An Unbiased Spectral Line Survey toward R CrA IRS7B in the 345 GHz Window with ASTE

TL;DR

This spectral line survey of R CrA IRS7B reveals a unique chemical composition with weak hot corino activity and abundant carbon-chain molecules, indicating a mixed chemical nature influenced by nearby UV radiation.

Contribution

First spectral line survey of R CrA IRS7B in the 345 GHz window, revealing its distinct chemical characteristics and potential influence of external UV radiation.

Findings

Weak hot corino activity indicated by low rotation temperature and deuterium ratios.

Abundant carbon-chain molecules, but not classified as WCCC source.

Chemical diversity in low-mass star-forming regions demonstrated.

Abstract

We have conducted a spectral line survey in the 332 - 364 GHz region with the ASTE 10 m telescope toward R CrA IRS7B, a low-mass protostar in the Class 0 or Class 0/I transitional stage. We have also performed some supplementary observations in the 450 GHz band. In total, 16 molecular species are identified in the 332 - 364 GHz region. Strong emission lines of CN and CCH are observed, whereas complex organic molecules and long carbon-chain molecules which are characteristics of hot corino and warm carbon-chain chemistry (WCCC) source, respectively, are not detected. The rotation temperature of CH3OH is evaluated to be 31 K, which is significantly lower than that reported for the prototypical hot corino IRAS 16293-2422 (~85 K). The deuterium fractionation ratios for CCH and H2CO are obtained to be 0.038 and 0.050, respectively, which are much lower than those in the hot corino. These results suggest a weak hot corino activity in R CrA IRS7B. On the other hand, the carbon-chain related molecules, CCH and c-C3H2, are found to be abundant. However, this source cannot be classified as a WCCC source, since long carbon-chain molecules are not detected. If WCCC and hot corino chemistry represent the two extremes in chemical compositions of low-mass Class 0 sources, R CrA IRS7B would be a source with a mixture of these two chemical characteristics. The UV radiation from the nearby Herbig Ae star R CrA may also affect the chemical composition. The present line survey demonstrates further chemical diversity in low-mass star-forming regions.