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SLY02 - Methanol Radio Emission at Millimeter Wavelengths: New Masers at 1.3 and 2.8 Millimeters

Short title: Slysh et al. (2002)
Authors: Slysh, V. I. Kalenskii, S. V. Val'tts, I. E.
Journal: Astronomy Reports, Volume 46, Issue 1, January 2002, pp.49-56
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_132(I),CH3OH_6(II),CH3OH_107(II),CH3OH_157(II)

Abstract
The results of a search for maser emission in the methanol lines 8-1-70 E at 229.8 GHz, 3-2-4-1 E at 230.0 GHz, 00-1-1 E at 108.9 GHz, and in the J 1-J 0 E series near 165 GHz in star-forming regions are reported. At least two masers and two candidates have been detected at 229.8 GHz. Thus, methanol masers have been detected in the 1-mm band for the first time. At 108.9 GHz, masers have been detected toward G345.01+1.79 and possibly toward M8E as well. Thermal emission was found toward 28 objects. The 229.8-GHz sources are class I masers, whereas the 108.9-GHz sources are class II masers. An analysis using a large velocity-gradient method shows that the 229.8-GHz masers can appear at densities of about 3𴡀 cm-3. The ratios of the flux densities in different class I lines toward DR 21(OH) and DR 21 West can be approximated in models with gas kinetic temperatures of about 50 K. Detection of the 108.9 GHz masers toward G345.01+1.79 and M8E may provide information about the geometry of these objects.

Abstract

The results of a search for maser emission in the methanol lines 8-1-70 E at 229.8 GHz, 3-2-4-1 E at 230.0 GHz, 00-1-1 E at 108.9 GHz, and in the J 1-J 0 E series near 165 GHz in star-forming regions are reported. At least two masers and two candidates have been detected at 229.8 GHz. Thus, methanol masers have been detected in the 1-mm band for the first time. At 108.9 GHz, masers have been detected toward G345.01+1.79 and possibly toward M8E as well. Thermal emission was found toward 28 objects. The 229.8-GHz sources are class I masers, whereas the 108.9-GHz sources are class II masers. An analysis using a large velocity-gradient method shows that the 229.8-GHz masers can appear at densities of about 3𴡀 cm-3. The ratios of the flux densities in different class I lines toward DR 21(OH) and DR 21 West can be approximated in models with gas kinetic temperatures of about 50 K. Detection of the 108.9 GHz masers toward G345.01+1.79 and M8E may provide information about the geometry of these objects.

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Detection table from Slysh et al. (2002)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	Thermal	V_peak	FWHM	∫T_a dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)	line mark	(km/s)	(km/s)	(K*km/s)		(arcsec)	Yes/No		(kpc)
1	16 56 47.6	-40 14 26.3	345.0094	1.7923	G345.010+1.792	G345.01+1.79	229 GHz (I);		-13.71(0.47)	4.91(0.83)	5.9(1.0)	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
2	16 56 47.6	-40 14 26.3	345.0094	1.7923	G345.010+1.792	G345.01+1.79	165 GHz;	*	-13.95(0.32)	6.01(0.00)	7.2(1.7); 13.7(1.7); 7.8(1.7); 8.7(1.7);3.3(1.6)*	IRAM	15	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
3	16 56 47.6	-40 14 26.3	345.0094	1.7923	G345.010+1.792	G345.01+1.79	108 GHz (II);		-22.55(0.11)	1.03(0.25)	0.7(0.2)	IRAM	22	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
	16 56 47.6	-40 14 26.3	345.0094	1.7923	G345.010+1.792	G345.01+1.79	108 GHz (II);		-21.90(0.01)	0.49(0.04)	0.8(0.1)	IRAM	22	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
	16 56 47.6	-40 14 26.3	345.0094	1.7923	G345.010+1.792	G345.01+1.79	108 GHz (II);		-13.60(0.09)	4.00(0.22)	2.2(0.1)	IRAM	22	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
6	17 20 56.5	-35 45 20.2	351.4459	0.6526	G351.446+0.660	NGC6334I(N)	229 GHz (I);		-4.88(0.20)	5.09(0.47)	10.4(0.8)*	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
7	17 20 56.5	-35 45 20.2	351.4459	0.6526	G351.446+0.660	NGC6334I(N)	165 GHz;	*	-4.27(0.16)	5.34(0.22)	7.3(0.9); 8.7(0.9); 9.3(0.9); 7.0(0.8); 8.1( 1.4)	IRAM	15	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
8	17 20 56.5	-35 45 20.2	351.4459	0.6526	G351.446+0.660	NGC6334I(N)	108 GHz (II);		-4.64(0.04)	5.42(0.10)	11.2(0.2)	IRAM	22	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
9	18 04 53.9	-24 26 41.3	6.0499	-1.4493	G6.050-1.449	M8E	108 GHz (II);		10.66(0.04)	0.83(0.13)	0.4(0.05)	IRAM	22	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		August 29-31, 1995
10	18 29 24.8	-15 15 17.9	16.8760	-2.1541	G16.868-2.158	L379 IRS3	229 GHz (I);		20.45(0.22)	4.72(1.07)	5.4(0.5)	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
11	18 29 24.8	-15 15 17.9	16.8760	-2.1541	G16.868-2.158	L379 IRS3	165 GHz;	*	19.78(0.34)	4.56(0.74)	1.9(0.7); 3.2(0.7); 1.9(0.7); 3.1(0.7)	IRAM	15	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
12	18 29 24.8	-15 15 17.9	16.8760	-2.1541	G16.868-2.158	L379 IRS3	108 GHz (II);		19.32(0.13)	5.56(0.43)	3.5(0.2)	IRAM	22	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		August 29-31, 1995
13	20 38 54.8	+42 19 22.5	81.6645	0.5515	G81.713+0.567	DR 21 West	229 GHz (I);		-2.55(0.02)	0.34(0.04)	1.1(0.2)	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		August 29-31, 1995
	20 38 54.8	+42 19 22.5	81.6645	0.5515	G81.713+0.567	DR 21 West	229 GHz (I);		-2.16(0.12)	1.70(0.25)	2.7(0.3)	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		August 29-31, 1995
15	20 38 59.2	+42 22 48.8	81.7183	0.5755	G81.713+0.567	DR 21(OH)	229 GHz (I);		-1.64(0.14)	4.18(0.28)	3.1(0.2)	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		August 29-31, 1995
	20 38 59.2	+42 22 48.8	81.7183	0.5755	G81.713+0.567	DR 21(OH)	229 GHz (I);		0.29(0.01)	0.65(0.03)	2.0(0.1)	IRAM	10.4	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		August 29-31, 1995
17	20 38 59.2	+42 22 48.8	81.7183	0.5755	G81.713+0.567	DR 21(OH)	165 GHz;	*	-2.65(0.20)	5.76(0.31)	1.7(0.3); 2.3(0.3); 2.2(0.3); 2.5(0.3)	IRAM	15	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		August 29-31, 1995
18	20 38 59.2	+42 22 48.8	81.7183	0.5755	G81.713+0.567	DR 21(OH)	108 GHz (II);		-2.75(0.08)	4.71(0.17)	2.1(0.1)	IRAM	22	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		August 29-31, 1995

Non-detection table from Slysh et al. (2002)