We present a study of star formation in the central molecular zone (CMZ) of our Galaxy through the association of three star formation indicators: 6.7GHz CH_3_OH masers, 22GHz H_2_O masers, and enhanced 4.5{mu}m emission ('green') sources. We explore how star formation in the CMZ (|l|<1.3{deg}, |b|l>345{deg}, |b|l>345{deg}, |b|<2{deg}). We find no significant difference between the correlation rate of CH_3_OH masers with green sources in the CMZ and the disk. This suggests that although the physical conditions of the gas are different in the CMZ from that of the Galactic disk, once gravitational instability sets in at sufficiently high densities, signatures of star formation appear to be similar in both regions. Moreover, the detection of green sources, even at the distance of the Galactic center, shows that our technique can easily identify the early stages of star formation, especially in low-extinction regions of the Galaxy. Through the association of H_2_O and CH_3_OH masers, we identify 15 star-forming sites in the CMZ. We find a higher correlation rate of coincident H_2_O and CH_3_OH masers within the CMZ compared to the Galactic disk, indicating a difference in the maser evolutionary sequence for star-forming cores in these two regions.

Cone search capability for table J/A+A/563/A68/table2 (H_2_O masers in the survey region)

Cone search capability for table J/A+A/563/A68/tableb1 (Association of green sources with CH_3_OH masers)

Cone search capability for table J/A+A/563/A68/tableb2 (Association of H_2_O masers with CH_3_OH masers)

Cone search capability for table J/A+A/563/A68/tableb3 (CH_3_OH masers not associated with H_2_O masers)

Cone search capability for table J/A+A/563/A68/tableb4 (H_2_O masers not associated with CH_3_OH masers)