Journal
ASTROPHYSICAL JOURNAL
Volume 896, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab8813
Keywords
Star formation; Low mass stars; Interstellar medium
Categories
Funding
- National Natural Science Foundation of China [11988101]
- CAS International Partnership Program [114A11KYSB20160008]
- EACOA fellowship from the East Asia Core Observatories Association (EACOA)
- French program Physique et Chimie du Milieu Interstellaire (PCMI) - Conseil National de la Recherche Scientifique (CNRS)
- French program Physique et Chimie du Milieu Interstellaire (PCMI) - Centre National d'Etudes Spatiales (CNES)
- Italian project PRIN-INAF 2016 The Cradle of Life-GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA)
- program PRIN-MIUR 2015 STARS in the CAOS-Simulation Tools for Astrochemical Reactivity and Spectroscopy in the Cyberinfrastructure for Astrochemical Organic Species [2015F59J3R]
- French Agence Nationale de la Recherche (ANR) [ANR-12-JS05-0005]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [741002]
- Ministry of Science and Technology (MoST) of Taiwan [108-2112-M-001-002-MY3]
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We present observations of SO and SO(2)lines toward the shocked regions along the L1157 chemically rich outflow, taken in the context of the Seeds of Life in Space IRAM Northern Extended Millimeter Array Large Program, and supported by data from the Submillimeter Array and IRAM-30 m telescope at 1.1-3.6 mm wavelengths. We simultaneously analyze, for the first time, all of the brightest shocks in the blueshifted lobe, namely, B0, B1, and B2. We found the following. (1) SO and SO(2)may trace different gas, given that the large(-scale) velocity gradient analysis indicates for SO(2)a volume density (10(5)-10(6) cm(-3)) denser than that of the gas emitting in SO by a factor up to an order of magnitude. (2) Investigating the 0.1 pc scale field of view, we note a tentative gradient along the path of the precessing jet. More specifically, chi(SO/SO2) decreases from the B0-B1 shocks to the older B2. (3) At a linear resolution of 500-1400 au, a tentative spatial displacement between the two emitting molecules is detected, with the SO peak closer (with respect to SO2) to the position where the recent jet is impinging on the B1 cavity wall. Our astrochemical modeling shows that the SO and SO(2)abundances evolve on timescales less than about 1000 years. Furthermore, the modeling requires high abundances (2 x 10(-6)) of both H2S/H and S/H injected in the gas phase due to the shock occurrence, so prefrozen OCS only is not enough to reproduce our new observations.
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