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

Colzi, L.L.ColziFONTANI, FRANCESCOFRANCESCOFONTANICaselli, P.P.CaselliCeccarelli, C.C.CeccarelliHily-Blant, P.P.Hily-BlantBizzocchi, L.L.Bizzocchi2020-10-142020-10-1420180004-6361http://hdl.handle.net/20.500.12386/27823The 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. IRAM data used in the paper (FITS) is only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A129">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A129STAMPAenNitrogen and hydrogen fractionation in high-mass star-forming cores from observations of HCN and HNCArticle10.1051/0004-6361/2017305762-s2.0-85041387397000429205200001https://www.aanda.org/articles/aa/abs/2018/01/aa30576-17/aa30576-17.html2018A&A...609A.129CFIS/05 - ASTRONOMIA E ASTROFISICA