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CHO12 - Water and Methanol Maser Activities in the NGC 2024 FIR 6 Region

Short title: Choi et al. (2012)
Authors: Choi, Minho Kang, Miju Byun, Do-Young Lee, Jeong-Eun
Journal: The Astrophysical Journal, Volume 759, Issue 2, article id. 136, 7 pp. (2012).
Bibcode:
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Target type: High_mass_SFR
Observations category: SF.variability
Transitions: CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I)

Abstract
The NGC 2024 FIR 6 region was observed in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz. The water maser spectra displayed several velocity components and month-scale time variabilities. Most of the velocity components may be associated with FIR 6n, while one component was associated with FIR 4. A typical lifetime of the water maser velocity components is about eight months. The components showed velocity fluctuations with a typical drift rate of about 0.01 km s^-1 day^-1. The methanol class I masers were detected toward FIR 6. The methanol emission is confined within a narrow range around the systemic velocity of the FIR 6 cloud core. The methanol masers suggest the existence of shocks driven by either the expanding H II region of FIR 6c or the outflow of FIR 6n. eprintid: arXiv:1209.5487	Target sources: 6.9mm continuum source FIR 6c (Choi et al. 2012) Comments: Methanol observations of NGC 2024 FIR 6 region

Abstract

The NGC 2024 FIR 6 region was observed in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz. The water maser spectra displayed several velocity components and month-scale time variabilities. Most of the velocity components may be associated with FIR 6n, while one component was associated with FIR 4. A typical lifetime of the water maser velocity components is about eight months. The components showed velocity fluctuations with a typical drift rate of about 0.01 km s^-1 day^-1. The methanol class I masers were detected toward FIR 6. The methanol emission is confined within a narrow range around the systemic velocity of the FIR 6 cloud core. The methanol masers suggest the existence of shocks driven by either the expanding H II region of FIR 6c or the outflow of FIR 6n. eprintid:

Target sources:
6.9mm continuum source FIR 6c (Choi et al. 2012)

Comments:
Methanol observations of NGC 2024 FIR 6 region

Input tables: Table 4, 5
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Detection table from Choi et al. (2012)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Line	V_peak	FWHM	F_peak	∫F dv	Telescope	Beam	Detection	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				CH₃OH (class I)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No	(kpc)
1	05 41 45.1	-01 56 4.4	206.5654	-16.3618	G206.564-16.361	G206.5654-16.3618	NGC 2024 FIR 6	44 GHz (I);	11.12 (0.08)	2.2 (0.2)	1.4	3.2 (0.2)	KVN	62	+H₂O +CH₃OH I +CH₃OH II +OH		2011-2012
2	05 41 45.1	-01 56 4.4	206.5654	-16.3618	G206.564-16.361	G206.5654-16.3618	NGC 2024 FIR 6	95 GHz (I);	10.99 (0.13)	1.8 (0.3)	2.5	4.7 (0.7)	KVN	29	+H₂O +CH₃OH I +CH₃OH II +OH		2011-2012
3	05 41 45.1	-01 56 4.4	206.5654	-16.3618	G206.564-16.361	G206.5654-16.3618	NGC 2024 FIR 6	132.8 GHz (I);	10.41 (0.19)	1.7 (0.4)	7.7	13.7 (2.7)	KVN	22	+H₂O +CH₃OH I +CH₃OH II +OH		2011-2012

Non-detection table from Choi et al. (2012)