Open clusters in Auriga OB2

Marco, A.; Negueruela, I.

doi:10.1093/mnras/stw640

Cited by 11 publications

(34 citation statements)

References 82 publications

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“…The specifications of the camera are given in Casali et al (2007). The total exposure time for each filter is 40 s. The procedure for obtaining the instrumental photometry and carry out the transformation from these instrumental magnitudes to the 2MASS magnitude system (Skrutskie et al 2006) is the same that we implemented in section 2.2 of Marco & Negueruela (2016). We obtained photometry for 2365 stars.…”

Section: Optical Photometry and Near-ir Photometrymentioning

confidence: 99%

The little-studied cluster Berkeley 90 – III. Cluster parameters

Marco

Negueruela

2016

Mon. Not. R. Astron. Soc.

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The open cluster Berkeley 90 is the home to one of the most massive binary systems in the Galaxy, LS III +46 • 11, formed by two identical, very massive stars (O3.5 If* + O3.5 If*), and a second early-O system (LS III +46 • 12 with an O4.5 IV((f)) component at least). Stars with spectral types earlier than O4 are very scarce in the Milky Way, with no more than 20 examples. The formation of such massive stars is still an open question today, and thus the study of the environments where the most massive stars are found can shed some light on this topic. To this aim, we determine the properties and characterize the population of Berkeley 90 using optical, near-infrared and WISE photometry and optical spectroscopy. This is the first determination of these parameters with accuracy. We find a distance of 3.5 +0.5 −0.5 kpc and a maximum age of 3 Ma. The cluster mass is around 1 000 M (perhaps reaching 1 500 M if the surrounding population is added), and we do not detect candidate runaway stars in the area. There is a second population of young stars to the Southeast of the cluster that may have formed at the same time or slightly later, with some evidence for low-activity ongoing star formation.

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Section: Optical Photometry and Near-ir Photometrymentioning

confidence: 99%

The little-studied cluster Berkeley 90 – III. Cluster parameters

Marco

Negueruela

2016

Mon. Not. R. Astron. Soc.

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“…The site S234 (IC 417) harbors a nebulous stream (or filamentary structure) and a young cluster "Stock 8" (Jose et al 2008;Marco & Negueruela 2016). Previous works also reported the presence of a dust shell lying between the nebulous stream and Stock 8 (see Figures 1 and 9 in Marco & Negueruela 2016), which was also found to be associated with the ionized emission (e.g. Jose et al 2008).…”

Section: Introductionmentioning

confidence: 96%

“…These authors also suggested that the site S234 is powered by a star LS V +34 • 23 (HD 35633), with a spectral type of O8 II(f). Jose et al (2008) and Marco & Negueruela (2016) reported a stream of embedded sources and an obscured cluster (i.e. CC 14) toward the nebulous stream, and suggested the ongoing star formation activity in the site S234.…”

Section: Introductionmentioning

confidence: 98%

“…The sub-mm map at 250 µm shows extended structures in these sites (see Figure 1a). The sites S234, V582, and S237 are situated at distances of 2.8 kpc (Marco & Negueruela 2016;Kun et al 2017), 1.3 kpc (Kun et al 2017;Ábrahám et al 2018), and 2.3 kpc (Pandey et al 2013;Dewangan et al 2017a), respectively. The CO radial velocities of the sites S234, V582, and S237 were reported to be −13.4 km s −1 (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Filamentary Structures and Star Formation Activity in the Sites S234, V582, and IRAS 05231+3512

Dewangan

Baug

Ojha

et al. 2018

ApJ

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To investigate the physical processes, we present observational results of the sites S234, V582, and IRAS 05231+3512 situated toward l = 171 • .7-174 • .1. Based on the CO line data, we find that these sites are not physically connected, and contain at least one filament (with length > 7 pc). The observed line masses (M line,obs ) of the filaments associated with V582 and IRAS 05231+3512 are ∼37 and ∼28 M pc −1 , respectively. These filaments are characterized as thermally supercritical, and harbor several clumps. Groups of infrared-excess sources and massive B-type stars are observed toward the filament containing V582, while a very little star formation (SF) activity is found around IRAS 05231+3512. Our results favour radial collapse scenario in the filaments harboring V582 and IRAS 05231+3512. In the site S234, two filaments (i.e. ns1 (M line,obs ∼130 M pc −1 ) and ns2 (M line,obs ∼45 M pc −1 )) are identified as thermally supercritical. An extended temperature structure at 27-30 K surrounds a relatively cold (∼19 K) ∼8.9 pc long filament ns1. At least four condensations (M clump ∼70-300 M ) are seen in ns1, and are devoid of the GMRT 610 MHz radio emission. The filament ns2 hosting clumps is devoid of ongoing SF, and could be at an early stage of fragmentation. An intense SF activity, having the SF efficiency ∼3.3% and SF rate ∼40-20 M Myr −1 (for t sf ∼1-2 Myr), is observed in ns1. The feedback of massive stars in S234 seems to explain the observed SF in the filament ns1.

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“…The H ii complex G173+1.5 associated with the Forbidden Velocity Wing features seems to be an excellent site to study SN-triggered star formation. A very general description of many star forming regions (SFRs) in Auriga is given in Reipurth & Yan (2008), and the individual regions have been discussed in several previous studies (e.g., Lafon et al 1983;Heyer et al 1996;Jose et al 2008;Pandey et al 2013;Mel'Nik & Dambis 2009;Marco & Negueruela 2016). By mapping the spatial distribution of YSOs around l ∼173 • , b ∼ 1.5 • , we can study the star formation in this whole region; it is, however, a challenging task to procure uniform optical data over such a large region (∼ 4 • .4 × 3 • .4).…”

Section: Introductionmentioning

confidence: 99%

Large-scale star formation in Auriga region

Pandey

Sharma

Kobayashi

et al. 2019

Monthly Notices of the Royal Astronomical Society

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New observations in the V I bands along with archival data from the 2MASS and W ISE surveys have been used to generate a catalog of young stellar objects (YSOs) covering an area of about 6 • × 6 • in the Auriga region centered at l ∼ 173 • and b ∼ 1 • .5. The nature of the identified YSOs and their spatial distribution are used to study the star formation in the region. The distribution of YSOs along with that of the ionized and molecular gas reveals two ring-like structures stretching over an area of a few degrees each in extent. We name these structures as Auriga Bubbles 1 and 2. The center of the Bubbles appears to be above the Galactic mid-plane. The majority of Class i YSOs are associated with the Bubbles, whereas the relatively older population, i.e., Class ii objects are rather randomly distributed. Using the minimum spanning tree analysis, we found 26 probable sub-clusters having 5 or more members. The sub-clusters are between ∼0.5 pc -∼ 3 pc in size and are somewhat elongated. The star formation efficiency in most of the sub-cluster region varies between 5% -20% indicating that the sub-clusters could be bound regions. The radii of these sub-clusters also support it.

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Open clusters in Auriga OB2

Cited by 11 publications

References 82 publications

The little-studied cluster Berkeley 90 – III. Cluster parameters

The little-studied cluster Berkeley 90 – III. Cluster parameters

Filamentary Structures and Star Formation Activity in the Sites S234, V582, and IRAS 05231+3512

Large-scale star formation in Auriga region

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