Warm gas towards young stellar objects in Corona Australis - Herschel/PACS observations from the DIGIT key programme

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Table 5

CO rotational temperatures and total number of molecules.

YSO	T _warm ^a	^a	T _hot ^a	^a
	[K]	[10⁴⁸]	[K]	[10⁴⁸]

IRS7A+SMM 1C^b	294 ± 16	33.0 ± 3.0	682 ± 34	2.7 ± 0.3
IRS7B	273 ± 14	12.0 ± 1.1	710 ± 54	0.51 ± 0.07
R CrA	287 ± 16	5.4 ± 0.5	992 ± 91	0.27 ± 0.03
IRS5A	293 ± 17	3.1 ± 0.3	1417 ± 780	0.12 ± 0.04
IRS5N	283 ± 24	0.7 ± 0.1	...	...

Res SW-l		5.0 ± 0.5		0.35 ± 0.06
Res E-l		1.7 ± 0.2	1015 ± 198	0.09 ± 0.02
Res N-l		3.3 ± 0.3	898 ± 334	0.11 ± 0.06
Res W-l		13.0 ± 1.2		0.40 ± 0.07

CrA point-source average	286 ± 3 ^c	10.8 ± 5.2 ^c	950 ± 148 ^c	0.90 ± 0.52 ^c
CrA extended average	277 ± 7 ^c	5.8 ± 2.2 ^c	829 ± 69 ^c	0.24 ± 0.07 ^c

NGC 1333 IRAS 4B^d	280	40	880	3
Serpens SMM1^e	337 ± 40	...	622 ± 30	...
Serpens SMM3/4 average^f	260 ± 10 ^c	49 ± 6 ^c	800 ± 60 ^c	2.2 ± 0.6 ^c

DIGIT average^g	355 ± 3 ^c	5.2 ± 0.4 ^c	814 ± 29 ^c	1.63 ± 0.20 ^c
HOPS average^h	288 ± 14 ^c	...	735 ± 37 ^c	...

Notes.

^(a)

The methods used for calculating the error estimates are discussed in Sects. 4.2.1 and 4.2.2.

^(b)

The separation between these sources is too small to allow treating their line fluxes independently using POMAC.

^(c)

For the sample averages, standard deviations of the mean (the standard deviation of the sample divided by the square root of the sample size) of the significant fits are given.

^(d)

From Herczeg et al. (2012).

^(e)

From Goicoechea et al. (2012).

^(f)

Average of SMM3b, SMM3c, SMM3r, and SMM4, from Dionatos et al. (2013), assuming a distance of 415 pc.

^(g)

From Green et al. (2013), including all DIGIT embedded sources except the CrA and Serpens SMM3/4 sources. The Serpens region is, like the CrA region, affected by confusion and is treated in a separate paper (Dionatos et al. 2013).

^(h)

From Manoj et al. (2013).

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