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 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 } ~ { } erg s ^ { -1 } , 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 } , 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 } 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 .