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CHE16 - Class I methanol megamasers: a potential probe of starburst activity and feedback in active galaxies

Short title: Chen et al. (2016)
Authors: Chen, X. Ellingsen, S. P. Zhang, J.-S. Wang, J.-Z. Shen, Z.-Q. Wu, Q.-W. Wu, Z.-Z.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 459, Issue 1, p.357-365
Bibcode:

Target type: Extragalactic
Transitions: SiO_1-0v0,CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_84(I),CH3OH_95(I),CH3OH_6(II),CH3OH_37(II),CH3OH_38(II)

Abstract
Previous observations have shown that the distribution of 36.2-GHz class I methanol megamaser (MM) emission in Arp 220 is highly correlated with the diffuse X-rays. On this basis it was suggested that methanol MM may be produced either by the effects of galactic-outflow-driven shocks and/or cosmic rays. Here we report the results of a single-dish survey undertaken with the Greenbank Telescope (GBT) to improve our understanding of the pumping conditions of extragalactic class I methanol masers and their relationship to starburst and feedback processes within the host galaxies, towards a sample which includes 16 galaxies which show both extended soft X-ray emission, and either OH or H₂O MM emission. Large baseline ripples in the GBT spectra limited our results to tentative detections towards 11 of the target galaxies. Analysis of these tentative detections shows that there are significant correlations between the methanol intensity and the host-galaxy infrared, radio and OH MM emission, but no correlation with the X-ray and H₂O MM emission. Some sources show methanol emission significantly offset from the systemic velocity of the galaxy (by up to 1000 km s^-1) and we propose that these are associated with galactic-scale outflows from active galactic nuclei (AGNs) feedback. The combined observational properties suggest that class I methanol MMs are related to significant starburst and molecular outflow activity and hence may provide a potential probe of AGN feedback and starburst processes in the host galaxies.	Comments: Extended X-ray galaxies which show megamaser emission from water or OH

Abstract

Previous observations have shown that the distribution of 36.2-GHz class I methanol megamaser (MM) emission in Arp 220 is highly correlated with the diffuse X-rays. On this basis it was suggested that methanol MM may be produced either by the effects of galactic-outflow-driven shocks and/or cosmic rays. Here we report the results of a single-dish survey undertaken with the Greenbank Telescope (GBT) to improve our understanding of the pumping conditions of extragalactic class I methanol masers and their relationship to starburst and feedback processes within the host galaxies, towards a sample which includes 16 galaxies which show both extended soft X-ray emission, and either OH or H₂O MM emission. Large baseline ripples in the GBT spectra limited our results to tentative detections towards 11 of the target galaxies. Analysis of these tentative detections shows that there are significant correlations between the methanol intensity and the host-galaxy infrared, radio and OH MM emission, but no correlation with the X-ray and H₂O MM emission. Some sources show methanol emission significantly offset from the systemic velocity of the galaxy (by up to 1000 km s^-1) and we propose that these are associated with galactic-scale outflows from active galactic nuclei (AGNs) feedback. The combined observational properties suggest that class I methanol MMs are related to significant starburst and molecular outflow activity and hence may provide a potential probe of AGN feedback and starburst processes in the host galaxies.

Comments:
Extended X-ray galaxies which show megamaser emission from water or OH

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Detection table from Chen et al. (2016)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	FWHM	∫F dv	Telescope	RMS	Beam	Detection	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class I)	(km/s)	(km/s)	(mJy*km/s)		(mJy)	(arcsec)	Yes/No
1	01 24 35.1	+03 47 32.7	138.7058	-58.0606	G138.706-58.061	NGC520	36 GHz (I)	2070(10)	185(23)	785(95)	GBT	157.000	20	+CH₃OH I	2015 February 4-8
2	11 28 32.2	+58 33 51	141.9020	55.4051	G141.905+55.405	NGC3690	36 GHz (I)	2976(23)	221(20)	692(17)	GBT	80.500	20	+CH₃OH I -CH₃OH II -OH	2015 February 4-8
3	12 13 46	+02 48 40.1	280.9872	64.0660	G280.987+64.066	IRAS12112+0305	36 GHz (I)	22020(16)	232(16)	352(13)	GBT	61.800	20	+CH₃OH I	2015 February 4-8
4	12 18 57.5	+47 18 14	138.3204	68.8421	G138.320+68.842	NGC4258	36 GHz (I)	476(26)	252(21)	405(18)	GBT	75.000	20	+CH₃OH I	2015 February 4-8
5	12 56 14.2	+56 52 25.2	121.6108	60.2423	G121.612+60.242	Mrk231	36 GHz (I)	11573(18)	323(25)	2140(145)	GBT	97.700	20	+CH₃OH I -OH	2015 February 4-8
	12 56 14.2	+56 52 25.2	121.6108	60.2423	G121.612+60.242	Mrk231	36 GHz (I)	12354(24)	316(18)	707(143)	GBT		20	+CH₃OH I -OH	2015 February 4-8
	12 56 14.2	+56 52 25.2	121.6108	60.2423	G121.612+60.242	Mrk231	36 GHz (I)	13689(17)	290(24)	2340(137)	GBT		20	+CH₃OH I -OH	2015 February 4-8
6	15 26 59.4	+35 58 37.3	57.8115	55.9426	G57.811+55.943	IRAS15250+3609	36 GHz (I)	16403(20)	301(50)	588(90)	GBT	82.800	20	+CH₃OH I	2015 February 4-8
7	00 53 34.9	+12 41 36	123.7483	-50.1750	G123.748-50.175	IRAS00509+1225	36 GHz (I)	17201(6)	42(20)	216(80)	GBT	67.500	20	+CH₃OH I	2015 February 4-8
	00 53 34.9	+12 41 36	123.7483	-50.1750	G123.748-50.175	IRAS00509+1225	36 GHz (I)	17648(20)	104(50)	347(142)	GBT		20	+CH₃OH I	2015 February 4-8
	00 53 34.9	+12 41 36	123.7483	-50.1750	G123.748-50.175	IRAS00509+1225	36 GHz (I)	18229(15)	90(35)	396(136)	GBT		20	+CH₃OH I	2015 February 4-8
8	12 25 46.7	+12 39 44	279.1201	74.3355	G279.120+74.335	NGC4388	36 GHz (I)	2190(10)	50(14)	118(43)	GBT	33.700	20	+CH₃OH I	2015 February 4-8
9	14 42 23.9	-17 15 11	337.3245	38.0985	G337.325+38.099	NGC5728	36 GHz (I)	2238(15)	217(36)	727(114)	GBT	110.200	20	+CH₃OH I	2015 February 4-8
10	23 39 1.3	+36 21 08	106.9979	-24.2688	G106.998-24.269	IR23365+3604	36 GHz (I)	20425(18)	164(24)	448(59)	GBT	104.200	20	+CH₃OH I	2015 February 4-8

Non-detection table from Chen et al. (2016)