Cold molecular gas in the hot nuclear wind of the Milky Way

Using the Large Millimeter Telescope and the SEQUOIA 3 mm focal plane array, we have searched for molecular line emission from two atomic clouds associated with the Fermi Bubble of the Milky Way. Neither 12CO nor 13CO J=1–0 emission is detected from the H <ns0:sc>I</ns0:sc> cloud, MW-C20. 12CO J=1–0 emission is detected from MW-C21 that is distributed within 11 clumps with most of the CO luminosity coming from a single clump. However, we find no 13CO emission to a 3σ brightness temperature limit of 0.3 K. Using this limit and <ns0:monospace>RADEX</ns0:monospace> non-local thermodynamic equilibrium (non-LTE) excitation models, we derive H2 column density upper limits of (0.4–3)×1021 cm−2 for a set of physical conditions and a H2 to 12CO abundance ratio of 104. Model CO-to-H2 conversion factors are derived for each set of physical conditions. We find the maximum value is 1.6×1020 cm−2/(K km s−1). Increasing [H2/12CO] to 105 to account for photodissociation and cosmic ray ionization increases the column density and X(CO) upper limits by a factor of 10. Applying these X(CO) limits to the CO luminosities, the upper limit on the total molecular mass in MW-C21 is 132±2 M⊙, corresponding to <27% of the neutral gas mass. For the three clumps that are fully resolved, lower limits to the virial ratios are 288±32, 68±28, and 157±39, which suggest that these structures are bound by external pressure to remain dynamically stable over the entrainment time of 2×106 years or are being disrupted by shear and expansion over the clump crossing times of 3–8×105 years. The observations presented in this study add to the growing census of cold gas entrained within the Galactic Center wind.