Astronomy:Abell 665
| Abell 665 | |
|---|---|
.jpg) | |
| Observation data (Epoch J2000) | |
| Constellation(s) | Ursa Major |
| Right ascension | 08h 30m 45.2s[1] |
| Declination | +65° 52′ 55″[1] |
| Brightest member | 2MASX J08305736+6550299 [2][3] |
| Richness class | 5[4] |
| Bautz–Morgan classification | III[1] |
| Velocity dispersion | 1 390+120−110 km/s[2] |
| Redshift | 0.1819[1] |
| Distance (co-moving) | 720 Mpc (2,348 Mly) h−10.73 [1] |
| ICM temperature | 7.7 ± 0.4 keV (r ≲ 100 h−10.73 kpc)[5] |
| Binding mass | ~1015 h−10.75[2] M☉ |
| X-ray flux | (11.8 ± 15.6%)×10−12 erg s−1 cm−2 (0.1–2.4 keV)[1] |
Abell 665 is a galaxy cluster in the Abell catalogue in the constellation Ursa Major. It is also known as the only cluster in his 1989 catalog to receive Abell's highest richness class of 5. This means that it contains at least 300 galaxies in the magnitude range of m3 to m3+2, where m3 is the magnitude of the third-brightest member of the cluster. The clusters in all other richness classes contain less than 300 such galaxies. Abell 665's combination of high brightness and large distance, made it an excellent candidate along with 37 other clusters to help determine the Hubble constant using the Sunyaev–Zel'dovich effect in 2006.[5]
Member velocity, cluster velocity dispersion, and X-ray data suggest that Abell 665 is composed of two similar-mass clusters which are at or very close to core crossing, give or take ≲ 0.5 gigayears.[2]
Gallery
Abell 665 was named after George O. Abell, who included it in his 1958 catalogue.[6]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "NED results for object ABELL 0665". NASA/IPAC Extragalactic Database (NED). http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Abell+665&extend=no.
- ↑ 2.0 2.1 2.2 2.3 Gómez, Percy L.; Hughes, John P.; Birkinshaw, Mark (September 2000). "A Merger Scenario for the Dynamics of Abell 665". The Astrophysical Journal (Chicago, Illinois, USA: The University of Chicago Press) 540 (2): 726–740. doi:10.1086/309360. Bibcode: 2000ApJ...540..726G.
- ↑ Oegerle, William R.; Fitchett, Michael J.; Hill, John M.; Hintzen, Paul (July 20, 1991). "Dynamics of the microwave-decrement cluster Abell 665". Astrophysical Journal, Part 1 376: 46–50. doi:10.1086/170254. ISSN 0004-637X. Bibcode: 1991ApJ...376...46O.
- ↑ Abell, George O.; Corwin, Harold G., Jr.; Olowin, Ronald P. (May 1989). "A catalog of rich clusters of galaxies". Astrophysical Journal Supplement Series 70 (May 1989): 1–138. doi:10.1086/191333. ISSN 0067-0049. Bibcode: 1989ApJS...70....1A.
- ↑ 5.0 5.1 Bonamente, Massimiliano; Joy, Marshall K.; LaRoque, Samuel J.; Carlstrom, John E.; Reese, Erik D.; Dawson, Kyle S. (August 2006). "Determination of the Cosmic Distance Scale from Sunyaev-Zel'dovich Effect and Chandra X-Ray Measurements of High-Redshift Galaxy Clusters". The Astrophysical Journal (Chicago, Illinois, USA: The University of Chicago Press) 647 (1): 25–54. doi:10.1086/505291. Bibcode: 2006ApJ...647...25B.
- ↑ "Abell's richest cluster". https://www.spacetelescope.org/images/potw1744a/.
Coordinates: 
08h 30m 45.2s, +65° 52′ 55″
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