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

Johan E. Lindberg; Jes K. Jørgensen; Joel D. Green; Gregory J. Herczeg; Odysseas Dionatos; Neal J. Evans; Agata Karska; Susanne F. Wampfler

doi:10.1051/0004-6361/201322184

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Volume 565 (May 2014)

A&A, 565 (2014) A29

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Table D.1

Flux densities used in the SED fits in Sect. 4.1.

Name	Wavelength	Flux density	Reference
Telescope	[μm]	[Jy]

IRS7A
Spitzer	3.6	0.0509	Peterson et al. (2011)
	4.5	0.239
	5.8	0.546
	8.0	1.05
SMM 1C
JCMT SCUBA^a	450	45	Nutter et al. (2005)
	850	5.6
IRS7B
Spitzer	3.6	0.0367	Peterson et al. (2011)
	4.5	0.257
	5.8	0.697
	8.0	0.957
JCMT SCUBA^a	450	50	Nutter et al. (2005)
	850	5.4
R CrA
SAAO	0.36	0.0141	Koen et al. (2010)
	0.45	0.0359
	0.555	0.0647
	0.67	0.116
	0.87	0.180
2MASS	1.25	2.68	Skrutskie et al. (2006)
	1.65	10.7
	2.2	47.9
IRS5A
Spitzer	3.6	0.389	Peterson et al. (2011)
	4.5	0.798
	5.8	1.27
	8.0	1.81
IRS5N
Spitzer	3.6	0.00856	Peterson et al. (2011)
	4.5	0.0262
	5.8	0.0528
	8.0	0.0809
JCMT SCUBA^a	450	12^b	Nutter et al. (2005)
	850	1.8^b

Notes.

^(a)

The integrated flux density in apertures of 16″ × 16″ (SMM 1C), 18″ × 17″ (IRS7B), and 24″ × 24″ (IRS5N) are given.

^(b)

This is the combined value for IRS5A and IRS5N, which are unresolved. For the SEDs, we assign half of the flux density to each source.

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