In this work , I have presented a multi-frequency variability and correlation study of the blazar Ton 599 , which was observed first time in flaring state at the end of 2017 .
Data from Fermi -LAT , Swift-XRT/UVOT , Steward Observatory , and OVRO ( 15 GHz ) is used , and it is found that the source is more variable in \gamma -ray and optical/UV than X-ray and radio .
Large variations in the degree of polarization ( DoP ) and position angle ( PA ) is noticed during the flaring period .
Maximum flux during \gamma -ray flare is found to be 12.63 \times 10 ^ { -7 } at MJD 58057.5 from the 1-day bin light curve ( LC ) , which is the maximum flux ever achieved by this source .
It is further found that all the peaks of flare are very symmetric , which suggests the cooling time of electrons is much smaller than light crossing time .
Using 1-day as a fast variability time , the size of the \gamma -ray emission region is estimated as 1.88 \times 10 ^ { 16 } cm .
Two 42 GeV of photons are detected during the flare which puts a constraint on the location of the emission region , and it is found that the \gamma -ray emitting blob is located at the outer edge or outside the broad line region ( BLR ) .
A trend of increasing fractional variability towards higher energies is also seen .
Strong correlations were seen between \gamma -ray , optical/UV , X-ray , and radio ( 15 GHz ) emission .
A small time lag between \gamma -ray and optical/UV suggest their emission to be co-spatial while lag of 27 days between \gamma -ray and OVRO ( 15 GHz ) suggest two different emission zone separated by a distance of \sim 5 pc .