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OUY19 - The Relationship between 6.7 GHz Methanol Masers and Radio Recombination Lines in High-mass Star-forming Regions

Short title: Ouyang et al. (2019)
Authors: Ouyang, Xu-JiaChen, XiShen, Zhi-QiangYang, KaiLi, Xiao-QiongChen, Hong-YingZhao, ZhangSobolev, Andrej M.
Journal: The Astrophysical Journal Supplement Series, Volume 245, Issue 1, article id. 12, 17 pp. (2019).
Bibcode:
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Target type: High_mass_SFR,MSX
Observations category: SF.general
Facility type: single-dish
Transitions: OH_4765,OH_6030,OH_6035,CH3OH_44(I),CH3OH_95(I),CH3OH_6(II)

Abstract
We report a systematic survey of a 6.7 GHz Class II methanol maser toward a sample of 448 sources selected from the Red Midcourse Space Experiment Source catalog. These sample sources are composed of high-mass star-forming region (HMSFR) candidates and have been studied as tracers of HMSFRs, such as water masers or radio continuum emission of ultracompact H II region. The survey was conducted using the Shanghai Tianma Radio Telescope. Through the observations, we simultaneously studied the 4.7 and 6.0 GHz excited-state interstellar hydroxyl (OH) maser lines and 10 hydrogen radio recombination lines (RRLs) in the C band. In total, we detected 6.7 GHz methanol masers and RRLs from 102 and 116 sources, respectively. In addition, 4, 3, and 10 sources exhibit OH masers at 4765.56, 6030.75, and 6035.09 MHz transitions, respectively. Through the survey, we identified four new 6.7 GHz methanol maser sources and three new excited-state OH maser sources (one at 4750 MHz and two at 6035 MHz). The statistical analysis demonstrated that there is a positive correlation of luminosity between 6.7 GHz methanol masers and RRLs. A good correlation of integrated luminosity between radio continuum emission and the 6.7 GHz methanol masers is presented with respect to the RRL emission sources. The average of the integrated luminosities of the RRLs in the sources with 6.7 GHz masers is greater than those without the 6.7 GHz masers; similarly, the average of integrated luminosities of the 6.7 GHz methanol masers in the sources with RRLs is greater than those without the RRLs. Moreover, we found that the averages of the emission measure and electron temperature of H II regions associated with 6.7 GHz methanol masers are larger than those without the 6.7 GHz methanol masers. This suggests that the masers are most likely produced in high gas density and luminous regions with brighter RRLs and higher radio continuum emission.

Abstract

We report a systematic survey of a 6.7 GHz Class II methanol maser toward a sample of 448 sources selected from the Red Midcourse Space Experiment Source catalog. These sample sources are composed of high-mass star-forming region (HMSFR) candidates and have been studied as tracers of HMSFRs, such as water masers or radio continuum emission of ultracompact H II region. The survey was conducted using the Shanghai Tianma Radio Telescope. Through the observations, we simultaneously studied the 4.7 and 6.0 GHz excited-state interstellar hydroxyl (OH) maser lines and 10 hydrogen radio recombination lines (RRLs) in the C band. In total, we detected 6.7 GHz methanol masers and RRLs from 102 and 116 sources, respectively. In addition, 4, 3, and 10 sources exhibit OH masers at 4765.56, 6030.75, and 6035.09 MHz transitions, respectively. Through the survey, we identified four new 6.7 GHz methanol maser sources and three new excited-state OH maser sources (one at 4750 MHz and two at 6035 MHz). The statistical analysis demonstrated that there is a positive correlation of luminosity between 6.7 GHz methanol masers and RRLs. A good correlation of integrated luminosity between radio continuum emission and the 6.7 GHz methanol masers is presented with respect to the RRL emission sources. The average of the integrated luminosities of the RRLs in the sources with 6.7 GHz masers is greater than those without the 6.7 GHz masers; similarly, the average of integrated luminosities of the 6.7 GHz methanol masers in the sources with RRLs is greater than those without the RRLs. Moreover, we found that the averages of the emission measure and electron temperature of H II regions associated with 6.7 GHz methanol masers are larger than those without the 6.7 GHz methanol masers. This suggests that the masers are most likely produced in high gas density and luminous regions with brighter RRLs and higher radio continuum emission.

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Detection table from Ouyang et al. (2019)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Line	V_peak	F_peak	∫F dv	Telescope	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				CH₃OH (class I)	(km/s)	(Jy)	(Jy*km/s)		Yes/No		(kpc)
1	18 12 23.7	-18 22 51.6	12.1994	-0.0344	G12.199-0.033	G12.1992-0.0335	G012.1993-00.0342	44 GHz (I);	52.7	4.3	6.5	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
2	18 12 23.7	-18 22 51.6	12.1994	-0.0344	G12.199-0.033	G12.1992-0.0335	G012.1993-00.0342	95 GHz (I);	49.4	4	7.5	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
3	18 11 50.7	-17 31 14.5	12.8910	0.4937	G12.889+0.490	G12.8887+0.4897	G012.8909+00.4938	44 GHz (I);	31.4	20.5	25.9	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
4	18 11 50.7	-17 31 14.5	12.8910	0.4937	G12.889+0.490	G12.8887+0.4897	G012.8909+00.4938	95 GHz (I);	31.4	21.9	30.8	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
5	18 14 39.7	-17 51 59	12.9092	-0.2609	G12.908-0.260	G12.9084-0.2602	G012.9090-00.2607	44 GHz (I);	36.4	9.6	23.4	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
6	18 14 39.7	-17 51 59	12.9092	-0.2609	G12.908-0.260	G12.9084-0.2602	G012.9090-00.2607	95 GHz (I);	36.4	9.3	18.6	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
7	18 17 24.4	-17 22 14.5	13.6564	-0.5998	G13.657-0.600	G13.6567-0.5995	G013.6562-00.5997	44 GHz (I);	48.6	52.4	67.2	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
8	18 17 24.4	-17 22 14.5	13.6564	-0.5998	G13.657-0.600	G13.6567-0.5995	G013.6562-00.5997	95 GHz (I);	48.4	40.5	51.6	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
9	18 17 20.9	-15 43 47.3	15.0941	0.1913	G15.094+0.192	G15.0942+0.1915	G015.0939+00.1913	44 GHz (I);	30.4	3.5	1.4	TMRT	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		2017 Mar-Aug
10	18 24 50.4	-12 39 20.9	18.6610	0.0371	G18.666+0.033	G18.6619+0.0345	G018.6608+00.0372	44 GHz (I);	79.4	7	16.9	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
11	18 24 50.4	-12 39 20.9	18.6610	0.0371	G18.666+0.033	G18.6619+0.0345	G018.6608+00.0372	95 GHz (I);	80.3	4	9.6	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
12	18 29 14.4	-11 50 30.1	19.8819	-0.5348	G19.884-0.535	G19.8838-0.5348	G019.8817-00.5347	44 GHz (I);	43.6	31.9	44.9	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
13	18 29 14.4	-11 50 30.1	19.8819	-0.5348	G19.884-0.535	G19.8838-0.5348	G019.8817-00.5347	95 GHz (I);	43.1	64.8	117.6	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
14	18 33 14.4	-08 23 57.5	23.3892	0.1851	G23.389+0.185	G23.3891+0.1853	G023.3891+00.1851	44 GHz (I);	77.7	7.2	5	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
15	18 33 14.4	-08 23 57.5	23.3892	0.1851	G23.389+0.185	G23.3891+0.1853	G023.3891+00.1851	95 GHz (I);	77.8	9.5	4.1	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
16	18 33 19.5	-07 55 38.3	23.8177	0.3841	G23.818+0.384	G23.8179+0.3841	G023.8176+00.3841	44 GHz (I);	75.4	7.5	11.1	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
17	18 33 19.5	-07 55 38.3	23.8177	0.3841	G23.818+0.384	G23.8179+0.3841	G023.8176+00.3841	95 GHz (I);	75	2.6	8.1	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
18	18 45 59.6	-02 45 7.9	29.8621	-0.0446	G29.862-0.044	G29.8624-0.0442	G029.8620-00.0444	44 GHz (I);	100.9	4.1	1.7	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
19	18 48 10.8	-01 45 29.2	30.9960	-0.0772	G31.000-0.075	G30.9996-0.0751	G030.9959-00.0771	44 GHz (I);	82.8	2.7	3.1	TMRT	+H₂O +CH₃OH I +CH₃OH II	SFR		2017 Mar-Aug
20	18 58 13.1	+01 40 39.4	35.1980	-0.7429	G35.197-0.743	G35.1970-0.7430	G035.1979-00.7427	44 GHz (I);	34.9	23.2	50	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
21	18 58 13.1	+01 40 39.4	35.1980	-0.7429	G35.197-0.743	G35.1970-0.7430	G035.1979-00.7427	95 GHz (I);	35	18.6	50.4	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
22	19 03 45.7	+05 40 41.5	39.3881	-0.1423	G39.388-0.141	G39.3877-0.1407	G039.3880-00.1421	44 GHz (I);	66.6	2.5	4.9	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
23	19 03 45.7	+05 40 41.5	39.3881	-0.1423	G39.388-0.141	G39.3877-0.1407	G039.3880-00.1421	95 GHz (I);	66.4	5.7	3.2	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
24	19 22 26.2	+14 06 37.8	48.9898	-0.2994	G48.990-0.299	G48.9901-0.2994	G048.9897-00.2992	44 GHz (I);	66.4	80.3	101.4	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
25	19 22 26.2	+14 06 37.8	48.9898	-0.2994	G48.990-0.299	G48.9901-0.2994	G048.9897-00.2992	95 GHz (I);	66.4	36.3	84.4	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
26	19 21 24.8	+15 28 10.6	50.0722	0.5591	G50.071+0.559	G50.0715+0.5586	G050.0721+00.5591	44 GHz (I);	-4.3	4	1.5	TMRT	+H₂O +CH₃OH I +CH₃OH II	SFR		2017 Mar-Aug
27	19 21 24.8	+15 28 10.6	50.0722	0.5591	G50.071+0.559	G50.0715+0.5586	G050.0721+00.5591	95 GHz (I);	-4.5	2.7	1.6	TMRT	+H₂O +CH₃OH I +CH₃OH II	SFR		2017 Mar-Aug
28	19 28 55.9	+17 52 0.5	53.0367	0.1110	G53.036+0.113	G53.0365+0.1118	G053.0366+00.1110	44 GHz (I);	6.2	4.5	10.5	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
29	19 28 55.9	+17 52 0.5	53.0367	0.1110	G53.036+0.113	G53.0365+0.1118	G053.0366+00.1110	95 GHz (I);	5.4	3.1	6.9	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
30	20 29 24.9	+40 11 19.3	78.8868	0.7087	G78.887+0.709	G78.8867+0.7090	G078.8867+00.7087	44 GHz (I);	-6	3.5	0.7	TMRT	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		2017 Mar-Aug
31	20 29 24.9	+40 11 19.3	78.8868	0.7087	G78.887+0.709	G78.8867+0.7090	G078.8867+00.7087	95 GHz (I);	-6.3	2.5	1.8	TMRT	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		2017 Mar-Aug
32	20 38 35.4	+42 37 16	81.8652	0.7799	G81.871+0.781	G81.8652+0.7799	G081.8652+00.7800	44 GHz (I);	8.8	13.6	23.5	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
33	20 38 35.4	+42 37 16	81.8652	0.7799	G81.871+0.781	G81.8652+0.7799	G081.8652+00.7800	95 GHz (I);	8.9	6.8	22	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
34	23 13 43.9	+61 26 58.2	111.5320	0.7593	G111.542+0.769	G111.5330+0.7577	G111.5320+00.7593	44 GHz (I);	-57.2	26	53.1	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
35	23 13 43.9	+61 26 58.2	111.5320	0.7593	G111.542+0.769	G111.5330+0.7577	G111.5320+00.7593	95 GHz (I);	-53.5	10.9	41.4	TMRT	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
36	02 25 31.1	+62 06 22.3	133.6946	1.2165	G133.694+1.216	G133.6945+1.2152	G133.6945+01.2166	44 GHz (I);	-42.6	2.2	5.2	TMRT	+H₂O +CH₃OH I -CH₃OH II -OH	SFR		2017 Mar-Aug
37	02 25 31.1	+62 06 22.3	133.6946	1.2165	G133.694+1.216	G133.6945+1.2152	G133.6945+01.2166	95 GHz (I);	-43.2	3	6	TMRT	+H₂O +CH₃OH I -CH₃OH II -OH	SFR		2017 Mar-Aug

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

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.grpv) as grpv,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 'OUY19' 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.grpv,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 'OUY19' AND detected=true AND hide=false ORDER BY detected DESC,id

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OUY19 - The Relationship between 6.7 GHz Methanol Masers and Radio Recombination Lines in High-mass Star-forming Regions

View as list of objects

Detection table from Ouyang et al. (2019)