Herschel observations of EXtra-Ordinary Sources (HEXOS): Observations of H2O and its isotopologues towards Orion KL

G. J. Melnick; V. Tolls; D. A. Neufeld; E. A. Bergin; T. G. Phillips; S. Wang; N. R. Crockett; T. A. Bell; G. A. Blake; S. Cabrit; E. Caux; C. Ceccarelli; J. Cernicharo; C. Comito; F. Daniel; M.-L. Dubernet; M. Emprechtinger; P. Encrenaz; E. Falgarone; M. Gerin; T. F. Giesen; J. R. Goicoechea; P. F. Goldsmith; E. Herbst; C. Joblin; D. Johnstone; W. D. Langer; W. D. Latter; D. C. Lis; S. D. Lord; S. Maret; P. G. Martin; K. M. Menten; P. Morris; H. S. P. Müller; J. A. Murphy; V. Ossenkopf; L. Pagani; J. C. Pearson; M. Pérault; R. Plume; S.-L. Qin; M. Salez; P. Schilke; S. Schlemmer; J. Stutzki; N. Trappe; F. F. S. van der Tak; C. Vastel; H. W. Yorke; S. Yu; J. Zmuidzinas

doi:10.1051/0004-6361/201015085

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Volume 521 (October 2010)

A&A, 521 (2010) L27

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Herschel/HIFI: first science highlights

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Table 3:

Best-Fit H $_2^{\;18}$ O Integrated Line Intensities $^{\dagger }$ .
			Emission Component
					Extended
		Upper-Level	Plateau	Hot Core	Warm Gas
Transition	Frequency	Energy	$\int T_A^{\;*} {\rm d}v$	$\int T_A^{\;*} {\rm d}v$	$\int T_A^{\;*} {\rm d}v$
	(GHz)	(K)	(K-km s^-1)	(K-km s^-1)	(K-km s^-1)
1 $_{1 1}\:-\:$ 0_{0 0}	1101.70	52.9	315.4	7.6	50.8
1 $_{1 0}\:-\:$ 1_{0 1}	547.68	60.5	199.0	8.2	34.6
2 $_{0 2}\:-\:$ 1_{1 1}	994.68	100.6	423.3	60.1	10.7
2 $_{1 2}\:-\:$ 1_{0 1}	1655.87	113.6	574.9	0.0	71.5
2 $_{1 1}\:-\:$ 2_{0 2}	745.32	136.4	276.6	66.3	17.7
2 $_{2 1}\:-\:$ 2_{1 2}	1633.48	192.0	220.6	10.1	6.4
3 $_{1 2}\:-\:$ 3_{0 3}	1095.63	248.7	444.9	70.2	5.2
3 $_{1 2}\:-\:$ 2_{2 1}	1181.39	248.7	178.8	50.4	1.8
3 $_{2 2}\:-\:$ 3_{1 3}	1894.32	294.6	65.7	34.7	2.4
3 $_{2 1}\:-\:$ 3_{1 2}	1136.70	303.3	424.4	65.3	11.8
4 $_{1 3}\:-\:$ 4_{0 4}	1605.96	395.4	46.6	38.6	0.0
4 $_{2 2}\:-\:$ 4_{1 3} $^{\dagger\dagger}$	1188.86	452.4	118.5	57.5	0.2
5 $_{2 4}\:-\:$ 4_{3 1}	1003.28	595.9	0.0	6.9	2.0
5 $_{3 2}\:-\:$ 5_{2 3}	1815.85	727.6	22.2	32.8	10.0
6 $_{2 4}\:-\:$ 6_{1 5}	1800.47	865.0	41.5	36.9	0.0

Notes. $^{(\dagger)}$ The line fitting procedure is described in Sect. 3. $^{({\dagger\dagger})}$ Some flux attributed to this transition may be due to the CH₃OH (12_5 1- 11_2 1) and H $_2^{\;13}$ CO (18 _2 17- 18_0 18) transitions, both of which lie within 27 km s^-1 of the H $_2^{\;18}$ O 4₂₂-4₁₃ line.

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