JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b We present two transit observations of the super-Earth TOI-836b (≈870 K, 1.7 R⊕) using JWST NIRSpec/G395H, resulting in a 2.8–5.2 μm transmission spectrum. Using two reduction pipelines, we achieve a median transit depth precision of 34 ppm for Visit 1 and 36 ppm for Visit 2, leading to a combined precision of 25 ppm in 30-pixel wide spectroscopic channels (≈0.02 μm). The transmission spectrum is well fit by a zero-sloped line, indicating no atmosphere with metallicities <250× Solar for an opaque pressure level of 0.1 bar, corresponding to mean molecular weights <6 g mol⁻¹. This suggests TOI-836b does not have a H₂-dominated atmosphere, in contrast to its larger sibling TOI-836c. Future observations should be cautious about requiring specific transit numbers to rule out scenarios, especially for high metallicities and bright host stars, as PandExo predictions are more optimistic than our data suggests. Keywords: Exoplanet atmospheric composition (2021); Exoplanet atmospheres (487); Exoplanets (498); Infrared spectroscopy (2285) The study of super-Earths is challenging due to their complex interior compositions and lack of solar system counterparts. JWST's NIRSpec/G395H mode enables detailed observations of small exoplanets, detecting molecular species inaccessible before. The COMPASS program focuses on 1–3 R⊕ planets to understand atmospheric compositions. TOI-836b, a super-Earth at the lower edge of the radius valley, shows no detectable atmospheric features, suggesting a low molecular weight atmosphere. The transmission spectrum is consistent with a zero-sloped line, ruling out high metallicity atmospheres. The results indicate TOI-836b has a low molecular weight atmosphere, unlike its larger sibling. Future observations should consider the limitations of current data when planning for specific transit numbers. The study highlights the importance of multi-visit observations and the potential of JWST for understanding exoplanet atmospheres.JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b We present two transit observations of the super-Earth TOI-836b (≈870 K, 1.7 R⊕) using JWST NIRSpec/G395H, resulting in a 2.8–5.2 μm transmission spectrum. Using two reduction pipelines, we achieve a median transit depth precision of 34 ppm for Visit 1 and 36 ppm for Visit 2, leading to a combined precision of 25 ppm in 30-pixel wide spectroscopic channels (≈0.02 μm). The transmission spectrum is well fit by a zero-sloped line, indicating no atmosphere with metallicities <250× Solar for an opaque pressure level of 0.1 bar, corresponding to mean molecular weights <6 g mol⁻¹. This suggests TOI-836b does not have a H₂-dominated atmosphere, in contrast to its larger sibling TOI-836c. Future observations should be cautious about requiring specific transit numbers to rule out scenarios, especially for high metallicities and bright host stars, as PandExo predictions are more optimistic than our data suggests. Keywords: Exoplanet atmospheric composition (2021); Exoplanet atmospheres (487); Exoplanets (498); Infrared spectroscopy (2285) The study of super-Earths is challenging due to their complex interior compositions and lack of solar system counterparts. JWST's NIRSpec/G395H mode enables detailed observations of small exoplanets, detecting molecular species inaccessible before. The COMPASS program focuses on 1–3 R⊕ planets to understand atmospheric compositions. TOI-836b, a super-Earth at the lower edge of the radius valley, shows no detectable atmospheric features, suggesting a low molecular weight atmosphere. The transmission spectrum is consistent with a zero-sloped line, ruling out high metallicity atmospheres. The results indicate TOI-836b has a low molecular weight atmosphere, unlike its larger sibling. Future observations should consider the limitations of current data when planning for specific transit numbers. The study highlights the importance of multi-visit observations and the potential of JWST for understanding exoplanet atmospheres.