2018
DOI: 10.1051/0004-6361/201732143
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HADES RV programme with HARPS-N at TNG

Abstract: We aim to investigate the presence of signatures of magnetic cycles and rotation on a sample of 71 early M-dwarfs from the HADES RV programme using high-resolution time-series spectroscopy of the Ca II H&K and Hα chromospheric activity indicators, the radial velocity series, the parameters of the cross correlation function and the V -band photometry. We used mainly HARPS-N spectra, acquired over 4 yr, and add HARPS spectra from the public ESO database and ASAS photometry light-curves as support data, exten… Show more

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Cited by 66 publications
(23 citation statements)
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References 56 publications
(74 reference statements)
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“…This choice is rather arbitrary but based on the known fact that more active stars tend to rotate faster (e.g. Stelzer et al 2016;Mascareño et al 2018).…”
Section: Stellar Activity Modelmentioning
confidence: 99%
See 1 more Smart Citation
“…This choice is rather arbitrary but based on the known fact that more active stars tend to rotate faster (e.g. Stelzer et al 2016;Mascareño et al 2018).…”
Section: Stellar Activity Modelmentioning
confidence: 99%
“…We defined them on the basis of the typical scatter observed in the RVs 2 for a low-activity star, h ∼3 m s −1 , and a high-activity star, h ∼15 m s −1 (e.g. Santos et al 2000;Suárez Mascareño et al 2017;Mascareño et al 2018;Damasso et al 2019). In a more general sense, our definition of low and high stellar activity levels should be intended as relative to the small semi-amplitude of the planetary signal investigated in this work, i.e.…”
Section: Stellar Activity Modelmentioning
confidence: 99%
“…4.1. For 13 stars over these 23, Suárez Mascareño et al (2018) were able to measure the rotation periods from the spectroscopic activity indexes (Ca II H&K and/or Hα) or RV time series, while for the other 10 the rotation period was estimated from activity-rotation relationships and their calculated values of log R ′ HK . The definition of log R ′ HK was extended for application on M dwarfs spectra, following a procedure very similar to the one used by Suárez Mascareño et al (2016).…”
Section: Spectroscopic Rotation Periodsmentioning
confidence: 99%
“…When it comes to M dwarf type planet hosts, the stellar temperate zone, within which the signals of potentially habitable planets can today be readily identified in principle (e.g., Anglada-Escudé et al 2016a;Dittmann et al 2017;Suárez Mascareño et al 2017a;Astudillo-Defru et al 2017b;Bonfils et al 2018;Zechmeister et al 2019), corresponds to orbital periods typically in the range of tens of days (e.g., Kopparapu et al 2013Kopparapu et al , 2014Kopparapu 2018). However, these timescales can coincide with those of stellar rotation periods of low-mass stars in the middle of their main-sequence lifetime (e.g., Barnes 2007;McQuillan et al 2013;Vanderburg et al 2016;Newton et al 2016;Suárez Mascareño et al 2018). Without a detailed understanding of stellar activity-induced effects in RVs to supporting spectroscopic and photometric information, ambiguities in the interpretation of RV signals with periods corresponding to habitable zone distances might be long-lasting (e.g., Robertson et al 2014;Anglada-Escudé & Tuomi 2015;Robertson et al 2015;Anglada-Escudé et al 2016b).…”
Section: Introductionmentioning
confidence: 99%
“…We derived the expected rotational period of M dwarfs using activity-rotation relationships as a first estimation. Several studies show a significant correlation between the activity and rotation for M dwarfs (e.g., SuárezMascareño et al 2018b;Astudillo-Defru et al 2017;Suárez Mascareño et al 2016). We used Eq.1 andTable 1from SuárezMascareño et al (2015) for the rotational period determination from the log(R HK ).…”
mentioning
confidence: 99%