Astronomy:J2341+0018

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J2341+0018
File:Image of J2341+0018.png
SDSS image of J2341+0018
Observation data (J2000.0 epoch)
ConstellationPisces
Right ascension 23h 41m 06.91s[1]
Declination+00° 18′ 33.33″[1]
Redshift0.276720[1]
Helio radial velocity82,959 ± 4 km/s[1]
Distance3,976.6 ± 278.4 Mly (1,219.24 ± 85.35 Mpc)[1]
Group or clusterRX J2341.1+0018
Characteristics
TypeEllip;BrClG NLAGN[1]
Size~667,000 ly (204.5 kpc) (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

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 has a total hydrogen-alpha (Hα) star formation of 55.84 Mʘ per year.[2] The optical spectrum of the galaxy shows presence of strong emission lines that is positioned on top of a stellar continuum thus ruling out the possibility of a blazar source. Further evidence also found the lines are significantly broad with full width at half maximum speeds of up to 1,400 kilometers per seconds, 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 is found to have an unresolved appearance. When observed, its spectral energy distribution has a steep radio spectrum at high frequencies, yet also flattening less than a few hundred GHz. Evidence also found 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 presence of 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 mainly concentrated inside a component within the central radius of 120 parsecs.[3] The jet on parsec-scales is estimated to have a jet 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

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NED Search results for J2341+0018". https://ned.ipac.caltech.edu/byname?objname=LEDA+1162543&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 Liu, F. S.; Mao, Shude; Meng, X. M. (2012-04-20). "Star formation activities in early-type brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society 423 (1): 422–436. doi:10.1111/j.1365-2966.2012.20886.x. ISSN 0035-8711. Bibcode: 2012MNRAS.423..422L. 
  3. ↑ 3.0 3.1 3.2 Murthy, Suma; Morganti, Raffaella; Oosterloo, Tom; Maccagni, Filippo M. (2021-10-01). "The H I absorption zoo: JVLA extension to z ∼ 0.4" (in en). Astronomy & Astrophysics 654: A94. doi:10.1051/0004-6361/202141566. ISSN 0004-6361. Bibcode: 2021A&A...654A..94M. https://www.aanda.org/articles/aa/abs/2021/10/aa41566-21/aa41566-21.html. 
  4. ↑ Ogle, Patrick M.; Lanz, Lauranne; Appleton, Philip N.; Helou, George; Mazzarella, Joseph (2019-07-15). "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. doi:10.3847/1538-4365/ab21c3. ISSN 1538-4365. Bibcode: 2019ApJS..243...14O. 
  5. ↑ Green, T. S.; Edge, A. C.; Stott, J. P.; Ebeling, H.; Burgett, W. S.; Chambers, K. C.; Draper, P. W.; Metcalfe, N. et al. (2016-06-07). "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. https://academic.oup.com/mnras/article/461/1/560/2595297#45847236. 
  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. doi:10.1093/mnras/stv1518. 
  7. ↑ Plavin, A. V.; Kovalev, Y. Y.; Pushkarev, A. B. (2022-05-01). "Direction of Parsec-scale Jets for 9220 Active Galactic Nuclei". The Astrophysical Journal Supplement Series 260 (1): 4. doi:10.3847/1538-4365/ac6352. ISSN 0067-0049. Bibcode: 2022ApJS..260....4P. 
  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. doi:10.1093/mnras/stab3217. 



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