The Distance to the S Dor Type Star HR Carinae

Genderen, A. M. van; Robijn, F. H. A.; Esch, B.P.M. van; Lamers, H. J. G. L. M.

doi:10.1007/978-94-011-3306-7_108

Cited by 11 publications

(19 citation statements)

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“…2MASS J10224377-5930182 = [VRV91] 85. This object is located in the little-studied open cluster [KPS2012] MWSC 1797 (Kharchenko et al 2013) and was classified as B0:V by van Genderen et al (1991). We observed it with GOSSS and we found it is an O8V(n), which is the first time it has been identified as an O star.…”

Section: New Systems In Gosssmentioning

confidence: 73%

“…We placed the nearby star Hen 3-406 on the slit and found is an early-type Be star. Note that van Genderen et al (1991) incorrectly claimed that Hen 3-406 was an O-type dwarf.…”

Section: New Systems In Gosssmentioning

confidence: 99%

“…2MASS J10224096-5930305 = [VRV91] 82. This object is also located in [KPS2012]MWSC1797 and it was classified as OV: by van Genderen et al (1991). The GOSSS spectral type is O7V((f))z.…”

Section: New Systems In Gosssmentioning

confidence: 99%

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The Galactic O-Star Spectroscopic Survey (Gosss). Iii. 142 Additional O-Type Systems*

Apellániz

Sota

Arias

et al. 2016

ApJS

133

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This is the third installment of theGalactic O-Star Spectroscopic Survey (GOSSS), a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R∼2500 digital observations selected from the Galactic O-Star Catalog. In this paper, we present 142 additional stellar systems with O stars from both hemispheres, bringing the total of O-type systems published within the project to 590. Among the new objects, there are 20 new O stars. We also identify 11 new double-lined spectroscopic binaries, 6of whichare of O+O type and 5 of O+B type, and an additional new tripled-lined spectroscopic binary of O+O+B type. We also revise some of the previous GOSSS classifications, present some egregious examples of stars erroneously classified as O-type in the past, introduce the use of luminosity class IV at spectral types O4-O5.5, and adapt the classification scheme to the work of Arias et al.

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Section: New Systems In Gosssmentioning

confidence: 73%

“…We placed the nearby star Hen 3-406 on the slit and found is an early-type Be star. Note that van Genderen et al (1991) incorrectly claimed that Hen 3-406 was an O-type dwarf.…”

Section: New Systems In Gosssmentioning

confidence: 99%

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The Galactic O-Star Spectroscopic Survey (Gosss). Iii. 142 Additional O-Type Systems*

Apellániz

Sota

Arias

et al. 2016

ApJS

133

View full text Add to dashboard Cite

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“…HR Car: The distance adopted in the literature for HRCar is usually 5±1 kpc (e.g., van Genderen et al 1991;Groh et al 2009a), placing it among the low-luminosity group of LBVs (see, e.g., Smith et al 2004). The Gaia distance in Table 1 is 2.92±2.04 kpc (π=0.34±0.24 mas) or 2.27±0.97 kpc (π=0.44±0.19 mas) according to the ABJ parallaxes, which is lower than previously assumed, but the 95% upper limit of 4.6 kpc is arguably consistent with the usual estimate.…”

Section: Hd168607mentioning

confidence: 99%

The Canonical Luminous Blue Variable AG Car and Its Neighbor Hen 3-519 Are Much Closer than Previously Assumed

Smith

Stassun

2017

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The strong mass loss of Luminous Blue Variables (LBVs) is thought to play a critical role in massive-star evolution, but their place in the evolutionary sequence remains debated. A key to understanding their peculiar instability is their high observed luminosities, which often depends on uncertain distances. Here we report direct distances and space motions of four canonical Milky Way LBVs-AGCar, HRCar, HD168607, and (candidate) Hen3-519-from the Gaia first data release. Whereas the distances of HRCar and HD168607 are consistent with previous literature estimates within the considerable uncertainties, Hen3-519 and AGCar, both at ∼2 kpc, are much closer than the 6-8 kpc distances previously assumed. As a result, Hen3-519 moves far from the locus of LBVs on the Hertzsprung-Russell diagram, making it a much less luminous object. For AGCar, considered a defining example of a classical LBV, its lower luminosity would also move it off the SDor instability strip. Lower luminosities allow both AGCar and Hen3-519 to have passed through a previous red supergiant phase, lower the mass estimates for their shell nebulae, and imply that binary evolution is needed to account for their peculiarities. These results may also impact our understanding of LBVs as potential supernova progenitors and their isolated environments. Improved distances will be provided in the Gaia second data release, which will include additional LBVs. AGCar and Hen3-519 hint that this new information may alter our traditional view of LBVs.

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“…The light variability of HD 10783 was detected by Van Genderen (1964) who preferred the value 4.1565 d of the period to the value 4.134 d derived by Steinitz (1964) from the analysis of Babcock's (1958) effective magnetic field data. UBV photometry and magnetic field measurements were carried out by Preston & Stepien (1968), who refined the period to the value 4.1327 d. Additional photometric observations by Van Genderen (1967, 1971 have shown the photometric period to be consistent with the value determined by Preston & Stepien (1968).…”

Section: Hd 10783 = Gc 2141 = Uz Pscmentioning

confidence: 99%