Two nearby M dwarf binaries from the Two Micron All Sky Survey

Gizis, John E.; Monet, D. G.; Reid, I. Neill; Kirkpatrick, J. Davy; Burgasser, Adam J.

doi:10.1046/j.1365-8711.2000.03060.x

Cited by 43 publications

(7 citation statements)

References 19 publications

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“…This would make them analogs of the GJ 1245ABC triple system, which consists of two M5.5 and one ∼M8 dwarfs (Reid et al 1995, Henry et al 1999) with separations of 32 and 5 AUs (McCarthy et al 1988). We note that Gizis et al (2000b) discovered a 230 AU VLM binary in the field, LP 213-67 (M6.5) and LP 213-68 (M8.0), which in the recent adaptive optics survey of Close et al (2003) turned out to be triple when LP 213-67AB (or 2MASS J1047+4026) was resolved into two components (see Fig. 5).…”

Section: Discussionmentioning

confidence: 69%

Discovery of a widely separated binary system of very low mass stars

Phan-Bao¹,

Martín

Reylé³

et al. 2005

A&A

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Abstract. We report our discovery of a nearby wide binary system, LP 714-37 AB. Phan-Bao et al. identified LP 714-37 as a mid-M dwarf during a cross-identification of the NLTT and DENIS catalogues. Our CCD images resolve the system into a binary with a projected angular separation of 1.8 , or 33 AU, and low-resolution optical spectra give spectral types of M5.5 (LP 714-37A) and M7.5 (LP 714-37B). This makes LP 714-37 AB one of very few widely separated (separation >30 AU) very low-mass binary systems known in the field, and we discuss it in the context of the multiplicity properties of very low-mass stars and brown dwarfs.

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Section: Discussionmentioning

confidence: 69%

Discovery of a widely separated binary system of very low mass stars

Phan-Bao¹,

Martín

Reylé³

et al. 2005

A&A

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“…Tables 6 and 7 present the results. Table 6 lists nine dwarfs with previous spectroscopic observations, including LHS 2090, an M6.5 dwarf recently identified as lying within the 8-parsec sample ; LP 944-20, the nearest isolated brown dwarf ; four dwarfs from the ultracool 2MASS sample selected by Gizis et al (1999); and an earlier type dwarf, LP 860-46, which appears coincident with one of the brighter stars in Ardila et al's (2001) U Sco photometric survey. Table 7 collects data for a further 42 ultracool dwarfs selected from our current sample based on the 2MASS photometry.…”

Section: Late-type Dwarfsmentioning

confidence: 97%

Meeting the Cool Neighbors. I. Nearby Stars in the NLTT Catalogue: Defining the Sample

Reid¹,

Cruz²

2002

The Astronomical Journal

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We are currently undertaking a program aimed at identifying previouslyunrecognised late-type dwarfs within 20 parsecs of the Sun. As a first step, we have cross-referenced Luyten's NLTT proper motion catalogue against the second incremental release of the 2MASS Point Source Catalogue, and use optical/infrared colours, derived by combining Luytens's m r estimates with 2MASS data, to identify candidate nearby stars. This paper describes the definition of a reference sample of 1245 stars, and presents a compilation of literature data for over one-third of the sample. Only 274 stars have trigonometric parallax measurements, but we have used data for nearby stars with well-determined trigonometric parallaxes to compute colour-magnitude relations in the (M V , (V-K)), (M V , (V-I)) and (M I , (I-J)) planes, and use those relations to determine photometric parallaxes for NLTT stars with optical photometry. Based on the 2MASS JHK S data alone, we have identified a further 42 ultracool dwarfs ((J-K S > 0.99) and use (J-K S ) colours to estimate photometric parallaxes. Combining these various techniques, we identify 308 stars with formal distances of less than 20 parsecs, while a further 46 have distance estimates within 1σ of our survey limit. Of these 354 stars, 75, including 39 of the ultracool dwarfs. are new to nearby star catalogues. Two stars with both optical and near-infrared photometry are potential additions to the immediate Solar Neighbourhood, with formal distance estimates of less than 10 parsecs.In the near future, 2MASS will provide broadband J, H and K s photometry for sources over the full celestial sphere. The J and H passbands match the standard Johnson system, while the K s passband, truncated at long wavelengths to avoid terrestial H 2 O absorption, is described and calibrated by Persson et al. (1998). The effective wavelength of the K S filter is 2.15µm, as opposed to 2.19µm for the standard system, but Carpenter's (2001) analysis reveals only minor differences with respect to standard systems. In particular, Carpenter findsThese differences are negligible compared with other sources of uncertainty in the present analysis, and we adopt the convention K S =K in this series of papers.The 2MASS catalogue includes sources which have a signal-to-noise ratio exceeding 7, corresponding to typical limiting magnitudes of J∼ 16.1, H∼ 15.2 and K s ∼ 14.9 in uncrowded fields. M dwarfs within 20 parsecs have near-infrared magnitudes significantly brighter than these limits -for example, even an M9.5 dwarf, comparable to BRI0021 or LP 944-20, has M K ∼ 11.1, or K s ∼ 12.6 at a distance of 20 parsecs. At those magnitudes, the typical photometric uncertainties are 0.02-0.04 magnitudes.2MASS survey observations were completed in early 2001, but at the time of writing, data are available publicly for only 46.5% of the sky via the second incremental release. The results described in this paper, and in subsequent papers in the series, rest on the latter dataset. In addition to photometry, the catalogue provides astromet...

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“…HD 86728 = HIP 49081: Gizis et al (2000) suggest that the B component is an unresolved binary (Ba/Bb) owing to the anomalous brightness and sustained magnetic activity of B. However, Bb has not yet been detected spectroscopically or resolved by imaging observations, so its existence is speculative.…”

Section: Appendix B Notes On Binary Companionsmentioning

confidence: 99%

Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc

Hirsch

Rosenthal

Fulton

et al. 2021

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We explore the impact of outer stellar companions on the occurrence rate of giant planets detected with radial velocities. We searched for stellar and planetary companions to a volume-limited sample of solar-type stars within 25 pc. Using adaptive optics imaging observations from the Lick 3 m and Palomar 200″ Telescopes, we characterized the multiplicity of our sample stars, down to the bottom of the main sequence. With these data, we confirm field star multiplicity statistics from previous surveys. We additionally combined three decades of radial velocity (RV) data from the California Planet Search with newly collected RV data from Keck/HIRES and the Automated Planet Finder/Levy Spectrometer to search for planetary companions in these same systems. Using an updated catalog of both stellar and planetary companions, as well as detailed injection/recovery tests to determine our sensitivity and completeness, we measured the occurrence rate of planets among the single-and multiple-star systems. We found that planets with masses in the range of 0.1-10 M J and with semimajor axes of 0.1-10 au have an occurrence rate of -+ 0.18 0.03 0.04 planets per star when they orbit single stars and an occurrence rate of 0.12 ± 0.04 planets per star when they orbit a star in a binary system. Breaking the sample down by the binary separation, we found that only one planet-hosting binary system had a binary separation <100 au, and none had a separation <50 au. These numbers yielded planet occurrence rates of -+ 0.20 0.06 0.07 planets per star for binaries with separation a B > 100 au and -+ 0.04 0.02 0.04 planets per star for binaries with separation a B < 100 au. The similarity in the planet occurrence rate around single stars and wide primaries implies that wide binary systems should actually host more planets than single-star systems, since they have more potential host stars. We estimated a system-wide planet occurrence rate of 0.3 planets per wide binary system for binaries with separations a B > 100 au. Finally, we found evidence that giant planets in binary systems have a different semimajor-axis distribution than their counterparts in single-star systems. The planets in the single-star sample had a significantly higher occurrence rate outside of 1 au than inside 1 au by nearly 4σ, in line with expectations that giant planets are most common near the snow line. However, the planets in the wide binary systems did not follow this distribution, but rather had equivalent occurrence rates interior and exterior to 1 au. This may point to binary-mediated planet migration acting on our sample, even in binaries wider than 100 au.

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Two nearby M dwarf binaries from the Two Micron All Sky Survey

Cited by 43 publications

References 19 publications

Discovery of a widely separated binary system of very low mass stars

Discovery of a widely separated binary system of very low mass stars

Meeting the Cool Neighbors. I. Nearby Stars in the NLTT Catalogue: Defining the Sample

Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc

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