2013A&A...554A..83V


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.19CEST18:45:26

2013A&A...554A..83V - Astronomy and Astrophysics, volume 554A, 83-83 (2013/6-1)

Water in star-forming regions with Herschel (WISH). IV. A survey of low-J H2O line profiles toward high-mass protostars.

VAN DER TAK F.F.S., CHAVARRIA L., HERPIN F., WYROWSKI F., WALMSLEY C.M., VAN DISHOECK E.F., BENZ A.O., BERGIN E.A., CASELLI P., HOGERHEIJDE M.R., JOHNSTONE D., KRISTENSEN L.E., LISEAU R., NISINI B. and TAFALLA M.

Abstract (from CDS):

Water is a key constituent of star-forming matter, but the origin of its line emission and absorption during high-mass star formation is not well understood. We study the velocity profiles of low-excitation H2O lines toward 19 high-mass star-forming regions and search for trends with luminosity, mass, and evolutionary stage. We decompose high-resolution Herschel-HIFI line spectra near 990, 1110and 1670GHz into three distinct physical components. Dense cores (protostellar envelopes) are usually seen as narrow absorptions in the H2O 1113 and 1669GHz ground-state lines, the H2O 987GHz excited-state line, and the H218O 1102GHz ground-state line. In a few sources, the envelopes appear in emission in some or all studied lines, indicating higher temperatures or densities. Broader features due to outflows are usually seen in absorption in the H2O 1113and 1669GHz lines, in 987GHz emission, and not seen in H218O, indicating a lower column density and a higher excitation temperature than the envelope component. A few outflows are detected in H218O, indicating higher column densities of shocked gas. In addition, the H2O 1113 and 1669GHz spectra show narrow absorptions by foreground clouds along the line of sight. The lack of corresponding features in the 987GHz and H218O lines indicates a low column density and a low excitation temperature for these clouds, although their derived H2O ortho/para ratios are close to 3. The intensity of the ground state lines of H2O at 1113 and 1669GHz does not show significant trends with source luminosity, envelope mass, or evolutionary state. In contrast, the flux in the excited-state 987GHz line appears correlated with luminosity and the H218O line flux appears correlated with the envelope mass. Furthermore, appearance of the envelope in absorption in the 987GHz and H218O lines seems to be a sign of an early evolutionary stage, as probed by the mid-infrared brightness and the Lbol/Menv ratio of the source. The ground state transitions of H2O trace the outer parts of the envelopes, so that the effects of star formation are mostly noticeable in the outflow wings. These lines are heavily affected by absorption, so that line ratios of H2O involving the ground states must be treated with caution, especially if multiple clouds are superposed as in the extragalactic case. The isotopic H218O line appears to trace the mass of the protostellar envelope, indicating that the average H2O abundance in high-mass protostellar envelopes does not change much with time. The excited state line at 987GHz increases in flux with luminosity and appears to be a good tracer of the mean weighted dust temperature of the source, which may explain why it is readily seen in distant galaxies.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: molecules - astrochemistry

Simbad objects: 26

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Number of rows : 26

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 330 0
2 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 703 0
3 IRAS 05358+3543 mul 05 39 10.4 +35 45 19           ~ 136 1
4 OH 327.29 -0.58 cor 15 53 07.65 -54 37 06.1           ~ 41 0
5 IRAS 16272-4837 HII 16 30 59.2 -48 43 48           ~ 22 0
6 NGC 6334 HII 17 20 51 -36 06.9           ~ 591 0
7 NAME NGC 6334 I(N) smm 17 20 54 -35 45.0           ~ 127 1
8 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1943 1
9 GAL 005.88-00.41 HII 18 00 30.388 -24 04 00.20           ~ 301 0
10 W 28a Rad 18 00 30.4 -24 03 58           ~ 28 0
11 GAL 010.47+00.03 HII 18 08 38.4 -19 51 52           ~ 110 0
12 GRS G012.89 +00.49 HII 18 11 51.3 -17 31 29           ~ 148 0
13 W 33a Y*O 18 14 39.0 -17 52 03           ~ 587 0
14 IRAS 18151-1208 Y*O 18 17 58.114 -12 07 24.84           ~ 100 0
15 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 334 1
16 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 445 0
17 IRAS 18449-0115 cor 18 47 34.4947 -01 12 40.269           ~ 315 0
18 [MSL2003] W43-MM1 cor 18 47 47.0 -01 54 28           ~ 96 0
19 OH 34.26 +0.15 SFR 18 53 18.54 +01 14 57.9           ~ 467 0
20 NAME W 51 IRS 1 PoC 19 23 41.9 +14 30 36           ~ 98 0
21 W 51e1 Rad 19 23 43.77 +14 30 25.9           ~ 115 0
22 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 571 0
23 [MBS2007c] CygX-N44 Rad 20 39 01.01 +42 22 50.2           ~ 363 0
24 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 948 0
25 NGC 7538 OpC 23 13 37 +61 30.0           ~ 831 0
26 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 369 3

    Equat.    Gal    SGal    Ecl

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2020.10.19-18:45:26

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