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              <p>The high sensitivity of the IRAM 30-m Astrochemical Surveys At IRAM (ASAI) unbiased spectral survey in the mm window allows us to detect NO emission towards both the Class I object SVS13-A and the protostellar outflow shock L1157-B1. We detect the hyperfine components of the &lt;SUP&gt;2&lt;/SUP&gt;Π&lt;SUB&gt;1/2&lt;/SUB&gt;J = 3/2 → 1/2 (at 151 GHz) and the &lt;SUP&gt;2&lt;/SUP&gt;Π&lt;SUB&gt;1/2&lt;/SUB&gt;J = 5/2 → 3/2 (at 250 GHz) spectral pattern. The two objects show different NO profiles: (i) SVS13-A emits through narrow (1.5 km s&lt;SUP&gt;-1&lt;/SUP&gt;) lines at the systemic velocity, while (ii) L1157-B1 shows broad (∼5 km s&lt;SUP&gt;-1&lt;/SUP&gt;) blueshifted emission. For SVS13-A, the analysis leads to T&lt;SUB&gt;ex&lt;/SUB&gt; ≥ 4 K, N(NO) ≤ 3 × 10&lt;SUP&gt;15&lt;/SUP&gt; cm&lt;SUP&gt;-2&lt;/SUP&gt;, and indicates the association of NO with the protostellar envelope. In L1157-B1, NO is tracing the extended outflow cavity: T&lt;SUB&gt;ex&lt;/SUB&gt; ≃ 4-5 K, and N(NO) = 5.5 ± 1.5 × 10&lt;SUP&gt;15&lt;/SUP&gt; cm&lt;SUP&gt;-2&lt;/SUP&gt;. Using C&lt;SUP&gt;18&lt;/SUP&gt;O, &lt;SUP&gt;13&lt;/SUP&gt;C&lt;SUP&gt;18&lt;/SUP&gt;O, C&lt;SUP&gt;17&lt;/SUP&gt;O, and &lt;SUP&gt;13&lt;/SUP&gt;C&lt;SUP&gt;17&lt;/SUP&gt;O ASAI observations, we derive an NO fractional abundance less than ∼10&lt;SUP&gt;-7&lt;/SUP&gt; for the SVS13-A envelope, in agreement with previous measurements towards extended photodissociation regions (PDRs) and prestellar objects. Conversely, a definite X(NO) enhancement is measured towards L1157-B1, ∼6 × 10&lt;SUP&gt;-6&lt;/SUP&gt;, showing that the NO production increases in shocks. The public code UCLCHEM was used to interpret the NO observations, confirming that the abundance observed in SVS13-A can be attained in an envelope with a gas density of 10&lt;SUP&gt;5&lt;/SUP&gt; cm&lt;SUP&gt;-3&lt;/SUP&gt; and a kinetic temperature of 40 K. The NO abundance in L1157-B1 is reproduced with pre-shock densities of 10&lt;SUP&gt;5&lt;/SUP&gt; cm&lt;SUP&gt;-3&lt;/SUP&gt; subjected to a ∼45 km s&lt;SUP&gt;-1&lt;/SUP&gt; shock.</p>
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