2013A&A...559A..51E


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.23CEST08:13:20

2013A&A...559A..51E - Astronomy and Astrophysics, volume 559A, 51-51 (2013/11-1)

Combined IRAM and Herschel/HIFI study of cyano(di)acetylene in Orion KL: tentative detection of DC3N.

ESPLUGUES G.B., CERNICHARO J., VITI S., GOICOECHEA J.R., TERCERO B., MARCELINO N., PALAU A., BELL T.A., BERGIN E.A., CROCKETT N.R. and WANG S.

Abstract (from CDS):

We present a study of cyanoacetylene (HC3N) and cyanodiacetylene (HC5N) in Orion KL using observations from two line surveys performed with the IRAM 30-m telescope and the HIFI instrument onboard the Herschel telescope. The frequency ranges covered are 80-280GHz and 480-1906GHz. This study (divided by families of molecules) is part of a global analysis of the physical conditions of Orion KL and the molecular abundances in the different components of this cloud. We modeled the observed lines of HC3N, HC5N, their isotopologues (including DC3N), and vibrational modes using a non-local thermodynamic equilibrium (non-LTE) radiative transfer code. In addition, to investigate the chemical origin of HC3N and DC3N in Orion KL, we used a time-dependent chemical model. We detect 40 lines of the ground vibrational state of HC3N and 68 lines of its 13C isotopologues. We also detect 297 lines of six vibrational modes of this molecule (ν7, 2ν7, 3ν7, ν6, ν5, and ν67) and 35 rotational lines of the ground vibrational state of HC5N. We report the first tentative detection of DC3N in a giant molecular cloud. We have obtained a DC3N/HC3N abundance ratio of 0.015±0.009, similar to typical D/H ratios of cold dark clouds. We provide column densities for all species and derived isotopic and molecular abundances. We also made a 2'x2' map around Orion IRc2 and present maps of the HC3N lines with energies from 34 to 154K and of the HC3N vibrational modes ν6 and ν7 with energies between 354 and 872K. In addition, a comparison of our results for HC3N with those in other clouds has allowed us to derive correlations between the column density, the FWHM, the mass, and the luminosity of the clouds. The high column densities of HC3N obtained in the hot core, in particular of the ground vibrational state and the vibrational mode ν7, make this molecule an excellent tracer of hot and dense gas. In addition, the wide frequency range covered reveals the need to consider a temperature and density gradient in the hot core to obtain better line fits. The high D/H ratio (similar to that obtained in cold clouds) that we derive suggests a deuterium enrichment. Our chemical models indicate that the possible deuterated HC3N in Orion KL is formed during the gas-phase. This fact provides new hints concerning the processes leading to deuteration.

Abstract Copyright:

Journal keyword(s): ISM: clouds - ISM: molecules - ISM: abundances - radio lines: ISM

VizieR on-line data: <Available at CDS (J/A+A/559/A51): tablea1.dat>

Simbad objects: 39

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Number of rows : 39

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 IRAS 01160+6529 IR 01 19 26.499 +65 45 44.82           ~ 18 0
2 NAME Polaris Cirrus Cloud MoC 01 52 29.6 +87 40 31           ~ 69 0
3 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 928 2
4 [HKM99] B1-b cor 03 33 20.32 +31 07 21.5           ~ 150 0
5 LDN 1489 DNe 04 04 47.5 +26 19 42           ~ 190 0
6 LDN 1400K DNe 04 10 48.6 +54 53 14           ~ 30 0
7 LDN 1498 DNe 04 11.0 +24 58           ~ 241 0
8 NAME [BM89] L1521B cor 04 24 12.7 +26 36 53           ~ 59 0
9 LDN 1400G DNe 04 25 10.5 +54 19 11           ~ 22 0
10 NAME [BM89] L1521E DNe 04 29 21.0 +26 14 19           ~ 82 1
11 NAME Kutner's Cloud MoC 04 32 44.6 +24 23 13           ~ 208 0
12 LDN 1527 DNe 04 39 53 +25 45.0           ~ 469 0
13 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3310 0
14 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1326 0
15 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 653 0
16 V* V2254 Ori Or* 05 35 14.113 -05 22 22.73           B 276 2
17 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 1939 1
18 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 171 0
19 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 559 1
20 M 42 HII 05 35 17.3 -05 23 28           ~ 3658 0
21 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 466 0
22 OMC 2 MoC 05 35 27 -05 10.1           ~ 374 1
23 NAME Ori A MoC 05 38 -07.1           ~ 2611 0
24 NAME Mon R2 HII 06 07 46.6 -06 22 59           ~ 633 2
25 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1545 1
26 IRC +10216 C* 09 47 57.406 +13 16 43.56     10.96     C9,5e 2102 0
27 [PCW91] Ced 110 IRS 10 Y*O 11 06 33.38 -77 23 34.6           ~ 57 1
28 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 674 1
29 OH 351.41 +0.64 Mas 17 20 53.4 -35 47 01           ~ 58 1
30 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11007 0
31 NAME Sgr B2N Mas 17 47 20.0 -28 22 40           ~ 28 1
32 NAME Sgr B2M Mas 17 47 20.13 -28 23 06.1           ~ 33 1
33 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1851 1
34 W 31 SFR 18 10 28.6 -19 55 51           ~ 240 0
35 NAME M 17 SW SFR 18 20 23.1 -16 11 43           ~ 241 0
36 NAME CrA C cor 19 03 56.1 -37 15 32           ~ 12 0
37 W 51 SNR 19 23 50 +14 06.0           ~ 1119 1
38 NAME DR 21 S IR 20 39 00.7 +42 19 15           ~ 12 0
39 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 628 2

    Equat.    Gal    SGal    Ecl

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2019.10.23-08:13:20

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