Close substellar-mass companions in stellar wide binaries: discovery and characterization with APOGEE and <i>Gaia</i> DR2

Lewis, Hannah M.; Anguiano, Borja; Majewski, Steven R.; Nidever, David L.; Badenes, Carles; Lee, Nathan De; Hasselquist, Sten; Daher, Christine Mazzola; Stassun, Keivan G.; Bizyaev, Dmitry; Godoy-Rivera, D.; Nitschelm, Christian; Oravetz, Audrey; Pan, Kaike; Román-Lópes, A.

doi:10.1093/mnras/stab2349

Cited by 3 publications

(2 citation statements)

References 70 publications

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“…and Orbital Period An advantage conferred by the APOGEE survey is that multi-epoch data were obtained, and RVs from these multiple epochs enable studies of stellar and substellar multiplicity (Troup et al 2016;Badenes et al 2018;Lewis et al 2022). 15 When a sufficient number of epochs are available for a particular star, it is possible to derive or constrain orbital parameters (e.g., Price-Whelan et al 2020; see below), however, this only applies to a minority fraction of APOGEE targets, since the more typical number of APOGEE visits is only three per star.…”

Section: Binary Properties As a Function Of Rv Variabilitymentioning

confidence: 99%

White dwarf binaries Across the H-R Diagram

Anguiano¹,

Majewski²,

Stassun³

et al. 2022

Preprint

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We created the APOGEE-GALEX-Gaia catalog to study white dwarfs binaries. This database aims to create a minimally biased sample of WD binary systems identified from a combination of GALEX, Gaia, and APOGEE data to increase the number of WD binaries with orbital parameters and chemical compositions. We identify 3,414 sources as WD binary candidates, with nondegenerate companions of spectral types between F and M, including main sequence, main sequence binaries, subgiants, sub-subgiants, red giants, and red clump stars. Among our findings are (a) a total of 1,806 systems having inferred WD radii R < 25 R ⊕ , which constitute a more reliable group of WD binary candidates within the main sample; (b) a difference in the metallicity distribution function between WD binary candidates and the control sample of most luminous giants (M H < −3.0); (c) the existence of a population of sub-subgiants with WD companions; (d) evidence for shorter periods in binaries that contain WDs compared to those that do not, as shown by the cumulative distributions of APOGEE radial velocity shifts; (e) evidence for systemic orbital evolution in a sample of 252 WD binaries with orbital periods, based on differences in the period distribution between systems with red clump, main sequence binary, and sub-subgiant companions and systems with main sequence or red giant companions; and (f) evidence for chemical enrichment during common envelope (CE) evolution, shown by lower metallicities in wide WD binary candidates (P > 100 days) compared to post-CE (P < 100 days) WD binary candidates. Subject headings: (stars:) binaries (including multiple): close

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Section: Binary Properties As a Function Of Rv Variabilitymentioning

confidence: 99%

White dwarf binaries Across the H-R Diagram

Anguiano¹,

Majewski²,

Stassun³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…An advantage conferred by the APOGEE survey is that multi-epoch data were obtained, and RVs from these multiple epochs enable studies of stellar and substellar multiplicity (Troup et al 2016;Badenes et al 2018;Lewis et al 2022). 15 When a sufficient number of epochs are available for a particular star, it is possible to derive or constrain orbital parameters (e.g., Price-Whelan et al 2020; see below); however, this only applies to a minority fraction of APOGEE targets, since the more typical number of APOGEE visits is only three per star.…”

Section: Binary Properties As a Function Of Rv Variability Andmentioning

confidence: 99%

White Dwarf Binaries across the H-R Diagram

Anguiano

Majewski

Stassun

et al. 2022

Self Cite

View full text Add to dashboard Cite

We created the APOGEE-GALEX-Gaia catalog to study white dwarf (WD) binaries. This database aims to create a minimally biased sample of WD binary systems identified from a combination of GALEX, Gaia, and APOGEE data to increase the number of WD binaries with orbital parameters and chemical compositions. We identify 3414 sources as WD binary candidates, with nondegenerate companions of spectral types between F and M, including main-sequence stars, main-sequence binaries, subgiants, sub-subgiants, red giants, and red clump stars. Among our findings are (a) a total of 1806 systems having inferred WD radii R < 25 R ⊕, which constitute a more reliable group of WD binary candidates within the main sample; (b) a difference in the metallicity distribution function between WD binary candidates and the control sample of most luminous giants (M H < −3.0); (c) the existence of a population of sub-subgiants with WD companions; (d) evidence for shorter periods in binaries that contain WDs compared to those that do not, as shown by the cumulative distributions of APOGEE radial velocity shifts; (e) evidence for systemic orbital evolution in a sample of 252 WD binaries with orbital periods, based on differences in the period distribution between systems with red clump, main-sequence binary, and sub-subgiant companions and systems with main-sequence or red giant companions; and (f) evidence for chemical enrichment during common envelope (CE) evolution, shown by lower metallicities in wide WD binary candidates (P > 100 days) compared to post-CE (P < 100 days) WD binary candidates.

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Multiplicity of stars with planets in the solar neighbourhood

González-Payo,

Caballero,

Gorgas

et al. 2024

A&A

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We intended to quantify the impact of stellar multiplicity on the presence and properties of exoplanets. We investigated all exoplanet host stars at less than 100\,pc using the latest astrometric data from Gaia DR3 and advanced statistical methodologies. We complemented our search for common proper motion and parallax companions with data from the Washington Double Star catalogue and the literature. After excluding a number of systems based on radial velocity data, and membership in clusters and open associations, or with resolved ultracool companions, we kept 215 exoplanet host stars in 212 multiple-star systems. We found 17 new companions in the systems of 15 known exoplanet host stars, and we measured precise angular and projected physical separations and position angles for 236 pairs of stars, compiled key parameters for 276 planets in multiple systems, and established a comparison sample comprising 687 single stars with exoplanets. With all of this, we statistically analysed a series of hypotheses regarding planets in multiple stellar systems. Although they are only statistically significant at a $2 level, our analysis pointed to several interesting results on the comparison in the mean number of planets in multiple versus single stellar systems and the tendency of high-mass planets to be located in closer orbits in multiple systems. We confirm that planets in multiple systems tend to have orbits with larger eccentricities than those in single systems. In particular, we found a significant ($> 4 preference for planets to exhibit high orbital eccentricities at small ratios between star-star projected physical separations and star-planet semi-major axes.

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Close substellar-mass companions in stellar wide binaries: discovery and characterization with APOGEE and Gaia DR2

Cited by 3 publications

References 70 publications

White dwarf binaries Across the H-R Diagram

White dwarf binaries Across the H-R Diagram

White Dwarf Binaries across the H-R Diagram

Multiplicity of stars with planets in the solar neighbourhood

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