B2 1441+26
From Wikipedia, the free encyclopedia
| B2 1441+26 | |
|---|---|
 SDSS image of B2 1441+26 | |
| Observation data (J2000 epoch) | |
| Constellation | Boötes |
| Right ascension | 14h 44m 06.29s[1] |
| Declination | +26° 01′ 11.68″[1] |
| Redshift | 0.061961[1] |
| Heliocentric radial velocity | 18575 ± 2 km/s[1] |
| Distance | 919.4 ± 64.4 Mly (281.89 ± 19.73 Mpc)[1] |
| magnitude (J) | 12.92[1] |
| magnitude (H) | 12.13[1] |
| Characteristics | |
| Size | ~195,000 ly (59.9 kpc) (estimated)[1] |
| Other designations | |
| 2MASX J14440631+2601118, 7C 1441+2614, CGCG 134-024, PGC 52616, 1441+26[1] | |
B2 1441+26 is a radio galaxy located in the constellation of Boötes. The redshift of the galaxy is (z) 0.061[1] and it was first discovered by astronomers in October 1983 from the B2 catalogue and such contains a double radio source.[2]
B2 1441+26 is categorized as a Fanaroff-Riley Class Type 1 low luminosity radio galaxy.[3][4][5] It is found to be hosted by a nearly face-on spiral galaxy although some studies suggest the host may might be an elliptical galaxy instead.[6][7][8] Studies also classify this as a weak radio galaxy (WRG) based on optical images with an ordinary galactic disk. There also a presence of an inner structure or a spiral patterned bar feature. Two companions have been found located both east and northeast from the galaxy's nucleus.[6] The extended emission-line region of the galaxy is shown unresolved.[9]
The source of the galaxy has been found as double,[2] being resolved into two separate components with further evidence that they contain a steep radio spectrum in addition.[10] There are presence of two asymmetric radio lobes, with the lobe on the eastern side being as twice more luminous and being more polarized three times more compared to the lobe on the western side.[11][12] The lobes also have a different magnetic field direction, being orientated parallel towards the axis of the source but also in an almost perpendicular direction.[11] Towards the inner region of the lobes, there is a steepening of the spectrum although the low brightness meant the tracing of steepening along the lobes' length is only halfway.[13] A radio core is found embedded inside the eastern lobe.[7]
References
- 1 2 3 4 5 6 7 8 9 10 "B2 1441+26". NASA/IPAC Extragalactic Database. Retrieved 2026-04-16.
- 1 2 Feretti, L.; Giovannini, G.; Gregorini, L.; Parma, P. (October 1983). "WSRT observations of elliptical galaxies from the B2 catalogue". Astronomy and Astrophysics. 126: 311–319. ISSN 0004-6361.
- ↑ Giovannini, G.; Taylor, G. B.; Feretti, L.; Cotton, W. D.; Lara, L.; Venturi, T. (January 2005). "The Bologna Complete Sample of Nearby Radio Sources". The Astrophysical Journal. 618 (2): 635–648. doi:10.1086/426106. ISSN 0004-637X.
- ↑ de Ruiter, H. R.; Parma, P.; Fanti, C.; Fanti, R. (July 1986). "VLA observations of low luminosity radio galaxies. II. Sources with angular size larger than two arcminutes". Astronomy and Astrophysics Supplement Series. 65: 111–144. ISSN 0365-0138.
- ↑ Fanti, C.; Fanti, R.; de Ruiter, H. R.; Parma, P. (April 1987). "VLA observations of low luminosity radio galaxies. IV. The B2 sample revisited". Astronomy and Astrophysics Supplement Series. 69: 57–76. ISSN 0365-0138.
- 1 2 Carrillo, R.; Cruz-González, I.; Guichard, J. (April 1997). "Weak Radio Galaxies. I. Broad-Band Optical Imaging". Revista Mexicana de Astronomia y Astrofisica. 33: 31–57. ISSN 0185-1101.
- 1 2 González-Serrano, J. I.; Carballo, R. (March 2000). "Surface photometry of radio loud elliptical galaxies from the B2 sample" (PDF). Astronomy and Astrophysics Supplement Series. 142: 353–368. doi:10.1051/aas:2000154. ISSN 0365-0138.
- ↑ Capetti, A.; de Ruiter, H. R.; Fanti, R.; Morganti, R.; Parma, P.; Ulrich, M.-H. (October 2000). "The HST snapshot survey of the B2 sample of low luminosity radio-galaxies: a picture gallery". Astronomy and Astrophysics. 362: 871–885. doi:10.48550/arXiv.astro-ph/0009056. ISSN 0004-6361.
- ↑ Carrillo, R.; Cruz-González, I.; Guichard, J. (April 1999). "Weak Radio Galaxies. II. Narrow-Band Optical Imaging and Physical Conditions". Revista Mexicana de Astronomia y Astrofisica. 35: 45. ISSN 0185-1101.
- ↑ Malumyan, V. G. (May 1987). "RATAN-600 Observations of Faint Bologna Radio Galaxies at 7.6-CM and 3.9-CM". Soviet Astronomy Letters. 13: 156.
- 1 2 Mack, K.-H.; Gregorini, L.; Parma, P.; Klein, U. (January 1994). "High-frequency radio continuum observations of radio galaxies with low and intermediate luminosity. II. Sources with sizes 4' to 5'". Astronomy and Astrophysics Supplement Series. 103: 157–182. ISSN 0365-0138.
- ↑ Capetti, A.; Morganti, R.; Parma, P.; Fanti, R. (June 1993). "Polarization in low luminosity radio galaxies". Astronomy and Astrophysics Supplement Series. 99: 407–435. ISSN 0365-0138.
- ↑ Parma, P.; Murgia, M.; Morganti, R.; Capetti, A.; de Ruiter, H. R.; Fanti, R. (April 1999). "Radiative ages in a representative sample of low luminosity radio galaxies". Astronomy and Astrophysics. 344: 7–16. doi:10.48550/arXiv.astro-ph/9812413. ISSN 0004-6361.
External links
- B2 1441+26 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
