Silicon-bearing molecules in the shock L1157-B1: first detection of SiS around a Sun-like protostar. (4th May 2017)

• Record Type: Journal Article
• Authors: Podio, L.; Codella, C.; Lefloch, B.; Balucani, N.; Ceccarelli, C.; Bachiller, R.; Benedettini, M.; Cernicharo, J.; Faginas-Lago, N.; Fontani, F.; Gusdorf, A.; Rosi, M.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 470:Number 1(2017:Sep.)
• Page Start: L16
• Page End: L20
• Publication Date: 2017-05-04
• Subjects: astrochemistry – stars: formation -- ISM: jets and outflows -- ISM: molecules; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slx068
• Languages: English
• ISSNs: 1745-3933

Abstract

Abstract: The shock L1157-B1 driven by the low-mass protostar L1157-mm is a unique environment to investigate the chemical enrichment due to molecules released from dust grains. IRAM-30m and Plateau de Bure Interferometer observations allow a census of Si-bearing molecules in L1157-B1. We detect SiO and its isotopologues and, for the first time in a shock, SiS. The strong gradient of the [SiO/SiS] abundance ratio across the shock (from ≥180 to ∼25) points to a different chemical origin of the two species. SiO peaks where the jet impacts the cavity walls ([SiO/H2 ] ∼ 10 −6 ), indicating that SiO is directly released from grains or rapidly formed from released Si in the strong shock occurring at this location. In contrast, SiS is only detected at the head of the cavity opened by previous ejection events ([SiS/H2 ] ∼ 2 × 10 −8 ). This suggests that SiS is not directly released from the grain cores but instead should be formed through slow gas-phase processes using part of the released silicon. This finding shows that Si-bearing molecules can be useful to distinguish regions where grains or gas-phase chemistry dominates.