An Interferometric and Spectroscopic Analysis of the Multiple Star System Hd 193322

Brummelaar, Theo A. ten; O’Brien, D. P.; Mason, Brian D.; Farrington, Christopher D.; Fullerton, A. W.; Gies, Douglas R.; Grundstrom, Erika D.; Harkopf, William I.; Matson, Rachel A.; McAlister, Harold A.; McSwain, M. Virginia; Roberts, Lewis C.; Schaefer, Gail H.; Simón‐Díaz, S.; Sturmann, J.; Sturmann, L.; Turner, N.; Williams, Stephen J.

doi:10.1088/0004-6256/142/1/21

Cited by 20 publications

(9 citation statements)

References 37 publications

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“…A blend is indicated by the second derivative test and we used the y-scan magnitude difference and second derivative amplitude to find |△x|. The solution using −|△x| is listed in Table 2, and the separation and position angle estimates agree well with contemporaneous CHARA Array measurements (ten Brummelaar et al 2011). 201851.71+381646.5 = HD193443A. This system appears in the WDS with the brighter component identified as B, so we added 180 • to the position angle and changed the sign of △m for consistency with the results in the WDS.…”

mentioning

confidence: 87%

“…These studies also demonstrate the high incidence of binaries and multiples among longer period systems. However, because of the great distances of most massive stars, there still exists a significant observational gap in our knowledge of binaries with periods of years to centuries that have radial velocity variations that are too small to measure or angular separations that are only resolvable with optical long baseline interferometry (Kraus et al 2009;ten Brummelaar et al 2011;Sana et al , 2014. It is critical to fill in this gap with new observations in order to determine the nature of the period distribution and to estimate the total binary frequency (Sana et al 2013b).…”

Section: Introductionmentioning

confidence: 99%

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THE MULTIPLICITY OF MASSIVE STARS: A HIGH ANGULAR RESOLUTION SURVEY WITH THEHSTFINE GUIDANCE SENSOR

Aldoretta¹,

Caballero-Nieves²,

Gies³

et al. 2014

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mentioning

confidence: 87%

Section: Introductionmentioning

confidence: 99%

THE MULTIPLICITY OF MASSIVE STARS: A HIGH ANGULAR RESOLUTION SURVEY WITH THEHSTFINE GUIDANCE SENSOR

Aldoretta¹,

Caballero-Nieves²,

Gies³

et al. 2014

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“…′′ 05-0. ′′ 07 and follow a 35 a orbit (ten Brummelaar et al 2011;Maíz Apellániz 2010). ten Brummelaar et al (2011) have used multiple-epoch high-resolution spectroscopy to analyze the AaAb system, determining a spectral type of O9 Vnn for Aa and that Ab is an SB2 system with spectral types of O8.5 III and B2.5: V:.…”

Section: Revisiting the Northern Sample From Paper Imentioning

confidence: 99%

The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars

Sota,

Apellániz,

Morrell

et al. 2013

Preprint

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We present the second installment of GOSSS, a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R ∼ 2500 digital observations from both hemispheres selected from the Galactic O-Star Catalog (GOSC). In this paper we include bright stars and other objects drawn mostly from the first version of GOSC, all of them south of δ = −20 • , for a total number of 258 O stars. We also revise the northern sample of paper I to provide the full list of spectroscopically classified Galactic O stars complete to B = 8, bringing the total number of published GOSSS stars to 448. Extensive sequences of exceptional objects are given, including the early Of/WN, O Iafpe, Ofc, ON/OC, Onfp, Of?p, and Oe types, as well as double/triple-lined spectroscopic binaries. The new spectral subtype O9.2 is also discussed. The magnitude and spatial distributions of the observed sample are analyzed. We also present new results from OWN, a multi-epoch high-resolution spectroscopic survey coordinated with GOSSS that is assembling the largest sample of Galactic spectroscopic massive binaries ever attained. The OWN data combined with additional information on spectroscopic and visual binaries from the literature indicate that only a very small fraction (if any) of the stars with masses above 15-20 M ⊙ are born as single systems. In the future we will publish the rest of the GOSSS survey, which is expected to include over 1000 Galactic O stars.

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“…In this case, the wider pair is a known speckle binary appropriate for speckle interferometry and SFP solutions. An orbital analysis of both systems from speckle interferometry, SFP work, baseline/visibilty interferometry data as well as spectroscopy has recently been presented (ten Brummelaar et al 2011). This orbit is also plotted in Figure 3.…”

Section: Chara Arraymentioning

confidence: 99%

“Visual” orbit solutions from observing techniques old and new

Mason¹

2012

AIP Conference Proceedings

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For the past couple of decades, the primary double star observational technique utilized at the US Naval Observatory has been speckle interferometry. Our two speckle cameras have been used on a variety of telescopes: our 26 ′′ in Washington, the USNO (NOFS) 61 ′′ , the McDonald 82 ′′ , the Mt. Wilson 100 ′′ and the twin 4 meter telescopes of KPNO and CTIO. While these instruments have each yielded many observations, they have been involved in rather different programs, with the 26 ′′ observing primarily the so-called "neglected" pairs and larger instruments conducting duplicity surveys and observing close, astrophysically interesting systems.While speckle is quite successful at resolving relatively close pairs, for those pairs which are both bright and very close long baseline optical interferometry may be the only viable solution. Utilizing both the CHARA Array and the Navy Prototype Optical Interferometer, numerous hard-to-observe pairs first resolved by speckle have been observed using these arrays' superior resolution capabilities; this has allowed these orbits to be significantly improved; examples of pairs observed by each of these instruments are presented.At the other separation extreme, a cache of photographic plates taken with the USNO double star camera has been digitized and processed. Some 66 plates of Sirius A and B taken between 1970 and 1984, which represents a 10% increase in the total number of measures, have been reduced, enabling a significant improvement over the current "best" Sirius orbit, almost one full revolution later. 26 ′′ Speckle ObservingDue to its modest aperture, our capability to observe orbital motion pairs of astrophysical signicance is quite limited. As a result, in 2000 the program shifted over to pairs that were unconfirmed or had not been observed in a decade or more. These we defined as "neglected". The eventual goal is the characterizing of pairs as either optical or physical. This definition was adopted by many others and has formed a productive operational observing program for us and other groups allowing the re-invigoration of observing programs with limited access to large telescopes. To date we have obtained 24,707 mean positions with our speckle camera on the 26 ′′ telescope in Washington. As a measure of our success observing these neglected pairs (as well as others with similar programs), the number of mean positions per system in the WDS has increased from 5.8 to 7.1 despite the number of new systems (n = 1) increasing by 36,852 pairs. Historically, when we obtained access to larger telescopes and observed off-base, 26 ′′ observing would shut down for approximately a month. Due to the success of of our 26 ′′ neglected doubles program, a second camera for use with our older ICCD was constructed in-house (Mason et al. 2007) and our primary camera has since been used when we have had access to larger telescopes, simultaneous with continued 26 ′′ operation with our secondary camera.

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An Interferometric and Spectroscopic Analysis of the Multiple Star System Hd 193322

Cited by 20 publications

References 37 publications

THE MULTIPLICITY OF MASSIVE STARS: A HIGH ANGULAR RESOLUTION SURVEY WITH THEHSTFINE GUIDANCE SENSOR

THE MULTIPLICITY OF MASSIVE STARS: A HIGH ANGULAR RESOLUTION SURVEY WITH THEHSTFINE GUIDANCE SENSOR

The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars

“Visual” orbit solutions from observing techniques old and new

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