Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars

By Lewis C. Roberts Jr., N. Turner, T. T. ten Brummelaar. 2005

280 citations recorded by the source corpus.

We carried out a search for companions to B stars using the adaptive optics system of the Advanced Electro-Optical System 3.6 m telescope. We observed 70 B stars in the I band, finding 16 companions, 10 of which are newly discovered companions. For each system with a detected companion we give its measured astrometry and differential magnitude. We then put the observation in context of the system's known multiplicity and provide a somewhat crude estimate of its spectral type based on the single differential magnitude measurement. The separations range from 0.2″ to 7.31″, and the differential magnitudes range from 1.41 ± 0.01 to 10.1 ± 0.5. Finally, we present a list of the null detections and discuss the implications of null detections of selected stars.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Biomedical Engineering

View Paper: https://www.semanticscholar.org/paper/6b94e7f281b121959a0001bfdca70be63f55f5d3

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In Astronomy and Astrophysics

1. A. Tokovinin
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6. Mark R. Krumholz
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In Atomic and Molecular Physics, and Optics

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In Biomedical Engineering

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Citations in the corpus

• Stellar Multiplicity (2013, background): “A consensus has emerged that the frequency of visual companions over two decades in projected separations is ∼ 45±5% (e.g., Peter et al. 2012, Turner et al. 2008).”
• The relation between the most-massive star and its parental star cluster mass (2009, background): “…stars (20% to 80%, Garmany et al. 1980; Garćıa & Mermilliod 2001; De Becker et al. 2006; Kiminki et al. 2007; Lucy 2006; Apai et al. 2007; Sana et al. 2008; Turner et al. 2008; Weidner et al. 2009), the effect of un-resolved binaries is smaller for the mass estimate than for the number estimate.”
• THE GALACTIC O-STAR SPECTROSCOPIC SURVEY (GOSSS). II. BRIGHT SOUTHERN STARS (2013, unknown): “′′26 and a ∆m of 1.6 mag (Turner et al. 2008; Máız Apellániz 2010).”
• Debris Disks in Main-Sequence Binary Systems (2006, background): “—HD 99028 is a triple system, with inner orbital distance of 1.9 AU (Söderhjelm 1999) and outer orbital radius 20 AU (Roberts et al. 2005).”
• A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS (2013, background): “The star appears single in speckle (Mason et al. 1997) and AO observations (Roberts et al. 2007).”
• THE HIGH ANGULAR RESOLUTION MULTIPLICITY OF MASSIVE STARS (2008, methodology): “This represents the sum of the number of close components found by speckle interferometry, wider and fainter components found by Turner et al. (2008b) in an adaptive optics survey, and other (usually wider) components listed in the WDS (Mason et al. 2001).”
• The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, methodology): “Gr ater sensitivity to fainter companion has been achieved using adaptive optics (AO) surveys (e.g. Roberts et al. 2007); however, the sample was magnitude- limited, introducing a potential selection bias.”
• OBSERVATIONS OF HIERARCHICAL SOLAR-TYPE MULTIPLE STAR SYSTEMS (2015, methodology): “Photometric error bars were assigned using the technique described in Roberts et al. (2005).”
• The MiMeS survey of Magnetism in Massive Stars : magnetic analysis of the O-type stars (2016, background): “The B, C and D components are found at angular separations greater than 2.68 arcsec and are not observed as part of our spectra (Turner et al. 2008).”
• THE GALACTIC O-STAR SPECTROSCOPIC SURVEY. I. CLASSIFICATION SYSTEM AND BRIGHT NORTHERN STARS IN THE BLUE-VIOLET AT R ∼ 2500 (2011, result): “…the literature for results similar to those obtained with AstraLux (e.g. McCaughrean & Stauffer 1994; Duchêne et al. 2001; Mason et al. 1998; Turner et al. 2008; Bouy et al. 2008; Mason et al. 2009) and we plotted information from Simbad using Aladin images to ensure the correct…”
• SOUTHERN MASSIVE STARS AT HIGH ANGULAR RESOLUTION: OBSERVATIONAL CAMPAIGN AND COMPANION DETECTION (2014, methodology): “′′12 (Turner et al. 2008), NACO/ SAM resolved a new faint companion at 36 mas with ΔH ≈ 4.0, i.e., too faint to be confirmed by PIONIER.”