CARMENES input catalogue of M dwarfs

Alonso, Eduardo; Caballero, J. A.; Montes, D.; Juez, Francisco Javier de Cos; Dreizler, S.; Dubois, Franky; Jeffers, S. V.; Lalitha, S.; Naves, R.; Reiners, A.; Ribas, I.; Vanaverbeke, Sigfried; Amado, P. J.; Béjar, V. J. S.; Cortés-Contreras, M.; Herrero, E.; Hidalgo, D.; Kürster, M.; Logie, Ludwig; Quirrenbach, A.; Rau, Steve; Seifert, W.; Schöfer, P.; Tal-Or, L.

doi:10.1051/0004-6361/201833316

Cited by 97 publications

(94 citation statements)

References 143 publications

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“…We observed HIP36985 with SPHERE in 2018 and confirm the presence of a however low-mass star companion (Biller et al in prep.). We find a period of 22 days for the short-term variations, while the rotation period is of 12±0.1 days (Díez Alonso et al 2019). The poor sampling of those shortterm variations probably explains the strong difference with the rotation period.…”

Section: Hip36985mentioning

confidence: 76%

A HARPS RV search for planets around young nearby stars

Grandjean

Lagrange

Keppler

et al. 2020

A&A

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Context. Young nearby stars are good candidates in the search for planets with both radial velocity (RV) and direct imaging techniques. This, in turn, allows for the computation of the giant planet occurrence rates at all separations. The RV search around young stars is a challenge as they are generally faster rotators than older stars of similar spectral types and they exhibit signatures of magnetic activity (spots) or pulsation in their RV time series. Specific analyses are necessary to characterize, and possibly correct for, this activity. Aims. Our aim is to search for planets around young nearby stars and to estimate the giant planet (GP) occurrence rates for periods up to 1000 days. Methods. We used the HARPS spectrograph on the 3.6 m telescope at La Silla Observatory to observe 89 A − M young (< 600 Myr) stars. We used our SAFIR (Spectroscopic data via Analysis of the Fourier Interspectrum Radial velocities ) software to compute the RV and other spectroscopic observables. Then, we computed the companion occurrence rates on this sample. Results. We confirm the binary nature of HD177171, HD181321 and HD186704. We report the detection of a close low mass stellar companion for HIP36985. No planetary companion was detected. We obtain upper limits on the GP (< 13 MJup) and BD (∈ [13; 80] MJup) occurrence rates based on 83 young stars for periods less than 1000 days, which are set, 2 +3 −2 % and 1 +3 −1 %.

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Section: Hip36985mentioning

confidence: 76%

A HARPS RV search for planets around young nearby stars

Grandjean

Lagrange

Keppler

et al. 2020

A&A

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“…The photometric measurements from SuperWASP, NSVS, and HATNet are densely sampled, and thus most of the GLS power appears significant, but it cannot be associated with the RV signals. The most likely stellar rotation frequency is shown with red dashed line, while the red shaded area denotes its uncertainties, as given by Díez Alonso et al (2019). extended HIRES data time series yields an additional RV signal with a period of ∼ 530 d, likely due to a second massive planet in the system. In Trifonov et al (2018b), we added 52 CARMENES RVs and performed a combined Doppler analysis, which revealed the two-planet configuration of the GJ 1148 system.…”

Section: The Gj 1148 Planetary Systemmentioning

confidence: 99%

“…In Fig. 2 the adopted stellar rotational period of 71.5 d from Díez Alonso et al (2019) of GJ 1148 is shown with a red dashed line in each panel.…”

Section: Carmenes Datamentioning

confidence: 99%

“…However, from the Hungarian-made Automated Telescope Network (HATNet; Bakos et al 2004) In the three bottom right panels of Fig. 2, we show the GLS periodograms of the SuperWASP, the NSVS light-curve data of Alonso et al (2019), and the HAT-Net photometry. These photometric measurements were taken with a higher cadence when compared to the RV data, and thus many frequencies in the GLS power spectrum appear significant.…”

Section: Periodogram Analysismentioning

confidence: 99%

“…These efforts are motivated by the fact that M dwarfs Notes. 2MASS: Skrutskie et al (2006); Cab16 Caballero et al (2016); DA18: Díez Alonso et al (2019); Gaia Gaia Collaboration et al (Gaia DR2;; Pas18: Passegger et al (2018); HIP: Perryman et al (1997); Rei18: Reiners et al (2018b); Ros39: Ross (1939); Schw19: Schweitzer et al (2019).…”

Section: Introductionmentioning

confidence: 99%

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The CARMENES search for exoplanets around M dwarfs

Trifonov

Lee²,

Kürster

et al. 2020

A&A

Self Cite

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Context. GJ 1148 is an M-dwarf star hosting a planetary system composed of two Saturn-mass planets in eccentric orbits with periods of 41.38 and 532.02 days. Aims. We reanalyze the orbital configuration and dynamics of the GJ 1148 multi-planetary system based on new precise radial velocity (RV) measurements taken with CARMENES. Methods. We combined new and archival precise Doppler measurements from CARMENES with those available from HIRES for GJ 1148 and modeled these data with a self-consistent dynamical model. We studied the orbital dynamics of the system using the secular theory and direct N-body integrations. The prospects of potentially habitable moons around GJ 1148 b were examined. Results. The refined dynamical analyses show that the GJ 1148 system is long-term stable in a large phase-space of orbital parameters with an orbital configuration suggesting apsidal alignment, but not in any particular high-order mean-motion resonant commensurability. GJ 1148 b orbits inside the optimistic habitable zone (HZ). We find only a narrow stability region around the planet where exomoons can exist. However, in this stable region exomoons exhibit quick orbital decay due to tidal interaction with the planet. Conclusions. The GJ 1148 planetary system is a very rare M-dwarf planetary system consisting of a pair of gas giants, the inner of which resides in the HZ. We conclude that habitable exomoons around GJ 1148 b are very unlikely to exist.

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The population of M dwarfs observed at low radio frequencies

et al. 2021

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INTRODUCTORY PARAGRAPHCoherent low-frequency ( 200 MHz) radio emission from stars encodes the conditions of the outer corona, mass-ejection events, and space weather 1,2,3,4,5 . Previous low-frequency searches for radio emitting stellar systems have lacked the sensitivity to detect the general population, instead largely focusing on targeted studies of anomalously active stars 2,6,7,8,9 . Here we present 19 detections of coherent radio emission associated with known M dwarfs from a blind flux-limited low-frequency survey. Our detections show that coherent radio emission is ubiquitous across the M dwarf main sequence, and that the radio luminosity is independent of known coronal and chromospheric activity indicators. While plasma emission can generate the low-frequency emission from the most chromospherically active stars of our sample 1,10 , the origin of the radio emission from the most quiescent sources is yet to be ascertained. Large-scale analogues of the magnetospheric processes seen in gas-giant planets 4,11,12 likely drive the radio emission associated with these quiescent stars. The slowest-rotating stars of this sample are candidate systems to search for star-planet interaction signatures.

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CARMENES input catalogue of M dwarfs

Cited by 97 publications

References 143 publications

A HARPS RV search for planets around young nearby stars

A HARPS RV search for planets around young nearby stars

The CARMENES search for exoplanets around M dwarfs

The population of M dwarfs observed at low radio frequencies

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