NVSS J141343+433945

NVSS J141343+433945
SDSS image of NVSS J141343+433945
Observation data (J2000.0 epoch)
ConstellationBoötes
Right ascension14h 13m 43.72s[1]
Declination+43° 39′ 45.04″[1]
Redshift0.089326[1]
Heliocentric radial velocity26,779 ± 3 km/s[1]
Distance1,307.4 ± 91.5 Mly (400.86 ± 28.06 Mpc)[1]
magnitude (J)14.20[1]
Characteristics
TypecD;BLRG blazar[1]
Size~236,000 ly (72.4 kpc) (estimated)[1]
Other designations
2MASX J14134379+4339450, Abell 1885:[CEF95], LEDA 2226096, BZU J1413+4339, RGB J1413+436, RX J1413.7+4339:[BEV98] 003[1]

NVSS J141343+433945 also known as RGB J1413+436, is a Type-cD galaxy[2] located in the constellation of Boötes. The redshift of the object is (z) 0.089[1] and it was first discovered from a sample of radio-loud active galactic nuclei by astronomers in 1998.[2] It is classified as a broad-line radio galaxy[2][3] and is the brightest cluster galaxy of Abell 1885, dominating the center of the galaxy cluster.[4]

Description

NVSS J141343+433945 contains a low luminosity active galactic nucleus. When observed with Very Long Baseline Interferometry (VLBI), the source is found compact but has no signs of any extended structures. The optical spectrum of the galaxy also displays strong signatures of emission lines mainly made up of ionized oxygen, hydrogen beta and hydrogen alpha. There is also a presence of an X-ray source with the total X-ray luminosity that is estimated to be 1.7 × 1044 erg s−1.[5] Evidence also suggested that the galaxy is also a BL Lacertae candidate.[6] The molecular line luminosity is 1.1 × 1040 erg s−1 while the hydrogen alpha luminosity is 5.4 × 1040 erg s−1.[7]

A study published in 2025, has found the active galactic nucleus of the galaxy is relatively young. Based on studies, the nucleus is depicted as bright in X-rays with the source being mainly resolved into a central point source. The radio core is found to be resolved and there are presence of two-sided radio jets towards both the east and west direction from the location of the core. The total jet power is about 102 ± 66 × 1042 erg s−1. On parsec-scale imaging made at 5 GHz frequencies, the flux density of the source is 34.3 ± 3.0 mJy. The supermassive black hole lying in the center of the galaxy is estimated to be 4.7 ± 1.1 × 108 M☉ and the total star formation rate is estimated to be 0.4 M☉ per year. The ionized gas is mainly concentrated on the nucleus, however it is also shown as elongated by 30 kiloparsecs.[4]

References

  1. 1 2 3 4 5 6 7 8 9 10 "NED Search results for NVSS J141343+433945". NASA/IPAC Extragalactic Database. Retrieved 2026-04-27.
  2. 1 2 3 Laurent-Muehleisen, S. A.; Kollgaard, R. I.; Ciardullo, R.; Feigelson, E. D.; Brinkmann, W.; Siebert, J. (September 1998). "Radio-loud Active Galaxies in the Northern ROSAT All-Sky Survey. III. New Spectroscopic Identifications from the RASS–Green Bank BL Lacertae Survey". The Astrophysical Journal Supplement Series. 118 (1): 127–175. arXiv:astro-ph/9711268. Bibcode:1998ApJS..118..127L. doi:10.1086/313134. ISSN 0067-0049.
  3. ↑ Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bloom, E. D.; Bonamente, E. (December 2009). "Fermi Observations of TeV-Selected Active Galactic Nuclei". The Astrophysical Journal. 707 (2): 1310–1333. arXiv:0910.4881. Bibcode:2009ApJ...707.1310A. doi:10.1088/0004-637X/707/2/1310. ISSN 0004-637X.
  4. 1 2 White, Laurel; McDonald, Michael; Ubertosi, Francesco; Gaspari, Massimo; Hlavacek-Larrondo, Julie; Russell, Helen; Somboonpanyakul, Taweewat (2025-07-11). "The Onset of Feedback in A1885: Evidence for Large-scale Quenching Despite a Young Central Active Galactic Nucleus". The Astrophysical Journal. 988 (1): 24. arXiv:2506.03277. Bibcode:2025ApJ...988...24W. doi:10.3847/1538-4357/ade14b. ISSN 0004-637X.
  5. ↑ Caccianiga, A.; Marchã, M. J. M.; Thean, A.; Dennett-Thorpe, J. (December 2001). "EVN observations of low-luminosity flat-spectrum active galactic nuclei". Monthly Notices of the Royal Astronomical Society. 328 (3): 867–872. arXiv:astro-ph/0108465. Bibcode:2001MNRAS.328..867C. doi:10.1046/j.1365-8711.2001.04928.x. ISSN 0035-8711.
  6. ↑ Green, T. S.; Edge, A. C.; Ebeling, H.; Burgett, W. S.; Draper, P. W.; Kaiser, N.; Kudritzki, R.-P.; Magnier, E. A.; Metcalfe, N.; Wainscoat, R. J.; Waters, C. (March 2017). "Hiding in plain sight - recovering clusters of galaxies with the strongest AGN in their cores". Monthly Notices of the Royal Astronomical Society. 465 (4): 4872–4885. arXiv:1611.07996. doi:10.1093/mnras/stw3059. ISSN 0035-8711.
  7. ↑ Edge, A. C.; Wilman, R. J.; Johnstone, R. M.; Crawford, C. S.; Fabian, A. C.; Allen, S. W. (November 2002). "A survey of molecular hydrogen in the central galaxies of cooling flows". Monthly Notices of the Royal Astronomical Society. 337 (1): 49–62. arXiv:astro-ph/0206379. Bibcode:2002MNRAS.337...49E. doi:10.1046/j.1365-8711.2002.05790.x. ISSN 0035-8711.
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