2018A&A...609A.129C


Query : 2018A&A...609A.129C

2018A&A...609A.129C - Astronomy and Astrophysics, volume 609A, 129-129 (2018/1-1)

Nitrogen and hydrogen fractionation in high-mass star-forming cores from observations of HCN and HNC.

COLZI L., FONTANI F., CASELLI P., CECCARELLI C., HILY-BLANT P. and BIZZOCCHI L.

Abstract (from CDS):

The ratio between the two stable isotopes of nitrogen, 14N and 15N, is well measured in the terrestrial atmosphere (∼272), and for the pre-solar nebula (∼441, deduced from the solar wind). Interestingly, some pristine solar system materials show enrichments in 15N with respect to the pre-solar nebula value. However, it is not yet clear if and how these enrichments are linked to the past chemical history because we have only a limited number of measurements in dense star-forming regions. In this respect, dense cores, which are believed to be the precursors of clusters and also contain intermediate- and high-mass stars, are important targets because the solar system was probably born within a rich stellar cluster, and such clusters are formed in high-mass star-forming regions. The number of observations in such high-mass dense cores has remained limited so far. In this work, we show the results of IRAM-30 m observations of the J=1-0 rotational transition of the molecules HCN and HNC and their 15N-bearing counterparts towards 27 intermediate- and high-mass dense cores that are divided almost equally into three evolutionary categories: high-mass starless cores, high-mass protostellar objects, and ultra-compact HII regions. We have also observed the DNC(2-1) rotational transition in order to search for a relation between the isotopic ratios D/H and 14N/15N. We derive average 14N/15N ratios of 359±16 in HCN and of 438±21 in HNC, with a dispersion of about 150-200. We find no trend of the 14N/15N ratio with evolutionary stage. This result agrees with what has been found for N2H+ and its isotopologues in the same sources, although the 14N/15N ratios from N2H+ show a higher dispersion than in HCN/HNC, and on average, their uncertainties are larger as well. Moreover, we have found no correlation between D/H and 14N/15N in HNC. These findings indicate that (1) the chemical evolution does not seem to play a role in the fractionation of nitrogen, and that (2) the fractionation of hydrogen and nitrogen in these objects is not related.

Abstract Copyright: © ESO, 2018

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

VizieR on-line data: <Available at CDS (J/A+A/609/A129): sources.dat dnc/* h13cn/* h15nc/* hc15n/* hn13c/*>

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 [PSB2010] MM1 cor 00 14 26.10 +64 28 44.0           ~ 15 1
2 [PSB2010] MM2 mm 00 14 26.3 +64 28 27           ~ 16 0
3 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 803 0
4 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 198 2
5 [BEZ2011] EC cor 05 30 48.7 +33 47 53           ~ 16 0
6 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1127 2
7 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2206 1
8 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 194 0
9 [BSG2002] mm3 mm 05 39 12.49 +35 45 55.2           ~ 19 0
10 [BSG2002] mm1 mm 05 39 13.08 +35 45 50.5           ~ 14 0
11 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 2147 1
12 RAFGL 2046 HII 18 00 30.388 -24 04 00.20           ~ 323 1
13 GRS G012.89 +00.49 HII 18 11 51.3 -17 31 29           ~ 169 0
14 AGAL G028.354+00.102 Y*O 18 42 44.02 -04 01 54.5           ~ 26 0
15 AGAL G028.324+00.067 Y*O 18 42 46.7 -04 04 08           ~ 52 0
16 [RJS2006] MSXDC G034.43+00.24 MM8 mm 18 53 16.4 +01 26 20           ~ 33 0
17 [RJS2006] MSXDC G034.43+00.24 MM7 mm 18 53 18.3 +01 27 13           ~ 34 0
18 IRAS 18517+0437 SFR 18 54 13.8 +04 41 32           ~ 69 0
19 [BT2009] G2 mm 18 56 50.3 +01 23 16           ~ 29 0
20 NAME I19035-VLA1 HII 19 06 01.5 +06 46 35           ~ 15 1
21 IRAS 19410+2336 SFR 19 43 11.5 +23 44 06           ~ 150 0
22 Onsala 1 cor 20 10 09.2036 +31 31 36.090           ~ 187 0
23 [HC96] G75.78-0.34 1 Mas 20 21 43.976 +37 26 37.98           ~ 10 1
24 [PEG2007] WCloud Cld 20 31 10.71 +40 03 30.3           ~ 15 0
25 [BSG2004] IRAS 20293+3952 mm 1 mm 20 31 12.88 +40 03 22.8           ~ 15 0
26 IRAS 21307+5049 Y*O 21 32 30.59280 +51 02 16.0368           ~ 42 0
27 [FPC2011] I22134-B cor 22 15 05.8 +58 48 59           ~ 12 0
28 [FPC2011] I22134-VLA1 cor 22 15 09.2 +58 49 08           ~ 11 0
29 [FPC2011] I22134-G cor 22 15 10.5 +58 48 59           ~ 12 0
30 IRAS 23033+5951 Y*O 23 05 25.1762883456 +60 08 15.374293800           ~ 88 0
31 IRAS 23118+6110 Y*O 23 14 01.63 +61 27 20.2           ~ 367 0
32 Mol 160 Rad 23 40 54.5 +61 10 28           ~ 94 0

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2023.01.27-00:15:10

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