VLT integral field spectroscopy of embedded protostars: using near-infrared emission lines as tracers of accretion and outflow

C. J. Davis; B. Cervantes; B. Nisini; T. Giannini; M. Takami; E. Whelan; M. D. Smith; T. P. Ray; A. Chrysostomou; T. S. Pyo

doi:10.1051/0004-6361/201015897

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Volume 528 (April 2011)

A&A, 528 (2011) A3

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Table C.2

Extinction and H₂ excitation temperature derived for each source from the line detections listed in Tables B.1 and B.2.

Source	A_v(poly)^a	A_v(line)^a	T_ex^a	A_v(poly,noQ)^b	A_v(line,noQ)^b	T_ex(noQ)^b	A_v(line,v = 1)^c	T_ex(v = 1)^c
	(mag)	(mag)	(K)	(mag)	(mag)	(K)	(mag)	(K)

HH 34-IRS	6	0	1616	0	0	1667	0	975
HH 300-IRS	27	10	5565	24	6	4629	0	1031
SVS 13	...	...	8028^d	...	...	...	...	...
HH 72-IRS	0	0	1355	0	0	1396	0	868
HH 999-IRS	...	...	3218^d	...	...	...	...	...
HH 26-IRS	18	27	2976	17	27	3077	24	1339

Notes.

^(a)

Extinction values derived by minimising the scatter of data points about a second-order polynomial fit and a linear fit, respectively; the excitation temperature is measured from the slope of the linear fit.

^(b)

A_v and T_ex derived from second-order polynomial and linear fits to all lines excluding the Q-branch transitions.

^(c)

A_v and T_ex derived from linear fits to only transitions from the v = 1 state.

^(d)

Value based on only two line intensities.

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