Outflows and Bubbles in Taurus: Star-formation Feedback Sufficient to
  Maintain Turbulence
  We have identified outflows and bubbles in the Taurus molecular cloud based
on the $\sim 100$ 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 $\bf \sim 3.9 \times
10^{45}$ erg, which is \textbf{1\%} of the cloud turbulent energy. The total
kinetic energy of the detected bubbles is estimated to be $\sim 9.2 \times
10^{46}$ erg, which is 29\% of the turbulent energy of Taurus. The energy
injection rate from outflows is $\bf \sim 1.3 \times 10^{33}~\rm erg\ s^{-1}$,
\textbf{0.4 - 2 times} the dissipation rate of the cloud turbulence. The energy
injection rate from bubbles is $\sim 6.4 \times 10^{33}$ erg s$^{-1}$,
\textbf{2 - 10 times} the turbulent dissipation rate of the cloud. The
gravitational binding energy of the cloud is $\bf \sim 1.5 \times 10^{48}$ {\bf
erg}, \textbf{385} and 16 times the energy of outflows and bubbles,
respectively. We conclude that neither outflows nor bubbles can \textbf{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.
