2017
DOI: 10.1051/0004-6361/201629223
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HADES RV Programme with HARPS-N at TNG

Abstract: Context. Understanding stellar activity in M dwarfs is crucial for the physics of stellar atmospheres and for ongoing radial velocity exoplanet programmes. Despite the increasing interest in M dwarfs, our knowledge of the chromospheres of these stars is far from being complete. Aims. We test whether the relations between activity, rotation, and stellar parameters and flux-flux relationships previously investigated for main-sequence FGK stars and for pre-main-sequence M stars also hold for early-M dwarfs on the… Show more

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Cited by 42 publications
(71 citation statements)
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References 93 publications
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“…For stars with more than one observation, we considered the standard deviation of the observed CCF width and the photon noise on the CCF in the error propagation equations. The mean value of the final uncertainties is of 0.47 km s −1 , which is compatible with the work of Browning et al (2010) and Maldonado et al (2017). Uncertainties coming from simple error propagation are by construction underestimations and the method needs a deeper analysis on the uncertainties and dependencies on both other astrophysical parameters as well as the systematic errors coming from the simplified model applied to link the v sin i to the FWHM of the CCF (Maldonado et al 2017;Browning et al 2010;Reiners et al 2018, and references therein).…”
Section: Projected Rotational Velocity (V Sin I)supporting
confidence: 92%
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“…For stars with more than one observation, we considered the standard deviation of the observed CCF width and the photon noise on the CCF in the error propagation equations. The mean value of the final uncertainties is of 0.47 km s −1 , which is compatible with the work of Browning et al (2010) and Maldonado et al (2017). Uncertainties coming from simple error propagation are by construction underestimations and the method needs a deeper analysis on the uncertainties and dependencies on both other astrophysical parameters as well as the systematic errors coming from the simplified model applied to link the v sin i to the FWHM of the CCF (Maldonado et al 2017;Browning et al 2010;Reiners et al 2018, and references therein).…”
Section: Projected Rotational Velocity (V Sin I)supporting
confidence: 92%
“…We estimated the v sin i using the FWHM of the CCF and B − V color and following the procedure described by several studies (e.g., Santos et al 2002;Maldonado et al 2017, with references therein) for HARPS data. We extended the calibration and used the stars that were observed with both HARPS and HARPS-N. Knowing that the instruments are very similar in design and in particular in resolution, a linear relationship was defined between the width of the CCF as measured by the two instruments.…”
Section: Projected Rotational Velocity (V Sin I)mentioning
confidence: 99%
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“…For example, the model suite may not span a large enough range of surface gravity at low temperatures, resulting in artificially inflated v i sin at low effective temperature if there is a physical correlation between g log and T eff . However, no such systematic effect has been found by other authors using PHOENIX templates (Houdebine & Mullan 2015;Maldonado et al 2017). Tests with template grids spanning a wide range of g log ( g 4.5 log 5.5   ) indicate that systematic bias of v i sin with g log is small and does not have a large impact on our detection threshold.…”
Section: Detection Limitcontrasting
confidence: 46%
“…We used the stellar parameters published by Maldonado et al (2017), which were calculated applying the empirical relations by Maldonado et al (2015) on the same HARPS-N spectra from which we derived the RV time series. This technique calculates stellar temperatures from ratios of pseudo-equivalent widths of spectral features, and calibrate the metallicity on combinations and ratios of different features.…”
Section: Stellar Properties Of Gl15a and Gl15bmentioning
confidence: 99%