ESO 286-19

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ESO 286-19
Hubble Interacting Galaxy ESO 286-19 (2008-04-24).jpg
HST image of ESO 286-19
Observation data (J2000 epoch)
Constellation Microscopium
Right ascension 20h 58m 26.80s
Declination −42° 39′ 00.43″
Redshift 0.042996
Heliocentric radial velocity 12,890 km/s
Distance 609 Mly (186.72 Mpc)
Apparent magnitude  (V)0.14
Apparent magnitude  (B)0.18
Characteristics
Type HII;ULRG, LINER
Apparent size  (V)1.05' x 0.40'
Notable features luminous infrared galaxy
Other designations
ESO 286-IG019, IRAS 20551-4250, PGC 65817, AM 2055-425

ESO 286-19 known as IRAS 20551-4250, is a galaxy merger located in the constellation of Microscopium. It is located 609 million light years away from Earth. [1] It is an ultraluminous infrared galaxy.

Characteristics

ESO 286-19 is a late-stager merger. [2] [3] A product of two colliding disk galaxies, it is found distorted, with a long tidal tail that is extending to the right from its main body while the shorter tidal tail is curving towards the left direction. [4] It has knotted structures. There is a distribution of cold molecular gas from the galaxy's southeast region. [5]

A single nucleus has been detected in ESO 286–19 by both XMM Newton and Chandra X-ray Observatory although undetected by NuSTAR. According to observations made by Chandra, the soft X-ray emission of the galaxy is elongated while having a point-like hard X-ray emission. [2] However, its polarized flux is faint. [6]

ESO 286-19 is also an extremely bright galaxy with a luminosity of LIR ~ 1012 LΘ. [7] It also experiences a starburst. [8] A spectroscopic and photometric analysis found the galaxy has an old stellar population mass of 3 x 1011 MΘ. It also has much young, recently formed stars of 8 x 109 MΘ contributing to ~ 2 of the stellar mass. The galaxy also has molecular hydrogen with a mass of 4 x 1010 MΘ. [9]

According to results from Cycle 2 observations conducted by Atacama Large Millimeter Array, ESO 286-19 harbors an obscured active galactic nucleus. The nucleus shows HCN/HCO+/HNC J = 3-2 emission lines that are found vibrationally excited with a high energy level of v 2 = 1. Due to a likely line opacity correction, the lines are found to have an excitation temperature and flux ratio amidst v 2 = 1f and v = 0. [10] Additionally, a broad emission line component was found from a CO J = 3-2 emission line with a measurement of full width at half maximum (FWHM) ~ 500 km s−1. This finding suggested it was caused by molecular outflow in the galaxy with a mass of Moutf ~ 5.8 x 106 MΘ and a kinetic power of Poutf ~ 1%. [7] Based on the outflow, it has an X-ray luminosity of L2-10keV = 2.1 x 1041 ergs −1. [11]

References

  1. ↑ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-09-26.
  2. 1 2 Ricci, C; Privon, GC; Pfeifle, RW; Armus, L; Iwasawa, K (2021). "A hard X-ray view of luminous and ultra-luminous infrared galaxies in GOALS – I. AGN obscuration along the merger sequence". Oxford Academic. 506 (4): 5935–5950. arXiv: 2107.10864 . doi: 10.1093/mnras/stab2052 .
  3. ↑ Rich, J. A.; Kewley, L. J.; Dopita, M. A. (2015-12-07). "Galaxy Mergers Drive Shocks: An Integral Field Study of Goals Galaxies". The Astrophysical Journal Supplement Series. 221 (2): 28. arXiv: 1509.08468 . Bibcode:2015ApJS..221...28R. doi:10.1088/0067-0049/221/2/28. ISSN   1538-4365.
  4. ↑ information@eso.org. "ESO 286-19". www.esahubble.org. Retrieved 2024-09-26.
  5. ↑ Ueda, Junko; Iono, Daisuke; Yun, Min S.; Crocker, Alison F.; Narayanan, Desika; Komugi, Shinya; Espada, Daniel; Hatsukade, Bunyo; Kaneko, Hiroyuki; Matsuda, Yuichi; Tamura, Yoichi; Wilner, David J.; Kawabe, Ryohei; Pan, Hsi-An (2014-08-12). "Cold Molecular Gas in Merger Remnants. I. Formation of Molecular Gas Disks". The Astrophysical Journal Supplement Series. 214 (1): 1. arXiv: 1407.6873 . Bibcode:2014ApJS..214....1U. doi:10.1088/0067-0049/214/1/1. ISSN   1538-4365.
  6. ↑ Pernechele, C.; Berta, S.; Marconi, A.; Bonoli, C.; Bressan, A.; Franceschini, A.; Fritz, J.; Giro, E. (2003-01-01). "Spectropolarimetric search for hidden active galactic nuclei in four southern ultraluminous infrared galaxies". Monthly Notices of the Royal Astronomical Society. 338 (1): L13 –L17. arXiv: astro-ph/0210690 . Bibcode:2003MNRAS.338L..13P. doi: 10.1046/j.1365-8711.2003.06112.x . ISSN   0035-8711.
  7. 1 2 Imanishi 今西, Masatoshi 昌俊; Nakanishi 中西, Kouichiro 康一郎; Izumi 泉, Takuma 拓磨 (2017-10-26). "ALMA Multiple-transition Molecular Line Observations of the Ultraluminous Infrared Galaxy IRAS 20551–4250: Different HCN, HCO+, and HNC Excitation, and Implications for Infrared Radiative Pumping". The Astrophysical Journal. 849 (1): 29. arXiv: 1708.08073 . Bibcode:2017ApJ...849...29I. doi: 10.3847/1538-4357/aa7ff9 . ISSN   0004-637X.
  8. ↑ Risaliti, G.; Maiolino, R.; Marconi, A.; Sani, E.; Berta, S.; Braito, V.; Ceca, R. Della; Franceschini, A.; Salvati, M. (January 2006). "Unveiling the nature of Ultraluminous Infrared Galaxies with 3-4 μm spectroscopy". Monthly Notices of the Royal Astronomical Society. 365 (1): 303–320. doi: 10.1111/j.1365-2966.2005.09715.x . ISSN   0035-8711.
  9. ↑ Johansson, L. (1991). "The extremely luminous galaxy merger ESO 286-IG19". Astronomy and Astrophysics. 241: 389. Bibcode:1991A&A...241..389J . Retrieved 2024-09-26.
  10. ↑ Imanishi, Masatoshi; Nakanishi, Kouichiro; Izumi, Takuma (2016-07-01). "ALMA Investigation of Vibrationally Excited HCN/HCO+/HNC Emission Lines in the AGN-Hosting Ultraluminous Infrared Galaxy IRAS 20551-4250". The Astrophysical Journal. 825 (1): 44. arXiv: 1605.00644 . Bibcode:2016ApJ...825...44I. doi: 10.3847/0004-637X/825/1/44 . ISSN   0004-637X.
  11. ↑ Laha, Sibasish; Guainazzi, Matteo; Piconcelli, Enrico; Gandhi, Poshak; Ricci, Claudio; Ghosh, Ritesh; Markowitz, Alex G.; Bagchi, Joydeep (2018-11-13). "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.
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