Display data from paper

Select data type:

CHE18 - Direct Evidence for Maser Emission from the 36.2 GHz Class I Transition of Methanol in NGC253

Interferometry data

Short title: Chen et al. (2018)
Authors: Chen, Xi Ellingsen, Simon P. Shen, Zhi-Qiang McCarthy, Tiege P. Zhong, Wei-Ye Deng, Hui
Journal: The Astrophysical Journal Letters, Volume 856, Issue 2, article id. L35, 6 pp. (2018).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection)
Target type: Extragalactic
Transitions: CH3OH_36(I)

Abstract
Observations made with the Jansky Very large Array (JVLA) at an angular resolution of ~0.1 arcsec have detected class I methanol maser emission from the 36.2 GHz transition toward the starburst galaxy NGC 253. The methanol emission is detected toward four sites which lie within the regions of extended methanol emission detected in previous lower angular resolution (a few arcseconds) observations. The peak flux densities of the detected compact components are in the range 3-9 mJy beam^-1. Combining the JVLA data with single-dish observations from the Shanghai Tianma Radio Telescope (TMRT) and previous interferometric observations with the Australia Telescope Compact Array (ATCA), we show that the 36.2 GHz class I methanol emission consists of both extended and compact structures, with typical scales of ~6 arcsec (0.1 kpc) and ~0.05 arcsec (1 pc), respectively. The strongest components have a brightness temperature of >10³ K, much higher than the maximum kinetic temperature (~100 K) of the thermal methanol emission from NGC 253. Therefore, these observations conclusively demonstrate for the first time the presence of maser emission from a class I methanol transition in an external galaxy.

Abstract

Observations made with the Jansky Very large Array (JVLA) at an angular resolution of ~0.1 arcsec have detected class I methanol maser emission from the 36.2 GHz transition toward the starburst galaxy NGC 253. The methanol emission is detected toward four sites which lie within the regions of extended methanol emission detected in previous lower angular resolution (a few arcseconds) observations. The peak flux densities of the detected compact components are in the range 3-9 mJy beam^-1. Combining the JVLA data with single-dish observations from the Shanghai Tianma Radio Telescope (TMRT) and previous interferometric observations with the Australia Telescope Compact Array (ATCA), we show that the 36.2 GHz class I methanol emission consists of both extended and compact structures, with typical scales of ~6 arcsec (0.1 kpc) and ~0.05 arcsec (1 pc), respectively. The strongest components have a brightness temperature of >10³ K, much higher than the maximum kinetic temperature (~100 K) of the thermal methanol emission from NGC 253. Therefore, these observations conclusively demonstrate for the first time the presence of maser emission from a class I methanol transition in an external galaxy.

Download as: Table (CSV)
View paper data

Detection table from Chen et al. (2018)

Export table to csv

Hide / Show individual components

ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Maser spot	Source name	Image	Line	V_peak	F_peak	∫F dv	Telescope	Beam	PA	Detection	Class	Dist. (parallax)
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						CH₃OH (class I)	(km/s)	(Jy/beam)	(Jy/beam*km/s)		(arcsec)	(deg.)	Yes/No		(kpc)
1	+00 47 33.1	-25 17 18			97.366075	-87.96407	G97.436-87.964			NGC 253	Image	36 GHz (I);				NRAOVLA	0.16 x 0.07	-28	+CH₃OH I	GALAXY
	+00 47 33.915	-25 17 10.47	12223.8 mas	7528.8 mas	97.469297	-87.963477		1	A	NGC 253			215	3.3	91.2
	+00 47 33.675	-25 17 13.55	8623.8 mas	4448.8 mas	97.436050	-87.963870		2	B	NGC 253			202	9.2	208.1
	+00 47 31.953	-25 17 28.15	-17206.2 mas	-10151.2 mas	97.222200	-87.964780		3	C	NGC 253			346	5.4	88.8
	+00 47 31.946	-25 17 30.1	-17311.2 mas	-12101.2 mas	97.215014	-87.965259		4	D	NGC 253			306	4.4	119.6

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 CHE18

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