Bonfils X., Bryan M., Canto Martins B.L., Cloutier R.,
Cowan N.B., Brito de Freitas D., Renan De Medeiros J., Delgado-Mena E.,
Figueira P., Dumusque X., Ehrenreich D., Lafreniere D., Lovis C., Malo L.,
Melo C., Mordasini C., Pepe F., Rebolo R., Rowe J., Santos N.C.,
Segransan D., Udry S., Valencia D., Wade G., Abreu M., Aguiar J.L.A.,
Al Moulla K., Allain G., Allart R., Arial T., Auger H., Bazinet L., Blind N.,
Bohlender D., Boisse I., Boucher A., Bourrier V., Bovay S., Broeg C.,
Brousseau D., Cabral A., Carmona A., Carteret Y., Challita Z., Chazelas B.,
Coelho J., Cointepas M., Conod U., Cristo E., Costa Silva A.R.,
Darveau-Bernier A., Dauplaise L., Delisle J.-B., de Lima Gomes R.,
Forveille T., Frensch Y.G.C., Gracia Temich F., Fontinele D.O., Gagne J.,
Genest F., Genolet L., Gomes da Silva J., Grieves N., Hernandez O.,
Hobson M.J., Hoeijmakers H.J., Hubin N., Jahandar F., Jayawardhana R.,
Kaeufl H.-U., Kerley D., Kolb J., Krishnamurthy V., Kung B., L'Heureux A.,
Larue P., Leath H., Lim O., Lo Curto G., Martins A.M., Matthews J.,
Mayer J.-S., Messias Y.S., Metchev S., Moranta L., Mounzer D., Nari N.,
Nielsen L.D., Osborn A., Ouellet M., Otegi J., Parc L., Pasquini L.,
Passegger V.M., Pelletier S., Peroux C., Piaulet-Ghorayeb C., Plotnykov M.,
Pompei E., Poulin-Girard A.-S., Rasilla J.L., Reshetov V., Saint-Antoine J.,
Sarajlic M., Saviane I., Schnell R., Segovia A., Seidel J., Silber A.,
Sinclair P., Sordet M., Sosnowska D., Srivastava A., Teixeira M.A.,
Thibault S., Vallee P., Vaulato V., Wardenier J.P., Wehbe B., Weisserman D.,
Wevers I., Wildi F., Yariv V., Zins G.
<Astron. Astrophys. 700, A11 (2025)>
=2025A&A...700A..11S 2025A&A...700A..11S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, dwarfs ; Exoplanets ;
Radial velocities ; Infrared ; Ultraviolet ; Optical
Keywords: instrumentation: spectrographs - techniques: radial velocities -
planets and satellites: detection - stars: individual: Proxima -
stars: rotation
Abstract:
We obtained 420 high-resolution spectra of Proxima, over 159 nights,
using the Near Infra Red Planet Searcher (NIRPS). We derived 149
nightly binned radial velocity measurements with a standard deviation
of 1.69m/s and a median uncertainty of 55cm/s, and performed a joint
analysis combining radial velocities, spectroscopic activity
indicators, and ground-based photometry, to model the planetary and
stellar signals present in the data, applying multi-dimensional
Gaussian process regression to model the activity signals. We detect
the radial velocity signal of Proxima b in the NIRPS data. All
planetary characteristics are consistent with those previously derived
using visible light spectrographs. In addition, we find evidence of
the presence of the sub-Earth Proxima d in the NIRPS data. When
combining the data with the HARPS observations taken simultaneous to
NIRPS, we obtain a tentative detection of Proxima d and parameters
consistent with those measured with ESPRESSO. By combining the NIRPS
data with simultaneously obtained HARPS observations and archival
data, we confirm the existence of Proxima d, and demonstrate that its
parameters are stable over time and against change of instrument. We
refine the planetary parameters of Proxima b and d, and find
inconclusive evidence of the signal attributed to Proxima c (P=1900d)
being present in the data. We measure Proxima b and d to have minimum
masses of 1.055±0.055M⊕, and 0.260±0.038M⊕,
respectively. Our results show that, in the case of Proxima, NIRPS
provides more precise radial velocity data than HARPS, and a more
significant detection of the planetary signals. The standard deviation
of the residuals of NIRPS after the fit is ∼80cm/s, showcasing the
potential of NIRPS to measure precise radial velocities in the
near-infrared.
Description:
Spectroscopic and photometric time series of Proxima obtained with
NIRPS, ESPRESSO, HARPS, UVES, ASAS-3, ASAS-4, ASAS-SN, and LCO.
Objects:
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RA (2000) DE Designation(s)
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14 29 42.95 -62 40 46.2 Proxima = Gl 551
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
spec.dat 120 722 Spectroscopic data
photo.dat 43 2212 Photometric data
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See also:
J/A+A/534/A133 : Proxima Cen chromospheric emission lines (Fuhrmeister+, 2011)
J/A+A/603/A58 : Full spectrum of Proxima Centauri (Ribas+, 2017)
J/AJ/153/93 : MOST photometry of Proxima (Kipping+, 2017)
J/AJ/155/12 : Photometry of Proxima Centauri observed by BSST (Liu+, 2018)
J/A+A/626/A111 : Proxima Cen flare activity temporal changes (Pavlenko+, 2019)
J/A+A/638/A120 : SPHERE maps around Proxima Cen (Gratton+, 2020)
J/A+A/639/A77 : Proxima Cen RV, FWHM and fluxes (Suarez Mascareno+, 2020)
J/A+A/658/A115 : Proxima Cen ESPRESSO RV and FWHM (Faria+, 2022)
J/A+A/666/A196 : Proxima telluric-corrected ESPRESSO RV (Allart+, 2022)
Byte-by-byte Description of file: spec.dat
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Bytes Format Units Label Explanations
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2- 10 F9.3 d BJD Barycentric Julian date (BJD-2450000)
17- 21 F5.2 m/s dRV Relative radial velocity
29- 32 F4.2 m/s e_dRV Relative radial velocity uncertainty
36- 43 F8.2 m/s dFWHM ?=-9999 Relative FWHM variation
47- 54 F8.2 m/s e_dFWHM ?=9999 Relative FWHM variation uncertainty
58- 65 F8.2 --- CRX ?=-9999 Chromatic RV slope
69- 76 F8.2 --- e_CRX ?=9999 Chromatic RV slope uncertainty
79- 87 F9.3 k dTeff ?=-9999 Relative effective temperature variation
90- 98 F9.3 k e_dTeff ?=9999 Relative effective temperature variation
uncertainty
101-109 F9.3 km/s BERV ?=-9999 Baricentric Earth Radial Velocity
120 A1 --- Inst Instrument (1)
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Note (1): Instruments as follows:
0 = UVES
1 = HARPS pre-upgrade
2 = HARPS post-upgrade
3 = ESPRESSO pre-upgrade
4 = ESPRESSO post-upgrade
5 = NIRPS
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Byte-by-byte Description of file: photo.dat
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Bytes Format Units Label Explanations
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2- 10 F9.3 d BJD Barycentric Julian date (BJD-2450000)
16- 21 F6.1 10-3 dFlux Relative flux variations (in ppt)
29- 32 F4.1 10-3 e_dFlux Relative flux variations uncertainty (in ppt)
43 A1 --- Inst Instrument (1)
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Note (1): Instruments as follows:
0 = ASAS-3
1 = ASAS-4
2 = LCO Red Dots
3 = LCO ESPRESSO GTO
4 = ASAS-SN V
5 = ASAS-SN g
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Acknowledgements:
Alejandro Suarez Mascareno, asm(at)iac.es
(End) Patricia Vannier [CDS] 28-Apr-2025