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LYO14 - Unbiased Water and Methanol Maser Surveys of NGC 1333

Short title: Lyo et al. (2014)
Authors: Lyo, A.-Ran Kim, Jongsoo Byun, Do-Young Lee, Ho-Gyu
Journal: The Astronomical Journal, Volume 148, Issue 5, article id. 80, 10 pp. (2014).
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (18 detection)
Target type: High_mass_SFR,Blind
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 present the results of unbiased 22 GHz H₂O water and 44 GHz class I CH₃OH methanol maser surveys in the central 7' � 10' area of NGC 1333 and two additional mapping observations of a 22 GHz water maser in a ~3' � 3' area of the IRAS4A region. In the 22 GHz water maser survey of NGC 1333 with a sensitivity of sigma ~ 0.3 Jy, we confirmed the detection of masers toward H₂O(B) in the region of HH 7-11 and IRAS4B. We also detected new water masers located ~20'' away in the western direction of IRAS4B or ~25'' away in the southern direction of IRAS4A. We could not, however, find young stellar objects or molecular outflows associated with them. They showed two different velocity components of ~0 and ~16 km s^-1, which are blue- and redshifted relative to the adopted systemic velocity of ~7 km s^-1 for NGC 1333. They also showed time variabilities in both intensity and velocity from multi-epoch observations and an anti-correlation between the intensities of the blue- and redshifted velocity components. We suggest that the unidentified power source of these masers might be found in the earliest evolutionary stage of star formation, before the onset of molecular outflows. Finding this kind of water maser is only possible through an unbiased blind survey. In the 44 GHz methanol maser survey with a sensitivity of sigma ~ 0.5 Jy, we confirmed masers toward IRAS4A2 and the eastern shock region of IRAS2A. Both sources are also detected in 95 and 132 GHz methanol maser lines. In addition, we had new detections of methanol masers at 95 and 132 GHz toward IRAS4B. In terms of the isotropic luminosity, we detected methanol maser sources brighter than ~5 � 10²⁵ erg s^-1 from our unbiased survey. eprintid: arXiv:1407.6776	Target sources: Coordinates from GAUSSCLUMPS

Abstract

We present the results of unbiased 22 GHz H₂O water and 44 GHz class I CH₃OH methanol maser surveys in the central 7' � 10' area of NGC 1333 and two additional mapping observations of a 22 GHz water maser in a ~3' � 3' area of the IRAS4A region. In the 22 GHz water maser survey of NGC 1333 with a sensitivity of sigma ~ 0.3 Jy, we confirmed the detection of masers toward H₂O(B) in the region of HH 7-11 and IRAS4B. We also detected new water masers located ~20'' away in the western direction of IRAS4B or ~25'' away in the southern direction of IRAS4A. We could not, however, find young stellar objects or molecular outflows associated with them. They showed two different velocity components of ~0 and ~16 km s^-1, which are blue- and redshifted relative to the adopted systemic velocity of ~7 km s^-1 for NGC 1333. They also showed time variabilities in both intensity and velocity from multi-epoch observations and an anti-correlation between the intensities of the blue- and redshifted velocity components. We suggest that the unidentified power source of these masers might be found in the earliest evolutionary stage of star formation, before the onset of molecular outflows. Finding this kind of water maser is only possible through an unbiased blind survey. In the 44 GHz methanol maser survey with a sensitivity of sigma ~ 0.5 Jy, we confirmed masers toward IRAS4A2 and the eastern shock region of IRAS2A. Both sources are also detected in 95 and 132 GHz methanol maser lines. In addition, we had new detections of methanol masers at 95 and 132 GHz toward IRAS4B. In terms of the isotropic luminosity, we detected methanol maser sources brighter than ~5 � 10²⁵ erg s^-1 from our unbiased survey. eprintid:

Target sources:
Coordinates from GAUSSCLUMPS

Input tables: Table 2,4
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Detection table from Lyo et al. (2014)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Line	V_peak	FWHM	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				CH₃OH (class I)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	03 29 9.7	+31 13 21.6	158.3945	-20.5783	G158.400-20.576	NGC 1333 IRAS4A2	Image	44 GHz (I);	4.52 (0.29)	9.42 (0.58)	1.09	10.89 (0.63)	KVN	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 11
	03 29 9.7	+31 13 21.6	158.3945	-20.5783	G158.400-20.576	NGC 1333 IRAS4A2		44 GHz (I);	6.79 (0.04)	1.54 (0.12)	2.69	4.41 (0.35)	KVN	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 11
3	03 29 9.7	+31 13 21.6	158.3945	-20.5783	G158.400-20.576	NGC 1333 IRAS4A2		95 GHz (I);	5.28 (0.16)	7.90 (0.49)	2.49	20.95 (0.82)	KVN	32	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 11
	03 29 9.7	+31 13 21.6	158.3945	-20.5783	G158.400-20.576	NGC 1333 IRAS4A2		95 GHz (I);	7.08 (0.02)	0.62 (0.11)	5.73	3.80 (0.46)	KVN	32	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 11
5	03 29 9.7	+31 13 21.6	158.3945	-20.5783	G158.400-20.576	NGC 1333 IRAS4A2		132.8 GHz (I);	3.98 (0.33)	9.38 (0.63)	2.97	29.68 (2.02)	KVN	23	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 11
	03 29 9.7	+31 13 21.6	158.3945	-20.5783	G158.400-20.576	NGC 1333 IRAS4A2		132.8 GHz (I);	6.69 (0.08)	2.32 (0.33)	3.18	7.85 (1.44)	KVN	23	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 11
7	03 29 11.7	+31 13 7.8	158.4031	-20.5770	G158.400-20.576	NGC 1333 IRAS4B		44 GHz (I);	4.84 (0.46)	10.39 (1.07)	0.7	7.79 (0.72)	KVN	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Apr 26
	03 29 11.7	+31 13 7.8	158.4031	-20.5770	G158.400-20.576	NGC 1333 IRAS4B		44 GHz (I);	6.67 (0.07)	1.82 (0.18)	2.04	3.96 (0.44)	KVN	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Apr 26
9	03 29 11.7	+31 13 7.8	158.4031	-20.5770	G158.400-20.576	NGC 1333 IRAS4B		95 GHz (I);	6.66 (0.59)	24.57 (10.69)	0.28	7.36 (2.17)	KVN	32	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Apr 26
	03 29 11.7	+31 13 7.8	158.4031	-20.5770	G158.400-20.576	NGC 1333 IRAS4B		95 GHz (I);	7.17 (0.13)	3.06 (0.32)	2.22	7.23 (0.86)	KVN	32	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Apr 26
11	03 29 11.7	+31 13 7.8	158.4031	-20.5770	G158.400-20.576	NGC 1333 IRAS4B		132.8 GHz (I);	5.45 (0.71)	14.90 (1.37)	0.95	15.00 (1.55)	KVN	23	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Apr 26
	03 29 11.7	+31 13 7.8	158.4031	-20.5770	G158.400-20.576	NGC 1333 IRAS4B		132.8 GHz (I);	7.69 (0.05)	3.16 (0.15)	5.44	18.29 (1.05)	KVN	23	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Apr 26
13	03 29 1.4	+31 14 18.6	158.3591	-20.5835	G158.355-20.586	NGC 1333 IRAS2A East		44 GHz (I);	10.03 (0.17)	4.66 (0.27)	1.21	6.02 (0.42)	KVN	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 20
	03 29 1.4	+31 14 18.6	158.3591	-20.5835	G158.355-20.586	NGC 1333 IRAS2A East		44 GHz (I);	10.03 (0.27)	4.77 (0.62)	0.81	4.11 (0.15)	KVN	62	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 20
15	03 29 1.4	+31 14 18.6	158.3591	-20.5835	G158.355-20.586	NGC 1333 IRAS2A East		95 GHz (I);	9.25 (0.44)	3.85 (0.78)	3.36	13.75 (3.34)	KVN	32	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 20
	03 29 1.4	+31 14 18.6	158.3591	-20.5835	G158.355-20.586	NGC 1333 IRAS2A East		95 GHz (I);	12.83 (0.96)	2.94 (1.20)	1.29	4.03 (2.97)	KVN	32	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 20
17	03 29 1.4	+31 14 18.6	158.3591	-20.5835	G158.355-20.586	NGC 1333 IRAS2A East		132.8 GHz (I);	8.56 (0.10)	2.87 (0.22)	9.14	27.94 (5.74)	KVN	23	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 20
	03 29 1.4	+31 14 18.6	158.3591	-20.5835	G158.355-20.586	NGC 1333 IRAS2A East		132.8 GHz (I);	11.24 (0.29)	5.14 (0.36)	9.54	52.16 (6.29)	KVN	23	+H₂O +CH₃OH I -CH₃OH II	SFR		2012 Mar 20

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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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 LYO14

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