2MASX J05210136-2521450

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2MASX J05210136-2521450
Hubble image of 2MASX J05210136-2521450
Observation data
ConstellationLepus
Right ascension05h 21m 01.392s
Declination-25d 21m 45.36s
Redshift0.042750
Heliocentric radial velocity12,816 Km/s
Distance603 Mly (185 Mpc)
Apparent magnitude (V)15.4
Characteristics
TypePec; ULIRG, Sy2
Size75,000 ly
Apparent size (V)0.46 x 0.44 arcmin
Notable featuresGalaxy merger, luminous infrared galaxy
Other designations
PGC 17155, 2MASS J05210139-2521452, IRAS 05189-2524, AKARI J0521013-252146, MRSS 486-006230, NVSS J052101-252145, 1WGA J0521.0-2521, SWIFT J0521.0-2522, LEDA 17155

2MASX J05210136-2521450 is a type E[1] elliptical galaxy located in the constellation Lepus. It is located 603 million light-years away from the Solar System and has an approximate diameter of 75,000 light-years.[2]

A luminous galaxy[edit]

2MASX J05210136-2521450 is classified as an ultraluminous infrared galaxy (ULIRG),[3] which is caused by the end product of two interacting gas-rich spiral galaxies that merged together.[4] There are signs left by merging process, such as single bright nucleus and an outer structure consisting one-sided extension of the inner arms, with its tidal tail heading towards the opposite direction formed through material ripped from the galaxies by gravitational forces.[5]

It is one of the brightest local ULIRG in X-ray with a E = 2–10 keV continuum luminosity of ∼1043 erg s−1[6] This tend to vary overtime in which the E = 0.5–2 keV was relatively constant during the 2001-2002 observation done by XMM Newton and Chandra. But in 2006 study done by Suzaku shows it was a factor of ∼30 lower.[7] The galaxy has a power output above 10 times that of our sun,[8] emitting a tremendous amount of light at infrared wavelengths.[5]

Moreover, it is classified an optical Seyfert 2 galaxy,[7][9] presenting a hidden broadline region.[10] A study noticed there is ∼70% percent of the bolometric luminosity attributed to its active galactic nucleus,[11] thus making it a quasar. It is represented by its dust enshrouded stage[12] which is shed overtime by the nuclei.[12] There is a sign of high-velocity large-scale outflows detached in neutral, ionized and molecular gas phrases.[13]

An observation by XMM Newton and NuSTAR, shows evidence for a blueshifted Fe K absorption feature at E = 7.8 KeV which indicates there is an ultrafast outflow (UFO) with vout = 0.11 ± 0.01c.[7] A relative disk reflection in the broadband X-ray spectrum, shows a highly asymmetric board Fe Kα emission line that extends down to 3 KeV with a Compton scattering component above 10 KeV.[14]

There are Na i D emission in the system traces dusty filaments on the near side of an extended active galactic nucleus which has projected velocities up to 2000 km s−1. These filaments simultaneously obscure the stellar continuum, serving as complementary probe of the wind, in which they are the strongest in regions of low foreground obscuration.[15]

References[edit]

  1. ^ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-08.
  2. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-08.
  3. ^ Sanders, D. B.; Surace, J. A.; Ishida, C. M. (1999). "Ultraluminous Infrared Galaxies". In Barnes, J. E.; Sanders, D. B. (eds.). Galaxy Interactions at Low and High Redshift. Dordrecht: Springer Netherlands. pp. 289–294. doi:10.1007/978-94-011-4665-4_73. ISBN 978-94-011-4665-4.
  4. ^ Nandi, S; Das, M; Dwarakanath, K S. "Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations". academic.oup.com. Retrieved 2024-05-08.
  5. ^ a b information@eso.org. "A tale of galactic collisions". www.spacetelescope.org. Retrieved 2024-05-08.
  6. ^ Teng, Stacy H.; Veilleux, Sylvain; Anabuki, Naohisa; Dermer, Charles D.; Gallo, Luigi C.; Nakagawa, Takao; Reynolds, Christopher S.; Sanders, D. B.; Terashima, Yuichi; Wilson, Andrew S. (2009-01-09). "SUZAKUOBSERVATIONS OF LOCAL ULTRALUMINOUS INFRARED GALAXIES". The Astrophysical Journal. 691 (1): 261–276. Bibcode:2009ApJ...691..261T. doi:10.1088/0004-637x/691/1/261. ISSN 0004-637X.
  7. ^ a b c Smith, Robyn N.; Tombesi, Francesco; Veilleux, Sylvain; Lohfink, Anne M.; Luminari, Alfredo (2019-12-10). "Discovery of an X-Ray Quasar Wind Driving the Cold Gas Outflow in the Ultraluminous Infrared Galaxy IRAS F05189-2524". The Astrophysical Journal. 887 (1): 69. arXiv:1910.14583. Bibcode:2019ApJ...887...69S. doi:10.3847/1538-4357/ab4ef8. ISSN 0004-637X.
  8. ^ Murphy, Thomas Williams (2000). Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence (phd thesis). California Institute of Technology.
  9. ^ Veilleux, Sylvain; Kim, D.-C.; Sanders, D. B. (1999-09-01). "Optical Spectroscopy of the IRAS 1 Jy Sample of Ultraluminous Infrared Galaxies". The Astrophysical Journal. 522 (1): 113. arXiv:astro-ph/9904149. Bibcode:1999ApJ...522..113V. doi:10.1086/307634. ISSN 0004-637X.
  10. ^ Veilleux, Sylvain; Sanders, D. B.; Kim, D.-C. (September 1999). "New Results from a Near-Infrared Search for Hidden Broad-Line Regions in Ultraluminous Infrared Galaxies". The Astrophysical Journal. 522 (1): 139–156. arXiv:astro-ph/9904148. Bibcode:1999ApJ...522..139V. doi:10.1086/307635. ISSN 0004-637X.
  11. ^ Veilleux, S.; Rupke, D. S. N.; Kim, D.-C.; Genzel, R.; Sturm, E.; Lutz, D.; Contursi, A.; Schweitzer, M.; Tacconi, L. J.; Netzer, H.; Sternberg, A.; Mihos, J. C.; Baker, A. J.; Mazzarella, J. M.; Lord, S. (2009-05-21). "SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS". The Astrophysical Journal Supplement Series. 182 (2): 628–666. arXiv:0905.1577. Bibcode:2009ApJS..182..628V. doi:10.1088/0067-0049/182/2/628. ISSN 0067-0049.
  12. ^ a b Sanders, D. B.; Soifer, B. T.; Elias, J. H.; Madore, B. F.; Matthews, K.; Neugebauer, G.; Scoville, N. Z. (1988-02-01). "Ultraluminous Infrared Galaxies and the Origin of Quasars". The Astrophysical Journal. 325: 74. Bibcode:1988ApJ...325...74S. doi:10.1086/165983. ISSN 0004-637X.
  13. ^ González-Alfonso, E.; Fischer, J.; Spoon, H. W. W.; Stewart, K. P.; Ashby, M. L. N.; Veilleux, S.; Smith, H. A.; Sturm, E.; Farrah, D.; Falstad, N.; Meléndez, M.; Graciá-Carpio, J.; Janssen, A. W.; Lebouteiller, V. (February 2017). "Molecular Outflows in Local ULIRGs: Energetics from Multitransition OH Analysis". The Astrophysical Journal. 836 (1): 11. arXiv:1612.08181. Bibcode:2017ApJ...836...11G. doi:10.3847/1538-4357/836/1/11. ISSN 0004-637X.
  14. ^ Xu, Yanjun; Baloković, Mislav; Walton, Dominic J.; Harrison, Fiona A.; García, Javier A.; Koss, Michael J. (2017-02-28). "Evidence for Relativistic Disk Reflection in the Seyfert 1h Galaxy/ULIRG IRAS 05189–2524 Observed by NuSTAR and XMM-Newton". The Astrophysical Journal. 837 (1): 21. arXiv:1702.00073. Bibcode:2017ApJ...837...21X. doi:10.3847/1538-4357/aa5df4. ISSN 0004-637X.
  15. ^ Rupke, David S. N.; Veilleux, Sylvain (2015-03-12). "SPATIALLY EXTENDED NA i D RESONANT EMISSION AND ABSORPTION IN THE GALACTIC WIND OF THE NEARBY INFRARED-LUMINOUS QUASAR F05189-2524". The Astrophysical Journal. 801 (2): 126. arXiv:1411.3744. Bibcode:2015ApJ...801..126R. doi:10.1088/0004-637x/801/2/126. ISSN 1538-4357.
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