Display data from paper

Select data type:

OLI06 - Massive young stellar objects in the Large Magellanic Cloud: water masers and ESO-VLT 3-4 μm spectroscopy

Short title: Oliveira et al. (2006)
Authors: Oliveira, J. M., van Loon, J. Th., Stanimirovic, S.Zijlstra, A. A.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 372, Issue 4, pp. 1509-1524.
Bibcode:

Target type: HII
Transitions: H2O_22

Abstract
We investigate the conditions of star formation in the Large Magellanic Cloud (LMC). We have conducted a survey for water maser emission arising from massive young stellar objects in the 30 Doradus region (N157) and several other HII regions in the LMC (N105A, N113 and N160A). We have identified a new maser source in 30Dor at the systemic velocity of the LMC. We have obtained 3-4 μm spectra, with the European Southern Observatory (ESO)-Very Large Telescope (VLT), of two candidate young stellar objects. N105AIRS1 shows H recombination line emission, and its Spectral Energy Distribution (SED) and mid-infrared colours are consistent with a massive young star ionizing the molecular cloud. N157BIRS1 is identified as an embedded young object, based on its SED and a tentative detection of water ice. The data on these four HII regions are combined with mid-infrared archival images from the Spitzer Space Telescope to study the location and nature of the embedded massive young stellar objects and signatures of stellar feedback. Our analysis of 30Dor, N113 and N160A confirms the picture that the feedback from the massive O- and B-type stars, which creates the HII regions, also triggers further star formation on the interfaces of the ionized gas and the surrounding molecular cloud. Although in the dense cloud N105A star formation seems to occur without evidence of massive star feedback, the general conditions in the LMC seem favourable for sequential star formation as a result of feedback. In an Appendix, we present water maser observations of the galactic red giants RDoradus and WHydrae.

Abstract

We investigate the conditions of star formation in the Large Magellanic Cloud (LMC). We have conducted a survey for water maser emission arising from massive young stellar objects in the 30 Doradus region (N157) and several other HII regions in the LMC (N105A, N113 and N160A). We have identified a new maser source in 30Dor at the systemic velocity of the LMC. We have obtained 3-4 μm spectra, with the European Southern Observatory (ESO)-Very Large Telescope (VLT), of two candidate young stellar objects. N105AIRS1 shows H recombination line emission, and its Spectral Energy Distribution (SED) and mid-infrared colours are consistent with a massive young star ionizing the molecular cloud. N157BIRS1 is identified as an embedded young object, based on its SED and a tentative detection of water ice. The data on these four HII regions are combined with mid-infrared archival images from the Spitzer Space Telescope to study the location and nature of the embedded massive young stellar objects and signatures of stellar feedback. Our analysis of 30Dor, N113 and N160A confirms the picture that the feedback from the massive O- and B-type stars, which creates the HII regions, also triggers further star formation on the interfaces of the ionized gas and the surrounding molecular cloud. Although in the dense cloud N105A star formation seems to occur without evidence of massive star feedback, the general conditions in the LMC seem favourable for sequential star formation as a result of feedback. In an Appendix, we present water maser observations of the galactic red giants RDoradus and WHydrae.

Download as: Table (CSV)
View as list of objects

Detection table from Oliveira et al. (2006)

Export table to csv

Hide / Show individual components

ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	V_peak	F_peak	Telescope	Beam	Detection	Type	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					H₂O	(km/s)	(Jy)		(arcsec)	Yes/No		(kpc)
1	05 38 49.9	-69 04 34	279.4347	-31.6636	G279.439-31.668	0539-691a	Image	Descr	22 GHz	269.5	2.75 (0.60)	PRS	20	+H₂O	MIXED		2001 June 30 - July 9
2	05 38 55.2	-69 04 12	279.4265	-31.6565	G279.439-31.668	0539-691b			22 GHz	261	0.38 (0.09)	PRS	20	+H₂O	MIXED		2001 June 30 - July 9
3	05 39 4.3	-69 07 52	279.4961	-31.6362	G279.496-31.636	0539-691B			22 GHz	194	0.36 (0.09)	PRS	20	+H₂O	MIXED		2001 June 30 - July 9
4	05 38 47.1	-69 06 06	279.4651	-31.6649	G279.465-31.665	0539-691C			22 GHz	266	1.01 (0.27)	PRS	20	+H₂O	MIXED		2001 June 30 - July 9
5	05 13 23.1	-69 22 34	280.2365	-33.8366	G280.236-33.837	N 113a	Image	Descr	22 GHz	253	73.8 (16.0)	PRS	20	+H₂O -CH₃OH II	MIXED		2001 June 30 - July 9
6	05 39 42.7	-69 38 26	280.0826	-31.5222	G280.098-31.526	N 160A	Image	Descr	22 GHz	253	3.3 (0.7)	PRS	20	+H₂O	MIXED		2001 June 30 - July 9
7	05 09 50.7	-68 53 23	279.7514	-34.2542	G279.753-34.252	N 105A	Image	Descr	22 GHz	260	1.5 (0.3)	PRS	20	+H₂O -CH₃OH I	MIXED		2001 June 30 - July 9

Non-detection table from Oliveira et al. (2006)