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KUR04 - A Catalog of CH3OH 70-61 A+ Maser Sources in Massive Star-forming Regions

Interferometry data

Short title: Kurtz et al. (2004)
Authors: Kurtz, Stan Hofner, Peter Álvarez, Carlos Vargas
Journal: The Astrophysical Journal Supplement Series, Volume 155, Issue 1, pp. 149-165.
Bibcode:

Target type: High_mass_SFR
Transitions: CH3OH_9(I),CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_84(I),CH3OH_95(I),CH3OH_104(I),CH3OH_6(II)

Abstract
We present a Very Large Array survey of 44 massive star-forming regions in the 44 GHz 7₀-6₁ A⁺ methanol transition 37 fields showed maser emission. Thirty-one sources were also observed in the 23 GHz 9₂-10₁ A⁺ methanol line two fields showed maser emission. Although the 44 GHz line is a class I maser, we find a large number of these masers in relatively close association with H II regions and water masers. Several sources show strong evidence for a correlation between 44 GHz masers and shocked molecular gas, supporting the interpretation that molecular outflows may give rise to class I maser emission. We provide maser positions with arcsecond accuracy that not only locate the masers with respect to other star formation phenomena, but also provide, for the stronger masers, phase referencing sources that can be used to calibrate future 7 mm (44 GHz) observations of these regions.	Comments: Both extremely young massive star formation regions, which have not yet developed an UC HII region, along with more evolved massive star formation regions, which have formed UC HII regions.

Abstract

We present a Very Large Array survey of 44 massive star-forming regions in the 44 GHz 7₀-6₁ A⁺ methanol transition 37 fields showed maser emission. Thirty-one sources were also observed in the 23 GHz 9₂-10₁ A⁺ methanol line two fields showed maser emission. Although the 44 GHz line is a class I maser, we find a large number of these masers in relatively close association with H II regions and water masers. Several sources show strong evidence for a correlation between 44 GHz masers and shocked molecular gas, supporting the interpretation that molecular outflows may give rise to class I maser emission. We provide maser positions with arcsecond accuracy that not only locate the masers with respect to other star formation phenomena, but also provide, for the stronger masers, phase referencing sources that can be used to calibrate future 7 mm (44 GHz) observations of these regions.

Comments:
Both extremely young massive star formation regions, which have not yet developed an UC HII region, along with more evolved massive star formation regions, which have formed UC HII regions.

Input tables: Table 5
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Detection table from Kurtz et al. (2004)

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Obs. RA	Obs. Dec	RA offset	Dec offset	#	Source name	V_peak	F_peak	∫F dv
(J2000)	(J2000)	(mas)	(mas)			(km/s)	(Jy)	(Jy*km/s)

Non-detection table from Kurtz et al. (2004)