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

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

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

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 367 0
2 W 33a Y*O 18 14 39.56547 -17 52 02.2260           ~ 746 0
3 CORNISH G029.9559-00.0168 Y*O 18 46 04.18 -02 39 21.3           ~ 385 0
4 W 43 SFR 18 47 32 -01 56.5           ~ 604 0
5 IRAS 18449-0115 cor 18 47 34.27 -01 12 43.2           ~ 430 1
6 AGAL G030.818-00.056 cor 18 47 47.0 -01 54 28           ~ 186 0
7 RAFGL 2271 SFR 18 53 18.54 +01 14 57.9           ~ 537 0
8 NAME W 51 North Rad 19 23 40.0 +14 30 51           ~ 169 0
9 W 51e1 HII 19 23 43.785 +14 30 26.11           ~ 141 0
10 W 51 SNR 19 23 50 +14 06.0           ~ 1352 1
11 RAFGL 2591 Y*O 20 29 24.8230 +40 11 19.590           ~ 640 0
12 DR 21 (OH) cor 20 39 01.01 +42 22 50.2           ~ 427 0
13 DR 21 SFR 20 39 01.6 +42 19 38           O4.5 1121 0
14 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 433 3

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