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IRAS 10565+2448

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IRAS 10565+2448
HST image of IRAS 10565+2448
Observation data (J2000 epoch)
ConstellationLeo
Right ascension10h 59m 18.13s
Declination+24° 32′ 34.54″
Redshift0.043100
Heliocentric 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

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  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-09-27.
  2. ^ a b Su, Renzhi; Mahony, Elizabeth K; Gu, Minfeng; Sadler, Elaine M; Curran, S J; Allison, James R; Yoon, Hyein; Aditya, J N H S; Chandola, Yogesh; Chen, Yongjun; Moss, Vanessa A; Wu, Zhongzu; Shao, Xi; Liu, Xiang; Glowacki, Marcin (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. arXiv:2302.00943. doi:10.1093/mnras/stad370. ISSN 0035-8711.
  3. ^ information@eso.org. "IRAS F10565+2448". www.esahubble.org. Retrieved 2024-09-27.
  4. ^ a b 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. arXiv:2402.10786. Bibcode:2024ApJ...966...61D. doi:10.3847/1538-4357/ad2c93. ISSN 0004-637X.
  5. ^ Ricci, C.; Bauer, F. E.; Treister, E.; Schawinski, K.; Privon, G. C.; Blecha, L.; Arevalo, P.; Armus, L.; Harrison, F.; Ho, L. C.; Iwasawa, K.; Sanders, D. B.; Stern, D. (2017-01-23). "Growing supermassive black holes in the late stages of galaxy mergers are heavily obscured". Monthly Notices of the Royal Astronomical Society: stx173. arXiv:1701.04825. 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. arXiv:1809.07906. Bibcode:2018ApJ...868...10L. doi:10.3847/1538-4357/aae390. ISSN 0004-637X.
  7. ^ "Scoville et al., NICMOS Imaging of IR-Luminous Galaxies". iopscience.iop.org. doi:10.1086/301248. Retrieved 2024-09-27.
  8. ^ Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. (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. arXiv:2107.12529. 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.; Stierwalt, S.; Barcos-Muñoz, L. (2015-02-01). "Radio continuum properties of luminous infrared galaxies - Identifying the presence of an AGN in the radio". Astronomy & Astrophysics. 574: A4. arXiv:1408.4177. Bibcode:2015A&A...574A...4V. doi:10.1051/0004-6361/201424125. ISSN 0004-6361.
  10. ^ Downes, D.; Solomon, P.M. (1998). "Rotating Nuclear Rings and Extreme Starbursts in Ultraluminous Galaxies". The Astrophysical Journal. 507 (2): 615–654. arXiv:astro-ph/9806377. Bibcode:1998ApJ...507..615D. doi:10.1086/306339.
  11. ^ "Massive molecular outflows and evidence for AGN feedback from CO observations | Astronomy & Astrophysics (A&A)". www.aanda.org. Retrieved 2024-09-27.
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