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BRE18 - Water masers and ammonia (1, 1) and (2, 2) towards six regions in the Carina Nebula

Short title: Breen et al. (2018)
Authors: Breen, S. L.Green, C. -E.Cunningham, M. R.Voronkov, M. A.Horiuchi, S.Green, J. A.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 473, Issue 1, p.2-13
Bibcode:

Target type: High_mass_SFR

Abstract
We present water maser and ammonia (1, 1) and (2, 2) observations, towards six regions in the Carina Nebula, conducted with the Australia Telescope Compact Array. In total five water masers were detected within two of the target fields, and we provide their accurate positions and characteristics. These five water masers constitute all of the known masers detected towards star formation regions in the Carina Nebula and we argue, that given the evidence for active star formation, and the presence of many high-mass stars, the Carina Nebula is uncharacteristically devoid of masers. Our results are consistent with the Carina Nebula having a lack of young high-mass stars, despite the presence of older high-mass stars. Ammonia (1, 1) and (2, 2) emission was detected towards all but one of the target fields and we find that their linewidths and derived temperatures are consistent with the presence of young star formation regions.

Abstract

We present water maser and ammonia (1, 1) and (2, 2) observations, towards six regions in the Carina Nebula, conducted with the Australia Telescope Compact Array. In total five water masers were detected within two of the target fields, and we provide their accurate positions and characteristics. These five water masers constitute all of the known masers detected towards star formation regions in the Carina Nebula and we argue, that given the evidence for active star formation, and the presence of many high-mass stars, the Carina Nebula is uncharacteristically devoid of masers. Our results are consistent with the Carina Nebula having a lack of young high-mass stars, despite the presence of older high-mass stars. Ammonia (1, 1) and (2, 2) emission was detected towards all but one of the target fields and we find that their linewidths and derived temperatures are consistent with the presence of young star formation regions.

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Detection table from Breen et al. (2018)

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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_peak	∫F dv	Telescope	Configuration	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			Other name			H₂O	(km/s)	(km/s)	(Jy)	(Jy*km/s)			(km/s)	(mJy)	(arcsec)	Yes/No		(kpc)
1	10 43 26	-59 34 00	287.3600	-0.6219	G287.360-0.622	Car I	Car I	Image	Descr	22 GHz;		10	-23.2		TID		0.1		48	+H₂O	SFR_MIXED		2011 April 12 and 13
2	10 43 23.2	-59 33 56.5	287.3544	-0.6238	G287.360-0.622	Car I_1	G 287.354-0.624	Image		22 GHz;	-30.8;44.8	3.6	13.3	14.8	ATCA	H75	0.5	24.000	26 x 20	+H₂O	SFR_MIXED		2019 July 21/22
3	10 43 25.2	-59 33 58.4	287.3583	-0.6223	G287.360-0.622	Car I_1	G 287.358-0.622	Image		22 GHz;	-24.1;-17.8	5.2	-19.4	8.1	ATCA	H75	0.5	24.000	26 x 20	+H₂O	SFR_MIXED		2019 July 21/22
4	10 43 29	-59 34 14.5	287.3675	-0.6225	G287.360-0.622	Car I_1	G 287.368-0.622	Image		22 GHz;	-43.4;-32	0.5	-32.9	0.9	ATCA	H75	0.5	24.000	26 x 20	+H₂O	SFR_MIXED		2019 July 21/22
5	10 43 29.6	-59 34 15.1	287.3686	-0.6221	G287.360-0.622	Car I_1	G 287.369-0.622			22 GHz;	-28.7;-11.9	1.7	-25.7	5.9	ATCA	H75	0.5	24.000	26 x 20	+H₂O	SFR_MIXED		2019 July 21/22
6	10 45 56.3	-59 56 37	287.8151	-0.8076	G287.815-0.812	G 287.84-0.82	G 287.815-0.808	Image	Descr	22 GHz;	-13.6;-11.9	0.9	-12.7	0.9	ATCA	H75	0.5	29.000	26 x 20	+H₂O -CH₃OH II	SFR_MIXED		2013 July 21/22

Non-detection table from Breen et al. (2018)