Searcharxiv⌕ Search

arXiv subjects

Chang Won Lee

Publications and source records attributed to Chang Won Lee.

182 records · Page 11Linked to original sources

A Catalogue of Optically Selected Cores

We present a new catalogue of 406 dense cores optically selected by using the STScI Digitized Sky Survey (DSS). In this catalogue 306 cores have neither an Embedded YSO (EYSO) nor a Pre-Main-Sequence (PMS) star, 94 cores have EYSOs (1 core has both an EYSO and a PMS star), and 6 cores have PMS star only. Our sample of dense cores in the catalogue is fairly complete within a category of northern Lynds class 5, 6 clouds, and southern Hartley et al. (1986)'s class A clouds, providing a database useful for the systematic study of dense cores. Most of the cores listed in the catalogue have diameters between $0.05 - 0.36$ pc with a mean of $\sim 0.24$ pc. The sizes ($\sim 0.33$ pc in the mean) of cores with EYSOs are found to be usually larger than the sizes ($\sim 0.22 $ pc in the mean) of starless cores. The typical mean gas density of the cores is $\sim7\times 10^3 cm^{-3}$. Most of the cores are more likely elongated than spherical (mean aspect ratio: $\sim 2.4$). The ratio of the number of cores with EYSOs to the number of starless cores for our sample is about 0.3, suggesting that the typical lifetime of starless cores is $0.3-1.6$ Myr, about 3 times longer than the duration of the Class 0 and Class I phases. This lifetime is shorter than expected from models of ambipolar diffusion, by factors of 2-44.

astro-ph↗

Dense Molecular Clouds In The Galactic Center Region : I. HCN (J=1$-$0) DATA

The Galactic Center regions $-6^\circ \le l \le 6^\circ$ and $-0.8^\circ \le b \le 0.87^\circ$ are surveyed with HCN J=1$-$0 line (88.6 GHz) on a 4$'$ grid with the 14 m telescope at the Taeduk Radio Astronomy Observatory. The data complement the previous $^{13}$CO, CS, and H$_2$CO measurements (Bally \etal 1988, Zylka \etal 1992) but cover a wider area with a better or comparable resolution. The asymmetry in emission found in the $^{13}$CO observations by Bally \etal (1988) is well confirmed in this study. Interestingly, the asymmetry in HCN emission is more pronounced here: more than $80 \%$ of the overall emission is found in the first quadrant ($l>0$) and $V_{LSR}>0$. Also confirmed is the existence of several emission components in the regions forbidden by the Galactic circular rotation. The HCN maps show clear absence of both more outer galactic emissions and the 3 kpc arm component, which are both visible in the $^{13}$CO map. This implies that the HCN emission lines are not contaminated by foreground or background gas components. Therefore HCN data are particularly useful in investigating the structures of molecular clouds in the Galactic Center. The $ΔV$s (FWHMs) of the most of the detected lines are found to be very large, \ie, about $15\sim $55 km s$^{-1}$ with the mode at $ΔV \approx25$ km s$^{-1}$. The typical value of $ΔV\approx 25$ km s$^{-1}$ may imply that clouds with mass of an order of $10^6 \msun$ are common in the GC region. Another trend found is that the maximum $ΔV$ decreases with $l$, which may be partly due to the overlapping effects of clouds.

astro-ph↗