# IRAS F11119+3257

IRAS F11119+3257 or simply as F11119+3257, is a galaxy located in constellation Ursa Major. With a redshift of 0.187580, it has a light travel time distance of 2.5 billion light-years and is considered an ultraluminous infrared galaxy (ULIRG).

## Characteristics

The nucleus of IRAS F11119+3257 is active. It has been classified as a narrow-line Seyfert 1 galaxy and has a post-merger morphology. It is also a type-1 quasar, emitting out (LX 10^44 erg/s at z=0.189) with a persistent ultra-fast outflow at v 0.25c, observed with both NuSTAR and Suzaku. IRAS F11119+3257 is said to be the first system which is possible to connect nuclear outflow with a galaxy-scale molecular outflow, observed in hydroxide (OH) and carbon monoxide (CO) transitions. The high-ionization emission lines ([O III], [Ne III], and [Ne V]) are dominated by blueshifted components at similar speeds to the mini-BAL QSOs.
The emission in IRAS F11119+3257, is dominated by its active galactic nucleus (AGN) component. Researchers found that there is direct evidence of a quasar accretion disk driving a massive (>100 M ⊙ yr-1) molecular outflow. They saw that the energetics of the accretion disk wind and molecular outflow are consistent with the predictions of quasar feedback models where the molecular outflow is driven by a hot energy-conserving bubble, inflated by its inner quasar accretion disk wind, but the conclusion is uncertain. However, they were able to confirm the presence of the molecular outflow in IRAS F11119+3257, based on the detection of ~±1000 km/s blue and redshifted wings in the CO(1–0) emission line profile derived from deep ALMA observations obtained in the compact array configuration (~2.8″ resolution).
With a supermassive black hole mass of M$_{bh}$ ≈ 2 × 107 M$_⊙$ calibrated for a sample of similar ULIRG sources, the bolometric luminosity for IRAS F11119+3257 is L$_b$ = 5L$_{Edd}$, where L$_{Edd}$ is the Eddington luminosity, suggesting that the active galactic nucleus is responsible for about 80 per cent of its emission, with a quasar-like luminosity of 1.5 × 1046 ergs per second. From the correlation relation between infrared and radio luminosities for starburst galaxies, the AGN component in IRAS F11119+3257 is found to exceed the starburst contribution. Apart from the molecular outflows, the galaxy hosts a wide-aperture energetic radiation-driven X-ray emitting winds, suggesting a likely energy conserving quasar-mode feedback.
Researchers also found that IRAS F11119+3257 has a relatively bright radio counterpart. The early survey of the Bologna Northern Cross Radio Telescope (BNCRT) at 408 MHz, conducted by Colla et al. (1970) found there is a half-Jy radio counterpart in the galaxy. Later, it was observed by more radio telescopes at multiple radio frequencies, whom they found IRAS F11119+3257 indicates a compact emission structure. Moreover, its radio spectrum between 0.15 and 96 GHz shows a peak at 0.53 ± 0.06 GHz and a steep slope of ν−1.31±0.02 in the optically thin part.
From the EVN Observation, at 1.66 and 4.93 GHz, IRAS F11119+3257 displays a two-sided jet with a projected separation of about 200 parsec, which has an intrinsic speed of ≥0.57c. This is higher than that observed in the X-ray winds.