Companions to Apogee Stars. I. A Milky Way-Spanning Catalog of Stellar and Substellar Companion Candidates and Their Diverse Hosts

Troup, Nicholas; Nidever, David L.; Lee, Nathan De; Carlberg, Joleen K.; Majewski, Steven R.; Fernández, M. A.; Covey, Kevin R.; Chojnowski, S. Drew; Pepper, Joshua; Nguyen, Duy Thanh; Stassun, Keivan G.; Nguyen, Duy Cuong; Wisniewski, John P.; Fleming, Scott W.; Bizyaev, Dmitry; Frinchaboy, Peter M.; García-Hernández, D. A.; Ge, Jian; Hearty, Fred; Mészáros, Szabolcs; Pan, Kaike; Prieto, C. Allende; Schneider, Donald P.; Shetrone, Matthew; Skrutskie, Michael F.; Wilson, John C.; Zamora, Olga

doi:10.3847/0004-6256/151/3/85

Cited by 82 publications

(43 citation statements)

References 88 publications

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“…We derive full orbital solutions for 64 binary systems which have sufficient visits and phase coverage to constrain the orbit. Our criteria for determining whether the available velocity data are sufficient to constrain a system's orbit are discussed in Appendix D. We only attempt to derive orbital solutions for systems in which at least two stars contribute to the spectrum; orbital solutions for SB1 systems in APOGEE can be found in Troup et al (2016).…”

Section: Deriving Orbital Parametersmentioning

confidence: 99%

Discovery and characterization of 3000+ main-sequence binaries from APOGEE spectra

El-Badry

Ting

Rix

et al. 2018

Monthly Notices of the Royal Astronomical Society

112

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We develop a data-driven spectral model for identifying and characterizing spatially unresolved multiple-star systems and apply it to APOGEE DR13 spectra of mainsequence stars. Binaries and triples are identified as targets whose spectra can be significantly better fit by a superposition of two or three model spectra, drawn from the same isochrone, than any single-star model. From an initial sample of ∼20,000 main-sequence targets, we identify ∼2,500 binaries in which both the primary and secondary star contribute detectably to the spectrum, simultaneously fitting for the velocities and stellar parameters of both components. We additionally identify and fit ∼200 triple systems, as well as ∼700 velocity-variable systems in which the secondary does not contribute detectably to the spectrum. Our model simplifies the process of simultaneously fitting single-or multi-epoch spectra with composite models and does not depend on a velocity offset between the two components of a binary, making it sensitive to traditionally undetectable systems with periods of hundreds or thousands of years. In agreement with conventional expectations, almost all the spectrally-identified binaries with measured parallaxes fall above the main sequence in the color-magnitude diagram. We find excellent agreement between spectrally and dynamically inferred mass ratios for the ∼600 binaries in which a dynamical mass ratio can be measured from multi-epoch radial velocities. We obtain full orbital solutions for 64 systems, including 14 close binaries within hierarchical triples. We make available catalogs of stellar parameters, abundances, mass ratios, and orbital parameters.

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Section: Deriving Orbital Parametersmentioning

confidence: 99%

Discovery and characterization of 3000+ main-sequence binaries from APOGEE spectra

El-Badry

Ting

Rix

et al. 2018

Monthly Notices of the Royal Astronomical Society

112

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“…Additional science programs are also included in the survey, with one such program monitoring KOIs to search for false positives through RV variations (Fleming et al 2015). APOGEE data reach an RV precision of ∼100 m s −1 (Troup et al 2016), allowing the search for eclipsing binaries and other grazing incidence geometries that may resemble transiting planets in the initial Kepler reduction pipeline. The APOGEE survey will eventually observe ∼1050 KOIs with ≥18 epochs across five APOGEE-2 fields (roughly the size of Kepler tiles), each KOI with a sufficient signal-to-noise ratio to get quality RVs at each epoch.…”

Section: Apogee Koi Rv Samplementioning

confidence: 99%

“…where VERR_MED is the median RV measurement error from all visits and VSCATTER is the RMS scatter of all the RV measurements. Because the RV measurement errors are often underreported in APOGEE (Troup et al 2016), we choose the cutoff as the median value for the 16 known binaries in our sample, which is ∼17. After these cuts, our final sample consists of 282 KOIs (all unique PHS's), listed in Table 3.…”

Section: Selected Samplementioning

confidence: 99%

Elemental Abundances of Kepler Objects of Interest in APOGEE. I. Two Distinct Orbital Period Regimes Inferred from Host Star Iron Abundances

Wilson¹,

Teske²,

Majewski³

et al. 2018

Self Cite

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The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has observed ∼600 transiting exoplanets and exoplanet candidates from Kepler (Kepler Objects of Interest, KOIs), most with 18 epochs. The combined multi-epoch spectra are of high signal-to-noise ratio (typically 100) and yield precise stellar parameters and chemical abundances. We first confirm the ability of the APOGEE abundance pipeline, ASPCAP, to derive reliable [Fe/H] and effective temperatures for FGK dwarf stars-the primary Kepler host stellar type-by comparing the ASPCAP-derived stellar parameters with those from independent high-resolution spectroscopic characterizations for 221 dwarf stars in the literature. With a sample of 282 close-in ( < P 100 days) KOIs observed in the APOGEE KOI goal program, we find a correlation between orbital period and host star [Fe/H] characterized by a critical period, = -+ P 8.3 crit 4.1 0.1 days, below which small exoplanets orbit statistically more metalenriched host stars. This effect may trace a metallicity dependence of the protoplanetary disk inner radius at the time of planet formation or may be a result of rocky planet ingestion driven by inward planetary migration. We also consider that this may trace a metallicity dependence of the dust sublimation radius, but we find no statistically significant correlation with host T eff and orbital period to support such a claim.

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“…Notably, the closest star to our Sun, Proxima Centauri, is an M-dwarf that orbits the αCen A/B system. Our closest neighbors beyond this system are primarily of very low mass-including Barnard's star (Barnard 1916), the binary BD Luhman16 (Luhman 2013), which may even have a third companion (Boffin et al 2014), the BD WISE0855-0714 (Luhman 2014), and many others, such as the M-stars Wolf359 and Lalande21185, as well as many BDs (e.g., Wolf 1919;Ross 1926;Luyten 1979;Strauss et al 1999;Burgasser et al 2004;Burningham et al 2010;Kirkpatrick et al 2013;Troup et al 2016, and numerous others). Given their faintness, it is likely that future surveys will reveal the presence of even more nearby low-mass stars and BDs.…”

Section: Introductionmentioning

confidence: 99%

The Long-Term Dynamical Evolution of Disk-Fragmented Multiple Systems in the Solar Neighborhood

Kouwenhoven

Stamatellos

et al. 2016

ApJ

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The origin of very low-mass hydrogen-burning stars, brown dwarfs (BDs), and planetary-mass objects (PMOs) at the low-mass end of the initial mass function is not yet fully understood. Gravitational fragmentation of circumstellar disks provides a possible mechanism for the formation of such low-mass objects. The kinematic and binary properties of very low-mass objects formed through disk fragmentation at early times (<10 Myr) were discussed in our previous paper. In this paper we extend the analysis by following the long-term evolution of diskfragmented systems up to an age of 10 Gyr, covering the ages of the stellar and substellar populations in the Galactic field. We find that the systems continue to decay, although the rates at which companions escape or collide with each other are substantially lower than during the first 10 Myr, and that dynamical evolution is limited beyond 1 Gyr. By t=10 Gyr, about one third of the host stars are single, and more than half have only one companion left. Most of the other systems have two companions left that orbit their host star in widely separated orbits. A small fraction of companions have formed binaries that orbit the host star in a hierarchical triple configuration. The majority of such double-companion systems have internal orbits that are retrograde with respect to their orbits around their host stars. Our simulations allow a comparison between the predicted outcomes of disk fragmentation with the observed low-mass hydrogen-burning stars, BDs, and PMOs in the solar neighborhood. Imaging and radial velocity surveys for faint binary companions among nearby stars are necessary for verification or rejection of the formation mechanism proposed in this paper.

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Companions to Apogee Stars. I. A Milky Way-Spanning Catalog of Stellar and Substellar Companion Candidates and Their Diverse Hosts

Cited by 82 publications

References 88 publications

Discovery and characterization of 3000+ main-sequence binaries from APOGEE spectra

Discovery and characterization of 3000+ main-sequence binaries from APOGEE spectra

Elemental Abundances of Kepler Objects of Interest in APOGEE. I. Two Distinct Orbital Period Regimes Inferred from Host Star Iron Abundances

The Long-Term Dynamical Evolution of Disk-Fragmented Multiple Systems in the Solar Neighborhood

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