We report deep optical integral-field spectroscopy with the Multi-Unit Spectroscopic Explorer ( MUSE ) at the Very Large Telescope of the luminous radio-quiet quasi-stellar object ( QSO ) PG 1307+085 ( z = 0.154 ) obtained during the commissioning of the instrument .
Given the high sensitivity and spatial resolution delivered by MUSE , we are able to resolve the compact ( r _ { \mathrm { e } } \sim 1.3 arcsec ) elliptical host galaxy .
After careful spectroscopic deblending of the QSO and host galaxy emission , we infer a stellar velocity dispersion of \sigma _ { * } = 155 \pm 19 km s ^ { -1 } .
This places PG 1307+085 local M _ { \mathrm { BH } } - \sigma _ { * } relation within the intrinsic scatter but offset towards a higher black hole mass with respect to the mean relation .
The observations with MUSE also reveal a large extended narrow-line region ( ENLR ) around PG 1307+085 reaching out to \sim 30 kpc .
In addition , we detect a faint bridge of ionized gas towards the most massive galaxy of the galaxy group being just \sim 20 arcsec ( 50 kpc ) away .
Previous long-slit spectroscopic observations missed most of these extended features due to a miss-aligned slit .
The ionized gas kinematics does not show any evidence for gas outflows on kpc scales despite the high QSO luminosity of L _ { \mathrm { bol } } > 10 ^ { 46 } ~ { } \mathrm { erg s } ^ { -1 } .
Based on the ionized gas distribution , kinematics and metallicity we discuss the origin of the ENLR with respect to its group environments including minor mergers , ram-pressure stripping or filamentary gas accretion as the most likely scenarios .
We conclude that PG 1307+085 is a normal elliptical host in terms of the scaling relations , but that the gas is most likely affected by the environment through gravity or ambient pressure .
It is possible that the ongoing interaction with the environment , mainly seen in the ionized gas , is also be responsible for driving sufficient gas to feed the black hole at the centre of the galaxy .