The RoPES project with HARPS and HARPS-N

Mascareño, A. Suárez; Hernández, J. I. González; Rebolo, R.; Velasco, Sergio; Toledo-Padrón, B.; Udry, S.; Motalebi, F.; Ségrasan, D.; Wyttenbach, A.; Mayor, M.; Pepe, F.; Santos, N. C.; Figueira, P.; Esposito, M.

doi:10.1051/0004-6361/201732042

Cited by 43 publications

(71 citation statements)

References 65 publications

(65 reference statements)

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“…Affer et al 2016). Also, the h hyperparameter, corresponding to the mean amplitude of the stellar signal, is fully compatible with the expected value derived by Suárez Mascareño et al (2018) from the mean activity level of the star, log R HK , that is K exp = 1.9 ± 0.4 m s …”

Section: Analysis Of the Combined Hires And Harps-n Rv Time Seriessupporting

confidence: 84%

“…For Gl15A they computed a mean level of chromospheric emission log R HK = −5.27 ± 0.04, and a rotation period P rot = 45.0 ± 4.4 d, fully consistent with the value found by Howard et al (2014). The definition of log R HK can be extended for application on M-dwarfs spectra (Suárez Mascareño et al 2018, and references therein). The stellar parameters for Gl15A used in this work are summarized in the left column of Table 1.…”

Section: Stellar Properties Of Gl15a and Gl15bsupporting

confidence: 73%

“…No long-period trend is found in either the HIRES or HARPS-N datasets. Suárez Mascareño et al (2018) found a magnetic-cycle type periodicity at P cycle = 2.8 ± 0.5 yr in the HARPS-N CaII H&K and Hα indexes, even if we find no similar signal in the respective HIRES time series. Nevertheless, the period of this cycle is far from the time span of the longperiod signal we investigate, so it could not be the origin of it.…”

Section: Analysis Of the Activity Indexescontrasting

confidence: 68%

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The HADES RV Programme with HARPS-N at TNG

Pinamonti

Damasso

Marzari

et al. 2018

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We present 20 yr of radial velocity (RV) measurements of the M1 dwarf Gl15A, combining five years of intensive RV monitoring with the HARPS-N spectrograph with 15 yr of archival HIRES/Keck RV data. We have carried out an MCMC-based analysis of the RV time series, inclusive of Gaussian Process (GP) approach to the description of stellar activity induced RV variations. Our analysis confirms the Keplerian nature and refines the orbital solution for the 11.44-day period super Earth, Gl15A b, reducing its amplitude to 1.68, and successfully models a long-term trend in the combined RV dataset in terms of a Keplerian orbit with a period around 7600 days and an amplitude of 2.5, corresponding to a super-Neptune mass (M sin i = 36 +25 −18 M ⊕ ) planetary companion. We also discuss the present orbital configuration of Gl15A planetary system in terms of the possible outcomes of Lidov-Kozai interactions with the wide-separation companion Gl15B in a suite of detailed numerical simulations. In order to improve the results of the dynamical analysis, we have derived a new orbital solution for the binary system, combining our RV measurements with astrometric data from the WDS catalogue. The eccentric Lidov-Kozai analysis shows the strong influence of Gl15B on the Gl15A planetary system, which can produce orbits compatible with the observed configuration for initial inclinations of the planetary system between 75• and 90• , and can also enhance the eccentricity of the outer planet well above the observed value, even resulting in orbital instability, for inclinations around 0• and 15• −30• . The Gl15A system is the multi-planet system closest to Earth, at 3.56 pc, and hosts the longest period RV sub-Jovian mass planet discovered so far. Its orbital architecture constitutes a very important laboratory for the investigation of formation and orbital evolution scenarios for planetary systems in binary stellar systems.

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Section: Analysis Of the Combined Hires And Harps-n Rv Time Seriessupporting

confidence: 84%

Section: Stellar Properties Of Gl15a and Gl15bsupporting

confidence: 73%

Section: Analysis Of the Activity Indexescontrasting

confidence: 68%

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The HADES RV Programme with HARPS-N at TNG

Pinamonti

Damasso

Marzari

et al. 2018

A&A

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“…The determination of the rotation periods (P rot ) was done by analysing time series high-resolution spectroscopy of the Ca II H & K lines and Hα activity indicators and was published in Suárez Mascareño et al (2018). The authors studied a fraction of our original M dwarf sample composed of 72 stars (out of a total of 78) providing 33 rotation periods measured from the spectral indicator modulation, and 34 periods derived from the Ca II H & K -rotational period relationship.…”

Section: Rotation Periodsmentioning

confidence: 99%

HADES RV Programme with HARPS-N at TNG

González-Álvarez

Micela

Maldonado

et al. 2019

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Aims. We extend the relationship between X-ray luminosity (Lx) and rotation period (Prot) found for main-sequence FGK stars, and test whether it also holds for early M dwarfs, especially in the non-saturated regime (Lx ∝ Prot−2) which corresponds to slow rotators. Methods. We use the luminosity coronal activity indicator (Lx) of a sample of 78 early M dwarfs with masses in the range from 0.3 to 0.75 M⊙ from the HArps-N red Dwarf Exoplanet Survey (HADES) radial velocity (RV) programme collected from ROSAT and XMM-Newton. The determination of the rotation periods (Prot) was done by analysing time series of high-resolution spectroscopy of the Ca II H & K and Hα activity indicators. Our sample principally covers the slow rotation regime with rotation periods from 15 to 60 days. Results. Our work extends to the low mass regime the observed trend for more massive stars showing a continuous shift of the Lx∕Lbol versus Prot power law towards longer rotation period values, and includes a more accurate way to determine the value of the rotation period at which the saturation occurs (Psat) for M dwarf stars. Conclusions. We conclude that the relations between coronal activity and stellar rotation for FGK stars also hold for early M dwarfs in the non-saturated regime, indicating that the rotation period is sufficient to determine the ratio Lx∕Lbol.

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“…We present high-precision, high-resolution spectroscopic measurements of the bright M1 dwarf Gl 686, gathered with the HARPS-N spectrograph (Cosentino et al 2012) on the Telescopio Nazionale Galileo (TNG) as part of the HArps-n red Dwarf Exoplanet Survey (HADES) 1 , described in detail in Affer et al (2016). The HADES collaboration has already produced many valuable results, regarding the statistics, activity, and characterization of M stars (Perger et al 2017a;Maldonado et al 2015Maldonado et al , 2017Scandariato et al 2017;Suárez Mascareño et al 2018), and has led to the discovery of several planets (Affer et al 2016;Suárez Mascareño et al 2017;Perger et al 2017b;Pinamonti et al 2018).…”

Section: Introductionmentioning

confidence: 99%

HADES RV program with HARPS-N at the TNG

Affer

Damasso

Micela

et al. 2019

A&A

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Aims. The HArps-n red Dwarf Exoplanet Survey (HADES) is providing a major contribution to the widening of the current statistics of low-mass planets, through the in-depth analysis of precise radial-velocity (RV) measurements in a narrow range of spectral sub-types. Using the HARPS-N spectrograph we reach the precision needed to detect small planets with a few earth masses. Our survey is mainly focused on the M-dwarf population of the northern hemisphere. Methods. As part of that program, we obtained RV measurements of Gl 686, an M1 dwarf at d = 8.2 pc. These measurements show a dispersion much in excess of their internal errors. The analysis of data obtained within an intensive observing campaign demonstrates that the excess dispersion is due to a coherent signal with a period of 15.53 d. Almost simultaneous photometric observations were carried out within the APACHE and EXORAP programs to characterize the stellar activity and to distinguish periodic variations related to activity from signals due to the presence of planetary companions, complemented also with ASAS photometric data. We used a Bayesian framework to estimate the orbital parameters and the planet minimum mass, and to properly treat the activity noise. We took advantage of the available RV measurements for this target from other observing campaigns. The analysis of the RV composite time series from the HIRES, HARPS, and HARPS-N spectrographs, consisting of 198 measurements taken over 20 yr, enabled us to address the nature of periodic signals and also to characterize stellar physical parameters (mass, temperature, and rotation). Results. We report the discovery of a super-Earth orbiting at a distance of 0.092 AU from the host star Gl 686. The planet has a minimum mass of 7.1 ± 0.9 M⊕ and an orbital period of 15.532 ± 0.002 d. The analysis of the activity indexes, of the correlated noise through a Gaussian process framework, and of the photometry provides an estimate of the stellar rotation period at 37 d, and highlights the variability of the spot configuration during the long timespan covering 20 yr. The observed periodicities around 2000 d likely point to the existence of an activity cycle.

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The RoPES project with HARPS and HARPS-N

Cited by 43 publications

References 65 publications

The HADES RV Programme with HARPS-N at TNG

The HADES RV Programme with HARPS-N at TNG

HADES RV Programme with HARPS-N at TNG

HADES RV program with HARPS-N at the TNG

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