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                <title xml:lang="en">Molecular ions in the protostellar shock L1157-B1</title>
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              <p>&lt;BR /&gt; Aims: We perform a complete census of molecular ions with an abundance greater than ~10&lt;SUP&gt;-10&lt;/SUP&gt; in the protostellar shock L1157-B1. This allows us to study the ionisation structure and chemistry of the shock. &lt;BR /&gt; Methods: An unbiased high-sensitivity survey of L1157-B1 performed with the IRAM-30 m and Herschel/HIFI as part of the CHESS and ASAI large programmes allows searching for molecular ions emission. Then, by means of a radiative transfer code in the large velocity gradient approximation, the gas physical conditions and fractional abundances of molecular ions are derived. The latter are compared with estimates of steady-state abundances in the cloud and their evolution in the shock calculated with the chemical model Astrochem. &lt;BR /&gt; Results: We detect emission from HCO&lt;SUP&gt;+&lt;/SUP&gt;, H&lt;SUP&gt;13&lt;/SUP&gt;CO&lt;SUP&gt;+&lt;/SUP&gt;, N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt;, HCS&lt;SUP&gt;+&lt;/SUP&gt;, and for the first time in a shock, from HOCO&lt;SUP&gt;+&lt;/SUP&gt; and SO&lt;SUP&gt;+&lt;/SUP&gt;. The bulk of the emission peaks at blue-shifted velocity, ~0.5-3 km s &lt;SUP&gt;-1&lt;/SUP&gt; with respect to systemic, has a width of ~3-7 km s&lt;SUP&gt;-1&lt;/SUP&gt; and is associated with the outflow cavities (T&lt;SUB&gt;kin&lt;/SUB&gt; ~ 20-70 K, n&lt;SUB&gt;H&lt;SUB&gt;2&lt;/SUB&gt;&lt;/SUB&gt; ~ 10&lt;SUP&gt;5&lt;/SUP&gt; cm&lt;SUP&gt;-3&lt;/SUP&gt;). A high-velocity component up to -40 km s&lt;SUP&gt;-1&lt;/SUP&gt;, associated with the primary jet, is detected in the HCO&lt;SUP&gt;+&lt;/SUP&gt; 1-0 line. Observed HCO&lt;SUP&gt;+&lt;/SUP&gt; and N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; abundances (X&lt;SUB&gt;HCO&lt;SUP&gt;+&lt;/SUP&gt;&lt;/SUB&gt; ~ 0.7-3 × 10&lt;SUP&gt;-8&lt;/SUP&gt;, X&lt;SUB&gt;N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt;&lt;/SUB&gt; ~ 0.4-8 × 10&lt;SUP&gt;-9&lt;/SUP&gt;) agree with steady-state abundances in the cloud and with their evolution in the compressed and heated gas in the shock for cosmic rays ionisation rate ζ = 3 × 10&lt;SUP&gt;-16&lt;/SUP&gt; s&lt;SUP&gt;-1&lt;/SUP&gt;. HOCO&lt;SUP&gt;+&lt;/SUP&gt;, SO&lt;SUP&gt;+&lt;/SUP&gt;, and HCS&lt;SUP&gt;+&lt;/SUP&gt; observed abundances (X&lt;SUB&gt;HOCO&lt;SUP&gt;+&lt;/SUP&gt;&lt;/SUB&gt; ~ 10&lt;SUP&gt;-9&lt;/SUP&gt;, X&lt;SUB&gt;SO&lt;SUP&gt;+&lt;/SUP&gt;&lt;/SUB&gt; ~ 8 × 10&lt;SUP&gt;-10&lt;/SUP&gt;, X&lt;SUB&gt;HCS&lt;SUP&gt;+&lt;/SUP&gt;&lt;/SUB&gt; ~ 3-7 × 10&lt;SUP&gt;-10&lt;/SUP&gt;), instead, are 1-2 orders of magnitude larger than predicted in the cloud; on the other hand, they are strongly enhanced on timescales shorter than the shock age (~2000 years) if CO&lt;SUB&gt;2&lt;/SUB&gt;, S or H&lt;SUB&gt;2&lt;/SUB&gt;S, and OCS are sputtered off the dust grains in the shock. &lt;BR /&gt; Conclusions: The performed analysis indicates that HCO&lt;SUP&gt;+&lt;/SUP&gt; and N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; are a fossil record of pre-shock gas in the outflow cavity, whilst HOCO&lt;SUP&gt;+&lt;/SUP&gt;, SO&lt;SUP&gt;+&lt;/SUP&gt;, and HCS&lt;SUP&gt;+&lt;/SUP&gt; are effective shock tracers that can be used to infer the amount of CO&lt;SUB&gt;2&lt;/SUB&gt; and sulphur-bearing species released from dust mantles in the shock. The observed HCS&lt;SUP&gt;+&lt;/SUP&gt; (and CS) abundance indicates that OCS should be one of the main sulphur carrier on grain mantles. However, the OCS abundance required to fit the observations is 1-2 orders of magnitude larger than observed. Laboratory experiments are required to measure the reactions rates involving these species and to fully understand the chemistry of sulphur-bearing species. &lt;P /&gt;The molecular ions line spectra shown in Fig. 2 are only available at the CDS via anonymous ftp to &lt;A href="http://cdsarc.u-strasbg.fr"&gt;http://cdsarc.u-strasbg.fr&lt;/A&gt; (ftp://130.79.128.5) or via &lt;A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/565/A64"&gt;http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/565/A64&lt;/A&gt;</p>
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          <idno type="ROR">https://ror.org/04gqg1a07</idno>
          <orgName>Université Savoie Mont Blanc</orgName>
          <orgName type="acronym">USMB [Université de Savoie] [Université de Chambéry]</orgName>
          <date type="start">1979-10-01</date>
          <desc>
            <address>
              <addrLine>27, rue Marcoz - 73000 Chambéry</addrLine>
              <country key="FR"/>
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            <ref type="url">https://www.univ-smb.fr</ref>
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          <idno type="ROR">https://ror.org/02feahw73</idno>
          <orgName>Centre National de la Recherche Scientifique</orgName>
          <orgName type="acronym">CNRS</orgName>
          <date type="start">1939-10-19</date>
          <desc>
            <address>
              <country key="FR"/>
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            <ref type="url">https://www.cnrs.fr/</ref>
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        <org type="institution" xml:id="struct-307314" status="VALID">
          <orgName>Centre National d'Études Spatiales [Toulouse]</orgName>
          <orgName type="acronym">CNES</orgName>
          <desc>
            <address>
              <addrLine>18 avenue Edouard Belin 31401 Toulouse</addrLine>
              <country key="FR"/>
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