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Table 1:

Summary of the main physical properties of selected cores in IRAS 20293+3952.

$\alpha$(J2000) $\delta$(J2000) $T_{\rm ex}$a   $T_{\rm rot}$c N(NH2D)d N(NH3)d   NH3/ Evol.
Core (h m s) ( $\hbox{$^\circ$ }$ ' '') (K) $\tau_{\rm m}$b (K) ( $\times10^{14}$ cm-2) ( $\times10^{14}$ cm-2) $D_{{\rm frac}}$e N2H+c stagef
Western cloud 20:31:10.70 40:03:28.2 $4.8\pm0.2$ 1.5 $15\pm3$ 10 $\pm$ 2 14$\pm$ 2 $0.8\pm0.2$ 300 PPC
BIMA 2-S 20:31:12.34 40:03:05.7 $5.4\pm0.3$ 1.1 $19\pm3$ $2.8\pm0.6$ $6.7\pm0.8$ $0.4\pm0.1$ 90 PPC
Dust ridge 20:31:12.98 40:03:08.5 $4.6\pm0.3$ 1.0 $16\pm3$ $2.8\pm0.7$ $4.9\pm0.9$ $0.6\pm0.2$ 90 PPC
BIMA 3 20:31:13.92 40:03:00.9 $5.4\pm1.0$ 0.4 $14\pm2$ $1.9\pm0.5$ 19 $\pm$ 3 $0.10\pm0.04$ 300 PPC
BIMA 4 20:31:14.56 40:03:06.8 $7.5\pm1.6$ 0.3 14$\pm2$ $1.2\pm0.4$ $7.4\pm0.8$ $0.16\pm0.05$ 200 PPC
BIMA 1 20:31:12.77 40:03:22.6 ... ... $24\pm3$ <1.1g $19\pm3$ <0.06 50 O, no IR
IRS 5 20:31:13.41 40:03:13.7 ... ... $24\pm3$ <1.5g $11\pm2$ <0.1 50 IR

Notes.  (a)  $T_{\rm ex}$ derived from the output parameters of the NH2D  111-101 hyperfine fit. (b) Derived from the fits to the hyperfine structure of NH2D  111-101. (c) Obtained from Palau et al. (2007). (d) Column densities derived using the same uv range and convolving the images to a circular beam of 7''. (e)  $D_{{\rm frac}}=N$(NH2D)/N(NH3). (f) PPC: pre-protostellar core; O: molecular outflow. (g) 3$\sigma$ upper limit estimated adopting $\Delta v$ from NH3 and $T_{\rm ex}$=5 K.


Source LaTeX | All tables | In the text

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