We have identified outflows and bubbles in the Taurus molecular cloud based on the ∼ 100 deg 2 Five College Radio Astronomy Observatory 12 CO(1-0) and 13 CO(1-0) maps and the Spitzer young stellar object catalogs. In the main 44 deg 2 area of Taurus we found 55 outflows, of which 31 were previously unknown. We also found 37 bubbles in the entire 100 deg 2 area of Taurus, all of which had not been found before. The total kinetic energy of the identified outflows is estimated to be ∼ 3.9 × 10 45 erg, which is 1% of the cloud turbulent energy. The total kinetic energy of the detected bubbles is estimated to be ∼ 9.2 × 10 46 erg, which is 29% of the turbulent energy of Taurus. The energy injection rate from outflows is ∼ 1.3 × 10 33 erg s −1 , 0.4 -2 times the dissipation rate of the cloud turbulence. The energy injection rate from bubbles is ∼ 6.4 × 10 33 erg s −1 , 2 -10 times the turbulent dissipation rate of the cloud. The gravitational binding energy of the cloud is ∼ 1.5 × 10 48 erg, 385 and 16 times the energy of outflows and bubbles, respectively. We conclude that neither outflows nor bubbles can provide enough energy to balance the overall gravitational binding energy and the turbulent energy of Taurus. However, in the current epoch, stellar feedback is sufficient to maintain the observed turbulence in Taurus.

Hydroxyl (OH) is expected to be abundant in diffuse interstellar molecular gas as it forms along with H 2 under similar conditions and within a similar extinction range. We have analyzed absorption measurements of OH at 1665 MHz and 1667 MHz toward 44 extragalactic continuum sources, together with the J=1-0 transitions of 12 CO, 13 CO, and C 18 O, and the J=2-1 of 12 CO. The excitation temperature of OH were found to follow a modified log-normal distribution