Display data from paper

Select data type:

SUN14 - 6.7 GHz methanol maser survey toward GLIMPSE point sources and BGPS 1.1 mm dust clumps

Short title: Sun et al. (2014)
Authors: Sun, Yan Xu, Ye Chen, Xi Zhang, Bo Wu, Yuan-Wei Henkel, Christian Brunthaler, Andreas Choi, Yoon Kyung Zheng, Xing-Wu
Journal: Astronomy & Astrophysics, Volume 563, id.A130, 21 pp.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (30 detection)
Target type: GLIMPSE,Bolocam
Transitions: CH3OH_6(II),CH3OH_12(II)

Abstract
We present the results of a 6.7 GHz methanol maser survey from the Effelsberg 100 m radio telescope. A sample of 404 sources from the Bolocam Galactic Plane Survey (BGPS) 1.1 mm dust clump survey that met specific Galactic Legacy Infrared Mid-Plane Survey Extraodinaire (GLIMPSE) point-source color criteria was selected and 318 of these were observed. The new observations resulted in the detection of 29 methanol masers, including 12 new ones. Together with the additional 74 detections from the literature, this means that a total of 103 methanol masers are coincident with 1.1 mm dust clumps, yielding an overall detection rate of 26%. A comparison of the properties of a 1.1 mm dust clump and a 6.7 GHz methanol maser indicates that methanol masers with a higher flux density and/or luminosity are generally associated with more massive but less dense 1.1 mm dust clumps. The overall detection rate of 26% appears to vary as a function of the derived H₂ column density of the associated 1.1 mm dust clump. The methanol masers were primarily detected toward the brighter and more massive 1.1 mm dust clumps. A subsample of 194 sources that overlapped sources with observations of the 95 GHz methanol line was investigated in more detail for the properties of 1.1 mm dust clumps. The statistical analysis reveals that 1.1 mm dust clumps with both class I and II counterparts have much higher mean and median values of mass, column density, and flux density than those with only class I or II counterparts. Based on our much larger sample, we slightly revise the boundary defined previously for selecting BGPS sources associated with a class II methanol maser, wherein ~80% of expected class II methanol masers will be detected with a detection rate in the range of 40-50%.

Abstract

We present the results of a 6.7 GHz methanol maser survey from the Effelsberg 100 m radio telescope. A sample of 404 sources from the Bolocam Galactic Plane Survey (BGPS) 1.1 mm dust clump survey that met specific Galactic Legacy Infrared Mid-Plane Survey Extraodinaire (GLIMPSE) point-source color criteria was selected and 318 of these were observed. The new observations resulted in the detection of 29 methanol masers, including 12 new ones. Together with the additional 74 detections from the literature, this means that a total of 103 methanol masers are coincident with 1.1 mm dust clumps, yielding an overall detection rate of 26%. A comparison of the properties of a 1.1 mm dust clump and a 6.7 GHz methanol maser indicates that methanol masers with a higher flux density and/or luminosity are generally associated with more massive but less dense 1.1 mm dust clumps. The overall detection rate of 26% appears to vary as a function of the derived H₂ column density of the associated 1.1 mm dust clump. The methanol masers were primarily detected toward the brighter and more massive 1.1 mm dust clumps. A subsample of 194 sources that overlapped sources with observations of the 95 GHz methanol line was investigated in more detail for the properties of 1.1 mm dust clumps. The statistical analysis reveals that 1.1 mm dust clumps with both class I and II counterparts have much higher mean and median values of mass, column density, and flux density than those with only class I or II counterparts. Based on our much larger sample, we slightly revise the boundary defined previously for selecting BGPS sources associated with a class II methanol maser, wherein ~80% of expected class II methanol masers will be detected with a detection rate in the range of 40-50%.

Download as: Table (CSV)
View paper data

Detection table from Sun et al. (2014)

Export table to csv

Hide / Show individual components

ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Line	V_range	V_peak	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			PID	CH₃OH (class II)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	18 01 2.6	-23 47 6.9	6.1908	-0.3591	G6.189-0.358	06.189-0.358	1175	6.6 GHz (II);	-37.5;-27.1	-30.2	0.5(0.25)	0.8	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		October and November 2011
2	18 12 23.8	-18 22 45	12.2013	-0.0340	G12.199-0.034	12.199-0.033	1682	6.6 GHz (II);	48.2;57.3	49.3	14.6(0.17)	22.3	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
3	18 14 36.4	-17 54 50.2	12.8612	-0.2721	G12.860-0.272	12.909-0.260	1796	6.6 GHz (II);	38.6;40.6	39.8	2.3(0.13)	2.4	EFF	120	+H₂O -CH₃OH I +CH₃OH II	SFR		October and November 2011
4	18 13 48.2	-17 45 34.4	12.9052	-0.0301	G12.904-0.031	12.904-0.031	1809	6.6 GHz (II);	58.2;60.4	58.8	60.3(0.24)	44.4	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
5	18 21 8.9	-15 03 48.2	16.1144	-0.3010	G16.117-0.291	16.112-0.303	2246	6.6 GHz (II);	34.1;35.1	34.5	2.2(0.11)	1	EFF	120	+H₂O -CH₃OH I +CH₃OH II +OH +SiO	SFR_MIXED		October and November 2011
6	18 27 08	-12 41 38.3	18.8881	-0.4754	G18.888-0.475	18.888-0.475	2467	6.6 GHz (II);	52.9;57.9	56.5	6.3(0.13)	8.2	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
7	18 26 8.7	-11 52 39.2	19.4979	0.1187	G19.485+0.151	19.496+0.115	2579	6.6 GHz (II);	120.7;121.8	121.1	4.8(0.14)	2.2	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		October and November 2011
8	18 27 31.9	-11 45 53.1	19.7560	-0.1292	G19.754-0.128	19.755-0.128	2619	6.6 GHz (II);	115.9;123.4	123	2.2(0.08)	1.7	EFF	120	-H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
9	18 34 45.7	-08 55 55.3	23.0898	-0.3942	G23.090-0.394	23.010-00.411	2994	6.6 GHz (II);	72.8;76.6	74.9	1.2(0.09)	1.9	EFF	120	-H₂O +CH₃OH II	SFR		October and November 2011
10	18 34 36	-08 29 32.2	23.4616	-0.1560	G23.462-0.156	23.437-0.184	3081	6.6 GHz (II);	96.3;108.1	97.7	2.4(0.11)	6.9	EFF	120	-H₂O -CH₃OH I +CH₃OH II	SFR		October and November 2011
11	18 35 39.9	-07 18 32.7	24.6334	0.1545	G24.633+0.154	24.63+00.16	3383	6.6 GHz (II);	113.8;115.6	114.4	1.3(0.09)	0.7	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
12	18 36 17.1	-06 43 11.8	25.2274	0.2887	G25.227+0.289	25.23+00.29	3474	6.6 GHz (II);	41.2;42.3	41.8	0.7(0.11)	0.2	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		October and November 2011
13	18 38 32	-06 21 28.6	25.8055	-0.0412	G25.805-0.041	25.81-00.04	3591	6.6 GHz (II);	97.1;98.1	97.4	1.3(0.20)	0.5	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		October and November 2011
14	18 39 5.9	-06 17 59.3	25.9215	-0.1392	G25.920-0.141	25.92-00.14	3616	6.6 GHz (II);	111.4;115.6	113.9	1.4(0.10)	1.2	EFF	120	+CH₃OH II +OH	SFR		October and November 2011
15	18 40 52.1	-05 48 15.5	26.5634	-0.3031	G26.555-0.303	26.53-0.27	3690	6.6 GHz (II);	102.1;110.5	107.1	1.0(0.09)	1.9	EFF	120	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		October and November 2011
16	18 41 20.3	-04 44 25	27.5630	0.0798	G27.563+0.080	27.56+00.08	3807	6.6 GHz (II);	78.2;88.5	87.2	2.5(0.11)	1.9	EFF	120	+H₂O -CH₃OH I +CH₃OH II	SFR		October and November 2011
17	18 41 33.5	-04 01 34.5	28.2231	0.3577	G28.223+0.358	28.22+00.36	3917	6.6 GHz (II);	48.4;51.5	50.3	7.7(0.15)	6.4	EFF	120	-H₂O -CH₃OH I +CH₃OH II	SFR		October and November 2011
18	18 47 40.8	-02 20 31.2	30.4194	-0.2324	G30.419-0.232	30.42-00.23	4398	6.6 GHz (II);	102.4;105.1	103	14.1(0.14)	6.6	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
19	18 45 12.2	-02 01 10.9	30.4236	0.4656	G30.423+0.465	30.42+0.46	4403	6.6 GHz (II);	4.5;9.2	6.4	0.7(0.06)	1.8	EFF	120	+H₂O +CH₃OH II	SFR		October and November 2011
20	18 47 6.6	-01 38 21.6	30.9796	0.2151	G30.980+0.216	30.98+00.22	4636	6.6 GHz (II);	110;111.8	110.9	1.0(0.10)	0.5	EFF	120	-H₂O -CH₃OH I +CH₃OH II	SFR_MIXED		October and November 2011
21	18 46 25.2	-01 26 26.8	31.0776	0.4591	G31.078+0.459	31.08+00.46	4673	6.6 GHz (II);	24.7;27.6	25.7	2.1(0.10)	2.1	EFF	120	-H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		October and November 2011
22	18 48 45.6	-01 37 25.9	31.1816	-0.1449	G31.182-0.148	31.18-00.15	4701	6.6 GHz (II);	42.6;50.1	46.2	2.7(0.17)	3.8	EFF	120	-CH₃OH I +CH₃OH II	SFR		October and November 2011
23	18 51 21.6	-00 10 4.9	32.7735	-0.0593	G32.773-0.059	32.745-0.076	5050	6.6 GHz (II);	29.4;39.8	38.5	8.9(0.26)	19.4	EFF	120	-H₂O +CH₃OH II	SFR		October and November 2011
24	18 54 37.1	+01 05 23.6	34.2644	-0.2105	G34.267-0.210	34.26-00.21	5342	6.6 GHz (II);	49.5;55.4	54.6	9.0(0.13)	7.3	EFF	120	-H₂O -CH₃OH I +CH₃OH II +OH	SFR		October and November 2011
25	19 23 6.9	+14 20 11	49.2666	-0.3379	G49.267-0.337	49.490-0.388	6323	6.6 GHz (II);	58.6;60.3	59.3	0.7(0.06)	0.4	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
26	19 23 30.1	+14 26 34.6	49.4047	-0.3698	G49.412-0.371	49.490-0.388	6346	6.6 GHz (II);	57.6;60.4	59.3	5.1(0.17)	3.9	EFF	120	+H₂O -CH₃OH I +CH₃OH II	SFR		October and November 2011
27	19 29 18.2	+17 56 19	53.1421	0.0677	G53.142+0.070	53.142+0.071	6414	6.6 GHz (II);	23.9;25.4	24.7	1.1(0.21)	0.6	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		October and November 2011
28	19 30 22.7	+18 20 20.9	53.6160	0.0356	G53.618+0.035	53.618+0.036	6433	6.6 GHz (II);	18.3;19.7	18.9	6.0(0.11)	2.7	EFF	120	-H₂O -CH₃OH I +CH₃OH II +OH	SFR		October and November 2011
29	19 38 16.8	+21 08 2.2	56.9618	-0.2340	G56.962-0.234	56.96-00.23	6470	6.6 GHz (II);	29.3;30.6	29.8	1.1(0.06)	0.4	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011
30	19 43 50.1	+23 28 59.7	59.6391	-0.1892	G59.634-0.189	59.63-0.19	6479	6.6 GHz (II);	28.4;31.2	29.6	0.9(0.10)	0.5	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		October and November 2011

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

Tip: Click on some source to get more informaiton

Distribution of sources in IRAS color-color diagram

Tip: Use "Box select" or "Lasso select" to display colour-selected sources in Aladin all-sky view

Tip: Click on some source to look at the different surveys. You must select some surveys in previous page at "View images"

Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from SUN14

Tip: Use "Box select" or "Lasso select" to display velocity-selected sources in Aladin all-sky view