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Globular clusters (GCs) in the Milky Way (MW) bulge are very difficult tostudy because: i) they suffer from the severe crowding and galactic extinction;which are characteristic of these inner Galactic regions ii) they are moreprone to be affected by dynamical processes. Therefore, they are relativelyfaint and difficult to map. However, deep near-infrared photometry like thatprovided by the VISTA Variables in the Via L\'actea Extended Survey (VVVX) isallowing us to map GCs in this crucial yet relatively uncharted region.  Our results confirm with high confidence that both FSR 19 and FSR 25 aregenuine MW bulge GCs. Each of the performed tests and resulting parametersprovides clear evidence for the GC nature of these targets. We derive distancesof 7.2$\pm$0.7 kpc and D=7.0$\pm$0.6 (corresponding to distance moduli of14.29$\pm$0.08 and  14.23$\pm$0.07) for FSR 19 and FSR 25, respectively. Their ages andmetallicities are 11 Gyr and [Fe/H]= -0.5 dex for both clusters, which weredetermined from Dartmouth and PARSEC isochrone fitting. The integratedluminosities are M$_{Ks}$(FSR 19) = -7.72 mag and M$_{Ks}$(FSR 25) = -7.31 magwhich places them in the faint tail of the GC Luminosity Function. By adoptinga King profile for their number distribution, we determine their core and tidalradii ($r_c$, $r_t$). For FSR 19, r$_{c}$= 2.76$\pm$0.36 pc andr$_{t}$=5.31$\pm$0.49 pc, while FSR 25 appears more extended with r$_{c}$=1.92$\pm$0.59 pc and r$_{t}$=6.85$\pm$1.78 pc. Finally their mean GC PMs (fromGaia EDR3) are $\mu_{\alpha^\ast}$= -2.50 $\pm$0.76 mas $yr^{-1}$,$\mu_{\delta}$= -5.02 $\pm$0.47 mas $yr^{-1}$ and $\mu_{\alpha^\ast}$= -2.61$\pm$ 1.27 mas $yr^{-1}$ , $\mu_{\delta}$= -5.23 $\pm$0.74 mas $yr^{-1}$ forFSR 19 and FSR 25, respectively. }

Confirmation Of Two New Galactic Bulge Globular Clusters: FSR 19 and FSR 25