Protostars and Planets VI, Heidelberg, July 15-20, 2013

Poster 1S032


GWANJEONG, KIM (Korea Astronomy and Space Science Institute, University of Science & Technology)
CHANG WON, LEE (Korea Astronomy and Space Science Institute, University of Science & Technology)
MAHESWAR, GOPINATHAN (Aryabhatta Research Institute of Observational Sciences)
WOONG-SEOB, JEONG (Korea Astronomy and Space Science Institute, University of Science & Technology)
MI-RYANG, KIM (Korea Astronomy and Space Science Institute, Chungbuk National University)

We present results of infrared observations toward eight dense molecular cores with the AKARI space telescope at eight bands (3, 4, 7, 11, 65, 90, 140, and 160 micrometers). These cores were previously known to be starless, and show characteristic features in their molecular lines such as a broad line width and/or asymmetric line shapes indicative of inward motions. With complementary IR data from WISE Space Telescope and our ground-based radio observations in N2H+ and HCN 1-0 lines, two of eight cores are found to harbor faint protostars and thus no longer starless. At least two new protostars having a bolometric luminosity of 0.3 -1.8 Lsun are identified in regions of L1582A and L1041-2, and seem to force the environment of the cores more turbulent than other starless cores, explaining the very broad N2H+ line widths (0.51 and 0.38 km/s) shown in L1582A and L1041-2, respectively. On the other hand, others are confirmed to be starless and may be at the moment of changing their dynamically stable to unstable status. Their far-infrared images at over 65 micron indicate that all these cores seem to be externally affected by nearby stars or Galactic interstellar radiation fields and to begin to expand or oscillate which may lead to trigger the inward motions in the cores for resulting in eventual star formation. We find interesting core-shine effects in five dense cores in near- and mid-infrared images at 3-11 micrometers implying existence of an average of 0.1 micrometer-size dust grains and will discuss their implication in the star forming process in the cores.

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