Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.8908s&link_type=abstract
American Astronomical Society, AAS Meeting #211, #89.08; Bulletin of the American Astronomical Society, Vol. 39, p.879
Astronomy and Astrophysics
Astronomy
Scientific paper
We present an analysis of Spitzer IRAC and MIPS 24 micron observations of 45 young stellar objects (YSOs) detected in the HII Region NGC 2467. The 45 YSOs were detected based on a mid-IR excess in two or more Spitzer colors. The candidate YSOs were also classified into protostellar evolutionary classes based on their colors; we found 14 Class 0/I sources, 18 Class I/II sources, and 13 Class II sources. The physical properties of the YSOs were analyzed using an online spectral energy distribution (SED) fitter from Robitaille et al. (2007). The candidate YSOs had best-fit masses ranging from 0.3 - 5.7 Msol, with at least seven sources that had a best-fit mass of less than 1.0 Msol.
In order to classify the effect ionization fronts (IFs) have on star formation, we calculated the distance of the YSOs from IFs in the region and looked at the amount of clustering of the YSOs. The distribution of YSOs is not correlated with the location of the OB stars themselves, instead the sources are distributed along the IFs created by massive stars. Using a Salpeter (1955) initial mass function (IMF) and comparing that to our mass distribution of YSOs, we estimate that at least 20% of the YSOs forming in this region are due to triggering from the advance of IFs. The sources we are detecting are very young objects, with the majority of these sources on the order of a fewx105 years, much younger than the age of the region and of the ages of the OB stars, which are around a fewx106 years. The 45 detected YSOs and the distribution of these objects suggest that NGC 2467 is a prime example of triggered star formation due to HII region expansion.
Bally John
Desch Steven J.
Healy Kevin R.
Hester Jeff J.
Snider Keely D.
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