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Table 1:

Far-infrared optical depth, mass, and column density estimates.

$\lambda$ 		f a f0 b $f_{\rm BG}$ c $\tau$ Mass N(H+He)
$\mu $m Jy/ $\sq \hbox{$^{\prime\prime}$ }$ Jy/ $\sq \hbox{$^{\prime\prime}$ }$ Jy/ $\sq \hbox{$^{\prime\prime}$ }$   ${M}_{\odot}$ cm-2
photProject (method 1)
70 0.002 0.003 0.001 0.23 0.1 $1.9 \times 10^{22}$
160 0.003 0.007 0.002 0.48 2.5 $3.8 \times 10^{23}$
MADmap (method 2)
70 0.002 0.003 0.001 0.2 0.1 $1.6 \times 10^{22}$
160 0.004 0.008 0.002 0.45 2.4 $3.5 \times 10^{23}$

Notes. (a) Derived in a ${\sim}7\hbox{$^{\prime\prime}$ }$ radius region centered on RA = $5^{\rm h} 36^{\rm m} 24.4^{\rm s}$, Dec = $-06\hbox {$^\circ $ }42\hbox {$^\prime $ }56.4\hbox {$^{\prime \prime }$ }$, indicated in Fig. 3 as the inner most circular overlay in the Herschel PACS images. (b) Derived in a ${\sim}15\hbox{$^{\prime\prime}$ }$ to ${\sim}30\hbox{$^{\prime\prime}$ }$ radius half-annulus, excluding bright areas associated with V 380 Ori, indicated in Fig. 3 as well. (c) Estimated background flux contribution to the PACS maps, estimated as 50% of the measurements from IRAS data (interpolated to 70 $\mu $m) and the 160 $\mu $m ISO Serendipity Survey near NGC 1999.


Source LaTeX | All tables | In the text

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