Carbon star luminosity indicators

Green, Paul; Margon, B.; Anderson, Scott F.; MacConnell, D. J.

doi:10.1086/172027

Cited by 36 publications

(61 citation statements)

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“…Their estimate of the proper motion is consistent with the new, longer baseline measurement in Table 1. 3.6 KA-2 Ratnatunga (1983) first proposed that this object might be a dwarf carbon star. However, Green et al (1992) noted that their proper-motion measurement has the same magnitude but opposite sign as that reported in Ratnatunga (1983). The magnitude in both papers and the direction of Ratnatunga (1983) is consistent with the proper motion derived here to well within the 1 cr error quoted in Table 1.…”

Section: Pg 0824+289mentioning

confidence: 70%

“…However, high proper motions and trigonometric parallax measurements (Dahn et al 1977) showed that the carbon star G 77-61 has the luminosity of a main-sequence dwarf. In recent years, more faint carbon stars have been shown to have measurable proper motion and dwarf star luminosities (Green et al 1991(Green et al , 1992Heber et al 1993;Warren et al 1993;Liebert et al 1994). …”

Section: Introductionmentioning

confidence: 99%

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Positions and proper motions of dwarf carbon stars

Deutsch¹

1994

PASP

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Section: Pg 0824+289mentioning

confidence: 70%

Section: Introductionmentioning

confidence: 99%

Positions and proper motions of dwarf carbon stars

Deutsch¹

1994

PASP

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“…It is a spectroscopic binary and mass transfer is a likely explanation for it (Dearborn et al, 1986). Additional examples have now been found Green et al, 1992;Warren et al, 1993). An abundance analysis of G77-61 (Gass et al, 1988) indicates that the dwarf carbon stars may not be simply cool close relatives of the barium F and G main sequence stars.…”

Section: Barium and Related Starsmentioning

confidence: 89%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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“…c No JHK photometry is available for this object as it is fainter than the 2MASS survey limit. Dwarf carbon stars exhibit a spectral signature which mimics that of a typical CH-type giant carbon star, however they have anomalous JHK colors (Green et al 1992) and high proper motions. The existence of the 4300 Å CH G band is representative of a CH-type carbon star and is found in all five of our carbon stars.…”

Section: Carbon Starsmentioning

confidence: 99%

Kinematics and Chemistry of Halo Substructures: The Vicinity of the Virgo Overdensity

Casey

Keller

Costa

2012

The Astronomical Journal

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We present observations obtained with the Anglo-Australian Telescope's 2dF wide field spectrograph AAOmega of K-type stars located within a region of the sky which contains the Virgo Overdensity and the leading arm of the Sagittarius Stream. On the basis of the resulting velocity histogram, we isolate halo substructures in these overlapping regions including Sagittarius and previously discovered Virgo groups. Through comparisons with N-body models of the Galaxy-Sagittarius interaction, we find a tri-axial dark matter halo is favored and we exclude a prolate shape. This result is contradictory with other observations along the Sagittarius leading arm, which typically favor prolate models. We have also uncovered K-giant members of Sagittarius that are notably more metal-poor ( [Fe/H] = −1.7 ± 0.3 dex) than previous studies. This suggests a significantly wider metallicity distribution exists in the Sagittarius Stream than formerly considered. We also present data on five carbon stars which were discovered in our sample.

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Carbon star luminosity indicators

Cited by 36 publications

References 0 publications

Positions and proper motions of dwarf carbon stars

Positions and proper motions of dwarf carbon stars

Synthesis of the elements in stars: forty years of progress

Kinematics and Chemistry of Halo Substructures: The Vicinity of the Virgo Overdensity

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