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NGC 708

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Galaxy in the constellation Andromeda
NGC 708
Pan-STARRS image of NGC 708
Observation data (J2000 epoch)
ConstellationAndromeda
Right ascension01 52 46.5
Declination36° 09′ 07″
Redshift0.016195
Heliocentric radial velocity4,855 km/s
Distance239 Mly (73.3 Mpc)
Group or clusterAbell 262
Apparent magnitude (V)13.70
Characteristics
TypeE
Size~200,000 ly (62 kpc) (estimated)
Apparent size (V)3.0 x 2.5
Other designations
CGCG 522-39, MCG 6-5-31, PGC 6962, UGC 1348, B2 0149+35

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

NGC 708 is surrounded by 4,700 globular clusters.

Dust lane

Discovered in 1979 by Kotanyi et al., NGC 708 has a thin dust lane with an irregular structure. Besides the dust lane, there are also patches of dust that cross the nucleus. These features are oriented nearly perpendicular to the radio emission of the galaxy. The lane appears to be a nearly edge-on dust disk with a length of 16,000 ly (5 kpc).

The dust lane appears to have formed from a cooling accretion flow of intracluster medium (ICM) onto NGC 708.

The dust lane in NGC 708 as imaged by the Hubble Space Telescope. NGC 705 can be seen at the lower right of the image.

Supermassive black hole

NGC 708 has a supermassive black hole with an estimated mass of (2.9×10 M☉) (10) M.

The supermassive black hole is powering the radio jets and lobes in the galaxy.

Radio morphology

NGC 708 contains two radio jets that are mildly bent and extend into ''s'' shaped double radio lobes with a total length of 200,000 ly (60 kpc).

Chandra observations have shown that the lobes have created a cavity in the intracluster medium of Abell 262.

Possible interaction

NGC 708 may be interacting with NGC 705 which lies about 67,000 ly (20.6 kpc) to the south-west.

See also

References

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  14. Reddy, Naveen A.; Yun, Min S. (2004-01-10). "Radio and Far-Infrared Emission as Tracers of Star Formation and AGN in Nearby Cluster Galaxies". The Astrophysical Journal. 600 (2): 695–715. arXiv:astro-ph/0309649. Bibcode:2004ApJ...600..695R. doi:10.1086/379871. ISSN 0004-637X. S2CID 15068448.
  15. Harris, William E.; Harris, Gretchen L. H.; Alessi, Matthew (2013-07-09). "A Catalog of Globular Cluster Systems: What Determines the Size of a Galaxy's Globular Cluster Population?". The Astrophysical Journal. 772 (2): 82. arXiv:1306.2247. Bibcode:2013ApJ...772...82H. doi:10.1088/0004-637X/772/2/82. ISSN 0004-637X. S2CID 119113886.
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  22. Wegner, G. A.; Corsini, E. M.; Thomas, J.; Saglia, R. P.; Bender, R.; Pu, S. B. (2012). "Further Evidence for Large Central Mass-to-light Ratios in Early-type Galaxies: The Case of Ellipticals and Lenticulars in the A262 Cluster". The Astronomical Journal. 144 (3): 78. arXiv:1206.5768. Bibcode:2012AJ....144...78W. doi:10.1088/0004-6256/144/3/78. hdl:11577/2526313. ISSN 1538-3881. S2CID 118679035.
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