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              <p>We present the first detection of N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; toward a low-mass protostellar outflow, namely, the L1157-B1 shock, at ~0.1 pc from the protostellar cocoon. The detection was obtained with the IRAM 30 m antenna. We observed emission at 93 GHz due to the J = 1-0 hyperfine lines. Analysis of this emission coupled with HIFI CHESS multiline CO observations leads to the conclusion that the observed N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt;(1-0) line originated from the dense (&gt;=10&lt;SUP&gt;5&lt;/SUP&gt; cm&lt;SUP&gt;-3&lt;/SUP&gt;) gas associated with the large (20''-25'') cavities opened by the protostellar wind. We find an N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; column density of a few 10&lt;SUP&gt;12&lt;/SUP&gt; cm&lt;SUP&gt;-2&lt;/SUP&gt; corresponding to an abundance of (2-8) × 10&lt;SUP&gt;-9&lt;/SUP&gt;. The N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; abundance can be matched by a model of quiescent gas evolved for more than 10&lt;SUP&gt;4&lt;/SUP&gt; yr, i.e., for more than the shock kinematical age (sime2000 yr). Modeling of C-shocks confirms that the abundance of N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; is not increased by the passage of the shock. In summary, N&lt;SUB&gt;2&lt;/SUB&gt;H&lt;SUP&gt;+&lt;/SUP&gt; is a fossil record of the pre-shock gas, formed when the density of the gas was around 10&lt;SUP&gt;4&lt;/SUP&gt; cm&lt;SUP&gt;-3&lt;/SUP&gt;, and then further compressed and accelerated by the shock.</p>
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