Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...433..535f&link_type=abstract
Astronomy and Astrophysics, Volume 433, Issue 2, April II 2005, pp.535-552
Astronomy and Astrophysics
Astrophysics
18
Stars: Formation, Stars: Pre-Main Sequence, Stars: Individual: Lkhα 234, Ism: Abundances, Ism: Clouds, Ism: Individual Objects: Ngc 7129
Scientific paper
We have carried out a molecular survey of the Class 0 IM protostar NGC 7129 - FIRS 2 (hereafter FIRS 2) and the Herbig Be star LkHα 234 with the aim of studying the chemical evolution of the envelopes of intermediate-mass (IM) young stellar objects (YSOs). The two objects have similar luminosities (~500 L_&sun;) and are located in the same molecular cloud which minimizes the chemical differences due to different stellar masses or initial cloud conditions. Moreover, since they are located at the same distance, we have the same spatial resolution in both objects. A total of 17 molecular species (including rare isotopes) have been observed in both objects and the structure of their envelopes and outflows has been determined with unprecedent detail. Our results show that the protostellar envelopes are dispersed and warmed up during the evolution of the YSO into a pre-main sequence star. In fact, the envelope mass decreases by a factor >5 from FIRS 2 to LkHα 234, while the kinetic temperature increases from ~13 K to 28 K. On the other hand, there is no molecular outflow associated with LkHα 234. The molecular outflow seems to stop before the star becomes visible. These physical changes strongly affect the chemistry of their envelopes. The N2H+ and NH3 abundances seem to be quite similar in the two objects. However, the H13CO+ abundance is a factor of ~3 lower in the densest part of FIRS 2 than in LkHα 234, very likely because of depletion. In contrast, the SiO abundance is larger by a factor of ~100 in FIRS 2 than in LkHα 234. CS presents complex behavior since its emission arises in different envelope components (outflow, cold envelope, hot core) and could also suffer from depletion. The CH3OH and H2CO column densities are very similar in FIRS 2 and LkHα 234 which implies that the beam-averaged abundances are a factor >5 larger in LkHα 234 than in FIRS 2. The same is found for the PDR tracers CN and HCN which have similar column densities in both objects. Finally, complex behavior is found for the deuterated compounds. While the DCO^+/H13CO+ ratio decreases by a factor of ~4 from FIRS 2 to LkHα 234, the D2CO/H2CO ratios is within a factor 1.5 in both objects. The detection of a warm CH3CN component with Tk >63 K shows the existence of a hot core in FIRS 2. Thus far, only a handful of hot cores have been detected in low and intermediate mass stars. Based on our results in FIRS 2 and LkHα 234, we propose some abundance ratios that can be used as chemical clocks for the envelopes of IM YSOs. The SiO/CS, CN/N2H^+, HCN/N2H^+, DCO^+/HCO+ and D2CO/DCO+ ratios are good diagnostics of the protostellar evolutionary stage.
Tables 1-3 are only available in electronic form at http://www.edpsciences.org
Bachiller Rafael
Caselli Paola
Fuente Asuncion
Henkel Carsten
Rizzo Ricardo J.
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