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IRAS F11119+3257

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IRAS F11119+3257
The quasar IRAS F11119+3257
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension11h 14m 38.91s
Declination+32d 41m 33.34s
Redshift0.187580
Heliocentric radial velocity56,235 km/s
Distance2.519 Gly (772.3 Mpc)
Apparent magnitude (V)0.54
Apparent magnitude (B)0.43
Surface brightness19.2
Characteristics
TypeSbrst; ULIRG, Sy1
Apparent size (V)0.13' x 0.10'
Notable featuresLuminous 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]

Characteristics[edit]

Artist's impression of strong galactic wind emitting out from supermassive black hole similar to IRAS F11119+3257

The nucleus of IRAS F11119+3257 is found out to be 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] Not to mention, 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]

Furthermore, 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 found to be 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-1 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]

References[edit]

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-21.
  2. ^ Kim, D. -C.; Sanders, D. B. (1998-11-01). "The IRAS 1 Jy Survey of Ultraluminous Infrared Galaxies. I. The Sample and Luminosity Function". The Astrophysical Journal Supplement Series. 119 (1): 41–58. arXiv:astro-ph/9806148. Bibcode:1998ApJS..119...41K. doi:10.1086/313148. ISSN 0067-0049.
  3. ^ Véron-Cetty, M. -P.; Véron, P. (2006-08-01). "A catalogue of quasars and active nuclei: 12th edition". Astronomy and Astrophysics. 455 (2): 773–777. Bibcode:2006A&A...455..773V. doi:10.1051/0004-6361:20065177. ISSN 0004-6361.
  4. ^ Lanzuisi, Giorgio (2020-10-01). "Physics and Energetics of the Ultra Fast Outflow in IRAS F11119+3257". XMM-Newton Proposal: 43. Bibcode:2020xmm..prop...43L.
  5. ^ Pan, Xiang; Zhou, Hongyan; Liu, Wenjuan; Liu, Bo; Ji, Tuo; Shi, Xiheng; Zhang, Shaohua; Jiang, Peng; Wang, Huiyuan; Hao, Lei (2019-10-01). "Discovery of Metastable He I* λ10830 Mini-broad Absorption Lines and Very Narrow Paschen α Emission Lines in the ULIRG Quasar IRAS F11119+3257". The Astrophysical Journal. 883 (2): 173. arXiv:1910.05068. Bibcode:2019ApJ...883..173P. doi:10.3847/1538-4357/ab40b5. ISSN 0004-637X.
  6. ^ Veilleux, S.; Meléndez, M.; Sturm, E.; Gracia-Carpio, J.; Fischer, J.; González-Alfonso, E.; Contursi, A.; Lutz, D.; Poglitsch, A.; Davies, R.; Genzel, R.; Tacconi, L.; de Jong, J. A.; Sternberg, A.; Netzer, H. (2013-10-01). "Fast Molecular Outflows in Luminous Galaxy Mergers: Evidence for Quasar Feedback from Herschel". The Astrophysical Journal. 776 (1): 27. arXiv:1308.3139. Bibcode:2013ApJ...776...27V. doi:10.1088/0004-637X/776/1/27. ISSN 0004-637X.
  7. ^ a b c d Veilleux, S.; Bolatto, A.; Tombesi, F.; Meléndez, M.; Sturm, E.; González-Alfonso, E.; Fischer, J.; Rupke, D. S. N. (2017-07-01). "Quasar Feedback in the Ultraluminous Infrared Galaxy F11119+3257: Connecting the Accretion Disk Wind with the Large-scale Molecular Outflow". The Astrophysical Journal. 843 (1): 18. arXiv:1706.00443. Bibcode:2017ApJ...843...18V. doi:10.3847/1538-4357/aa767d. ISSN 0004-637X.
  8. ^ Kawakatu, Nozomu; Imanishi, Masatoshi; Nagao, Tohru (2007-06-01). "Anticorrelation between the Mass of a Supermassive Black Hole and the Mass Accretion Rate in Type 1 Ultraluminous Infrared Galaxies and Nearby QSOs". The Astrophysical Journal. 661 (2): 660. arXiv:astro-ph/0702552. Bibcode:2007ApJ...661..660K. doi:10.1086/516563. ISSN 0004-637X.
  9. ^ a b Tombesi, F.; Meléndez, M.; Veilleux, S.; Reeves, J. N.; González-Alfonso, E.; Reynolds, C. S. (2015-03-01). "Wind from the black-hole accretion disk driving a molecular outflow in an active galaxy". Nature. 519 (7544): 436–438. arXiv:1501.07664. Bibcode:2015Natur.519..436T. doi:10.1038/nature14261. hdl:2108/209839. ISSN 0028-0836. PMID 25810204.
  10. ^ Yang, Jun; Paragi, Zsolt; An, Tao; A Baan, Willem; Mohan, Prashanth; Liu, Xiang. "A two-sided but significantly beamed jet in the supercritical accretion quasar IRAS F11119+3257". academic.oup.com. Retrieved 2024-05-21.
  11. ^ Tombesi, F.; Veilleux, S.; Meléndez, M.; Lohfink, A.; Reeves, J. N.; Piconcelli, E.; Fiore, F.; Feruglio, C. (2017-12-01). "NuSTAR View of the Black Hole Wind in the Galaxy Merger IRAS F11119+3257". The Astrophysical Journal. 850 (2): 151. arXiv:1710.07485. Bibcode:2017ApJ...850..151T. doi:10.3847/1538-4357/aa9579. ISSN 0004-637X.
  12. ^ Colla, G.; Fanti, C.; Ficarra, A.; Formiggini, L.; Gandolfi, E.; Grueff, G.; Lari, C.; Padrielli, L.; Roffi, G.; Tomasi, P.; Vigotti, M. (1970-03-01). "A catalogue of 3235 radio sources at 408 MHz". Astronomy and Astrophysics Supplement Series. 1 (3): 281. Bibcode:1970A&AS....1..281C. ISSN 0365-0138.
  13. ^ Berton, M.; Congiu, E.; Järvelä, E.; Antonucci, R.; Kharb, P.; Lister, M. L.; Tarchi, A.; Caccianiga, A.; Chen, S.; Foschini, L.; Lähteenmäki, A.; Richards, J. L.; Ciroi, S.; Cracco, V.; Frezzato, M. (2018-06-01). "Radio-emitting narrow-line Seyfert 1 galaxies in the JVLA perspective". Astronomy and Astrophysics. 614: A87. arXiv:1801.03519. Bibcode:2018A&A...614A..87B. doi:10.1051/0004-6361/201832612. ISSN 0004-6361.
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