Astronomy:UGC 9799

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UGC 9799
The radio galaxy UGC 9799.
Observation data (J2000 epoch)
ConstellationSerpens
Right ascension 15h 16m 44.50s[1]
Declination+07° 01′ 18.07″[1]
Redshift0.034547[1]
Helio radial velocity10357 km/s[1]
Distance543 Mly
Group or clusterAbell 2052
Apparent magnitude (V)14.17
Characteristics
TypecD; E, Sy2, LEG
Size~331,500 ly (101.65 kpc) (estimated)[1]
Other designations
3C 317, 4C +07.40, CoNFIG 214, CGCG 049-090, CTA 067, DA 379, GIN 419, LHE 388, MCG +01-39-012, PKS 1514+07, PGC 54526[1]

UGC 9799 also known as 3C 317, is a radio galaxy located in the constellation of Serpens. The redshift of the galaxy is (z) 0.034[1] estimating a light-travel time distance of 543 million light-years[2] and it was first discovered as an astronomical radio source by astronomers in 1959.[3] It is classified as a type-cD galaxy[4][5] and is the brightest cluster galaxy of the cluster Abell 2052.[6]

Description

UGC 9799 is categorized as an elliptical galaxy with a slightly elongated appearance but its nucleus is unresolved. There is an ultraviolet filament present in the galaxy four kiloparsecs to the south from the nucleus region. This evidence suggests star formation activity is triggered by a galaxy merger of an nearby satellite galaxy.[7][6] Imaging made by the Hubble Space Telescope (HST), found the core isophotes seem to be extending towards a dark band feature suggested to be a diffused dust lane.[8] A secondary nucleus is likely present in UGC 9799.[9]

The galaxy contains a radio source that has a steep radio spectrum. When observed with the Very Large Array (VLA), the structure is mainly irregular and its spectra index is mainly 0.8 below the frequencies of 200 MHz but gets much steeper upon reaching more than 750 MHz.[10] A compact radio core is found at the center of the source; however there are no signs that the core is significantly variable. There is a large bipolar structure surrounding the core region, which in turn is enveloped inside a halo. There is also a loop structure linking together with its northern radio lobe and a plume feature.[11] New observations at 4.9 GHz found the radio morphology is classified as S-shaped with two short jet features that have a bending angle of 5 milliarcseconds from the radio peak. At 8.3 GHz, these jets are shown to have an alignment to around -32°.[12]

Studies published in 1995 and in 2017 have found the presence of globular clusters inside UGC 9799 based on imaging.[13][14] Further evidence also found there are 46,000 clusters in total, making these the largest amount found so far.[15] A supermassive black hole mass of 108 Mʘ has been estimated for the galaxy.[16]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "NED Search results for UGC 9799". https://ned.ipac.caltech.edu/byname?objname=UGC+9799&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ "Elliptical Galaxy UGC 9799 - Galaxy Cluster Abell 2052". https://www.kopernik.org/images/archive/u9799.htm. 
  3. ↑ Goldstein, Samuel J. (April 1962). "Observations of sixty discrete sources at 1423 MC" (in en). The Astronomical Journal 67: 171. doi:10.1086/108688. ISSN 0004-6256. Bibcode: 1962AJ.....67..171G. https://articles.adsabs.harvard.edu/pdf/1962AJ.....67..171G. 
  4. ↑ Zirbel, Esther L.; Baum, Stefi A. (Feb 1998). "The Ultraviolet Continuum Emission of Radio Galaxies. I. Description of Sources from the Hubble Space Telescope Archives" (in en). The Astrophysical Journal Supplement Series 114 (2): 177–235. doi:10.1086/313070. ISSN 0067-0049. Bibcode: 1998ApJS..114..177Z. https://iopscience.iop.org/article/10.1086/313070/pdf. 
  5. ↑ Blanton, Elizabeth L.; Sarazin, Craig L.; McNamara, Brian R.; Wise, Michael W. (2001-09-01). "[ITALChandra[/ITAL] Observation of the Radio Source/X-Ray Gas Interaction in the Cooling Flow Cluster Abell 2052"]. The Astrophysical Journal 558 (1): L15–L18. doi:10.1086/323269. ISSN 0004-637X. https://iopscience.iop.org/article/10.1086/323269/pdf. 
  6. ↑ 6.0 6.1 Martel, André R.; Sparks, William B.; Allen, Mark G.; Koekemoer, Anton M.; Baum, Stefi A. (March 2002). "Discovery of a Star Formation Region in Abell 2052" (in en). The Astronomical Journal 123 (3): 1357–1363. doi:10.1086/338848. ISSN 0004-6256. Bibcode: 2002AJ....123.1357M. https://iopscience.iop.org/article/10.1086/338848/pdf. 
  7. ↑ Floyd, David J. E.; Axon, David; Baum, Stefi; Capetti, Alessandro; Chiaberge, Marco; Macchetto, Duccio; Madrid, Juan; Miley, George et al. (July 2008). "Hubble Space Telescope Near-infrared Snapshot Survey of 3CR Radio Source Counterparts. II. An Atlas and Inventory of the Host Galaxies, Mergers, and Companions" (in en). The Astrophysical Journal Supplement Series 177 (1): 148–173. doi:10.1086/587622. ISSN 0067-0049. Bibcode: 2008ApJS..177..148F. 
  8. ↑ Martel, André R.; Baum, Stefi A.; Sparks, William B.; Wyckoff, Eric; Biretta, John A.; Golombek, Daniel; Macchetto, Ferdinando D.; de Koff, Sigrid et al. (May 1999). "[ITALHUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL] Snapshot Survey of 3CR Radio Source Counterparts. III. Radio Galaxies with [FORMULA][F]z<0.1[/F][/FORMULA]"]. The Astrophysical Journal Supplement Series 122 (1): 81–108. doi:10.1086/313205. ISSN 0067-0049. https://iopscience.iop.org/article/10.1086/313205/pdf. 
  9. ↑ Malumuth, E. M.; Kriss, G. A.; Borne, K. D. (Sep 1985). "Velocity Dispersion Profiles of the cD Galaxies A2052 and A2589" (in en). Bulletin of the American Astronomical Society 17: 866. Bibcode: 1985BAAS...17..866M. https://articles.adsabs.harvard.edu/pdf/1985BAAS...17..866M. 
  10. ↑ Roland, J.; Hanisch, R. J.; Veron, P.; Fomalont, E. (July 1985). "WSRT and VLA observations of very steep spectrum radio galaxies in clusters." (in en). Astronomy and Astrophysics 148: 323–334. ISSN 0004-6361. Bibcode: 1985A&A...148..323R. https://articles.adsabs.harvard.edu/pdf/1985A%26A...148..323R. 
  11. ↑ Zhao, Jun-Hui; Sumi, Dean M.; Burns, J. O.; Duric, Nebojsa (Oct 1993). "3C 317: an Amorphous Radio Source in the Cooling Flow Cluster Abell 2052" (in en). The Astrophysical Journal 416: 51. doi:10.1086/173214. ISSN 0004-637X. Bibcode: 1993ApJ...416...51Z. https://articles.adsabs.harvard.edu/full/1993ApJ...416...51Z. 
  12. ↑ Venturi, T.; Dallacasa, D.; Stefanachi, F. (2004-08-01). "Radio galaxies in cooling core clusters. Renewed activity in the nucleus of 3C 317?" (in en). Astronomy & Astrophysics 422 (2): 515–522. doi:10.1051/0004-6361:20040089. ISSN 0004-6361. Bibcode: 2004A&A...422..515V. https://www.aanda.org/articles/aa/pdf/2004/29/aa0089-04.pdf. 
  13. ↑ Harris, William E.; Pritchet, Christopher J.; McClure, Robert D. (March 1995). "Globular Cluster Systems in Three cD Galaxies within Rich Abell Clusters" (in en). The Astrophysical Journal 441: 120. doi:10.1086/175341. ISSN 0004-637X. Bibcode: 1995ApJ...441..120H. https://articles.adsabs.harvard.edu//full/1995ApJ...441..120H/0000124.000.html. 
  14. ↑ Harris, William E.; Ciccone, Stephanie M.; Eadie, Gwendolyn M.; Gnedin, Oleg Y.; Geisler, Douglas; Rothberg, Barry; Bailin, Jeremy (Jan 2017). "Globular Cluster Systems in Brightest Cluster Galaxies. III: Beyond Bimodality" (in en). The Astrophysical Journal 835 (1): 101. doi:10.3847/1538-4357/835/1/101. ISSN 0004-637X. Bibcode: 2017ApJ...835..101H. 
  15. ↑ Lee, Myung Gyoon; Kim, Eunhyeuk; Geisler, Doug; Bridges, Terry; Ashman, Keith (2002). "A Comparative Study of Globular Cluster Systems in UGC 9799 and NGC 1129" (in en). Extragalactic Star Clusters 207: 330. ISSN 1743-9221. Bibcode: 2002IAUS..207..330L. 
  16. ↑ Balmaverde, Barbara; Capetti, Alessandro; Marconi, Alessandro; Venturi, Giacomo (2018-04-01). "The VLT/MUSE view of the central galaxy in Abell 2052 - Ionized gas swept by the expanding radio source" (in en). Astronomy & Astrophysics 612: A19. doi:10.1051/0004-6361/201732022. ISSN 0004-6361. Bibcode: 2018A&A...612A..19B. https://www.aanda.org/articles/aa/abs/2018/04/aa32022-17/aa32022-17.html. 



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