Robo-AO M-dwarf Multiplicity Survey: Catalog*

Lamman, Claire; Baranec, Christoph; Berta-Thompson, Zachory K.; Law, Nicholas M.; Schonhut-Stasik, Jessica; Ziegler, Carl; Salama, M.S.; Jensen-Clem, Rebecca; Duev, Dmitry A.; Riddle, Reed; Kulkarni, S. R.; Winters, Jennifer G.; Irwin, Jonathan

doi:10.3847/1538-3881/ab6ef1

Cited by 34 publications

(28 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Lucky-imaging observations with FastCam (Cortés-Contreras et al 2017) and Robo AO images (Lamman et al 2020) have not detected any resolved visual companion. The TESS aperture includes several objects.…”

Section: Transit Search and Analysis With Tessmentioning

confidence: 98%

The CARMENES search for exoplanets around M dwarfs

Stock

Nagel

Kemmer

et al. 2020

A&A

View full text Add to dashboard Cite

We announce the discovery of two planets orbiting the M dwarfs GJ 251 (0.360 ± 0.015M⊙) and HD 238090 (0.578 ± 0.021M⊙) based on CARMENES radial velocity (RV) data. In addition, we independently confirm with CARMENES data the existence of Lalande 21185 b, a planet that has recently been discovered with the SOPHIE spectrograph. All three planets belong to the class of warm or temperate super-Earths and share similar properties. The orbital periods are 14.24 d, 13.67 d, and 12.95 d and the minimum masses are 4.0 ± 0.4 M⊕, 6.9 ± 0.9 M⊕, and 2.7 ± 0.3 M⊕ for GJ 251 b, HD 238090 b, and Lalande 21185 b, respectively. Based on the orbital and stellar properties, we estimate equilibrium temperatures of 351.0 ± 1.4 K for GJ 251 b, 469.6 ± 2.6 K for HD 238090 b, and 370.1 ± 6.8 K for Lalande 21185 b. For the latter we resolve the daily aliases that were present in the SOPHIE data and that hindered an unambiguous determination of the orbital period. We find no significant signals in any of our spectral activity indicators at the planetary periods. The RV observations were accompanied by contemporaneous photometric observations. We derive stellar rotation periods of 122.1 ± 2.2 d and 96.7 ± 3.7 d for GJ 251 and HD 238090, respectively. The RV data of all three stars exhibit significant signals at the rotational period or its first harmonic. For GJ 251 and Lalande 21185, we also find long-period signals around 600 d, and 2900 d, respectively, which we tentatively attribute to long-term magnetic cycles. We apply a Bayesian approach to carefully model the Keplerian signals simultaneously with the stellar activity using Gaussian process regression models and extensively search for additional significant planetary signals hidden behind the stellar activity. Current planet formation theories suggest that the three systems represent a common architecture, consistent with formation following the core accretion paradigm.

show abstract

Section: Transit Search and Analysis With Tessmentioning

confidence: 98%

The CARMENES search for exoplanets around M dwarfs

Stock

Nagel

Kemmer

et al. 2020

A&A

View full text Add to dashboard Cite

show abstract

“…To test how this excess noise statistic is elevated by close binarity we followed a similar approach to Rizzuto et al (2018). We took close, directly imaged binaries (with separations within 1 arcsecond) from Kraus et al (2016) and binaries found to be unresolved in Gaia from Ziegler et al (2018) and Lamman et al (2020). This sample in this latter work is a compilation of directly imaged binaries from Law et al (2014), Baranec et al (2016) and Ziegler et al (2017) and counts binaries as resolved in Gaia if the secondary has a Gaia DR2 entry of its own.…”

Section: Stars With Noisy Astrometric Solutionsmentioning

confidence: 99%

Wide binaries are rare in open clusters

Deacon

Kraus

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The population statistics of binary stars are an important output of star formation models. However, populations of wide binaries evolve over time due to interactions within a system’s birth environment and the unfolding of wide, hierarchical triple systems. Hence, the wide binary populations observed in star-forming regions or OB associations may not accurately reflect the wide binary populations that will eventually reach the field. We use Gaia DR2 data to select members of three open clusters, Alpha Per, the Pleiades, and Praesepe and to flag cluster members that are likely unresolved binaries due to overluminosity or elevated astrometric noise. We then identify the resolved wide binary population in each cluster, separating it from coincident pairings of unrelated cluster members. We find that these clusters have an average wide binary fraction in the 300–3000 au projected separation range of 2.1$\pm ^{0.4}_{0.2}$ per cent increasing to 3.0$\pm ^{0.8}_{0.7}$ per cent for primaries with masses in the 0.5–1.5 M⊙ range. This is significantly below the observed field wide binary fraction, but shows some wide binaries survive in these dynamically highly processed environments. We compare our results with another open cluster (the Hyades) and two populations of young stars that likely originated in looser associations (young moving groups and the Pisces-Eridanus stream). We find that the Hyades also has a deficit of wide binaries while the products of looser associations have wide binary fractions at or above field level.

show abstract

“…GJ 740 (HD 176029, BD+05 3993) is a bright (m V =9.2) M1Vtype high-proper motion star, located at 11.1 pc from the Sun (Gaia Collaboration et al 2018). The search for companions of this star has produced null detections (Carson et al 2005;Lamman et al 2020), reporting only some faint field background objects (Carson et al 2005). Stellar parameters from the literature are shown in Table 1 along with new values established in this work.…”

Section: Gj 740mentioning

confidence: 86%

A super-Earth on a close-in orbit around the M1V star GJ 740. A HADES and CARMENES collaboration

Toledo-Padrón,

Mascareño,

Hernández

et al. 2021

Preprint

View full text Add to dashboard Cite

Context. M-dwarfs have proven to be ideal targets for planetary radial velocity (RV) searches due to their higher planet-star mass contrast, which favors the detection of low-mass planets. The abundance of super-Earth and Earth-like planets detected around this type of stars motivates further such research on hosts without reported planetary companions. Aims. The HADES and CARMENES programs aim to carry out extensive searches of exoplanetary systems around M-type stars in the northern hemisphere, allowing us to address statistically the properties of the planets orbiting these objects. In this work, we perform a spectroscopic and photometric study of one of the program stars (GJ 740), which exhibits a short-period RV signal compatible with a planetary companion. Methods. We carried out a spectroscopic analysis based on 129 HARPS-N spectra taken over a time-span of 6 yr combined with 57 HARPS spectra taken over 4 yr, as well as 32 CARMENES spectra taken during more than 1 yr, resulting in a dataset with a time coverage of 10 yr. We also relied on 459 measurements from the public ASAS survey with a time-coverage of 8 yr along with 5 yr of photometric magnitudes from the EXORAP project taken in the V, B, R, and I filters to carry out a photometric study. Both analyses were made using Markov Chain Monte Carlo (MCMC) simulations and Gaussian Process regression to model the activity of the star. Results. We present the discovery of a short-period super-Earth with an orbital period of 2.37756 +0.00013 −0.00011 d and a minimum mass of 2.96 +0.50 −0.48 M ⊕ . We offer an update to the previously reported characterization of the magnetic cycle and rotation period of the star, obtaining values of P rot =35.563 ±0.071 d and P cycle =2800±150 d. Furthermore, the RV time-series exhibits a possibly periodic longterm signal which might be related to a Saturn-mass planet of ∼ 100 M ⊕ .

show abstract

Robo-AO M-dwarf Multiplicity Survey: Catalog*

Cited by 34 publications

References 48 publications

The CARMENES search for exoplanets around M dwarfs

The CARMENES search for exoplanets around M dwarfs

Wide binaries are rare in open clusters

A super-Earth on a close-in orbit around the M1V star GJ 740. A HADES and CARMENES collaboration

Contact Info

Product

Resources

About