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We present a study of star formation in the Central Molecular Zone (CMZ) ofour Galaxy through the association of three star formation indicators: 6.7 GHzCH3OH masers, 22 GHz H2O masers, and enhanced 4.5 micron emission (`green')sources. We explore how star formation in the Galactic center (l < 1.3 deg, |b|< 10', where l and b are Galactic longitude and Galactic latitude) compareswith that of the Galactic disk (6 deg < l < 345 deg, |b| < 2 deg). Using anautomated algorithm, we search for enhanced 4.5 micron emission sources toward6.7 GHz CH3OH masers detected in the Parkes Methanol Multibeam Survey. Wecombine these results with our 22 GHz H2O maser survey of the CMZ carried outwith the Mopra telescope. We find that the correlation of CH3OH masers withgreen sources is a function of Galactic latitude, with a minimum close to b=0and increasing with |b| (toward the central part of the Galaxy, 6 deg < l < 345deg, |b| < 2 deg). We find no significant difference between the correlationrate of CH3OH masers with green sources in the CMZ and the disk. This suggeststhat although the physical conditions of the gas are different in the Galacticcenter from that of the Galactic disk, once gravitational instability sets inat sufficiently high densities, signatures of star formation appear to besimilar in both regions. Moreover, the detection of green sources, even at thedistance of the Galactic center, shows that our technique can easily identifythe early stages of star formation, especially in low extinction regions of theGalaxy. Through the association of H2O and CH3OH masers, we identify 15star-forming sites in the CMZ. We find no coincident H2O and CH3OH masersoutside the CMZ (with limited H2O maser survey coverage outside the CMZ),possibly indicating a difference in the maser evolutionary sequence forstar-forming cores in the Galactic center region and the disk.

Star Formation Sites toward the Galactic Center Region: The Correlation of CH3OH Masers, H2O Masers, and Near-IR Green Sources