4C 10.45

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4C 10.45
Image of 4C 10.45.png
SDSS image of 4C 10.45.
Observation data (J2000.0 epoch)
Constellation Serpens
Right ascension 16h 08m 46.20s [1]
Declination +10° 29′ 07.77″ [1]
Redshift 1.232890 [1]
Heliocentric radial velocity 369,611 km/s [1]
Distance 8.772 Gly
Apparent magnitude  (V)18.70
Characteristics
Type FSRQ; LPQ blazar [1]
Size~160,000  ly (49  kpc) (estimated) [1]
Other designations
PKS 1606+10, 2MASS J16084620+1029075, LEDA 2818941, OS +111, DA 401, NVSS J160846+102908, FIRST J160846.1+102907, CoNFIG 238, TXS 1606+105, VERA J1608+1029, WMAP 009, RX J1608.7+1028, SDSS J160846.20+102907.7 [1]

4C 10.45 is a radio-loud [2] quasar located in the constellation of Serpens. The redshift of the object is (z) 1.232 [1] and it was first discovered in 1968 by astronomers, designated as PKS 1606+10 based on a Parkes Catalogue of Radio Sources survey. [3] The radio spectrum of the quasar is flat, hereby classifying it a flat-spectrum radio quasar. [4] [5]

Contents

Description

4C 10.45 has been categorized as a blazar, being variable on the electromagnetic spectrum. It has shown extreme gamma-ray activity on 29 October, 2024 and on 27 May 2025, with daily average fluxes of 0.9 ± 0.2 x 10-6 photons cm-2 s-1 and 1.0 ± 0.2 x 10-6 photons cm-2 s-1 respectively. [5] [6] It was also shown to be a bright optical state indicating an active state. [7] EGERT (Energetic Gamma Ray Experiment Telescope) observations have showed the source having a gamma-ray spectrum of 1.64 ± 0.24 x 10-9. [8]

The source of 4C 10.45 is compact, being made of a radio core that is 0.5 milliarcseconds in size, with evidence of radio emission extending towards northwest direction. [9] The total peak flux density of the core and extended components at six centimeters are estimated to be 1.5 and 1.6. [10]

Observations with Very Long Baseline Interferometry (VLBI) also showed the source has a presence of a jet made out of various components. [11] This jet also displays a sharp bend by one milliarcsecond from the core region between the position angles of -80° and -40°. A weak knot feature is seen at the position of the jet bend. [12] The jet angle along the line of sight is estimated to be 1.8° with an apparent opening angle of 8.8°. [13] VLBI observations found four of the components in the jet are moving in superluminal motions while the other component is stationary. The velocities of the four moving components are estimated to be 3.4 ± 1.7, 2.4 ± 1.1, 8.0 ± 5.9 and 6.1 ± 6.0 hours per second while the stationary component barely moves at 0.0 ± 0.9 hours per second. [11]

The optical spectrum of the quasar shows two emission lines classified as being broad. When studied, it has lines of mainly C III and ionized magnesium (Mg II). It is also found the quasar shows a narrow-line type and is surrounded by foreground galaxies. [14]

References

  1. 1 2 3 4 5 6 7 8 "4C 10.45". NASA/IPAC Extragalactic Database. Retrieved 2025-09-01.
  2. ↑ Fichtel, Carl E. (February 1994). "High-Energy Gamma-Ray Observations of Active Galaxies". The Astrophysical Journal Supplement Series. 90: 917. Bibcode:1994ApJS...90..917F. doi:10.1086/191925. ISSN   0067-0049.
  3. ↑ Murdoch, H. S.; Large, M. I. (1968-08-01). "Revised Spectra for 74 Radio Sources" (PDF). Monthly Notices of the Royal Astronomical Society. 141 (4): 377–388. doi: 10.1093/mnras/141.4.377 . ISSN   0035-8711.
  4. ↑ Pohl, M.; Hartman, R. C.; Jones, B. B.; Sreekumar, P. (October 1997). "A spectral study of gamma-ray emitting active galactic nuclei". Astronomy and Astrophysics. 326: 51–58. Bibcode:1997A&A...326...51P. ISSN   0004-6361.
  5. 1 2 "ATel #16889: Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ 4C +10.45". The Astronomer's Telegram. Retrieved 2025-09-01.
  6. ↑ "ATel #17206: Fermi-LAT detection of renewed gamma-ray activity from the FSRQ 4C +10.45". The Astronomer's Telegram. Retrieved 2025-09-01.
  7. ↑ "ATel #17213: 4C+10.45 optically bright". The Astronomer's Telegram. Retrieved 2025-09-01.
  8. ↑ Sreekumar, P.; Bertsch, D. L.; Dingus, B. L.; Esposito, J. A.; Fichtel, C. E.; Fierro, J.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Mayer-Hasselwander, H. A.; Mattox, J. R.; Michelson, P. F.; von Montigny, C. (June 1996). "EGRET Observations of the North Galactic Pole Region". The Astrophysical Journal. 464: 628. Bibcode:1996ApJ...464..628S. doi:10.1086/177352. ISSN   0004-637X.
  9. ↑ Dodson, R.; Fomalont, E. B.; Wiik, K.; Horiuchi, S.; Hirabayashi, H.; Edwards, P. G.; Murata, Y.; Asaki, Y.; Moellenbrock, G. A.; Scott, W. K.; Taylor, A. R.; Gurvits, L. I.; Paragi, Z.; Frey, S.; Shen, Z.-Q. (April 2008). "The VSOP 5 GHz Active Galactic Nucleus Survey. V. Imaging Results for the Remaining 140 Sources". The Astrophysical Journal Supplement Series. 175 (2): 314–355. arXiv: 0710.5707 . Bibcode:2008ApJS..175..314D. doi:10.1086/525025. ISSN   0067-0049.
  10. ↑ Zhang, Jiang-Shui; Fan, Jun-Hui (October 2003). "Spectral Indices of Core and Extended Components of Extragalactic Radio Sources". Chinese Journal of Astronomy and Astrophysics. 3 (5): 415–422. Bibcode:2003ChJAA...3..415Z. doi:10.1088/1009-9271/3/5/415. ISSN   1009-9271.
  11. 1 2 Piner, B. Glenn; Kingham, Kerry A. (November 1998). "Geodetic VLBI Observations of EGRET Blazars". The Astrophysical Journal. 507 (2): 706–725. arXiv: astro-ph/9806224 . Bibcode:1998ApJ...507..706P. doi:10.1086/306346. ISSN   0004-637X.
  12. ↑ Jorstad, Svetlana G.; Marscher, Alan P.; Mattox, John R.; Wehrle, Ann E.; Bloom, Steven D.; Yurchenko, Alexei V. (June 2001). "Multiepoch Very Long Baseline Array Observations of EGRET-detected Quasars and BL Lacertae Objects: Superluminal Motion of Gamma-Ray Bright Blazars". The Astrophysical Journal Supplement Series. 134 (2): 181–240. arXiv: astro-ph/0101570 . Bibcode:2001ApJS..134..181J. doi:10.1086/320858. ISSN   0067-0049.
  13. ↑ Hervet, Olivier; Boisson, Catherine; Sol, Hélène (2016-05-08), "An innovative blazar classification based on radio jet kinematics", Astronomy and Astrophysics, 592: A22, arXiv: 1605.02272 , Bibcode:2016A&A...592A..22H, doi:10.1051/0004-6361/201628117
  14. ↑ Stickel, M.; Kuehr, H. (May 1994). "Optical spectra and redshifts of 1 Jy, S4 and S5 radio source identifications. V." Astronomy and Astrophysics Supplement Series. 105: 67–75. ISSN   0365-0138.
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