DA 193

DA 193
The blazar DA 193
Observation data (J2000.0 epoch)
ConstellationAuriga
Right ascension05h 55m 30.805s
Declination+39° 48′ 49.165″
Redshift2.365000
Heliocentric radial velocity709,009 km/s
Distance10.545 Gly
Apparent magnitude (V)18.3
Characteristics
TypeBlazar
Other designations
SWIFT J0555.5+3946, WMAP 100, TXS 0552+398, 2XMM J055530.7+394848

DA 193 is a blazar located in the constellation of Auriga. It has a high redshift of 2.365. It was first discovered as an unknown astronomical radio source in 1971 by D.G. MacDonell and A.H. Bridle. This is a low polarized quasar containing a classic homogeneous synchrotron self-absorption spectrum. The radio spectrum of this source shows a turnover frequency at 5 GHz and this object has also been referred to as a gigahertz-peak spectrum source.

DA 193 is found variable on the electromagnetic spectrum. It is bright in X-rays and displays a flat X-ray spectrum that is above 10 keV. During the first week of January 2018, it underwent a giga-electron volt (GeV) flare which was detected by Fermi-LAT. This GeV flare exhibited from DA 193 showed an exceeded binned gamma ray flux (1 × 10−6 ph cm−2 s−1) and was found to be extremely luminous (Lγ = (1.3 ± 0.4) × 1050 erg s−1). When observing its hard gamma-ray spectrum, the flare in DA 193 was confirmed to be a rare sight. In the optical-X-ray energy range, it shows an insignificant flux meaning its source went back to its quiescence state.

DA 193 contains one of the most compact radio sources known on both millisecond and arcsecond scales. In its radio structure, there are four components in the core region with the suggestion of a weak component located 2.3 mas. There is presence of a short jet extending towards the western direction. Furthermore, DA 193 has a simple core-halo structure according to VLBI Observations, with the major axis of the halo having a 110° position angle. This halo's position angle is found alike to the linear polarization position angle.

The central supermassive black hole of DA 193 is estimated to be (5.5 ± 0.9) × 109 M☉ based on calculations of a single optical spectroscopic emission line information, derived from usage of C IV emission lines and acquiring empirical relations proposed by Yue Shen. Its accretion disk luminosity is estimated as (1.3 ± 0.1) × 1047 erg s−1.

DA 193 has one close companion 2.9" to the north. The companion is found connected to the quasar via tidal interactions. Both objects are situated in a dense compact galaxy group.

References

  1. ↑ Nowakowski, Tomasz; Phys.org. "Luminous gamma-ray flare detected from the blazar DA 193". phys.org. Retrieved 2024-10-29.
  2. 1 2 Wang, W. H.; Hong, X. Y.; Jiang, D. R.; Venturi, T.; Chen, Y. J.; An, T. (December 2001). "An accelerated jet in DA193?" (PDF). Astronomy & Astrophysics. 380 (1): 123–129. doi:10.1051/0004-6361:20011439. ISSN 0004-6361.
  3. ↑ Fey, A. L.; Spangler, S. R.; Mutel, R. L.; Benson, J. M. (August 1985). "VLBI observations at 22.2 gigahertz of the radio source 0552 + 398 (DA 193)". The Astrophysical Journal. 295: 134. Bibcode:1985ApJ...295..134F. doi:10.1086/163357. ISSN 0004-637X.
  4. ↑ MacDonell, D. G.; Bridle, A. H. (1971-11-01). "Two Variable Radio Sources". Nature Physical Science. 234 (48): 88–90. Bibcode:1971NPhS..234...88M. doi:10.1038/physci234088a0. ISSN 0300-8746.
  5. 1 2 3 Schilizzi, R.T.; Shaver, P.A. (1981). "VLBI observations of the quasar DA 193". Astronomy & Astrophysics. 96 (1–2): 365–368. Bibcode:1981A&A....96..365S.
  6. ↑ Spangler, S. R.; Mutel, R. L.; Benson, J. M. (August 1983). "VLBI observations of the radio sources 0552 + 398 and 1848 + 283 - Measurements of the departure from equipartition". The Astrophysical Journal. 271: 44. Bibcode:1983ApJ...271...44S. doi:10.1086/161174. ISSN 0004-637X.
  7. ↑ Lister, M. L.; Cohen, M. H.; Homan, D. C.; Kadler, M.; Kellermann, K. I.; Kovalev, Y. Y.; Ros, E.; Savolainen, T.; Zensus, J. A. (2009-11-05). "MOJAVE: Monitoring Of Jets in Active Galactic Nuclei With VLBA Experiments. VI. Kinematics Analysis Of a Complete Sample of Blazar Jets". The Astronomical Journal. 138 (6): 1874–1892. arXiv:0909.5100. Bibcode:2009AJ....138.1874L. doi:10.1088/0004-6256/138/6/1874. ISSN 0004-6256.
  8. 1 2 Torniainen, I.; Tornikoski, M.; Teräsranta, H.; Aller, M. F.; Aller, H. D. (2005-05-13). "Long term variability of gigahertz-peaked spectrum sources and candidates" (PDF). Astronomy & Astrophysics. 435 (3): 839–856. Bibcode:2005A&A...435..839T. doi:10.1051/0004-6361:20041886. ISSN 0004-6361.
  9. ↑ Angioni, R.; Cheung, C. C. (2018-01-01). "Fermi-LAT detection of a new gamma-ray source associated with the high-redshift FSRQ TXS 0552+398". The Astronomer's Telegram (11137): 1. Bibcode:2018ATel11137....1A.
  10. 1 2 Paliya, Vaidehi S.; Ajello, M.; Ojha, R.; Angioni, R.; Cheung, C. C.; Tanada, K.; Pursimo, T.; Galindo, P.; Losada, I. R.; Siltala, L.; Djupvik, A. A.; Marcotulli, L.; Hartmann, D. (February 2019). "Detection of a Gamma-Ray Flare from the High-redshift Blazar DA 193". The Astrophysical Journal. 871 (2): 211. arXiv:1812.07350. Bibcode:2019ApJ...871..211P. doi:10.3847/1538-4357/aafa10. ISSN 0004-637X.
  11. ↑ Lister, Matthew L.; Marscher, Alan P.; Gear, W. K. (1998-09-10). "Submilliarcsecond Polarimetric Imaging of Blazar Jets at 43 GHz". The Astrophysical Journal. 504 (2): 702–719. Bibcode:1998ApJ...504..702L. doi:10.1086/306112. ISSN 0004-637X.
  12. ↑ Hutchings, J. B.; Crampton, David; Morris, S. L.; Durand, D.; Steinbring, E. (March 1999). "QSO Hosts and Environments at z = 0.9–4.2: JHK Images with Adaptive Optics". The Astronomical Journal. 117 (3): 1109–1121. arXiv:astro-ph/9812159. Bibcode:1999AJ....117.1109H. doi:10.1086/300787. ISSN 0004-6256.