Abstract
A hybrid JHK s −W 1 W 2 W 3 W 4 high-spectral index (α) selection scheme was employed to identify (sub)-clusters of class I/f candidate protostars (YSOs) in WISE observations (the Wide-Field Infrared Survey Explorer). n>104 candidate YSOs were detected owing to WISE’s advantageous all-sky spatial coverage, and a subsample (n∼200) of their heavily-obscured host (sub)clusters were correlated with the Avedisova (Astron. Rep. 46:193, 2002) and Dias et al. (Astron. Astrophys. 389:871, 2002) catalogs of star-forming regions. Forthcoming observations from the VVV/UKIDSS surveys shall facilitate the detection of additional protostars and bolster efforts to delineate the Galactic plane, since the campaigns aim to secure deep JHK s photometry for a pertinent fraction of the WISE targets lacking 2MASS detections, and to provide improved data for YSOs near the limits of the 2MASS survey.
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Notes
Chené et al. (2012) discovered numerous Wolf-Rayet stars residing in those clusters using infrared spectra from the VLT, NTT, and SOAR facilities.
Rosvick et al. (2012) detail a new YSO subcluster discovered in JHK s images acquired from l’Observatoire Mont-Mégantic (OMM, Artigau et al., 2010). The group was likely triggered by adjacent luminous O-type stars in Berkeley 59 (e.g., the O5V((f))n BD+64∘1673, Majaess et al., 2008, see also Koenig et al., 2012). The Doppmann et al. (2005) results are tied to high-resolution infrared Keck spectra for 41 class I/f YSOs.
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Acknowledgements
DM is grateful to the following individuals and consortia whose efforts and advice enabled the research: 2MASS, WISE, V. Avedisova, E. Paunzen (WEBDA), W. Dias (DAML), CDS, arXiv, NASA/IPAC ISA, and NASA ADS. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
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Majaess, D. Discovering protostars and their host clusters via WISE. Astrophys Space Sci 344, 175–186 (2013). https://doi.org/10.1007/s10509-012-1308-y
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DOI: https://doi.org/10.1007/s10509-012-1308-y