4C 32.26

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4C 32.26
Image of 4C 32.26.png
The radio galaxy 4C 32.26.
Observation data (J2000 epoch)
Constellation Cancer
Right ascension 08h 41m 13.08s [1]
Declination +32° 24′ 59.45″ [1]
Redshift 0.068488 [1]
Heliocentric radial velocity 20,532 km/s [1]
Distance 950 Mly
Group or cluster Abell 695
Apparent magnitude  (B)14.08
Characteristics
Type E; BrCLG [1]
Size~287,000  ly (88.1  kpc) (estimated) [1]
Other designations
2MASX J08411308+3224596, B2 0838+32A, PGC 24412, NVSS J084112+322459, TXS 0838+325, VERA J0841+325, 2CXO J084113.0+322459 [1]

4C 32.26 is a radio galaxy [2] located in the constellation of Cancer. The redshift of the galaxy is (z) 0.068, estimating a light travel time of 950 million light-years away, [1] and it was first discovered as an astronomical radio source by astronomers in 1969 who were conducting the Fourth Cambridge Survey. [3] The galaxy is considered to be part of the dumbbell system and is the brightest cluster galaxy (BCG) in the center of the galaxy cluster, Abell 695. [4]

Contents

Description

4C 32.26 is classified as both a wide-angle tail (WAT) and weak radio galaxy. [5] [6] Its host is a large elliptical galaxy found described to have the presence of a central component that is associated with it and a western component that is found to be displaced by 70 kiloparsecs. [5] Studies of this host galaxy shows it has an undisturbed appearance without any signs of a major galaxy merger, although it is found interacting with the other cluster members. [2] A faint companion is located away from it by 11 arcseconds. [7]

The radio structure of 4C 32.26 is found as compact. When observed, the structure is to be reminiscent of Fanaroff-Riley Class Type II sources with its radio core having a total flux density of 7.5 MJy. [4] Radio observations made by Very Large Array (VLA) at 1.4 GHz frequencies, showed a compact source instead surrounded by radio emission. At 4.9 GHz, there is an inner source present with two radio lobes. These lobes are found to span around 16 kiloparsecs with much fainter asymmetric lobes that have a projected size of 150 kiloparsecs from the position of the nucleus. A jet appears to lead towards a faint lobe but it is instead at 90° in terms of projection. Further evidence also pointed out the galaxy is also a restarted source whose first pair of lobes are old and no longer fueled while the second pair of lobes are consider as young with approximate ages of between 3 and 7 million years old. [2] Earlier observations found the presence of two jet-like structures that ends in hotspot positions. [8]

A study has found 4C 32.26 has an extended emission line region (EELR) based on narrow-band optical imaging. Based on results, the EELR emission is mainly concentrated mainly on the host galaxy. [9]

References

  1. 1 2 3 4 5 6 7 8 "NED Search results for 4C 32.26". NASA/IPAC Extragalactic Database. Retrieved 2025-12-06.
  2. 1 2 3 Jetha, Nazirah N.; Hardcastle, Martin J.; Ponman, Trevor J.; Sakelliou, Irini (2008-12-11). "Shock heating in the group atmosphere of the radio galaxy B2 0838+32A". Monthly Notices of the Royal Astronomical Society. 391 (3): 1052–1062. arXiv: 0809.2534 . Bibcode:2008MNRAS.391.1052J. doi: 10.1111/j.1365-2966.2008.13959.x . ISSN   0035-8711.
  3. ↑ Fanti, C.; Fanti, R.; Londrillo, P.; Padrielli, L. (August 1969). "The radiospectra of a homogeneous sample of 4C radio sources". Astronomy and Astrophysics. 2: 477–483. Bibcode:1969A&A.....2..477F. ISSN   0004-6361.
  4. 1 2 Liuzzo, E.; Giovannini, G.; Giroletti, M.; Taylor, G. B. (2009-10-01). "The Bologna complete sample of nearby radio sources - II. Phase referenced observations of faint nuclear sources". Astronomy & Astrophysics. 505 (2): 509–520. arXiv: 0908.4391 . Bibcode:2009A&A...505..509L. doi:10.1051/0004-6361/200912586. ISSN   0004-6361.
  5. 1 2 Valentijn, E. A. (1979). "A Westerbork survey of clusters of galaxies. X. A 610 MHz survey of extended radio emission from 8 Abell clusters". Astronomy and Astrophysics Supplement Series. 38: 319–333. ISSN   0365-0138.
  6. ↑ 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. Bibcode:1997RMxAA..33...31C. ISSN   0185-1101.
  7. ↑ González-Serrano, J. I.; Carballo, R. (2000-03-01). "Surface photometry of radio loud elliptical galaxies from the B2 sample" (PDF). Astronomy and Astrophysics Supplement Series. 142 (3): 353–368. Bibcode:2000A&AS..142..353G. doi:10.1051/aas:2000154. ISSN   0365-0138.
  8. ↑ 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. Bibcode:1986A&AS...65..111D. ISSN   0365-0138.
  9. ↑ 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. Bibcode:1999RMxAA..35...45C. ISSN   0185-1101.
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