2013A&A...551A.116T


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.06CET09:23:10

2013A&A...551A.116T - Astronomy and Astrophysics, volume 551A, 116-116 (2013/3-1)

High-pressure, low-abundance water in bipolar outflows. Results from a Herschel-WISH survey.

TAFALLA M., LISEAU R., NISINI B., BACHILLER R., SANTIAGO-GARCIA J., VAN DISHOECK E.F., KRISTENSEN L.E., HERCZEG G.J. and YILDIZ U.A.

Abstract (from CDS):

Water is a potential tracer of outflow activity because it is heavily depleted in cold ambient gas and is copiously produced in shocks. We present a survey of the water emission in a sample of more than 20 outflows from low-mass young stellar objects with the goal of characterizing the physical and chemical conditions of the emitting gas. We used the HIFI and PACS instruments on board the Herschel Space Observatory to observe the two fundamental lines of ortho-water at 557 and 1670GHz. These observations were part of the ``Water In Star-forming regions with Herschel'' (WISH) key program, and have been complemented with CO and H2 data. The emission of water has a different spatial and velocity distribution from that of the J=1-0 and 2-1 transitions of CO. On the other hand, it has a similar spatial distribution to H2, and its intensity follows the H2 intensity derived from IRAC images. This suggests that water traces the outflow gas at hundreds of kelvins that is responsible for the H2 emission, and not the component at tens of kelvins typical of low-J CO emission. A warm origin of the water emission is confirmed by a remarkable correlation between the intensities of the 557 and 1670GHz lines, which also indicates that the emitting gas has a narrow range of excitations. A radiative transfer analysis shows that while there is some ambiguity in the exact combination of density and temperature values, the gas thermal pressure nT is constrained within less than a factor of 2. The typical nT over the sample is 4x109cm–3K, which represents an increase of 104 with respect to the ambient value. The data also constrain the water column density within a factor of 2 and indicate values in the sample between 2x1012 and 1014cm–2. When these values are combined with estimates of the H2 column density, the typical water abundance is only 3x10–7, with an uncertainty of a factor of 3. Our data challenge current C-shock models of water production through the combination of wing-line profiles, high gas compressions, and low abundances.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: abundances - ISM: molecules - ISM: jets and outflows

Simbad objects: 36

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Number of rows : 36

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 LDN 1448 DNe 03 22.5 +30 35           ~ 459 0
2 NGC 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1184 1
3 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 158 1
4 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 373 3
5 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 332 0
6 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 570 1
7 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 462 0
8 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 544 0
9 IRAS 03407+3152 cor 03 43 56.52 +32 00 52.8           ~ 288 0
10 IRAS 04166+2706 Y*O 04 19 42.627 +27 13 38.43           M 107 1
11 LDN 1551 DNe 04 31 30.0 +18 12 30           ~ 764 1
12 LDN 1527 DNe 04 39 53 +25 45.0           ~ 472 0
13 HH 1 HH 05 36 20.8 -06 45 13           ~ 401 1
14 NAME HH 1-2 HH 05 36 22.8 -06 46 03           ~ 199 1
15 HH 2 HH 05 36.4 -06 47           ~ 335 1
16 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 257 1
17 NAME HH 25MMS Y*O 05 46 07.8 -00 13 41           ~ 53 0
18 HH 111 HH 05 51 44.2 +02 48 34           ~ 377 0
19 2MASS J08254384-5100326 Y*O 08 25 43.85 -51 00 32.7           ~ 295 1
20 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 111 0
21 HH 54 HH 12 55 49.5 -76 56 08           ~ 118 0
22 HH 54B HH 12 55 50.3 -76 56 23           ~ 30 0
23 IC 4166 GiC 13 05 18.589 +31 26 32.43   15.2       ~ 21 0
24 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 366 0
25 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1001 1
26 LDN 483 DNe 18 17 35 -04 39.8           ~ 196 0
27 SH 2-68 N Y*O 18 29 48.09 +01 16 45.0           ~ 96 1
28 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 230 2
29 NAME Serpens Cluster Cl* 18 29 57 +01 14.4           ~ 57 0
30 NAME Serpens SMM 4 cor 18 29 57.1 +01 13 15           ~ 119 0
31 LDN 663 DNe 19 36 55 +07 34.4           ~ 538 0
32 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 463 0
33 [DE95] LDN 1157 B1 out 20 39 11 +68 01.3           ~ 166 0
34 LDN 1148 DNe 20 40 31.6 +67 21 45           ~ 59 0
35 NAME NGC 7129 FIR 2 IR 21 44 01.5 +66 03 40           ~ 81 0
36 NAME Cep E HII 23 03 12.779 +61 42 25.75           ~ 151 0

    Equat.    Gal    SGal    Ecl

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2019.12.06-09:23:10

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