Dense and warm molecular gas in the envelopes and outflows of southern low-mass protostars

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Volume 508 / No 1 (December II 2009)

A&A, 508 1 (2009) 259-274

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Table 4:

HCO⁺ and H¹³CO⁺ results.
Source	HCO⁺ 4-3		H¹³CO⁺ 4-3		$V_{\rm LSR}^a$
	$\int T_{\rm MB} {\rm d} V^b$	$T_{\rm MB}$	$\int T_{\rm MB} {\rm d} V^b$	$T_{\rm MB}$
	(K km s^-1)	(K)	(K km s^-1)	(K)	(km s^-1)
Chamaeleon
Ced 110 IRS 4	4.0	3.1	0.38	0.25	4.3
Ced 110 IRS 6	0.5	0.4	<0.06	-	4.8
Cha IRS 6a	<0.2	-	<0.06	-	4.6
Cha IRN	0.87	0.95	<0.06	-	4.5
Cha INa 2	<0.2	-	<0.06	-	4.8
Corona australis
CrA IRAS 32	4.1	2.9	0.72	0.53	5.6
HH 100-off	4.8	3.2	<0.06	-	5.9
RCrA IRS 5	14.2	7.0	0.96	0.86	5.7
RCrA IRS 7A	63.7	17.4	3.8	1.6	5.5
RCrA IRS 7B	49.0	18.7	3.8	2.2	5.7
RCrA TS 3.5	<0.2	-	<0.06	-	5.9
Isolated
HH 46	8.4	5.4	1.1	1.0	5.3
IRAS 07178-4429	1.0	0.6	<0.08	-	3.4
IRAS 12496-7650	1.9	1.5	<0.06	-	1.9
IRAS 13546-3941	<0.12	-	<0.06	-	-5.7
IRAS 15398-3359^c	5.9	4.6	-	-	5.2

^a The rest velocity $V_{\rm {LSR}}$ was determined by fitting Gaussians to either the H¹³CO⁺ 4-3 (preferred) or C¹⁸O 3-2 lines (see Table 3); ^b calibration uncertainties estimated at 20 $\%$ dominate the uncertainty of the integrated intensity; ^c data from HARP-B map.

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