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VAL05 - H2O maser emission from bright rimmed clouds in the northern hemisphere

Short title: Valdettaro et al. (2005)
Authors: Valdettaro, R.Palla, F.Brand, J.Cesaroni, R.
Journal: Astronomy and Astrophysics, Volume 443, Issue 2, November IV 2005, pp.535-540
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Target type: BRC
Observations category: variability
Facility type: single-dish
Transitions: H2O_22

Abstract
We report the results of a multi-epoch survey of water maser observations at 22.2 GHz with the Medicina radiotelescope from 44 bright rimmed clouds (BRCs) of the northern hemisphere identified by Sugitani et al. (1989, ApJ, 342, L87) as potential sites of star formation. The data span 16 years of observations and allow to draw conclusions about the maser detection rate in this class of objects. In spite of the relatively high far-infrared luminosities of the embedded sources (L_FIR⪆ 102 L_⊙), H2O maser emission was detected towards three globules only. Since the occurrence of water masers is higher towards bright IRAS sources, the lack of frequent H2O maser emission is somewhat surprising if the suggestion of induced intermediate- and high-mass star formation within these globules is correct. The maser properties of two BRCs are characteristic of exciting sources of low-mass, while the last one (BRC 38) is consistent with an intermediate-mass object. We argue that most BRCs host young stellar objects of low-luminosity, likely in an evolutionary phase later than the protostellar Class 0 sources, and that a significant contribution to the observd IRAS luminosity comes from warm dust heated by the radiation from the bright rim.

Abstract

We report the results of a multi-epoch survey of water maser observations at 22.2 GHz with the Medicina radiotelescope from 44 bright rimmed clouds (BRCs) of the northern hemisphere identified by Sugitani et al. (1989, ApJ, 342, L87) as potential sites of star formation. The data span 16 years of observations and allow to draw conclusions about the maser detection rate in this class of objects. In spite of the relatively high far-infrared luminosities of the embedded sources (L_FIR⪆ 102 L_⊙), H2O maser emission was detected towards three globules only. Since the occurrence of water masers is higher towards bright IRAS sources, the lack of frequent H2O maser emission is somewhat surprising if the suggestion of induced intermediate- and high-mass star formation within these globules is correct. The maser properties of two BRCs are characteristic of exciting sources of low-mass, while the last one (BRC 38) is consistent with an intermediate-mass object. We argue that most BRCs host young stellar objects of low-luminosity, likely in an evolutionary phase later than the protostellar Class 0 sources, and that a significant contribution to the observd IRAS luminosity comes from warm dust heated by the radiation from the bright rim.

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Detection table from Valdettaro et al. (2005)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Image	Descr.	Line	V_range	V_peak	∫F dv	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)						H₂O	(km/s)	(km/s)	(Jy*km/s)		(km/s)	(Jy)	(arcsec)	Yes/No		(kpc)
1	18 18 45.1	-13 44 53.2	17.0001	0.8314	G17.000+0.831	G17.0001+0.8314	BRC 30		Descr	22 GHz;	22.3;23.6	23	12.6	MED	0.13	0.730	114	+H₂O -CH₃OH II	SFR		18.12.2004
	18 18 45.1	-13 44 53.2	17.0001	0.8314	G17.000+0.831	G17.0001+0.8314	BRC 30	Image		22 GHz;	19.9;22.4	21.8	8.9	MED	0.13	2.510	114	+H₂O -CH₃OH II	SFR		14.04.2005
3	21 36 12.4	+57 27 34.2	98.9944	3.9635	G98.987+3.962	G98.9944+3.9635	BRC 36		Descr	22 GHz;	-6.5;-5.6	-6.1	5.4	MED	0.165	1.200	114	+H₂O -CH₃OH I -CH₃OH II	SFR		28.01.1993
	21 36 12.4	+57 27 34.2	98.9944	3.9635	G98.987+3.962	G98.9944+3.9635	BRC 36			22 GHz;	-11;-9.4	-10.1	33.7	MED	0.13	0.870	114	+H₂O -CH₃OH I -CH₃OH II	SFR		18.12.2004
	21 36 12.4	+57 27 34.2	98.9944	3.9635	G98.987+3.962	G98.9944+3.9635	BRC 36	Image		22 GHz;	11.3;9.7	10.5	17.8	MED	0.13	1.200	114	+H₂O -CH₃OH I -CH₃OH II	SFR		14.04.2005
6	21 40 42.4	+58 16 9.7	99.9825	4.1696	G99.982+4.170	G99.9825+4.1696	BRC 38	Image	Descr	22 GHz;		-8		MED	0.13		114	+H₂O +CH₃OH I -CH₃OH II +OH	GALAXY

Non-detection table from Valdettaro et al. (2005)