The stellar distribution at (l,b) = (268,0) in Vela. I - The OB associations

Slawson, Robert W.; Reed, B. Cameron

doi:10.1086/114858

Cited by 10 publications

(13 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The latter are generally bright, blue (B − V ≤ 0.13), and of small interstellar reddening, consistent with the small reddenings of E B−V ≤ 0.05 observed for stars of d ≤ 1 kpc in adjacent fields lying closer to the Galactic plane (Neckel & Klare 1980;Slawson & Reed 1988). In those fields the reddening increases beyond distances of ∼1 kpc, so we assume that the more heavily reddened B-type stars near T Ant are at least that distant.…”

Section: A Cluster Near T Antliaesupporting

confidence: 73%

“…Four, bright, early-type stars near T Ant have MK spectral types (B8 II, A0 V, A0 V, and A1 V), and their derived mean reddening of E B−V = 0.05 ± 0.01 confirms their foreground status and is consistent with the foreground reddening typical of nearby Galactic fields (Neckel & Klare 1980;Slawson & Reed 1988). The reddening near T Ant must also be relatively smooth, given the lack of any obvious patchiness in star densities, which is typical of fields containing differential reddening.…”

Section: A Cluster Near T Antliaesupporting

confidence: 69%

“…The B-star densities increase to 50% of the values in the Galactic plane between V = 11 and 12, however, whereas a decrease is expected given that fainter stars are also more distant stars, which should become less common as one views further from the main plane of the Galaxy. In Vela there is also a significant increase in extinction beyond distances of 1 kpc and the line of sight intersects at least three OB associations (Slawson & Reed 1988), so the lack of a noticeable decrease in B-star densities at faint magnitudes towards T Ant implies that the line of sight must contain one or more distant stellar groups. A distant group of B-type stars in the field of the Cepheid could provide most of the additional B-type stars detected in the present survey.…”

Section: A Cluster Near T Antliaementioning

confidence: 99%

See 2 more Smart Citations

The nature of the Cepheid T Antliae

Turner

Бердников

2003

A&A

View full text Add to dashboard Cite

Abstract. The variable star T Antliae, sometimes suspected to be a type II pulsator, is demonstrated to be a classical Cepheid in the third crossing of the instability strip. It exhibits a positive period change of +0.514 ± 0.016 s yr −1 , consistent with a star on the blue side of the instability strip and evolving through it for the third time. The Cepheid exhibits no random fluctuations in pulsation period, although superimposed upon its evolutionary O-C trend are very subtle variations that may be indicative of orbital motion about an unseen companion. Archival spectroscopic data also indicate that the star sits on the edge of a putative cluster of B-type stars that may be physically associated with the Cepheid. Additional photometric and spectroscopic data for the Cepheid and cluster are needed to strengthen the case. The field reddening of T Ant established from nearby early-type stars is E B−V = 0.30 ± 0.01 (E B−V (B0) = 0.316 ± 0.014).

show abstract

Section: A Cluster Near T Antliaesupporting

confidence: 73%

Section: A Cluster Near T Antliaesupporting

confidence: 69%

Section: A Cluster Near T Antliaementioning

confidence: 99%

See 1 more Smart Citation

The nature of the Cepheid T Antliae

Turner

Бердников

2003

A&A

View full text Add to dashboard Cite

show abstract

“…On a larger scale gamma Velorum lies in the so-called Vela complex (see Pettersson 2008;Sushch et al 2011), a very composite region characterized, inter alia, by the presence of a number of PMS clusters (e.g., gamma Velorum, Tr 10, and NGC 2547), three OB associations (Humphreys 1978;Brandt & Maran 1971;Slawson & Reed 1988) and two supernova remnants (the Gum nebula and the Vela SNR). The latter have been created by two or more supernovae explosions that occurred 1-6 Myr and 11 400 yr ago (Pettersson 2008).…”

Section: The Gamma Velorum Open Clustermentioning

confidence: 99%

TheGaia-ESO Survey: the first abundance determination of the pre-main-sequence cluster gamma Velorum

Spina

Randich

Palla

et al. 2014

A&A

View full text Add to dashboard Cite

Context. Knowledge of the abundance distribution of star forming regions and young clusters is critical to investigate a variety of issues, from triggered star formation and chemical enrichment by nearby supernova explosions to the ability to form planetary systems. In spite of this, detailed abundance studies are currently available for relatively few regions. Aims. In this context, we present the analysis of the metallicity of the gamma Velorum cluster, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods. The gamma Velorum candidate members have been observed with FLAMES, using both UVES and Giraffe, depending on the target brightness and spectral type. In order to derive a solid metallicity determination for the cluster, membership of the observed stars must be first assessed. To this aim, we use several membership criteria including radial velocities, surface gravity estimates, and the detection of the photospheric lithium line. Results. Out of the 80 targets observed with UVES, we identify 14 high-probability members. We find that the metallicity of the cluster is slightly subsolar, with a mean [Fe/H] = −0.057 ± 0.018 dex. Although J08095427-4721419 is one of the high-probability members, its metallicity is significantly larger than the cluster average. We speculate about its origin as the result of recent accretion episodes of rocky bodies of ∼60 M ⊕ hydrogen-depleted material from the circumstellar disk.

show abstract

“…Vel OB1 is one of the largest OB associations known : based on HumphreysÏs derived mean distance of 1690 pc and angular extent (l \ 262¡ to 268¡, to one infers linear dimensions of some b \ [2¡ .7 ]1¡ .4), 180 by 120 pc in longitude by latitude. A hint that Vel OB1 may be more populous than indicated by Humphreys emerged from the work of Slawson & Reed (1988), who concluded on the basis of photographic photometry that several stars not listed by her (among others, CaseHamburg southern luminous stars [LS] 1211[LS] , 1216[LS] , 1233[LS] , 1236[LS] , and 1238Stephenson & Sanduleak 1971) are also likely members. The general vicinity of Vel OB1 appears to be quite rich in stellar aggregations, as three small open clusters also lie in this general direction : Pismis 6 [(l, b) \ (265¡, [3¡) ; r \ 1.65 kpc], Markarian 18 [(l, b) \ (269¡, [2¡) ; r \ 1.61 kpc] (both Vogt &Mo †at 1973), andNGC 2659 [(l, b) \ (264¡, [2¡) ; r \ 1.45 kpc] (Stetson 1981).…”

Section: Introductionmentioning

confidence: 99%

Vela OB1: Probable New Members and Hertzsprung-Russell Diagram

Reed

2000

The Astronomical Journal

Self Cite

View full text Add to dashboard Cite

Several dozen stars are identiÐed as probable previously unrecognized members of the association Vel OB1, including the Vela X-1 binary pulsar system. Based on a variable extinction analysis of 70 stars, the distance and ratio of total to selective absorption of the association are determined to be 1750 pc and 3.70, respectively. Vel OB1 may be signiÐcantly larger than previously appreciated, perhaps up to 600 by 300 pc in the sense of longitude by latitude. This physical extent, and the fact that the H-R diagram includes both low-mass evolved yellow supergiants and massive, early-type supergiants, indicates that Vel OB1 is probably not coeval.

show abstract

The stellar distribution at (l,b) = (268,0) in Vela. I - The OB associations

Cited by 10 publications

References 0 publications

The nature of the Cepheid T Antliae

The nature of the Cepheid T Antliae

TheGaia-ESO Survey: the first abundance determination of the pre-main-sequence cluster gamma Velorum

Vela OB1: Probable New Members and Hertzsprung-Russell Diagram

Contact Info

Product

Resources

About