We study X-ray and UV emission from the narrow-line Seyfert 1 galaxy II Zw 177 using a 137 { ~ { } ks } long and another 13 { ~ { } ks } short XMM-Newton observation performed in 2012 and 2001 , respectively .
Both observations show soft X-ray excess emission contributing 76.9 \pm 4.9 \% in 2012 and 58.8 \pm 10.2 \% in 2001 in the 0.3 - 2 { ~ { } keV } band .
We find that both blurred reflection from an ionized disc and Comptonized disc emission describe the observed soft excess well .
Time-resolved spectroscopy on scales of \sim 20 { ~ { } ks } reveals strong correlation between the soft excess and the powerlaw components .
The fractional variability amplitude F _ { var } derived from EPIC-pn lightcurves at different energy bands is nearly constant ( F _ { var } \sim 20 \% ) .
This is in contrast to other AGNs where the lack of short term variation in soft X-ray excess emission has been attributed to intense light bending in the framework of the “ lamppost ” model .
Thus , the variations in powerlaw emission are most likely intrinsic to corona rather than just due to the changes of height of compact corona .
The variable UV emission ( F _ { var } \sim 1 \% ) is uncorrelated to any of the X-ray components on short timescales suggesting that the UV emission is not dominated by the reprocessed emission .
The gradual observed decline in the UV emission in 2012 may be related to the secular decline due to the changes in the accretion rate .
In this case , the short term X-ray variability is not due to the changes in the seed photons but intrinsic to the hot corona .