2014A&A...572A...9K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST19:39:36

2014A&A...572A...9K - Astronomy and Astrophysics, volume 572A, 9-9 (2014/12-1)

Shockingly low water abundances in Herschel/PACS observations of low-mass protostars in Perseus.

KARSKA A., KRISTENSEN L.E., VAN DISHOECK E.F., DROZDOVSKAYA M.N., MOTTRAM J.C., HERCZEG G.J., BRUDERER S., CABRIT S., EVANS II N.J., FEDELE D., GUSDORF A., JORGENSEN J.K., KAUFMAN M.J., MELNICK G.J., NEUFELD D.A., NISINI B., SANTANGELO G., TAFALLA M. and WAMPFLER S.F.

Abstract (from CDS):

Protostars interact with their surroundings through jets and winds impinging on the envelope and creating shocks, but the nature of these shocks is still poorly understood. Our aim is to survey far-infrared molecular line emission from a uniform and significant sample of deeply-embedded low-mass young stellar objects (YSOs) in order to characterize shocks and the possible role of ultraviolet radiation in the immediate protostellar environment. Herschel/PACS spectral maps of 22 objects in the Perseus molecular cloud were obtained as part of the William Herschel Line Legacy (WILL) survey. Line emission from H2O, CO, and OH is tested against shock models from the literature. Observed line ratios are remarkably similar and do not show variations with physical parameters of the sources (luminosity, envelope mass). Most ratios are also comparable to those found at off-source outflow positions. Observations show good agreement with the shock models when line ratios of the same species are compared. Ratios of various H2O lines provide a particularly good diagnostic of pre-shock gas densities, nH∼105cm–3, in agreement with typical densities obtained from observations of the post-shock gas when a compression factor on the order of 10 is applied (for non-dissociative shocks). The corresponding shock velocities, obtained from comparison with CO line ratios, are above 20km/s. However, the observations consistently show H2O-to-CO and H2O-to-OH line ratios that are one to two orders of magnitude lower than predicted by the existing shock models. The overestimated model H2O fluxes are most likely caused by an overabundance of H2O in the models since the excitation is well-reproduced. Illumination of the shocked material by ultraviolet photons produced either in the star-disk system or, more locally, in the shock, would decrease the H2O abundances and reconcile the models with observations. Detections of hot H2O and strong OH lines support this scenario.

Abstract Copyright:

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

Simbad objects: 56

goto Full paper

goto View the reference in ADS

Number of rows : 56

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           ~ 466 0
2 NAME LDN 1448 IRS 2 Y*O 03 25 22.32 +30 45 13.9           ~ 117 0
3 LDN 1448NW Y*? 03 25 35.66 +30 45 34.2           ~ 59 0
4 [SDA2014] West8 Y*O 03 25 36.22 +30 45 15.7           ~ 98 0
5 IRAS 03225+3034 IR 03 25 36.49 +30 45 22.2           ~ 149 1
6 LDN 1448NA smm 03 25 36.49 +30 45 22.2           ~ 171 1
7 SSTc2d J032536.4+304522 Y*O 03 25 36.49 +30 45 22.2           ~ 186 1
8 NAME LDN 1448-mm Y*O 03 25 38.83 +30 44 06.2           ~ 301 0
9 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 242 1
10 [BCM90] R4 ? 03 25 42 +30 41.9           ~ 12 0
11 LDN 1451 DNe 03 26.1 +30 10           ~ 42 0
12 IRAS 03235+3004 Y*O 03 26 37.425 +30 15 28.39           ~ 70 0
13 NAME LDN 1455 IRS 5 Y*O 03 27 38.255 +30 13 58.57           ~ 43 0
14 NAME LDN 1455 IRS 1 cor 03 27 39.08 +30 13 03.1           ~ 142 0
15 NAME LDN 1455 IRS 4 cor 03 27 43.23 +30 12 28.9           ~ 62 0
16 NAME LDN 1455 IRS 2 cor 03 27 47.6826386762 +30 12 04.459144041     19.6     ~ 94 1
17 2MASS J03283258+3111040 cor 03 28 32.581 +31 11 04.10           ~ 43 0
18 [EYG2006] Bolo 28 cor 03 28 34.53 +31 07 05.5           ~ 33 0
19 IRAS 03255+3103 Y*O 03 28 37.068 +31 13 31.00           ~ 78 1
20 [EYG2006] Bolo 30 Y*O 03 28 39.10 +31 06 01.7           ~ 34 0
21 [HFR2007] 55 cor 03 28 40.63 +31 17 56.5           ~ 37 1
22 IRAS 03256+3055 Y*O 03 28 45.306 +31 05 42.05           ~ 48 3
23 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 390 3
24 BD+30 547 Y*O 03 28 57.2107612240 +31 14 19.076624755   10.73 9.98 9.1   G4V 93 1
25 HH 12 HH 03 28 59.4 +31 20 11           ~ 116 1
26 [EYG2006] Bolo 40 cor 03 28 59.63 +31 21 33.9           ~ 25 0
27 [SK2001] 1 Y*O 03 29 00.55 +31 12 00.8           ~ 51 1
28 [KJT2007] SMM 62 Y*O 03 29 01.66 +31 20 28.5           ~ 6 0
29 V* V512 Per Or* 03 29 03.7567945196 +31 16 03.959183877           ~ 348 0
30 [SDA2014] West40 Y*O 03 29 04.06 +31 14 46.5           ~ 49 0
31 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 596 1
32 [JJK2007] 23 Y*O 03 29 10.68 +31 18 20.6           ~ 31 1
33 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 465 0
34 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1219 1
35 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 553 0
36 [JCC87] IRAS 4C Y*O 03 29 13.54 +31 13 58.2           ~ 84 1
37 IRAS 03267+3128 cor 03 29 51.82 +31 39 06.0           ~ 50 0
38 IRAS 03271+3013 cor 03 30 15.159 +30 23 49.38           ~ 60 0
39 IRAS 03282+3035 cor 03 31 20.98 +30 45 30.1           ~ 160 0
40 IRAS 03292+3039 cor 03 32 17.96 +30 49 47.5           ~ 59 0
41 [KJT2007] SMM 34 smm 03 33 05.8 +31 04 59           ~ 9 0
42 [WBK2005] SMM 3 Y*O 03 33 16.3 +31 06 53           ~ 15 0
43 [DCE2008] 093 cor 03 33 16.44 +31 06 52.5           ~ 35 0
44 [HKM99] B1-b cor 03 33 20.32 +31 07 21.5           ~ 158 0
45 SSTc2d J033327.2+310710 cor 03 33 27.29 +31 07 10.2           ~ 45 0
46 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1061 0
47 HH 211 cor 03 43 56.52 +32 00 52.8           ~ 293 0
48 NAME HH 211 FIR Y*O 03 43 56.770 +32 00 49.90           ~ 16 0
49 NAME IC 348 MMS cor 03 43 56.84 +32 03 04.7           ~ 66 1
50 IC 348 OpC 03 44 34 +32 09.8           ~ 1227 1
51 Cl* IC 348 LRL 1872 Y*O 03 44 43.308 +32 01 31.57           ~ 44 1
52 NAME SERPENS SMM 3 smm 18 29 59.7 +01 14 00           ~ 84 1
53 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 484 0
54 [DE95] LDN 1157 B2 out 20 39 09.3 +68 00 44           ~ 59 0
55 [DE95] LDN 1157 B1 out 20 39 11 +68 01.3           ~ 180 0
56 NAME Gould Belt PoG ~ ~           ~ 711 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2014A&A...572A...9K and select 'bookmark this link' or equivalent in the popup menu


2020.07.11-19:39:36

© Université de Strasbourg/CNRS

    • Contact