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J2341+0018

From Wikipedia, the free encyclopedia
BL Lacertae object in the constellation Pisces
J2341+0018
SDSS image of J2341+0018
Observation data (J2000.0 epoch)
Constellation Pisces
Right ascension 23h 41m 06.91s[1]
Declination +00°18′33.33′′[1]
Redshift 0.276720[1]
Heliocentric radial velocity 82,959 ± 4 km/s [1]
Distance 3,976.6±278.4Mly (1,219.24±85.35Mpc)[1]
Group or cluster RX J2341.1+0018
magnitude(J)14.83[1]
Characteristics
Type Ellip;BrClG NLAGN[1]
Size~667,000ly (204.5kpc) (estimated)[1]
Other designations
2MASX J23410687+0018332, BZU J2341+0018, LEDA 1162543, NVSS J234106+001833, OGC 123, PKS 2338+000, PMN J2341+0018, RX J2341.1+0018:[REK2022] BCG, WHL J234106.9+001833 BCG[1]

J2341+0018 also known as PKS 2338+000 and OGC 123, is a BL Lacertae object located in the constellation of Pisces. The redshift of the object is (z) 0.276[1] and it is the brightest cluster galaxy (BCG) of an X-ray galaxy cluster called RX J2341.1+0018.[2]

Description

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J2341+0018 is an elliptical galaxy with a radio-loud active galactic nucleus (AGN) and has an R-band luminosity of 12.3 magnitude based on the R-band luminosity estimation made with Sloan Digital Sky Survey (SDSS).[3] [4] It is also an early-type galaxy with a total stellar mass that is estimated to be 11.58 Mʘ and a total hydrogen-alpha (Hα) star formation of 55.84 Mʘ per year.[2] The optical spectrum of the galaxy shows the presence of strong emission lines positioned on top of a stellar continuum, thus ruling out the possibility of a blazar source. The lines are significantly broad, with full width at half maximum speeds of up to 1,400 kilometers per second, suggesting the line kinematics are disturbed.[3] The g – r color offset of J2341+0018 is -0.58 magnitude.[5]

The radio source of J2341+0018 has an unresolved appearance. Its spectral energy distribution has a steep radio spectrum at high frequencies, yet also flattening less than a few hundred GHz. The spectral energy distribution of the source has a turnover frequency based on its flux density at 365 MHz. The spectral energy distribution component has parameters of 2.62 ± 0.01, -0.16 ± 0.06 and -0.15 ± 0.04 respectively based on a fit measurement with a low peak gigahertz peaked component.[6]

Further radio imaging of J2341+0018 made with Very Long Baseline Interferometry (VLBI) detected a radio core with an inverted spectrum as well as a radio jet. The core has a total flux density of 70 mJy,while the jet has a flux density of 270 mJy. Most of the radio emission is concentrated inside a component within the central radius of 120 parsecs.[3] The jet on parsec-scales is estimated to have a position angle of 52°, while the median distance between the core and jet components is 5.4 milliarcseconds.[7] A study published in 2022, described J2341+0018 as a weak source with detected variability of 4.5% and has a mean flux density of 98 mJy at 15 GHz.[8]

References

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  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for J2341+0018". NASA/IPAC Extragalactic Database. Retrieved 2026年05月27日.
  2. 1 2 Liu, F. S.; Mao, Shude; Meng, X. M. (2012年04月20日). "Star formation activities in early-type brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 423 (1): 422–436. arXiv:1203.1840 . Bibcode:2012MNRAS.423..422L. doi:10.1111/j.1365-2966.2012.20886.x . ISSN 0035-8711.
  3. 1 2 3 Murthy, Suma; Morganti, Raffaella; Oosterloo, Tom; Maccagni, Filippo M. (2021年10月01日). "The H I absorption zoo: JVLA extension to z ∼ 0.4". Astronomy & Astrophysics. 654: A94. arXiv:2108.08122 . Bibcode:2021A&A...654A..94M. doi:10.1051/0004-6361/202141566. ISSN 0004-6361.
  4. ↑ Ogle, Patrick M.; Lanz, Lauranne; Appleton, Philip N.; Helou, George; Mazzarella, Joseph (2019年07月15日). "A Catalog of the Most Optically Luminous Galaxies at z < 0.3: Super Spirals, Super Lenticulars, Super Post-mergers, and Giant Ellipticals". The Astrophysical Journal Supplement Series. 243 (1): 14. arXiv:1904.02806 . Bibcode:2019ApJS..243...14O. doi:10.3847/1538-4365/ab21c3 . ISSN 1538-4365.
  5. ↑ Green, T. S.; Edge, A. C.; Stott, J. P.; Ebeling, H.; Burgett, W. S.; Chambers, K. C.; Draper, P. W.; Metcalfe, N.; Kaiser, N.; Wainscoat, R. J.; Waters, C. (2016年06月07日). "A multiwavelength photometric census of AGN and star formation activity in the brightest cluster galaxies of X-ray selected clusters". Monthly Notices of the Royal Astronomical Society. 461 (1): 560–577. doi:10.1093/mnras/stw1338 . ISSN 0035-8711.
  6. ↑ Hogan, M. T.; Edge, A. C.; Geach, J. E.; Grainge, K. J. B.; Hlavacek-Larrondo, J. (October 2015). "High radio-frequency properties and variability of brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 453 (2): 1223–1240. arXiv:1507.03022 . doi:10.1093/mnras/stv1518 .
  7. ↑ Plavin, A. V.; Kovalev, Y. Y.; Pushkarev, A. B. (2022年05月01日). "Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei". The Astrophysical Journal Supplement Series. 260 (1): 4. arXiv:2203.13750 . Bibcode:2022ApJS..260....4P. doi:10.3847/1538-4365/ac6352 . ISSN 0067-0049.
  8. ↑ Rose, Tom; Edge, Alastair; Kiehlmann, Sebastian; Baek, Junhyun; Chung, Aeree; Jung, Tae-Hyun (January 2022). "The variability of brightest cluster galaxies at high radio frequencies". Monthly Notices of the Royal Astronomical Society. 509 (2): 2869–2884. arXiv:2109.03241 . doi:10.1093/mnras/stab3217 .
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