Display data from paper

Select data type:

MAT14 - The First Very Long Baseline Interferometry Image of a 44 GHz Methanol Maser with the KVN and VERA Array (KaVA)

Interferometry data

Short title: Matsumoto et al. (2014)
Authors: Matsumoto, Naoko Hirota, Tomoya Sugiyama, Koichiro Kim, Kee-Tae Kim, Mikyoung Byun, Do-Young Jung, Taehyun Chibueze, James O. Honma, Mareki Kameya, Osamu Kim, Jongsoo Lyo, A.-Ran Motogi, Kazuhito Oh, Chungsik Shino, Nagisa Sunada, Kazuyoshi Bae, Jaehan Chung, Hyunsoo Chung, Moon-Hee Cho, Se-Hyung Han, Myoung-Hee Han, Seog-Tae Hwang, Jung-Wook Je, Do-Heung Jike, Takaaki Jung, Dong-Kyu Jung, Jin-seung Kang, Ji-hyun Kang, Jiman Kang, Yong-Woo Kan-ya, Yukitoshi Kawaguchi, Noriyuki Kim, Bong Gyu Kim, Jaeheon Ryoung Kim, Hyo Kim, Hyun-Goo Kobayashi, Hideyuki Kono, Yusuke Kurayama, Tomoharu Lee, Changhoon Lee, Jeong Ae Lee, Jeewon Lee, Jung-Won Lee, Sang Hyun Lee, Sang-Sung Minh, Young Chol Miyazaki, Atsushi Oh, Se-Jin Oyama, Tomoaki Park, Sun-youp Roh, Duk-Gyoo Sasao, Tetsuo Sawada-Satoh, Satoko Shibata, Katsunori M. Sohn, Bong Won Song, Min-Gyu Tamura, Yoshiaki Wajima, Kiyoaki Wi, Seog-Oh Yeom, Jae-Hwan Yun, Young Joo
Journal: The Astrophysical Journal Letters, Volume 789, Issue 1, article id. L1, 6 pp. (2014).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (1 detection)
Target type: High_mass_SFR
Transitions: CH3OH_23.4(I),CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_95(I),CH3OH_132(I),CH3OH_19(II)

Abstract
We have carried out the first very long baseline interferometry (VLBI) imaging of a 44 GHz class I methanol maser (7₀-6₁ A ⁺) associated with a millimeter core MM2 in a massive star-forming region IRAS 18151-1208 with KaVA (KVN and VERA Array), which is a newly combined array of KVN (Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). We have succeeded in imaging compact maser features with a synthesized beam size of 2.7 milliarcseconds × 1.5 milliarcseconds (mas). These features are detected at a limited number of baselines within the length of shorter than ≈ 650 km corresponding to 100 Mlambda in the uv-coverage. The central velocity and the velocity width of the 44 GHz methanol maser are consistent with those of the quiescent gas rather than the outflow traced by the SiO thermal line. The minimum component size among the maser features is ~5 mas × 2 mas, which corresponds to the linear size of ~15 AU × 6 AU assuming a distance of 3 kpc. The brightness temperatures of these features range from ~3.5 × 10⁸ to 1.0 × 10¹⁰ K, which are higher than the estimated lower limit from a previous Very Large Array observation with the highest spatial resolution of ~50 mas. The 44 GHz class I methanol maser in IRAS 18151-1208 is found to be associated with the MM2 core, which is thought to be less evolved than another millimeter core MM1 associated with the 6.7 GHz class II methanol maser. eprintid: arXiv:1406.2086

Abstract

We have carried out the first very long baseline interferometry (VLBI) imaging of a 44 GHz class I methanol maser (7₀-6₁ A ⁺) associated with a millimeter core MM2 in a massive star-forming region IRAS 18151-1208 with KaVA (KVN and VERA Array), which is a newly combined array of KVN (Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). We have succeeded in imaging compact maser features with a synthesized beam size of 2.7 milliarcseconds × 1.5 milliarcseconds (mas). These features are detected at a limited number of baselines within the length of shorter than ≈ 650 km corresponding to 100 Mlambda in the uv-coverage. The central velocity and the velocity width of the 44 GHz methanol maser are consistent with those of the quiescent gas rather than the outflow traced by the SiO thermal line. The minimum component size among the maser features is ~5 mas × 2 mas, which corresponds to the linear size of ~15 AU × 6 AU assuming a distance of 3 kpc. The brightness temperatures of these features range from ~3.5 × 10⁸ to 1.0 × 10¹⁰ K, which are higher than the estimated lower limit from a previous Very Large Array observation with the highest spatial resolution of ~50 mas. The 44 GHz class I methanol maser in IRAS 18151-1208 is found to be associated with the MM2 core, which is thought to be less evolved than another millimeter core MM1 associated with the 6.7 GHz class II methanol maser. eprintid:

Download as: Table (CSV)
View paper data

Detection table from Matsumoto et al. (2014)

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	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						CH₃OH (class I)	(km/s)	(Jy/beam)	(Jy/beam*km/s)		Yes/No		(kpc)
1	+18 17 50.1	-12 07 48			18.320205	1.793897	G18.317+1.792			IRAS 18151-1208	Image	44 GHz (I);	29.4 .. 31.1	0.55 .. 16.33	0.55 .. 16.33	KaVA	+H₂O +CH₃OH I	UNK		2012 April 8
	+18 17 50.1	-12 07 48	-0.0001 mas	-0.00019 mas	18.320205	1.793897		1	1	IRAS 18151-1208			29.4	10.74 (12)	10.74 (12)
	+18 17 50.1	-12 07 48	-7e-05 mas	-7e-05 mas	18.320205	1.793897		2	1	IRAS 18151-1208			29.6	16.33 (17)	16.33 (17)
	+18 17 50.1	-12 07 48	-0.00027 mas	3e-05 mas	18.320205	1.793897		3	1	IRAS 18151-1208			29.8	14.90 (12)	14.90 (12)
	+18 17 50.1	-12 07 48	9e-05 mas	0.00012 mas	18.320205	1.793897		4	1	IRAS 18151-1208			30	2.30 (9)	2.30 (9)
	+18 17 50.1	-12 07 47.9999	-0.00353 mas	0.08052 mas	18.320205	1.793897		5	2	IRAS 18151-1208			30.4	5.43 (10)	5.43 (10)
	+18 17 50.1	-12 07 47.9999	-0.00406 mas	0.08125 mas	18.320205	1.793897		6	2	IRAS 18151-1208			30.6	4.49 (8)	4.49 (8)
	+18 17 50.1	-12 07 47.9999	-0.00306 mas	0.08082 mas	18.320205	1.793897		7	2	IRAS 18151-1208			30.9	0.74 (6)	0.74 (6)
	+18 17 50.1	-12 07 47.9999	-0.0575 mas	0.08732 mas	18.320205	1.793897		8	3	IRAS 18151-1208			30.9	0.87 (6)	0.87 (6)
	+18 17 50.1	-12 07 47.9999	-0.05882 mas	0.08662 mas	18.320205	1.793897		9	3	IRAS 18151-1208			31.1	0.55 (1)	0.55 (1)

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 MAT14

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