2013A&A...556A..89Y


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.25CET06:20:29

2013A&A...556A..89Y - Astronomy and Astrophysics, volume 556A, 89-89 (2013/8-1)

High-J CO survey of low-mass protostars observed with Herschel-HIFI.

YILDIZ U.A., KRISTENSEN L.E., VAN DISHOECK E.F., SAN JOSE-GARCIA I., KARSKA A., HARSONO D., TAFALLA M., FUENTE A., VISSER R., JORGENSEN J.K. and HOGERHEIJDE M.R.

Abstract (from CDS):

In the deeply embedded stage of star formation, protostars start to heat and disperse their surrounding cloud cores. The evolution of these sources has traditionally been traced through dust continuum spectral energy distributions (SEDs), but the use of CO excitation as an evolutionary probe has not yet been explored due to the lack of high-J CO observations. The aim is to constrain the physical characteristics (excitation, kinematics, column density) of the warm gas in low-mass protostellar envelopes using spectrally resolved Herschel data of CO and compare those with the colder gas traced by lower excitation lines. Herschel-HIFI observations of high-J lines of 12CO, 13CO, and C18O (up to Ju=10, Eu up to 300K) are presented toward 26 deeply embedded low-mass Class 0 and Class I young stellar objects, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. This is the first large spectrally resolved high-J CO survey conducted for these types of sources. Complementary lower J CO maps were observed using ground-based telescopes, such as the JCMT and APEX and convolved to matching beam sizes. The 12CO 10-9 line is detected for all objects and can generally be decomposed into a narrow and a broad component owing to the quiescent envelope and entrained outflow material, respectively. The 12CO excitation temperature increases with velocity from ∼60K up to ∼130K. The median excitation temperatures for 12CO, 13CO, and C18O derived from single-temperature fits to the J_ u_=2-10 integrated intensities are ∼70K, 48K and 37K, respectively, with no significant difference between Class 0 and Class I sources and no trend with Menv or L_ bol_. Thus, in contrast to the continuum SEDs, the spectral line energy distributions (SLEDs) do not show any evolution during the embedded stage. In contrast, the integrated line intensities of all CO isotopologs show a clear decrease with evolutionary stage as the envelope is dispersed. Models of the collapse and evolution of protostellar envelopes reproduce the C18O results well, but underproduce the 13CO and 12CO excitation temperatures, due to lack of UV heating and outflow components in those models. The H2O 110-101/CO 10-9 intensity ratio does not change significantly with velocity, in contrast to the H2O/CO 3-2 ratio, indicating that CO 10-9 is the lowest transition for which the line wings probe the same warm shocked gas as H2O. Modeling of the full suite of C18O lines indicates an abundance profile for Class 0 sources that is consistent with a freeze-out zone below 25K and evaporation at higher temperatures, but with some fraction of the CO transformed into other species in the cold phase. In contrast, the observations for two Class I sources in Ophiuchus are consistent with a constant high CO abundance profile. The velocity resolved line profiles trace the evolution from the Class 0 to the Class I phase through decreasing line intensities, less prominent outflow wings, and increasing average CO abundances. However, the CO excitation temperature stays nearly constant. The multiple components found here indicate that the analysis of spectrally unresolved data, such as provided by SPIRE and PACS, must be done with caution.

Abstract Copyright:

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

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 - 2021
#notes
1 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 242 1
2 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 304 0
3 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 405 3
4 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 611 1
5 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 468 0
6 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1235 1
7 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 562 0
8 LDN 1489 DNe 04 04 47.5 +26 19 42           ~ 198 0
9 RAFGL 5123 Y*O 04 31 34.07736 +18 08 04.9020           K3V/M3III 816 0
10 IRAS 04361+2547 Y*O 04 39 13.89767 +25 53 20.6340           ~ 185 1
11 IRAS 04365+2535 Y*O 04 39 35.19360 +25 41 44.7252           ~ 242 0
12 LDN 1527 DNe 04 39 53 +25 45.0           ~ 508 0
13 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1382 0
14 2MASS J08254384-5100326 Y*O 08 25 43.85 -51 00 32.7           ~ 298 1
15 Ass Cha T 2-21 TT* 11 06 15.3485848381 -77 21 56.737939872   12.58 11.01   9.35 G5Ve 123 0
16 IRAS 11051-7706 Y*O 11 06 46.025 -77 22 29.67           ~ 71 0
17 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 120 0
18 V* DK Cha Or* 12 53 17.2028372976 -77 07 10.727661977           F0 132 0
19 IRAS 15398-3359 Y*? 15 43 02.21016 -34 09 07.7112       18.38 21.72 ~ 131 0
20 GSS 30 Y*O 16 26 21.38160 -24 23 04.0524           ~ 200 1
21 [GY92] 63 * 16 26 32.9 -24 45 34           ~ 4 0
22 Elia 2-29 Y*O 16 27 09.43032 -24 37 18.7716           ~ 267 1
23 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3083 0
24 IRAS 16285-2355 Y*O 16 31 35.65752 -24 01 29.4708           ~ 106 0
25 HBC 650 TT* 16 34 29.32 -15 47 01.4           K3.0 165 2
26 NAME LDN 483-mm mm 18 17 29.8 -04 39 38           ~ 18 0
27 LDN 483 DNe 18 17 35 -04 39.8           ~ 215 0
28 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 935 2
29 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 238 2
30 NAME Serpens SMM 4 cor 18 29 57.1 +01 13 15           ~ 123 0
31 NAME SERPENS SMM 3 smm 18 29 59.7 +01 14 00           ~ 85 1
32 NAME LDN 723-mm smm 19 17 53.70 +19 12 20.0           ~ 15 0
33 LDN 723 DNe 19 18 12 +19 13.6           ~ 153 0
34 LDN 663 DNe 19 36 55 +07 34.4           ~ 562 0
35 [HSW99] B 335 SMM 1 cor 19 37 00.7 +07 34 08           ~ 20 0
36 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 493 0

    Equat.    Gal    SGal    Ecl

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2020.11.25-06:20:29

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