Astronomy:IRAS 10565+2448

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IRAS 10565+2448
HST image of IRAS 10565+2448
Observation data (J2000 epoch)
ConstellationLeo
Right ascension 10h 59m 18.13s
Declination+24° 32′ 34.54″
Redshift0.043100
Helio radial velocity12,921 km/s
Distance625 Mly (191.62 Mpc)
Apparent magnitude (B)15.7
Characteristics
TypeLINER; ULIRG, HII
Apparent size (V)0.4' x 0.3'
Notable featuresluminous infrared galaxy
Other designations
IRAS F10565+2448, 2XMM J105918.1+243234, PGC 33083, NVSS J105918+243235, LEDA 1709876

IRAS 10565+2448 known as IRAS F10565+2448, is a galaxy merger located in the constellation of Leo. It is located at a distance of 625 million light years from Earth. It is classified as an ultraluminous infrared galaxy[1] with an infrared luminosity of 1.2 x 1012 LΘ. It has a star formation rate of 131.8 MΘ yr−1.[2]

IRAS 10565+2448 has a disturbed morphology. The large galaxy in the system shows dust lanes running through its main body while the smaller galaxy (the westernmost object), has a curved tidal tail pulled downwards from the object.[3] A third galaxy is possibly shown as secondary smaller nucleus located northwest from the primary nucleus in the large galaxy.[4] It is also a late-stage merger as both east and west nuclei components in the system have a projected separation of 6.7 kiloparsecs.[5] It has an obscured X-ray emission with a luminosity of both LSX = 1.21 x 1041 erg s−1 and LHX = 1.6 x 1041 erg s−1. The source appears as Compton-thin obscurer with an absorption column density of 0.05+0.07-0.04 x 1022 cm−2.[6]

The large galaxy in the IRAS 10565+2448 is found to be active. It is categorized as a H II galaxy and a starburst galaxy.[4] It is more luminous when compared to its smaller companion galaxy.[7] It contains a superficial and broad blueshifted HI absorption interpreted as molecular outflows with a mass rate of 140 MΘ yr−1 suggesting it is driven by a radio jet.[2] The large galaxy also shows detections of dust continuum, J = 4-3 ground rotational transition of carbon monoxide (CO) and atomic carbon.[8] It has a compact radio source appearing structured at 8.44 GHz[9] with a rotating CO ring found nearly-face on but lesser inside an outer disk beyond the galaxy's nuclear ring.[10]

The smaller galaxy contains a source of CO(1–0) emission. It has blue and redshifted CO(1–0) wings with an approximate size of 2.15 ± 0.32 kiloparsecs and 2.22 ± 0.30 kiloparsecs based on a circular Gaussian fit. However, the emission from the CO(1–0) narrow core is more condensed than its wings. There is also proof of a plume of CO(1–0) stretching southwest at blueshifted velocities of -150 km−1 and systematic velocity.[11]

References

  1. ↑ "Your NED Search Results". https://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Obj_id&objid=106194&objname=1&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1. 
  2. ↑ 2.0 2.1 Su, Renzhi; Mahony, Elizabeth K; Gu, Minfeng; Sadler, Elaine M; Curran, S J; Allison, James R; Yoon, Hyein; Aditya, J N H S et al. (2023-02-03). "Does a radio jet drive the massive multiphase outflow in the ultra-luminous infrared galaxy IRAS 10565 + 2448?". Monthly Notices of the Royal Astronomical Society 520 (4): 5712–5723. doi:10.1093/mnras/stad370. ISSN 0035-8711. 
  3. ↑ information@eso.org. "IRAS F10565+2448". https://esahubble.org/images/heic0810ch/. 
  4. ↑ 4.0 4.1 Dey, Subhrata; Goyal, Arti; Małek, Katarzyna; Díaz-Santos, Tanio (April 2024). "Radio-only and Radio-to-far-ultraviolet Spectral Energy Distribution Modeling of 14 ULIRGs: Insights into the Global Properties of Infrared Bright Galaxies". The Astrophysical Journal 966 (1): 61. doi:10.3847/1538-4357/ad2c93. ISSN 0004-637X. Bibcode: 2024ApJ...966...61D. 
  5. ↑ Ricci, C.; Bauer, F. E.; Treister, E.; Schawinski, K.; Privon, G. C.; Blecha, L.; Arevalo, P.; Armus, L. et al. (2017-01-23). "Growing supermassive black holes in the late stages of galaxy mergers are heavily obscured". Monthly Notices of the Royal Astronomical Society. doi:10.1093/mnras/stx173. ISSN 0035-8711. 
  6. ↑ Laha, Sibasish; Guainazzi, Matteo; Piconcelli, Enrico; Gandhi, Poshak; Ricci, Claudio; Ghosh, Ritesh; Markowitz, Alex G.; Bagchi, Joydeep (November 2018). "A Study of X-Ray Emission of Galaxies Hosting Molecular Outflows (MOX Sample)". The Astrophysical Journal 868 (1): 10. doi:10.3847/1538-4357/aae390. ISSN 0004-637X. Bibcode: 2018ApJ...868...10L. 
  7. ↑ Scoville et al., NICMOS Imaging of IR-Luminous Galaxies. doi:10.1086/301248. https://iopscience.iop.org/article/10.1086/301248/fulltext/. Retrieved 2024-09-27. 
  8. ↑ Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran et al. (2021-11-12). "An ACA Survey of [C i] 3 P 1−3 P 0, CO J = 4 − 3, and Dust Continuum in Nearby U/LIRGs". The Astrophysical Journal Supplement Series 257 (2): 28. doi:10.3847/1538-4365/ac16df. ISSN 0067-0049. 
  9. ↑ Vardoulaki, E.; Charmandaris, V.; Murphy, E. J.; Diaz-Santos, T.; Armus, L.; Evans, A. S.; Mazzarella, J. M.; Privon, G. C. et al. (2015-02-01). "Radio continuum properties of luminous infrared galaxies - Identifying the presence of an AGN in the radio". Astronomy & Astrophysics 574: A4. doi:10.1051/0004-6361/201424125. ISSN 0004-6361. Bibcode: 2015A&A...574A...4V. https://www.aanda.org/articles/aa/full_html/2015/02/aa24125-14/aa24125-14.html#S5. 
  10. ↑ Downes, D.; Solomon, P.M. (1998). "Rotating Nuclear Rings and Extreme Starbursts in Ultraluminous Galaxies". The Astrophysical Journal 507 (2): 615–654. doi:10.1086/306339. Bibcode: 1998ApJ...507..615D. https://iopscience.iop.org/article/10.1086/306339/fulltext/. 
  11. ↑ "Massive molecular outflows and evidence for AGN feedback from CO observations | Astronomy & Astrophysics (A&A)". https://www.aanda.org/articles/aa/olm/2014/02/aa22464-13/aa22464-13.html. 



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