Revealing Gas Inflows Toward the Galactic Central Molecular Zone

Abstract

Abstract We study the gas inflows toward the Galactic Central Molecular Zone (CMZ) based on the gas morphological and kinematic features from the Milky Way Imaging Scroll Painting in the region of l = 1.°2–19.°0 and ∣b∣ ≲ 3.°0. We find that the near dust lane appears to extend to l ∼ 15°, in which the end of the large-scale gas structure intersects with the 3 kpc ring at a distance of ∼5 kpc. Intriguingly, many filamentary molecular clouds (MCs), together with the bow-like/ballistic-like clouds and continuous CO features with notable velocity gradient, are finely outlined along the long structure. These MCs also have relatively large velocity dispersions, indicating the shocked gas generated by local continuous accretion and thus the enhanced turbulence along the entire gas structure. We suggest that the ∼3.1–3.6 kpc-long CO structure originates from the accretion molecular gas driven by the Galactic bar. The gas near the bar end at the 3 kpc ring region becomes an important reservoir for the large-scale accreting flows inward to the CMZ through the bar channel. The inclination angle of the bar is estimated to be ϕ bar = 23° ± 3°, while the pattern speed of the bar is Ωbar ≲ 32.5 ± 2.5 km s−1 kpc−1. The total mass of the whole near gas lane is about 1.3 ± 0.4 × 107 M ⊙ according to the calculated X CO ∼ 1.0 ± 0.4 × 1020 cm−2(K km s−1)−1 from the large-scale 12CO and 13CO data and the complementary H i data. We revisit the gas inflow rate as a mean value of 1.1 ± 0.3 M ⊙ yr−1, which seems to be comparable to the outflow's rate of the Galactic nuclear winds after applying the updated lower X-factor above.