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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	Image	Line	Frequency	V_range	V_peak	F_peak	∫F dv	Telescope	V_step	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					OH	(MHz)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(km/s)	(arcsec)	Yes/No		(kpc)
1	18 20 19.4	-16 13 31.1	14.9960	-0.6734	G15.034-0.677	G14.9963-0.6733	G014.9958-00.6732		6035 MHz;	6035	20.5;24	21.6	4.1	1.8	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH			2017 Mar-Aug
	18 20 19.4	-16 13 31.1	14.9960	-0.6734	G15.034-0.677	G14.9963-0.6733	G014.9958-00.6732		6035 MHz;	6035	20.5;24	21.6	4.1	1.8	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH			2017 Mar-Aug
3	18 20 25.5	-16 11 35.5	15.0357	-0.6797	G15.034-0.677	G15.0346-0.6770	G015.0357-00.6795	Image	6030;	6031	20;24	21.8	0.9	0.5	TMRT	0.07	157.8	+H₂O +CH₃OH I +CH₃OH II +OH			2017 Mar-Aug
4	18 20 25.5	-16 11 35.5	15.0357	-0.6797	G15.034-0.677	G15.0346-0.6770	G015.0357-00.6795	Image	6035 MHz;	6035	20.5;24	21.7	13.8	7	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH			2017 Mar-Aug
	18 20 25.5	-16 11 35.5	15.0357	-0.6797	G15.034-0.677	G15.0346-0.6770	G015.0357-00.6795	Image	6035 MHz;	6035	20.5;24	21.7	13.8	7	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH			2017 Mar-Aug
6	18 36 10.7	-07 11 18.6	24.7991	0.0969	G24.790+0.084	G24.7991+0.0969	G024.7989+00.0969	Image	6035 MHz;	6035	111;116	113.1	0.3	0.2	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
	18 36 10.7	-07 11 18.6	24.7991	0.0969	G24.790+0.084	G24.7991+0.0969	G024.7989+00.0969	Image	6035 MHz;	6035	111;116	113.1	0.3	0.2	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
8	18 38 2.9	-06 23 46	25.7162	0.0485	G25.710+0.044	G25.7160+0.0486	G025.7161+00.0486	Image	6035 MHz;	6035	92;98	94.7	0.5	0.6	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
	18 38 2.9	-06 23 46	25.7162	0.0485	G25.710+0.044	G25.7160+0.0486	G025.7161+00.0486	Image	6035 MHz;	6035	92;98	94.7	0.5	0.6	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
10	18 42 58.2	-04 13 56.3	28.2008	-0.0495	G28.200-0.050	G28.2001-0.0493	G028.2007-00.0494	Image	6030;	6031	93;100	95.8	0.6	0.6	TMRT	0.07	157.8	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
11	18 42 58.2	-04 13 56.3	28.2008	-0.0495	G28.200-0.050	G28.2001-0.0493	G028.2007-00.0494	Image	6035 MHz;	6035	92;100	95.7	1.3	2.2	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
	18 42 58.2	-04 13 56.3	28.2008	-0.0495	G28.200-0.050	G28.2001-0.0493	G028.2007-00.0494	Image	6035 MHz;	6035	92;100	95.7	1.3	2.2	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
13	19 10 21.8	+09 05 2.4	43.1651	-0.0286	G43.166+0.011	G43.1648-0.0283	G043.1650-00.0285	Image	6035 MHz;	6035	8;20	11.7	0.5	0.9	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
	19 10 21.8	+09 05 2.4	43.1651	-0.0286	G43.166+0.011	G43.1648-0.0283	G043.1650-00.0285	Image	6035 MHz;	6035	8;20	11.7	0.5	0.9	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
15	19 22 26.2	+14 06 37.8	48.9898	-0.2994	G48.990-0.299	G48.9901-0.2994	G048.9897-00.2992	Image	6035 MHz;	6035	66;71	68	1.2	1.1	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
	19 22 26.2	+14 06 37.8	48.9898	-0.2994	G48.990-0.299	G48.9901-0.2994	G048.9897-00.2992	Image	6035 MHz;	6035	66;71	68	1.2	1.1	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
17	19 23 40.1	+14 31 07	49.4903	-0.3695	G49.489-0.385	G49.4894-0.3695	G049.4903-00.3694	Image	6030;	6031	51;55	52.7	0.7	0.6	TMRT	0.07	157.8	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR_MIXED		2017 Mar-Aug
18	19 23 40.1	+14 31 07	49.4903	-0.3695	G49.489-0.385	G49.4894-0.3695	G049.4903-00.3694	Image	6035 MHz;	6035	51;64	55.6	3.4	5.4	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR_MIXED		2017 Mar-Aug
	19 23 40.1	+14 31 07	49.4903	-0.3695	G49.489-0.385	G49.4894-0.3695	G049.4903-00.3694	Image	6035 MHz;	6035	51;64	55.6	3.4	5.4	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR_MIXED		2017 Mar-Aug
20	19 23 50.7	+14 32 56.4	49.5375	-0.3930	G49.537-0.393	G49.5375-0.3930	G049.5373-00.3929		6035 MHz;	6035	53;59	55.4	0.3	0.5	TMRT	0.07		+H₂O -CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
	19 23 50.7	+14 32 56.4	49.5375	-0.3930	G49.537-0.393	G49.5375-0.3930	G049.5373-00.3929		6035 MHz;	6035	53;59	55.4	0.3	0.5	TMRT	0.07		+H₂O -CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
22	20 39 1.4	+42 22 47.3	81.7221	0.5699	G81.718+0.571	G81.7215+0.5721	G081.7220+00.5699	Image	4765 MHz;	4765	1;6	3.8	4.1	4.7	TMRT	0.09	199.8	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		2017 Mar-Aug
23	20 38 35.4	+42 37 16	81.8652	0.7799	G81.871+0.781	G81.8652+0.7799	G081.8652+00.7800	Image	6035 MHz;	6035	5;10	7.2	1.3	1.5	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
	20 38 35.4	+42 37 16	81.8652	0.7799	G81.871+0.781	G81.8652+0.7799	G081.8652+00.7800	Image	6035 MHz;	6035	5;10	7.2	1.3	1.5	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
25	21 43 1.5	+54 56 19	98.0361	1.4462	G98.035+1.446	G98.0354+1.4458	G098.0361+01.4462	Image	6035 MHz;	6035	-64;-60	-61.8	0.5	0.2	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
	21 43 1.5	+54 56 19	98.0361	1.4462	G98.035+1.446	G98.0354+1.4458	G098.0361+01.4462	Image	6035 MHz;	6035	-64;-60	-61.8	0.5	0.2	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2017 Mar-Aug
27	23 13 43.9	+61 26 58.2	111.5320	0.7593	G111.542+0.769	G111.5330+0.7577	G111.5320+00.7593	Image	6035 MHz;	6035	-62;-57	-59.4	0.7	0.5	TMRT	0.07		+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2017 Mar-Aug
	23 13 43.9	+61 26 58.2	111.5320	0.7593	G111.542+0.769	G111.5330+0.7577	G111.5320+00.7593	Image	6035 MHz;	6035	-62;-57	-59.4	0.7	0.5	TMRT	0.07		+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
UKIDSS K Download UKIDSS K FITS	2MASS K Download 2MASS K FITS

select MAX(oh_data_all.ra_hms) as ra_hms,MAX(oh_data_all.dec_dms) as dec_dms,MAX(oh_data_all.source_name) as source_name,MAX(oh_data_all.ra) as ra,MAX(oh_data_all.dec) as dec,MAX(oh_data_all.l) as l,MAX(oh_data_all.b) as b,MAX(oh_data_all.grp) as grp,MAX(oh_data_all.grpv) as grpv,MAX(oh_data_all.other_name) as other_name,MAX(oh_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(oh_data_all.line) as line,MAX(oh_data_all.freq) as freq,MAX(oh_data_all.pol) as pol,MAX(oh_data_all.vrange) as vrange,MAX(oh_data_all.vpeak) as vpeak,MAX(oh_data_all.peak) as peak,MAX(oh_data_all.fwhm) as fwhm,MAX(oh_data_all.int) as int,MAX(oh_data_all.rms) as rms,MAX(oh_data_all.units) as units,MAX(oh_data_all.units_rms) as units_rms,MAX(oh_data_all.date_txt) as date_txt,MAX(oh_data_all.telescope_ref) as telescope_ref,MAX(oh_data_all.telescope_conf) as telescope_conf,MAX(oh_data_all.v_step) as v_step,MAX(oh_data_all.beam) as beam,MAX(oh_data_all.beam_maj) as beam_maj,MAX(oh_data_all.beam_min) as beam_min,MAX(oh_data_all.beam_pa) as beam_pa,MAX(oh_data_all.ref) as ref,MAX(oh_data_all.list_ref) as list_ref,MAX(oh_data_all.ascii) as ascii,MAX(oh_data_all.url) as url,MAX(oh_data_all.image) as image,MAX(oh_data_all.image2) as image2,MAX(oh_data_all.image3) as image3,MAX(oh_data_all.descr) as descr,MAX(oh_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(oh_data_all.dist) as dist,1 as dist_parallax,MAX(oh_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 oh_data_all  LEFT JOIN all_objects_withmet ON oh_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 oh_data_all.line=transitions."Line"  WHERE ref ilike 'OUY19' AND detected=true AND hide=false GROUP BY ref

select oh_data_all.ra_hms,oh_data_all.dec_dms,oh_data_all.source_name,oh_data_all.ra,oh_data_all.dec,oh_data_all.l,oh_data_all.b,oh_data_all.grp,oh_data_all.grpv,oh_data_all.other_name,oh_data_all.other_desc,oh_data_all.thermal,oh_data_all.line,oh_data_all.freq,oh_data_all.pol,oh_data_all.vrange,oh_data_all.vpeak,oh_data_all.peak,oh_data_all.fwhm,oh_data_all.int,oh_data_all.rms,oh_data_all.units,oh_data_all.units_rms,oh_data_all.date_txt,oh_data_all.telescope_ref,oh_data_all.telescope_conf,oh_data_all.v_step,oh_data_all.beam,oh_data_all.beam_maj,oh_data_all.beam_min,oh_data_all.beam_pa,oh_data_all.ref,oh_data_all.list_ref,oh_data_all.ascii,oh_data_all.url,oh_data_all.image,oh_data_all.image2,oh_data_all.image3,oh_data_all.descr,oh_data_all.id,oh_data_all.mjy_flag,oh_data_all.rms_mjy_flag,oh_data_all.dist,oh_data_all.dist_parallax,oh_data_all.date_txt,line_det,type,simbad_types_cat FROM oh_data_all   LEFT JOIN all_objects_withmet ON oh_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 oh_data_all.line=transitions."Line"  WHERE ref ilike 'OUY19' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

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)