J2341+0018
| 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] |
| Helio radial velocity | 82,959 ± 4 km/s[1] |
| Distance | 3,976.6 ± 278.4 Mly (1,219.24 ± 85.35 Mpc)[1] |
| Group or cluster | RX J2341.1+0018 |
| Characteristics | |
| Type | Ellip;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 M☉ and a total hydrogen-alpha (Hα) star formation of 55.84 M☉ 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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NED Search results for J2341+0018". NASA/IPAC Extragalactic Database. Retrieved 2026-05-27.
- ↑ 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. arXiv:1203.1840. Bibcode:2012MNRAS.423..422L. doi:10.1111/j.1365-2966.2012.20886.x. ISSN 0035-8711.
- ↑ 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". Astronomy & Astrophysics. 654: A94. arXiv:2108.08122. Bibcode:2021A&A...654A..94M. doi:10.1051/0004-6361/202141566. ISSN 0004-6361.
- ↑ 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. arXiv:1904.02806. Bibcode:2019ApJS..243...14O. doi:10.3847/1538-4365/ab21c3. ISSN 1538-4365.
- ↑ 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. (2016-06-07). "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.
- ↑ 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.
- ↑ 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. arXiv:2203.13750. Bibcode:2022ApJS..260....4P. doi:10.3847/1538-4365/ac6352. ISSN 0067-0049.
- ↑ 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.
External links
- J2341+0018 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
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