2017A&A...605A..57F


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET01:42:18

2017A&A...605A..57F - Astronomy and Astrophysics, volume 605A, 57-57 (2017/9-1)

Seeds of Life in Space (SOLIS). I. Carbon-chain growth in the Solar-type protocluster OMC2-FIR4.

FONTANI F., CECCARELLI C., FAVRE C., CASELLI P., NERI R., SIMS I.R., KAHANE C., ALVES F.O., BALUCANI N., BIANCHI E., CAUX E., JABER AL-EDHARI A., LOPEZ-SEPULCRE A., PINEDA J.E., BACHILLER R., BIZZOCCHI L., BOTTINELLI S., CHACON-TANARRO A., CHOUDHURY R., CODELLA C., COUTENS A., DULIEU F., FENG S., RIMOLA A., HILY-BLANT P., HOLDSHIP J., JIMENEZ-SERRA I., LAAS J., LEFLOCH B., OYA Y., PODIO L., PON A., PUNANOVA A., QUENARD D., SAKAI N., SPEZZANO S., TAQUET V., TESTI L., THEULE P., UGLIENGO P., VASTEL C., VASYUNIN A.I., VITI S., YAMAMOTO S. and WIESENFELD L.

Abstract (from CDS):

The interstellar delivery of carbon atoms locked into molecules might be one of the key ingredients for the emergence of life. Cyanopolyynes are carbon chains delimited at their two extremities by an atom ofhydrogen and a cyano group, meaning that they could be excellent reservoirs of carbon. The simplest member, HC3N, is ubiquitous in the galactic interstellar medium and found also in external galaxies. Thus, understanding the growth of cyanopolyynes in regions forming stars similar to our Sun, and what affects them, is particularly relevant. In the framework of the IRAM/NOEMA Large Program SOLIS (Seeds Of Life In Space), we have obtained a map of two cyanopolyynes, HC3N and HC5N, in the protocluster OMC-2 FIR4. Because our Sun is thought to be born in a rich cluster, OMC-2 FIR4 is one of the closest and best known representatives of the environment in which the Sun may have been born. We find a HC3N/HC5N abundance ratio across the source in the range ∼1-30, with the smallest values (≤10) in FIR5 and in the eastern region of FIR4. The ratios ≤10 can be reproduced by chemical models only if: (1) the cosmic-ray ionisation rate ζ is ∼4x10–14s–1; (2) the gaseous elemental ratio C/O is close to unity; and (3) oxygen and carbon are largely depleted. The large ζ is comparable to that measured in FIR4 by previous works and was interpreted as due to a flux of energetic (≥10 MeV) particles from embedded sources. We suggest that these sources could lie east of FIR4 and FIR5. A temperature gradient across FIR4, with T decreasing from east to west by about 10K, could also explain the observed change in the HC3N/HC5N line ratio, without the need of a cosmic ray ionisation rate gradient. However, even in this case, a high constant cosmic-ray ionisation rate (of the order of 10–14s–1) is necessary to reproduce the observations.

Abstract Copyright: © ESO, 2017

Journal keyword(s): radio lines: ISM - stars: formation - ISM: molecules - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/605/A57): list.dat fits/*>

Simbad objects: 15

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Number of rows : 15

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 NAME [BM89] L1521E DNe 04 29 21.0 +26 14 19           ~ 89 1
2 EM* LkHA 101 Em* 04 30 14.438 +35 16 24.03   17.91 15.71 13.33   F 306 1
3 LDN 1527 DNe 04 39 53 +25 45.0           ~ 519 0
4 LDN 1512 MoC 05 04 09.7 +32 43 09           ~ 160 0
5 QSO J0527+0331 BLL 05 27 32.70544796 +03 31 31.5166429     20.00 18.43   ~ 54 1
6 NAME OMC-2 IRS 3 HII 05 35 26.00 -05 10 16.6           ~ 61 0
7 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 120 0
8 OMC 2 MoC 05 35 27 -05 10.1           ~ 399 1
9 2MASS J05352762-0509337 Y*O 05 35 27.622 -05 09 33.78           ~ 73 0
10 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 889 1
11 [PCW91] Ced 110 IRS 10 Y*O 11 06 33.38 -77 23 34.6           ~ 60 1
12 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1078 1
13 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 720 0
14 LDN 1251A DNe 22 30 31.8 +75 14 17           ~ 71 2
15 3C 454.3 Bla 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2557 2

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2021.03.03-01:42:18

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