2007
DOI: 10.1051/0004-6361:20066654
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Pre-main-sequence stars in the young open cluster NGC 1893

Abstract: Context. The open cluster NGC 1893 illuminating the H ii region IC 410 contains a moderately large population of O-type stars and is one of the youngest clusters observable in the optical range. It is suspected of harbouring a large population of pre-main-sequence (PMS) stars. Aims. We have probed the stellar population of NGC 1893 in an attempt to determine its size and extent. In particular, we look for signs of sequential star formation. Methods. We classify a large sample of cluster members with new interm… Show more

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Cited by 24 publications
(43 citation statements)
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“…There are nine new candidate late-O and B-type stars, although two of them (MOBc NGC 1893 4 & 5) may be foreground A-type stars (Table 3). None lie in dense cluster cores or are associated with optical nebulosity, and most appear to trace the extended OB population reported by Negueruela et al (2007). The most luminous OB candidate is MOBc NGC 1893 9, located toward the edge of the field beside a prominent pillar that does not appear to know about this star (Figure 2r).…”
Section: A13 Ngc 1893mentioning
confidence: 81%
“…There are nine new candidate late-O and B-type stars, although two of them (MOBc NGC 1893 4 & 5) may be foreground A-type stars (Table 3). None lie in dense cluster cores or are associated with optical nebulosity, and most appear to trace the extended OB population reported by Negueruela et al (2007). The most luminous OB candidate is MOBc NGC 1893 9, located toward the edge of the field beside a prominent pillar that does not appear to know about this star (Figure 2r).…”
Section: A13 Ngc 1893mentioning
confidence: 81%
“…To separate both populations, we used (when available) the spectrophotometric analysis previously described, obtaining the corresponding color excesses and spectrophotometric distances. For stars without spectral classification, we used all the photometric diagrams and the reddening-free photometric parameter Q NIR = (J − H) − 1.7(H − K) (Negueruela et al 2007) to avoid the intrinsic degeneracy between reddening and spectral type. In In our procedure, we adopted as cluster members those stars that were placed approximately redder than an adopted consistent MS (red curve) along all the photometric diagrams.…”
Section: Photometric Diagramsmentioning
confidence: 99%
“…If a cluster is embedded in a cloud which produces much of the extinction along the line of sight to the cluster, we would not only get a contribution to differential extinction from the angular position of each star, but also from its distance, as more distant stars would be, on average, more heavily extinguished. We attempt to negate the effect of differential reddening by employing the reddening free parameter Q = (J − H) − 1.70(H − K S ), as defined by Negueruela et al (2007) for OB stars (see also Catelan et al 2011, for a list of several other reddeningfree indices, in the ZYJHK system). We chose this parameter in order to avoid the intrinsic degeneracy between reddening and spectral type (and since we expect to find early OB stars in the majority of the clusters in our sample).…”
Section: Parameters Of Some Vvv Cluster Candidatesmentioning
confidence: 99%
“…7 shows this reddening free parameter vs. K S magnitude. According to Negueruela et al (2007) the OB stars will have 8.3 ± 0.5 10.7 ± 0.7 1.4 ± 0.5 400 ± 50 VVV CL009 4.5 ± 0.3 11.9 ± 0.6 2.4 ± 0.5 200 ± 40 VVV CL039…”
Section: Parameters Of Some Vvv Cluster Candidatesmentioning
confidence: 99%