B2 1144+35

B2 1144+35
SDSS image of B2 1144+35.
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension11h 47m 22.13s[1]
Declination+35° 01′ 07.52″[1]
Redshift0.062958[1]
Heliocentric radial velocity18,874 km/s[1]
Distance880 Mly
Apparent magnitude (V)16.83
Apparent magnitude (B)17.89
Characteristics
TypeBLLAC? Sy2[1]
Size~340,000 ly (104.2 kpc) (estimated)[1]
Other designations
CGCG 186-048, 2MASX J11472209+3501071, PGC 36775, TXS 1144+352, RFC J1147+3501, VIPS 0477, VERA J1147+3501, 7C 1144+3517, SDSS J114722.14+350107.6[1]

B2 1144+35 commonly known as B2 1144+35B, is a radio galaxy located in the constellation of Ursa Major. The redshift of the object is (z) 0.062[1] and it was first discovered in 1978 as an astronomical radio source in the Green Bank Second survey by astronomers.[2] This galaxy contains a gigahertz peaked radio spectrum (GPS).[3] It has also been classified as a BL Lacertae object candidate.[4]

Description

B2 1144+35 is categorized as a giant low-power radio galaxy.[5][6] Its host has a faint magnitude of 15.7 and has a boxy shape appearance, suggesting a galaxy merger event.[7][8][9] It is also located inside a medium compact galaxy group and has a companion galaxy located 25 kiloparsecs to the west.[3] The stellar population of the galaxy is mainly made up old supergiant stars between 109-1010 years.[10]

The radio source of B2 1144+35 is large. When imaged in parsec-scales at 8.4 GHz frequencies by Very Long Baseline Interferometry (VLBI), the structure is found to made up of four main substructures including two compact components that have a separation gap of between 2-3 milliarcseconds. The north direction of both components also has radio emission described as faint and extended.[8]

Images made with the Very Large Array (VLA) showed the source is a double with a clearly resolved radio lobe component and a secondary component that is unresolved at. Further imaging has shown the eastern part has a radio lobe of Fanaroff Riley Class Type I morphology and a leading hotspot feature, while the southern part of the western part has a radio lobe, but with an elongated radio tail feature.[3] A short jet is found on both sides of the source.[11][12] Further observations noted the radio emission on megaparsec scales, and is suggested as a relic source between 50-90 million years old.[13]

A radio core has been detected in B2 1144+35, dominating the northwestern side of the source. When observed on arcsecond scales at both 1.4 and 5 GHz, this core is shown as variable, displaying a flux density increase by a factor of two. There are also smooth flux density variations after 1980, but decreases after the years between 1990 and 1992.[7] Observations made in 2007 found the core has superluminal motion, indicating the emergence of a new component.[11] In 2020, the nucleus of the galaxy was shown to change its position.[14]

References

  1. ^ a b c d e f g h "NED Search results for B2 1144+35". NASA/IPAC Extragalactic Database. Retrieved 2025-10-19.
  2. ^ Machalski, J. (1978). "The Green Bank Second(GB2) Survey of extragalactic radio sources at 1400 MHz. The catalogue of sources". Acta Astronomica. 28: 367–440. Bibcode:1978AcA....28..367M. ISSN 0001-5237.
  3. ^ a b c Schoenmakers, A. P.; de Bruyn, A. G.; Röttgering, H. J. A.; van der Laan, H. (January 1999). "The Mpc-scale radio source associated with the GPS galaxy B1144+352". Astronomy and Astrophysics. 341: 44–57. arXiv:astro-ph/9810178. Bibcode:1999A&A...341...44S. ISSN 0004-6361.
  4. ^ Marcha, M. J. M.; Browne, I. W. A.; Impey, C. D.; Smith, P. S. (1996-07-11). "Optical spectroscopy and polarization of a new sample of optically bright flat radio spectrum sources" (PDF). Monthly Notices of the Royal Astronomical Society. 281 (2): 425–448. doi:10.1093/mnras/281.2.425. ISSN 0035-8711.
  5. ^ Titov, Oleg; Frey, Sándor; Melnikov, Alexey; Lambert, Sébastien; Shu, Fengchun; Xia, Bo; González, Javier; Tercero, Belén; Gulayev, Sergey; Weston, Stuart; Natusch, Tim (2022-03-14). "Unprecedented change in the position of four radio sources". Monthly Notices of the Royal Astronomical Society. 512 (1): 874–883. doi:10.1093/mnras/stac038. ISSN 0035-8711.
  6. ^ Gonçalves, A. C.; Serote Roos, M. (January 2004). "The nuclear region of low luminosity flat radio spectrum sources. II. Emission-line spectra". Astronomy and Astrophysics. 413: 97–105. arXiv:astro-ph/0309620. Bibcode:2004A&A...413...97G. doi:10.1051/0004-6361:20031494. ISSN 0004-6361.
  7. ^ a b Giovannini, G.; Taylor, G. B.; Arbizzani, E.; Bondi, M.; Cotton, W. D.; Feretti, L.; Lara, L.; Venturi, T. (November 1999). "1144+35: A giant radio galaxy with superluminal motion". New Astronomy Reviews. 43 (8–10): 651–655. arXiv:astro-ph/9904068. Bibcode:1999NewAR..43..651G. doi:10.1016/S1387-6473(99)00072-X. ISSN 1387-6473.
  8. ^ a b Arbizzani, E.; Giovannini, G.; Taylor, G. B.; Bondi, M.; Cotton, W. D.; Feretti, L.; Lara, L.; Venturi, T. (1999). "VLBI observations of B2 1144+35: a peculiar radio galaxy". Memorie della Societa Astronomica Italiana. 70: 125–128. Bibcode:1999MmSAI..70..125A. ISSN 0037-8720.
  9. ^ G, Bruni; M, Brienza; F, Panessa; L, Bassani; D, Dallacasa; T, Venturi; D, Baldi, R; A, Botteon; A, Drabent; A, Malizia; F, Massaro; Röttgering, H J A; P, Ubertini; F, Ursini; van Weeren, R J (2021-04-20). "Hard X-ray selected giant radio galaxies – III. The LOFAR view". Monthly Notices of the Royal Astronomical Society. 503 (4). doi:10.1093/mnra (inactive 19 October 2025). ISSN 0035-8711. Archived from the original on 2023-08-01. Retrieved 2025-10-19.{{cite journal}}: CS1 maint: DOI inactive as of October 2025 (link) CS1 maint: multiple names: authors list (link)
  10. ^ Roos, M. Serote; Gonçalves, A. C. (2004-01-01). "The nuclear region of low luminosity flat radio spectrum sources - I. Stellar content" (PDF). Astronomy & Astrophysics. 413 (1): 91–96. arXiv:astro-ph/0309534. Bibcode:2004A&A...413...91S. doi:10.1051/0004-6361:20031493. ISSN 0004-6361.
  11. ^ a b Giovannini, G.; Giroletti, M.; Taylor, G. B. (2007-11-01). "B2 1144+35B, a giant low power radio galaxy with superluminal motion - Orientation and evidence for recurrent activity". Astronomy & Astrophysics. 474 (2): 409–414. arXiv:0708.3902. Bibcode:2007A&A...474..409G. doi:10.1051/0004-6361:20078058. ISSN 0004-6361.
  12. ^ Liuzzo, E.; Buttiglione, S.; Giovannini, G.; Giroletti, M.; Capetti, A.; Taylor, G. B. (2013-02-01). "Compact sources in the Bologna Complete Sample: high-resolution VLA observations and optical data" (PDF). Astronomy & Astrophysics. 550: A76. arXiv:1209.4204. Bibcode:2013A&A...550A..76L. doi:10.1051/0004-6361/201220012. ISSN 0004-6361.
  13. ^ Bruni, G; Panessa, F; Bassani, L; Dallacasa, D; Venturi, T; Saripalli, L; Brienza, M; Hernández-García, L; Chiaraluce, E; Ursini, F; Bazzano, A; Malizia, A; Ubertini, P (2020-03-19). "Hard X-ray selected giant radio galaxies – II. Morphological evidence of restarted radio activity". Monthly Notices of the Royal Astronomical Society. 494 (1): 902–914. doi:10.1093/mnras/staa735. ISSN 0035-8711.
  14. ^ Titov, Oleg; Frey, Sándor (2020-07-01). "An Apparent Jump in the Radio Position of J1147+3501". Research Notes of the AAS. 4 (7): 108. Bibcode:2020RNAAS...4..108T. doi:10.3847/2515-5172/aba42c. ISSN 2515-5172.
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