Discovering protostars and their host clusters via WISE

Majaess, D.

doi:10.1007/s10509-012-1308-y

Cited by 34 publications

(40 citation statements)

References 33 publications

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“…We found that only 5 new GLIMPSE clusters (they are indicated in Table 2) are associated with objects from the published list by Majaess (2013), in particular these 5 clusters are contained within the corresponding objects identified by Majaess (2013), which cover a much larger area. Due to the coarser angular resolution of WISE data with respect to GLIMPSE data, the typical stellar densities in our ECs are probably too high to make all the individual members detectable at the WISE resolution, and consequently they are hidden in the Majaess (2013) YSO selection.…”

Section: New Search For Ecs In Glimpsementioning

confidence: 89%

Stellar clusters in the inner Galaxy and their correlation with cold dust emission

Morales

Wyrowski

Schüller

et al. 2013

A&A

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Context. Stars are born within dense clumps of giant molecular clouds, and constitute young stellar agglomerates known as embedded clusters, which only evolve into bound open clusters under special conditions. Aims. We statistically study all embedded clusters (ECs) and open clusters (OCs) known so far in the inner Galaxy, in particular investigating their interaction with the surrounding molecular environment and the differences in their evolution. Methods. We first compiled a merged list of 3904 clusters from optical and infrared cluster catalogs in the literature, including 75 new (mostly embedded) clusters discovered by us in the GLIMPSE survey. From this list, 695 clusters are within the Galactic range | | ≤ 60 • and |b| ≤ 1.5 • covered by the ATLASGAL survey, which was used to search for correlations with submm dust continuum emission tracing dense molecular gas. We defined an evolutionary sequence of five morphological types: deeply embedded cluster (EC1), partially embedded cluster (EC2), emerging open cluster (OC0), OC still associated with a submm clump in the vicinity (OC1), and OC without correlation with ATLASGAL emission (OC2). Together with this process, we performed a thorough literature survey of these 695 clusters, compiling a considerable number of physical and observational properties in a catalog that is publicly available. Results. We found that an OC defined observationally as OC0, OC1, or OC2 and confirmed as a real cluster is equivalent to the physical concept of OC (a bound exposed cluster) for ages in excess of ∼16 Myr. Some observed OCs younger than this limit can actually be unbound associations. We found that our OC and EC samples are roughly complete up to ∼1 kpc and ∼1.8 kpc from the Sun, respectively, beyond which the completeness decays exponentially. Using available age estimates for a few ECs, we derived an upper limit of 3 Myr for the duration of the embedded phase. Combined with the OC age distribution within 3 kpc of the Sun, which shows an excess of young exposed clusters compared to a theoretical fit that considers classical disruption mechanisms, we computed an embedded and young cluster dissolution fraction of 88 ± 8%. This high fraction is thought to be produced by several factors and not only by the classical paradigm of fast gas expulsion.

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Section: New Search For Ecs In Glimpsementioning

confidence: 89%

Stellar clusters in the inner Galaxy and their correlation with cold dust emission

Morales

Wyrowski

Schüller

et al. 2013

A&A

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“…In the recent compilation of stellar clusters, updated to August 2011 of all Galactic star cluster catalogs (e.g., Dias et al 2002;Mercer el at 2005;Dutra et al 2003;Bica et al 2003;Borissova et al 2011), Morales et al (2013) counted 2247 clusters visible in the optical and 1950 and 197 cluster candidates found in the near-and mid-infrared, respectively. Since then, Solin et al (2012Solin et al ( , 2014, Majaess (2013), and Zasowski et al (2013) reported 137; 88; 229 and 20 new embedded cluster candidates in the UKIDSS GPS, VVV, WISE, and Spitzer GLIMPSE-360 areas. This increases the number of near-infrared cluster candidates to 2404.…”

Section: Cluster Search and Methods Of Analysismentioning

confidence: 99%

New galactic star clusters discovered in the VVV survey. Candidates projected on the inner disk and bulge

Borissova

Chené

Alegría

et al. 2014

A&A

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Context. VISTA Variables in the Vía Láctea (VVV) is one of six ESO Public Surveys using the 4 meter Visible and Infrared Survey Telescope for Astronomy (VISTA). The VVV survey covers the Milky Way bulge and an adjacent section of the disk, and one of the principal objectives is to search for new star clusters within previously unreachable obscured parts of the Galaxy. Aims. The primary motivation behind this work is to discover and analyze obscured star clusters in the direction of the inner Galactic disk and bulge. Methods. Regions of the inner disk and bulge covered by the VVV survey were visually inspected using composite JHK S color images to select new cluster candidates on the basis of apparent overdensities. DR1, DR2, CASU, and point spread function photometry of 10 × 10 arcmin fields centered on each candidate cluster were used to construct color-magnitude and color-color diagrams. Follow-up spectroscopy of the brightest members of several cluster candidates was obtained in order to clarify their nature. Results. We report the discovery of 58 new infrared cluster candidates. Fundamental parameters such as age, distance, and metallicity were determined for 20 of the most populous clusters.

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“…Majaess (2013) has also made a significant contribution on young clusters (see also, Bica et al 2003a,b;Lada & Lada 2003;Mercer et al 2005;Froebrich, Scholz & Raftery 2007;Borissova et al 2011;Solin, Haikala & Ukkonen 2014).…”

Section: Introductionmentioning

confidence: 93%

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

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In the present work we investigate the properties of 18 embedded clusters (ECs). The sample includes 11 previously known clusters and we report the discovery of 7 ECs on WISE images, thus complementing our recent list of 437 new clusters. The main goal is to use such clusters to shed new light on the Galactic structure by tracing the spiral arms with cluster distances. Our results favour a four-armed spiral pattern tracing three arms, Sagitarius-Carina, Perseus, and the Outer arm. The SagitariusCarina spiral arm is probed in the borderline of the third and fourth quadrants at a distance from the Galactic centre of d 1 ∼ 6.4 kpc adopting R ⊙ = 7.2 kpc, or d 2 ∼ 7.2 kpc for R ⊙ = 8.0 kpc. Most ECs in our sample are located in the Perseus arm that is traced in the second and third quadrants and appear to be at Galactocentric distances in the range d 1 = 9 − 10.5 kpc or d 2 = 9.8 − 11.3 kpc. Dolidze 25, Bochum 2, and Camargo 445 are located in the Outer arm that extends along the second and third Galactic quadrants with a distance from the Galactic centre in the range of d 1 = 12.5 − 14.5 kpc or d 2 = 13.5 − 15.5 kpc. We find further evidence that in the Galaxy ECs are predominantly located within the thin disc and along spiral arms. They are excellent tools for tracing these Galactic features and therefore new searches for ECs can contribute to a better understanding of the Galactic structure. We also report an EC aggregate located in the Perseus arm.

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Discovering protostars and their host clusters via WISE

Cited by 34 publications

References 33 publications

Stellar clusters in the inner Galaxy and their correlation with cold dust emission

Stellar clusters in the inner Galaxy and their correlation with cold dust emission

New galactic star clusters discovered in the VVV survey. Candidates projected on the inner disk and bulge

Tracing the Galactic spiral structure with embedded clusters

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