SPIRou Input Catalogue: global properties of 440 M dwarfs observed with ESPaDOnS at CFHT

Fouqué, P.; Moutou, C.; Malo, Lison; Martioli, Eder; Lim, Olivia; Rajpurohit, A. S.; Artigau, Étienne; Delfosse, X.; Donati, J.‐F.; Forveille, T.; Morin, J.; Allard, F.; Delage, Raphaël; Doyon, René; Hébrard, E.; Neves, V.

doi:10.1093/mnras/stx3246

Cited by 51 publications

(28 citation statements)

References 131 publications

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“…First, current and future spectroscopic surveys and adaptive optics observations will probably resolve some of the single stars into multiple components (e.g. Baroch et al 2018;Fouqué et al 2018;Winters et al 2019a). Second, the component of the 10 pc catalogue that will see the largest increase in number corresponds to new exoplanets that will be discovered or confirmed in the coming years as most stars are orbited by at least one exoplanet.…”

Section: Obsolescencementioning

confidence: 99%

The 10 parsec sample in the Gaia era

Reylé

Jardine²,

Fouqué

et al. 2021

A&A

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Context. The nearest stars provide a fundamental constraint for our understanding of stellar physics and the Galaxy. The nearby sample serves as an anchor where all objects can be seen and understood with precise data. This work is triggered by the most recent data release of the astrometric space mission Gaia and uses its unprecedented high precision parallax measurements to review the census of objects within 10 pc. Aims. The first aim of this work was to compile all stars and brown dwarfs within 10 pc observable by Gaia and compare it with the Gaia Catalogue of Nearby Stars as a quality assurance test. We complement the list to get a full 10 pc census, including bright stars, brown dwarfs, and exoplanets. Methods. We started our compilation from a query on all objects with a parallax larger than 100 mas using the Set of Identifications, Measurements, and Bibliography for Astronomical Data database (SIMBAD). We completed the census by adding companions, brown dwarfs with recent parallax measurements not in SIMBAD yet, and vetted exoplanets. The compilation combines astrometry and photometry from the recent Gaia Early Data Release 3 with literature magnitudes, spectral types, and line-of-sight velocities. Results. We give a description of the astrophysical content of the 10 pc sample. We find a multiplicity frequency of around 28%. Among the stars and brown dwarfs, we estimate that around 61% are M stars and more than half of the M stars are within the range from M3.0 V to M5.0 V. We give an overview of the brown dwarfs and exoplanets that should be detected in the next Gaia data releases along with future developments. Conclusions. We provide a catalogue of 541 stars, brown dwarfs, and exoplanets in 339 systems, within 10 pc from the Sun. This list is as volume-complete as possible from current knowledge and it provides benchmark stars that can be used, for instance, to define calibration samples and to test the quality of the forthcoming Gaia releases. It also has a strong outreach potential.

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Section: Obsolescencementioning

confidence: 99%

The 10 parsec sample in the Gaia era

Reylé

Jardine²,

Fouqué

et al. 2021

A&A

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“…For most of the stars, mass estimates are provided in the catalogues. For the stars from Fouqué et al (2018) and Reiners & Basri (2009), we estimate mass from temperature according to the 2 Gyr evolutionary track from Baraffe et al (1998). We did not estimate masses for the Gaia DR2 data because the uncertainties would be too high for a meaningful Figure 1.…”

Section: Introductionmentioning

confidence: 99%

“…Stars from F-, G-, and K-star catalogues are shown in orange (Chandler et al 2016;Nordström et al 2004;Brewer et al 2016). Stars from the cool dwarf catalogues are added cumulatively in red (Gaidos et al 2014;Fouqué et al 2018;Terrien et al 2015;Reiners & Basri 2009). The Gaia DR2 sample is overplotted with no color filling.…”

Section: Introductionmentioning

confidence: 99%

Radial Velocity Photon Limits for the Dwarf Stars of Spectral Classes F–M

Reiners¹,

Zechmeister²

2020

ApJS

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The determination of extrasolar planet masses with the radial velocity (RV) technique requires spectroscopic Doppler information from the planet's host star, which varies with stellar brightness and temperature. We analyze Doppler information in spectra of F-M dwarfs utilizing empirical information from HARPS and CARMENES, and from model spectra. We come to the conclusions that an optical setup (BV R-bands) is more efficient that a near-infrared one (Y JHK) in dwarf stars hotter than 3200 K.We publish a catalogue of 46,480 well-studied F-M dwarfs in the solar neighborhood and compare their distribution to more than one million stars from Gaia DR2. For all stars, we estimate the RV photon noise achievable in typical observations assuming no activity jitter and slow rotation. We find that with an ESPRESSO-like instrument at an 8m-telescope, a photon noise limit of 10 cm s −1 or lower can be reached in more than 280 stars in a 5 min observation. At 4m-telescopes, a photon noise limit of 1 m s −1 can be reached in a 10 min exposure in approx. 10,000 predominantly sun-like stars with a HARPS-like (optical) instrument. The same applies to ∼3000 stars for a red-optical setup covering the RIz-bands, and to ∼700 stars for a near-infrared instrument. For the latter two, many of the targets are nearby M dwarfs. Finally, we identify targets in which Earth-mass planets within the liquid water habitable zone can cause RV amplitudes comparable to the RV photon noise. Assuming the same exposure times, we find that an ESPRESSO-like instrument can reach this limit for 1 M ⊕ planets in more than 1000 stars. The optical, red-optical, and near-infrared configurations reach the limit for 2 M ⊕ planets in approximately 500, 700, and 200 stars, respectively.

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“…areDelfosse et al (1998),Browning et al (2010), López-Santiago et al (2010,Reiners et al (2012), Luck (2017),Fouqué et al (2018,Reiners et al (2018), and, especially, Schweitzer et al (…”

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confidence: 99%

CARMENES input catalog of M dwarfs

Perdelwitz

Mittag

Tal-Or

et al. 2021

A&A

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Context. Radial-velocity (RV) jitter caused by stellar magnetic activity is an important factor in state-of-the-art exoplanet discovery surveys such as CARMENES. Stellar rotation, along with heterogeneities in the photosphere and chromosphere caused by activity, can result in false-positive planet detections. Hence, it is necessary to determine the stellar rotation period and compare it to any putative planetary RV signature. Long-term measurements of activity indicators such as the chromospheric emission in the Ca ii H&K lines (R HK ) enable the identification of magnetic activity cycles. Aims. In order to determine stellar rotation periods and study the long-term behavior of magnetic activity of the CARMENES guaranteed time observations (GTO) sample, it is advantageous to extract R HK time series from archival data, since the CARMENES spectrograph does not cover the blue range of the stellar spectrum containing the Ca ii H&K lines. Methods. We have assembled a catalog of 11 634 archival spectra of 186 M dwarfs acquired by seven different instruments covering the Ca ii H&K regime: ESPaDOnS, FEROS, HARPS, HIRES, NARVAL, TIGRE, and UVES. The relative chromospheric flux in these lines, R HK , was directly extracted from the spectra by rectification with PHOENIX synthetic spectra via narrow passbands around the Ca ii H&K line cores. Results. The combination of archival spectra from various instruments results in time series for 186 stars from the CARMENES GTO sample. As an example of the use of the catalog, we report the tentative discovery of three previously unknown activity cycles of M dwarfs. Conclusions. We conclude that the method of extracting R HK with the use of model spectra yields consistent results for different instruments and that the compilation of this catalog will enable the analysis of long-term activity time series for a large number of M dwarfs.

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SPIRou Input Catalogue: global properties of 440 M dwarfs observed with ESPaDOnS at CFHT

Cited by 51 publications

References 131 publications

The 10 parsec sample in the Gaia era

The 10 parsec sample in the Gaia era

Radial Velocity Photon Limits for the Dwarf Stars of Spectral Classes F–M

CARMENES input catalog of M dwarfs

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