IRAS F11119+3257 | |
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![]() The quasar IRAS F11119+3257 | |
Observation data (J2000 epoch) | |
Constellation | Ursa Major |
Right ascension | 11h 14m 38.91s |
Declination | +32d 41m 33.34s |
Redshift | 0.187580 |
Heliocentric radial velocity | 56,235 km/s |
Distance | 2.519 Gly (772.3 Mpc) |
Apparent magnitude (V) | 0.54 |
Apparent magnitude (B) | 0.43 |
Surface brightness | 19.2 |
Characteristics | |
Type | Sbrst; ULIRG, Sy1 |
Apparent size (V) | 0.13' x 0.10' |
Notable features | Luminous infrared galaxy |
Other designations | |
B2 1111+32, PGC 34264, F2M J111438.91+324133.29, NVSS J111438+324133, FIRST J111438.9+324133, IVS B1111+329 |
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 [1] and is considered an ultraluminous infrared galaxy (ULIRG). [2]
The nucleus of IRAS F11119+3257 is active. It has been classified as a narrow-line Seyfert 1 galaxy [3] 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. [4] 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. [5]
The emission in IRAS F11119+3257, is dominated by its active galactic nucleus (AGN) component. [6] Researchers found that there is direct evidence of a quasar accretion disk driving a massive (>100 M ⊙ yr-1) molecular outflow. [7] 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). [7]
With a supermassive black hole mass of Mbh ≈ 2 × 107 M⊙ calibrated for a sample of similar ULIRG sources, [8] the bolometric luminosity for IRAS F11119+3257 is Lb = 5LEdd, where LEdd 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. [9] 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. [10] 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. [9] [11]
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) [12] 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. [13] 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. [7]
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. [7]