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

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Volume 528 (April 2011)

A&A, 528 (2011) A3

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Table 1

Log of the SINFONI observations, plus target information.

Source	MHO^a	RA	Dec	d^a	UT Date of	Integ^b	PA^c	AM^d	Standard^e	Seeing^e	Ref.
		(J2000)	(J2000)	(pc)	Observations	(sec)	(degs)		(Hip)

HH 34-IRS	103	5:35:29.88	–06:26:57.8	450	18, 22 Oct. 2006	2400	77	1.3	026213	0.42″	3, 4
HH 300-IRS	732	4:26:56.30	24:43:35.2	140	22 Oct. 2006	1200	–31	1.5	043763	0.66″	3
SVS 13	512	3:29:03.75	31:16:04.0	220	6 Oct. 2006	2400	69	1.8	041620	0.63″	1, 2
HH 72-IRS	1407	7:20:08.35	–24:02:22.9	1500	20 Oct. 2006	1200	4	1.1	033641	0.29″	5
HH 999-IRS	1329/30	6:07:08.51	–11:17:50.9	500	22 Oct. 2006	1200	60	1.2	032112	0.37″	6
HH 26-IRS	326	5:46:03.63	–00:14:49.3	400	22 Oct. 2006	1200	–48	1.1	026579	0.64″	5
HH 83-IRS	181	5:33:32.58	–06:29:45.4	450	24 Oct. 2006	1200	38	1.1	031028	0.41″	3

Notes.

^(a)

MHO catalogue reference (Davis et al. 2010), and the distance to the target adopted in this paper.

^(b)

Total integration time spent on source.

^(c)

Position Angle of the IFS, measured East of North.

^(d)

Mean airmass during the observations on the source.

^(e)

Standard star used to calibrate the source data, and the seeing measured from the standard at 2.12 μm.

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