The galaxy shows a "warm" far-IR color similar to luminous quasars. It is suggested much of the far-IR emission is emitted from dust heated by the central ultraviolet (UV) continuum source.[9][10] The rest frame of UV/optical spectrum of the nucleus shows a type 2 spectrum with strong, narrow emission lines covering a range of ionizations. This implies photoionization by a strong UV nonthermal continuum.[11][12]
A study conducted in 2007, proves IRAS 09104+4109 as the first "changing-look quasar". The X-ray emission in the EPIC band is dominated by the intra-cluster mediumthermal emission, which the quasar contributes ~35% of the total flux in the 2–10 keV band.[16]
Further studies in 2012, showed that IRAS 09104+4109 is a rare example of a dust enshrouded quasar, associated with a double-lobed radio source at the position angle of =333°.[17] However, the steep radio spectral index and misalignment between the jets and ionized optical emission suggested that the orientation of the quasar in IRAS 09104+4109 had changed. Proving this hypothesis, researchers used a combination of new, multiband Giant Metrewave Radio Telescopeobservations and archival radio data and confirmed that the jets in IRAS 09104+ 4109, estimated to 20-160 Myr, are no longer actively fed by energetic particles.[13] This results suggested that the realignment of the quasar, the cessation of jet activity and the onset of rapid star formation in IRAS 09104+4109, may have been caused by a gas-rich galaxy merger.[18]
A Northern Extended Millimeter Array (NOEMA) found traces of carbon oxide (2–1) in the z=0.4418 cluster-central IRAS 09104+4109, which ~4.5x1010 M sol of molecular gas is found, in and around the galaxy. The gas is located in a series of clumps extending along the old radio jets and lobes. It has a relatively low velocity dispersion of (336 [+39,-35] km/s FWHM) and shows no velocity gradients indicative of outflow or infall. Roughly, half its gas is located in a central clump on the northeast side of the galaxy overlapping a bright ionized gas filament and a spur of excess X-ray emission, suggesting that this is a location of rapid cooling.[19]
The molecular gas is extended usually to a ~55 kpc radius. This gas is comparable to the scale of the filamentary nebula in the Perseus cluster, falling within the thermal instability radius of the intracluster medium (ICM), within ~70 kpc. Continuum measurements at 159.9 GHz from NOEMA and 850 micron from the JCMT SCUBA-2 show excess far infrared emission, which was interpreted as free-free emission arising from ongoing starburst. These observations suggest that the ICM cooling is not strongly affected by its buried quasar which can build gas reservoirs to fuel reorientation and quasar-activity of its central AGN.[19]
