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Fig. 9


Plots showing candidate YSOs in the CMZ selected using our criterion and their distribution in the (l, b) plane. Left: HKS vs. H [8.0] diagram is used to select YSOs from the source sample constructed by combining NIR catalogue of Galactic centre using SIRIUS (Nagashima et al. 1999; Nagayama et al. 2003), 3.68.0 μm photometry from Ramírez et al. (2008), 24 μm photometry from Gutermuth & Heyer (2015) and 15 μm photometry from ISOGAL PSC. The dashed line represents our proposed criteria to separate YSOs and late-type stars. Right: spatial distribution of YSOs in the (l, b) plane colour coded with the number of YSOs in (l, b) bins of 0.̊05 each. The white patch close to (l, b) ~ (0.̊0, 0.̊0) is the observational artefact from the Gutermuth & Heyer (2015) and the ISOGAL PSC catalogues where data are lacking.

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