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VAL07 - H2O maser emission from bright rimmed clouds in the southern hemisphere

Short title: Valdettaro et al. (2007)
Authors: Valdettaro, R.Chapman, J. M.Lovell, J. E. J.Palla, F.
Journal: Astronomy and Astrophysics, Volume 466, Issue 1, April IV 2007, pp.247-253
Bibcode:

Target type: Other

Abstract
Context: Water maser emission is a powerful tracer of the presence of embedded sources in dense clouds since it requires elevated temperatures (>100 K) and densities (>10⁷ cm^-3) that can be found in circumstellar disks and/or jets/outflows associated with Young Stellar Objects. Bright rimmed clouds compressed by ionization fronts from nearby massive stars are considered good examples of externally triggered star formation, possibly resulting in the formation of massive stars. Aims: We aim to determine the water maser emission frequency and characteristics of 45 bright rimmed clouds in the southern hemisphere identified by Sugitani & Ogura (1994, ApJS, 92, 163). Methods: We have used the Tidbinbilla 70-m radiotelescope to perform a high sensitivity survey at 22.2 GHz of the maser emission from the 6₁₆-5₂₃ rotational transition of H2O molecules. Results: We found 7 water maser sources out of 44 (16% detection rate), 5 being new detections. With the exception of the maser associated with BRC 68, all the other maser are characterized by low integrated fluxes and luminosities. Conclusions: Most maser sources fall below the correlation between the H2O and far-infrared luminosity found in other studies towards a variety of star forming regions. These results are similar to those found in the companion survey of BRCs in the northern hemisphere by Valdettaro et al. (2005, A&A, 443, 535). The low detection frequency and the properties of water maser emission from BRCs indicate that low-mass star formation is the most natural outcome of the external compression induced by the ionization front from nearby massive stars. Based on observations obtained with the 70-m Tidbinbilla radiotelescope.

Abstract

Context: Water maser emission is a powerful tracer of the presence of embedded sources in dense clouds since it requires elevated temperatures (>100 K) and densities (>10⁷ cm^-3) that can be found in circumstellar disks and/or jets/outflows associated with Young Stellar Objects. Bright rimmed clouds compressed by ionization fronts from nearby massive stars are considered good examples of externally triggered star formation, possibly resulting in the formation of massive stars.
Aims: We aim to determine the water maser emission frequency and characteristics of 45 bright rimmed clouds in the southern hemisphere identified by Sugitani & Ogura (1994, ApJS, 92, 163).
Methods: We have used the Tidbinbilla 70-m radiotelescope to perform a high sensitivity survey at 22.2 GHz of the maser emission from the 6₁₆-5₂₃ rotational transition of H2O molecules.
Results: We found 7 water maser sources out of 44 (16% detection rate), 5 being new detections. With the exception of the maser associated with BRC 68, all the other maser are characterized by low integrated fluxes and luminosities.
Conclusions: Most maser sources fall below the correlation between the H2O and far-infrared luminosity found in other studies towards a variety of star forming regions. These results are similar to those found in the companion survey of BRCs in the northern hemisphere by Valdettaro et al. (2005, A&A, 443, 535). The low detection frequency and the properties of water maser emission from BRCs indicate that low-mass star formation is the most natural outcome of the external compression induced by the ionization front from nearby massive stars.

Based on observations obtained with the 70-m Tidbinbilla radiotelescope.

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Detection table from Valdettaro et al. (2007)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Image	Descr.	Line	V_range	V_peak	∫F dv	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			BRC			H₂O	(km/s)	(km/s)	(Jy*km/s)		(km/s)	(Jy)	(arcsec)	Yes/No		(kpc)
1	08 41 13	-40 52 3.3	260.7751	0.6784	G260.775+0.678	08393-4041	55	Image		22 GHz;	-8;10	2.48	58	TID	0.25	0.052	39	+H₂O -CH₃OH II	SFR		13/06/03
	08 41 13	-40 52 3.3	260.7751	0.6784	G260.775+0.678	08393-4041	55	Image		22 GHz;	-8.4;9.6	1.3	51.9	TID	0.25	0.056	39	+H₂O -CH₃OH II	SFR		27/08/03
3	11 12 18	-58 46 19.9	290.3740	1.6612	G290.374+1.661	11101-5829	64	Image	Descr	22 GHz;	-51;42	-17.4	21.9	TID	0.25	0.082	39	+H₂O +CH₃OH II +OH	SFR		10/04/03
	11 12 18	-58 46 19.9	290.3740	1.6612	G290.374+1.661	11101-5829	64	Image		22 GHz;	-42;28	-15.2	17.7	TID	0.25	0.096	39	+H₂O +CH₃OH II +OH	SFR		30/04/03
5	11 33 49.5	-63 16 20.4	294.3351	-1.7034	G294.335-1.703	11315-6259	66	Image	Descr	22 GHz;	-18.9;2.6	0.49	1	TID	0.25	0.087	39	+H₂O +CH₃OH II	SFR_MIXED		10/04/03
	11 33 49.5	-63 16 20.4	294.3351	-1.7034	G294.335-1.703	11315-6259	66	Image		22 GHz;	-1;0.8	0.54	1.4	TID	0.25	0.110	39	+H₂O +CH₃OH II	SFR_MIXED		30/04/03
7	11 35 31.9	-63 14 51.3	294.5116	-1.6235	G294.512-1.622	11332-6258	68	Image	Descr	22 GHz;	-21.5;-8.7	-12.6	480.2	TID	0.25	0.102	39	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		30/04/03
8	13 08 12.6	-62 10 26.5	304.8880	0.6340	G304.888+0.635	13050-6154	71	Image	Descr	22 GHz;	-43.2;-40.7	-41.8	6.5	TID	0.25	0.106	39	+H₂O -CH₃OH I +CH₃OH II	SFR		30/04/03
9	16 10 38.6	-49 05 51.6	332.9563	1.8039	G332.956+1.804	16069-4858	76	Image	Descr	22 GHz;	-26;-23	-25	2.2	TID	0.25	0.126	39	+H₂O -CH₃OH II	SFR		14/02/05
10	16 40 0.1	-48 51 44.6	336.4912	-1.4751	G336.491-1.475	16362-4845	79	Image	Descr	22 GHz;	7.7;12.1	10.9	4.5	TID	0.25	0.130	39	+H₂O -CH₃OH II	SFR		14/02/05

Non-detection table from Valdettaro et al. (2007)