2010A&A...521L..34W

Query : 2010A&A...521L..34W

2010A&A...521L..34W - Astronomy and Astrophysics, volume 521, L34-34 (2010/10-1)

Variations in H₂O⁺/H₂O ratios toward massive star-forming regions.

WYROWSKI F., VAN DER TAK F., HERPIN F., BAUDRY A., BONTEMPS S., CHAVARRIA L., FRIESWIJK W., JACQ T., MARSEILLE M., SHIPMAN R., VAN DISHOECK E.F., BENZ A.O., CASELLI P., HOGERHEIJDE M.R., JOHNSTONE D., LISEAU R., BACHILLER R., BENEDETTINI M., BERGIN E., BJERKELI P., BLAKE G., BRAINE J., BRUDERER S., CERNICHARO J., CODELLA C., DANIEL F., DI GIORGIO A.M., DOMINIK C., DOTY S.D., ENCRENAZ P., FICH M., FUENTE A., GIANNINI T., GOICOECHEA J.R., DE GRAAUW T., HELMICH F., HERCZEG G.J., JORGENSEN J.K., KRISTENSEN L.E., LARSSON B., LIS D., McCOEY C., MELNICK G., NISINI B., OLBERG M., PARISE B., PEARSON J.C., PLUME R., RISACHER C., SANTIAGO J., SARACENO P., TAFALLA M., VAN KEMPEN T.A., VISSER R., WAMPFLER S., YILDIZ U.A., BLACK J.H., FALGARONE E., GERIN M., ROELFSEMA P., DIELEMAN P., BEINTEMA D., DE JONGE A., WHYBORN N., STUTZKI J. and OSSENKOPF V.

Abstract (from CDS):

Early results from the Herschel Space Observatory revealed the water cation H₂O⁺ to be an abundant ingredient of the interstellar medium. Here we present new observations of the H₂O and H₂O⁺ lines at 1113.3 and 1115.2GHz using the Herschel Space Observatory toward a sample of high-mass star-forming regions to observationally study the relation between H₂O and H₂O⁺. Nine out of ten sources show absorption from H₂O⁺ in a range of environments: the molecular clumps surrounding the forming and newly formed massive stars, bright high-velocity outflows associated with the massive protostars, and unrelated low-density clouds along the line of sight. Column densities per velocity component of H₂O⁺ are found in the range of 10¹² to a few 10¹³cm^–2. The highest N(H₂O⁺) column densities are found in the outflows of the sources. The ratios of H₂O⁺/H₂O are determined in a range from 0.01 to a few and are found to differ strongly between the observed environments with much lower ratios in the massive (proto)cluster envelopes (0.01-0.1) than in outflows and diffuse clouds. Remarkably, even for source components detected in H₂O in emission, H₂O⁺ is still seen in absorption.

Abstract Copyright: ∼

Journal keyword(s): ISM: clouds - ISM: molecules - submillimeter: ISM - stars: formation

Simbad objects: 14

Full paper

View the references in ADS

Number of rows : 14

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Sp type	#ref 1850 - 2023	#notes
1	NAME W3 IRS 5	Y*O	02 25 40.54	+62 05 51.4	B1	349	0
2	W 33a	Y*O	18 14 39.56547	-17 52 02.2260	~	683	0
3	CORNISH G029.9559-00.0168	Y*O	18 46 04.18	-02 39 21.3	~	364	0
4	SNR G030.8-00.0	SNR	18 47 32	-01 56.5	~	512	0
5	IRAS 18449-0115	cor	18 47 34.29	-01 12 44.5	~	374	0
6	AGAL G030.818-00.056	cor	18 47 47.0	-01 54 28	~	153	0
7	RAFGL 2271	SFR	18 53 18.54	+01 14 57.9	~	499	0
8	NAME W 51 North	Rad	19 23 40.0	+14 30 51	~	157	0
9	W 51e1	HII	19 23 43.785	+14 30 26.11	~	131	0
10	W 51	SNR	19 23 50	+14 06.0	~	1258	1
11	RAFGL 2591	Y*O	20 29 24.8230	+40 11 19.590	~	613	0
12	[MBS2007c] CygX-N44	Rad	20 39 01.01	+42 22 50.2	~	396	0
13	DR 21	SFR	20 39 01.6	+42 19 38	O4.5	1036	0
14	[WBN74] NGC 7538 IRS 1	Y*O	23 13 45.318	+61 28 11.69	~	408	3

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