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FON10 - Class I and Class II methanol masers in high-mass star-forming regions

Short title: Fontani et al. (2010)
Authors: Fontani, F. Cesaroni, R. Furuya, R. S.
Journal: Astronomy and Astrophysics, Volume 517, id.A56, 24 pp.
Bibcode:

Target type: High_mass_SFR,IRAS
Transitions: OH_1665,SiO_1-0v0,CH3OH_9(I),CH3OH_23.4(I),CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_6(II),CH3OH_23.1(II)

Abstract
Context. Among the tracers of the earliest phases in the massive star formation process, methanol masers have gained increasing importance. The phenomenological distinction between Class I and II methanol masers is based on their spatial association with objects such as jets, cores, and ultracompact Hii regions, but is also believed to correspond to different pumping mechanisms: radiation for Class II masers, collisions for Class I masers. Aims: We surveyed a large sample of massive star-forming regions in Class I and II methanol masers. The sample consists of 296 sources, divided into two groups named high and low according to their [25-12] and [60-12] IRAS colours. Previous studies indicate that the two groups may contain similar sources in different evolutionary stages, with the high sources representing the more evolved stages. Therefore, the sample can be used to assess a sequence for the occurrence of Class I and II methanol masers during the evolution of a massive star-forming region. Methods: We observed the 6 GHz (Class II) CH₃OH maser with the Effelsberg 100-m telescope, and the 44 GHz and 95 GHz (Class I) CH₃OH masers with the Nobeyama 45-m telescope. Results: We detected 55 sources in the Class II line (39 high and 16 low, 12 new detections) 27 sources in the 44 GHz Class I line (19 high and 8 low, 17 new detections) 11 sources in the 95 GHz Class I line (eight high and three low, all except one are new detections). The detection rate of Class II masers decreases with the distance of the source (as expected), whereas that of Class I masers peaks at ~5 kpc. This could be due to the Class I maser spots being spread over a region &lap1 pc, comparable to the telescope beam diameter at a distance of ~5 kpc. We also find that the two Class I lines have similar spectral shapes at 44 GHz and 95 GHz, which confirms that they have the same origin. Conclusions: Our statistical analysis shows that the ratio between the detection rates of Class II and Class I methanol masers is basically the same in high and low sources. Therefore, both maser types seem to be equally associated with each evolutionary phase. In contrast, all maser species (including H₂O) have about three times higher detection rates in high than in low sources. This could indicate that the phenomena from which all masers originate become progressively more active with time during the earliest evolutionary phases of a high-mass star-forming region. Appendices are only available in electronic form at	Target sources: IRAS Comments: Large sample of massive star-forming regions

Abstract

Context. Among the tracers of the earliest phases in the massive star formation process, methanol masers have gained increasing importance. The phenomenological distinction between Class I and II methanol masers is based on their spatial association with objects such as jets, cores, and ultracompact Hii regions, but is also believed to correspond to different pumping mechanisms: radiation for Class II masers, collisions for Class I masers.
Aims: We surveyed a large sample of massive star-forming regions in Class I and II methanol masers. The sample consists of 296 sources, divided into two groups named high and low according to their [25-12] and [60-12] IRAS colours. Previous studies indicate that the two groups may contain similar sources in different evolutionary stages, with the high sources representing the more evolved stages. Therefore, the sample can be used to assess a sequence for the occurrence of Class I and II methanol masers during the evolution of a massive star-forming region.
Methods: We observed the 6 GHz (Class II) CH₃OH maser with the Effelsberg 100-m telescope, and the 44 GHz and 95 GHz (Class I) CH₃OH masers with the Nobeyama 45-m telescope.
Results: We detected 55 sources in the Class II line (39 high and 16 low, 12 new detections) 27 sources in the 44 GHz Class I line (19 high and 8 low, 17 new detections) 11 sources in the 95 GHz Class I line (eight high and three low, all except one are new detections). The detection rate of Class II masers decreases with the distance of the source (as expected), whereas that of Class I masers peaks at ~5 kpc. This could be due to the Class I maser spots being spread over a region &lap1 pc, comparable to the telescope beam diameter at a distance of ~5 kpc. We also find that the two Class I lines have similar spectral shapes at 44 GHz and 95 GHz, which confirms that they have the same origin.
Conclusions: Our statistical analysis shows that the ratio between the detection rates of Class II and Class I methanol masers is basically the same in high and low sources. Therefore, both maser types seem to be equally associated with each evolutionary phase. In contrast, all maser species (including H₂O) have about three times higher detection rates in high than in low sources. This could indicate that the phenomena from which all masers originate become progressively more active with time during the earliest evolutionary phases of a high-mass star-forming region. Appendices are only available in electronic form at

Target sources:
IRAS

Comments:
Large sample of massive star-forming regions

Input tables: Table 2
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Detection table from Fontani et al. (2010)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	FWHM	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	05 20 16.1	+36 37 21	170.6566	-0.2692	G170.657-0.269	05168+3634	44 GHz (I);	-4.9 (0.2)	1.3 (0.4)	0.8	1.12 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		April 2002
2	05 51 10.6	+25 46 14	183.3482	-0.5770	G183.348-0.577	05480+2545	44 GHz (I);	-9.79 (0.02)	0.77 (0.05)	4.08	3.3 (0.1)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
3	06 04 34.2	+30 30 39	180.7127	4.3468	G180.713+4.347	06013+3030	44 GHz (I);	16.4 (0.7)	5 (1.5)	0.51	2.7 (0.6)	NRO	38	-H₂O +CH₃OH I -CH₃OH II	EVOLVED		April 2002
4	18 11 51.3	-17 31 29	12.8887	0.4897	G12.889+0.490	18089-1732	44 GHz (I);	31.94 (0.01)	0.86 (0.04)	11.8	10.9 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
5	18 17 57.1	-12 07 22	18.3401	1.7722	G18.340+1.772	18151-1208	44 GHz (I);	30.5 (0.1)	1.5 (0.3)	1.34	2.2 (0.2)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
	18 17 57.1	-12 07 22	18.3401	1.7722	G18.340+1.772	18151-1208	44 GHz (I);	33.8 (0.2)	2.1 (0.5)	0.89	2.0 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
7	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	44 GHz (I);	13.2 (0.1)	0.9 (0.1)	3.95	4.0 (0.6)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	44 GHz (I);	19.5 (0.1)	1.0 (0.1)	10.01	10.9 (0.6)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	44 GHz (I);	20.9 (0.1)	1.0 (0.1)	6.97	15.8 (0.6)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	44 GHz (I);	22.9 (0.1)	0.9 (0.1)	32.11	31.4 (0.6)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	44 GHz (I);	23.9 (0.1)	0.6 (0.1)	27.9	18.5 (0.6)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
12	18 34 19.8	-05 59 44	25.6471	1.0533	G25.649+1.050	18316-0602	44 GHz (I);	42.060 (0.008)	0.62 (0.02)	9.88	6.6 (0.1)	NRO	38	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		April 2002
	18 34 19.8	-05 59 44	25.6471	1.0533	G25.649+1.050	18316-0602	44 GHz (I);	43.10 (0.04)	0.70 (0.09)	2.07	1.6 (0.2)	NRO	38	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		April 2002
	18 34 19.8	-05 59 44	25.6471	1.0533	G25.649+1.050	18316-0602	44 GHz (I);	44.52 (0.09)	1.6 (0.3)	1.67	2.9 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		April 2002
15	18 38 40.3	-05 35 06	26.5080	0.2829	G26.509+0.283	18360-0537	44 GHz (I);	102.4 (0.1)	2.83 (0.2)	2.23	6.7 (0.4)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		April 2002
	18 38 40.3	-05 35 06	26.5080	0.2829	G26.509+0.283	18360-0537	44 GHz (I);	106.4 (0.3)	1.9 (0.7)	0.74	1.6 (0.4)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		April 2002
17	18 53 17.4	+01 24 55	34.4026	0.2333	G34.403+0.232	18507+0121	44 GHz (I);	60.33 (0.04)	1.3 (0.1)	7	10.0 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
18	18 54 13.8	+04 41 32	37.4267	1.5182	G37.427+1.518	18517+0437	44 GHz (I);	43.97 (0.05)	1.1 (0.1)	2.7	3.1 (0.2)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
19	19 06 47.6	+07 31 38	41.3764	0.0379	G41.377+0.038	19043+0726	44 GHz (I);	58.69 (0.03)	0.65 (0.09)	3.52	2.5 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
	19 06 47.6	+07 31 38	41.3764	0.0379	G41.377+0.038	19043+0726	44 GHz (I);	59.89 (0.08)	0.7 (0.2)	1.31	1.1 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
21	19 11 15.9	+09 07 27	43.3035	-0.2073	G43.303-0.207	19088+0902	44 GHz (I);	58.67 (0.07)	2.2 (0.2)	2	10 (1)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
22	19 40 59.3	+24 04 39	59.8316	0.6713	G59.833+0.671	19388+2357	44 GHz (I);	35.4 (0.2)	1.6 (0.4)	1.07	1.8 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
23	20 07 6.7	+27 28 53	65.7802	-2.6122	G65.780-2.612	20050+2720	44 GHz (I);	6.6 (0.1)	1.8 (0.3)	1.09	2.0 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II	SFR_MIXED		April 2002
24	20 08 9.7	+35 59 20	73.0615	1.7967	G73.062+1.796	20062+3550	44 GHz (I);	0.60 (0.06)	1.0 (0.1)	2.36	2.5 (0.2)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
25	20 14 26	+41 13 32	78.1221	3.6328	G78.122+3.633	20126+4104	44 GHz (I);	-2.43 (0.04)	2.0 (0.1)	4.17	8.9 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
26	20 20 39.3	+39 37 52	77.4622	1.7595	G77.462+1.760	20188+3928	44 GHz (I);	3 (1)	3 (2)	0.76	2 (1)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
27	21 40 42.3	+58 16 10	99.9824	4.1698	G99.982+4.170	21391+5802	44 GHz (I);	-0.49 (0.02)	0.73 (0.08)	5.33	4.2 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	GALAXY		April 2002
	21 40 42.3	+58 16 10	99.9824	4.1698	G99.982+4.170	21391+5802	44 GHz (I);	6.6 (0.1)	2.3 (0.3)	2.25	5.4 (0.4)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	GALAXY		April 2002
29	22 52 38.6	+60 00 56	108.5957	0.4925	G108.595+0.492	22506+5944	44 GHz (I);	-51.3 (0.1)	1.6 (0.6)	1.81	3 (1)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
	22 52 38.6	+60 00 56	108.5957	0.4925	G108.595+0.492	22506+5944	44 GHz (I);	-48 (1)	5 (2)	0.8	4 (2)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
31	00 44 57.6	+55 47 18	122.0145	-7.0719	G122.014-7.072	00420+5530	44 GHz (I);	-48.8 (0.3)	2.0 (0.5)	0.8	1.6 (0.4)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
32	18 04 53.9	-24 26 41	6.0501	-1.4494	G6.050-1.449	18018-2426	44 GHz (I);	11.280 (0.003)	0.669 (0.002)	339	241.1 (0.4)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
33	18 05 25.4	-21 19 41	8.8273	-0.0292	G8.832-0.028	18024-2119	44 GHz (I);	0.31 (0.02)	1.28 (0.05)	7.34	10.0 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
	18 05 25.4	-21 19 41	8.8273	-0.0292	G8.832-0.028	18024-2119	44 GHz (I);	2.7 (0.1)	2.3 (0.3)	1.4	3.1 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
35	18 17 24.4	-17 22 13	13.6568	-0.5998	G13.657-0.600	18144-1723	44 GHz (I);	48.590 (0.005)	1.54 (0.01)	25.6	42.1 (0.2)	NRO	38	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
36	18 19 7.5	-16 11 21	14.8919	-0.4026	G14.891-0.404	18162-1612	44 GHz (I);	62.80 (0.03)	0.84 (0.07)	3.2	5.1 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II	SFR_MIXED		April 2002
37	18 42 18.8	-04 28 37	27.9084	-0.0159	G27.908-0.016	18396-0431	44 GHz (I);	97.6 (0.1)	1.0 (0.3)	1	1.0 (0.2)	NRO	38	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
38	19 11 37.4	+08 46 30	43.0348	-0.4473	G43.038-0.453	19092+0841	44 GHz (I);	59.07 (0.4)	5.7 (0.7)	0.65	4.0 (0.4)	NRO	38	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
39	23 40 53.2	+61 10 21	114.5307	-0.5432	G114.531-0.543	23385+6053	44 GHz (I);	-50.6 (0.3)	3.2 (0.7)	0.9	2.9 (0.4)	NRO	38	+H₂O +CH₃OH I -CH₃OH II	SFR		April 2002
40	05 51 10.6	+25 46 14	183.3482	-0.5770	G183.348-0.577	05480+2545	95 GHz (I);	-10.6 (0.1)	1.3 (0.3)	2.2	3.1 (0.6)	NRO	18	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
41	18 11 51.3	-17 31 29	12.8887	0.4897	G12.889+0.490	18089-1732	95 GHz (I);	31.38 (0.02)	0.45 (0.05)	5.5	2.7 (0.4)	NRO	18	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
	18 11 51.3	-17 31 29	12.8887	0.4897	G12.889+0.490	18089-1732	95 GHz (I);	32.4 (0.2)	3.2 (0.4)	4.2	14 (2)	NRO	18	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
43	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	95 GHz (I);	20.1 (0.1)	1.6 (0.4)	2.7	4.7 (0.8)	NRO	18	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
	18 18 53	-16 47 39	14.3314	-0.6376	G14.332-0.642	18159-1648	95 GHz (I);	22.56 (0.06)	1.4 (0.1)	5.2	7.6 (0.6)	NRO	18	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		April 2002
45	18 34 19.8	-05 59 44	25.6471	1.0533	G25.649+1.050	18316-0602	95 GHz (I);	41.63 (0.05)	0.5 (0.1)	2.1	1.1 (0.2)	NRO	18	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		April 2002
46	18 38 40.3	-05 35 06	26.5080	0.2829	G26.509+0.283	18360-0537	95 GHz (I);	102.5 (0.1)	4.1 (0.4)	4	13.2 (0.8)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		April 2002
47	20 14 26	+41 13 32	78.1221	3.6328	G78.122+3.633	20126+4104	95 GHz (I);	-2.75 (0.08)	2.3 (0.2)	2.5	6.0 (0.4)	NRO	18	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
48	21 40 42.3	+58 16 10	99.9824	4.1698	G99.982+4.170	21391+5802	95 GHz (I);	12.1 (0.1)	1.2 (0.5)	2	2.5 (0.6)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	GALAXY		April 2002
49	22 52 38.6	+60 00 56	108.5957	0.4925	G108.595+0.492	22506+5944	95 GHz (I);	-47.1 (0.2)	2.4 (0.6)	2	5 (1)	NRO	18	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		April 2002
50	18 04 53.9	-24 26 41	6.0501	-1.4494	G6.050-1.449	18018-2426	95 GHz (I);	10.800 (0.004)	0.622 (0.009)	50	33.5 (0.4)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
51	18 17 24.4	-17 22 13	13.6568	-0.5998	G13.657-0.600	18144-1723	95 GHz (I);	47.91 (0.03)	2.07 (0.08)	12	26.4 (0.6)	NRO	18	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		April 2002
52	18 42 18.8	-04 28 37	27.9084	-0.0159	G27.908-0.016	18396-0431	95 GHz (I);	50.37 (0.08)	1.24 (0.2)	2.9	3.8 (0.4)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
	18 42 18.8	-04 28 37	27.9084	-0.0159	G27.908-0.016	18396-0431	95 GHz (I);	57.4 (0.6)	7 (1)	1.9	14 (2)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
	18 42 18.8	-04 28 37	27.9084	-0.0159	G27.908-0.016	18396-0431	95 GHz (I);	61.5 (0.1)	1.3 (0.4)	2.5	4 (1)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
	18 42 18.8	-04 28 37	27.9084	-0.0159	G27.908-0.016	18396-0431	95 GHz (I);	71.3 (0.2)	3.4 (0.6)	2.2	8.0 (0.8)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002
	18 42 18.8	-04 28 37	27.9084	-0.0159	G27.908-0.016	18396-0431	95 GHz (I);	130.50 (0.08)	0.7 (0.1)	2.1	1.6 (0.2)	NRO	18	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		April 2002

DSS colored	2MASS colored	WISE colored
PACS color (70-160 um)	SPIRE color (250-500 um)	GLIMPSE 360
SDSS color	IRAC color I1,I2,I4	NVSS (1.4GHz)
ATLASGAL 870 um	ATLASGAL 870 um + Planck	Bolocam 1.1 mm
UKIDSS K Download UKIDSS K FITS	2MASS K Download 2MASS K FITS

select MAX(met1_data_all.ra_hms) as ra_hms,MAX(met1_data_all.dec_dms) as dec_dms,MAX(met1_data_all.source_name) as source_name,MAX(met1_data_all.ra) as ra,MAX(met1_data_all.dec) as dec,MAX(met1_data_all.l) as l,MAX(met1_data_all.b) as b,MAX(met1_data_all.grp) as grp,MAX(met1_data_all.other_name) as other_name,MAX(met1_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(met1_data_all.line) as line,MAX(met1_data_all.vrange) as vrange,MAX(met1_data_all.vpeak) as vpeak,MAX(met1_data_all.peak) as peak,MAX(met1_data_all.fwhm) as fwhm,MAX(met1_data_all.int) as int,MAX(met1_data_all.rms) as rms,MAX(met1_data_all.units) as units,MAX(met1_data_all.units_rms) as units_rms,MAX(met1_data_all.date_txt) as date_txt,MAX(met1_data_all.telescope_ref) as telescope_ref,MAX(met1_data_all.telescope_conf) as telescope_conf,MAX(met1_data_all.v_step) as v_step,MAX(met1_data_all.beam) as beam,MAX(met1_data_all.beam_maj) as beam_maj,MAX(met1_data_all.beam_min) as beam_min,MAX(met1_data_all.beam_pa) as beam_pa,MAX(met1_data_all.ref) as ref,MAX(met1_data_all.list_ref) as list_ref,MAX(met1_data_all.ascii) as ascii,MAX(met1_data_all.url) as url,MAX(met1_data_all.image) as image,MAX(met1_data_all.image2) as image2,MAX(met1_data_all.image3) as image3,MAX(met1_data_all.descr) as descr,MAX(met1_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(met1_data_all.dist) as dist,1 as dist_parallax,MAX(met1_data_all.date_txt) as date_txt,MAX(line_det) as line_det,MAX(type) as type,MAX(simbad_types_cat) as simbad_types_cat FROM met1_data_all  LEFT JOIN all_objects_withmet ON met1_data_all.grp=all_objects_withmet.group_name LEFT JOIN object_categories ON all_objects_withmet.group_name = object_categories.group_name_cat AND object_categories.tbl_cat = 'all_objects_withmet' LEFT JOIN transitions ON met1_data_all.line=transitions."Line"  WHERE ref ilike 'FON10' AND detected=true AND hide=false GROUP BY ref

select met1_data_all.ra_hms,met1_data_all.dec_dms,met1_data_all.source_name,met1_data_all.ra,met1_data_all.dec,met1_data_all.l,met1_data_all.b,met1_data_all.grp,met1_data_all.other_name,met1_data_all.other_desc,met1_data_all.thermal,met1_data_all.line,met1_data_all.vrange,met1_data_all.vpeak,met1_data_all.peak,met1_data_all.fwhm,met1_data_all.int,met1_data_all.rms,met1_data_all.units,met1_data_all.units_rms,met1_data_all.date_txt,met1_data_all.telescope_ref,met1_data_all.telescope_conf,met1_data_all.v_step,met1_data_all.beam,met1_data_all.beam_maj,met1_data_all.beam_min,met1_data_all.beam_pa,met1_data_all.ref,met1_data_all.list_ref,met1_data_all.ascii,met1_data_all.url,met1_data_all.image,met1_data_all.image2,met1_data_all.image3,met1_data_all.descr,met1_data_all.id,met1_data_all.mjy_flag,met1_data_all.rms_mjy_flag,met1_data_all.dist,met1_data_all.dist_parallax,met1_data_all.date_txt,line_det,type,simbad_types_cat FROM met1_data_all   LEFT JOIN all_objects_withmet ON met1_data_all.grp=all_objects_withmet.group_name LEFT JOIN object_categories ON all_objects_withmet.group_name = object_categories.group_name_cat AND object_categories.tbl_cat = 'all_objects_withmet' LEFT JOIN transitions ON met1_data_all.line=transitions."Line"  WHERE ref ilike 'FON10' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

FON10 - Class I and Class II methanol masers in high-mass star-forming regions

View as list of objects

Detection table from Fontani et al. (2010)