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WAT80 - Observations of interstellar H2O emission at 183 gigahertz

Short title: Waters et al. (1980)
Authors: Waters, J. W.Kakar, R. K.Kuiper, T. B. H.Roscoe, H. K.Swanson, P. N.Rodriguez Kuiper, E. N.Kerr, A. R.Thaddeus, P.Gustincic, J. J.
Journal: Astrophysical Journal, Part 1, vol. 235, Jan. 1, 1980, p. 57-62.
Bibcode:

Target type: High_mass_SFR
Transitions: H2O_183

Abstract
Observations of the 183-GHz rotational transition of water vapor in interstellar molecular clouds are reported. The observations were made with a portable double-sideband superheterodyne radiometer used with the 91-cm Cassegrain telescope on board the Kuiper Airborne Observatory. An emission feature was detected in the direction of the Kleinmann-Low nebula in Orion with a peak antenna temperature of 15 K, a local standard of rest velocity of 8 km/sec, and a width of 15 km/sec. A plateau component of the emission profile is attributed to the 1-arcmin region characteristic of plateau emission from other observed molecules, with emission enhanced over that expected for thermal excitation, while the spike component observed is consistent with an optically thick source of the size of the molecular ridge in Orion at a temperature of 50 K and a column density greater than or equal to 3 x 10 to the 17th/sq cm, implying that H2O is one of the more abundant species in the Orion Molecular Cloud. Emission at 183 GHz was not detected in Sgr A, Sgr B2, W3, W43, W49, W51, DR 21, NGC 1333, NGC 7027, GL 2591 or the Rho Oph cloud it may have been detected in M 17.

Abstract

Observations of the 183-GHz rotational transition of water vapor in interstellar molecular clouds are reported. The observations were made with a portable double-sideband superheterodyne radiometer used with the 91-cm Cassegrain telescope on board the Kuiper Airborne Observatory. An emission feature was detected in the direction of the Kleinmann-Low nebula in Orion with a peak antenna temperature of 15 K, a local standard of rest velocity of 8 km/sec, and a width of 15 km/sec. A plateau component of the emission profile is attributed to the 1-arcmin region characteristic of plateau emission from other observed molecules, with emission enhanced over that expected for thermal excitation, while the spike component observed is consistent with an optically thick source of the size of the molecular ridge in Orion at a temperature of 50 K and a column density greater than or equal to 3 x 10 to the 17th/sq cm, implying that H2O is one of the more abundant species in the Orion Molecular Cloud. Emission at 183 GHz was not detected in Sgr A, Sgr B2, W3, W43, W49, W51, DR 21, NGC 1333, NGC 7027, GL 2591 or the Rho Oph cloud it may have been detected in M 17.

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Detection table from Waters et al. (1980)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Line	V_range	V_peak	FWHM	T_a	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				H₂O	(km/s)	(km/s)	(km/s)	(K)		(arcsec)	Yes/No		(kpc)
1	05 35 14.5	-05 22 30.6	208.9930	-19.3848	G208.993-19.385	Ori A (center)	Image	183 GHz;	-25;45	8	15	14 (1)	Kuiper	450	+H₂O +CH₃OH I +CH₃OH II +OH +SiO	SFR_MIXED		1976 Oct 14
2	05 35 14.6	-05 18 30.6	208.9302	-19.3544	G208.930-19.354	Ori A (4'N)		183 GHz;	-25;45	8	15	3.8 (1.4)	Kuiper	450	+H₂O	SFR_MIXED		1977 Dec 15
3	05 35 14.4	-05 26 30.6	209.0559	-19.4153	G209.056-19.415	Ori A (4'S)		183 GHz;	-25;45	8	10	7.7 (1.6)	Kuiper	450	+H₂O	SFR_MIXED		1977 Dec 15
4	05 35 30.5	-05 22 31.7	209.0252	-19.3258	G209.025-19.326	Ori A (4'E)		183 GHz;	-25;45	8	15	6.4 (2.8)	Kuiper	450	+H₂O	SFR		1977 Dec 15
5	05 34 58.5	-05 22 29.4	208.9609	-19.4439	G208.961-19.444	Ori A (4'W)		183 GHz;	-25;45	8	13	6.6 (2.8)	Kuiper	450	+H₂O	SFR_MIXED		1977 Dec 15
6	18 20 19.7	-16 13 31.5	14.9963	-0.6743	G15.033-0.674	M17		183 GHz;	-13;52	20	5	1.0 (0.5)	Kuiper	450	+H₂O +CH₃OH I +CH₃OH II +OH	GALAXY		1977 July 22

Non-detection table from Waters et al. (1980)