OQ 530
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| OQ 530 | |
|---|---|
 The BL Lacertae object OQ 530 | |
| Observation data (J2000.0 epoch) | |
| Constellation | Boötes |
| Right ascension | 14h 19m 46.59s[1] |
| Declination | +54° 23′ 14.78″[1] |
| Redshift | 0.152500[1] |
| Heliocentric radial velocity | 45,718 km/s[1] |
| Distance | 1.989 Gly |
| Apparent magnitude (V) | 15.65 |
| Apparent magnitude (B) | 16.17 |
| Characteristics | |
| Type | Opt. Var. BLLAC[1] |
| Size | ~177,600 ly (54.44 kpc) (estimated)[1] |
| Other designations | |
| 2MASS J14194660+5423147, 1418+546, CSO 0633, IVS B1418+546, NVSS J141946+542315, PG 1418+546[1] | |
OQ 530 is a BL Lacertae object[2][3][4] located in the constellation of Boötes. The redshift of the object is (z) 0.152[1] and it was first discovered in 1978 by astronomers who classified the object to be violently variable based on it displaying optical variations.[5]
OQ 530 is extremely variable, with several outbursts being displayed between 1915 and 1942. Its most prominent outburst was in 1938, when the object underwent a series of violent changes in brightness levels, reaching a maximum peak of 12.5 magnitude.[5] A brightening phase was detected on the first day of April 1990, followed by a faint state three days later.[6] It is also said that OQ 530 can be classified as a blazar due to its variability in the electromagnetic spectrum.[7]
The host galaxy of OQ 530 is a luminous disk galaxy[8][9] based on high resolution imaging, with its surface brightness profile resembling something like a lenticular galaxy.[10][11]
The radio structure of the galaxy is compact. When observed with Very Long Baseline Interferometry (VLBI), it is found to have a radio jet extending outwards by 40 milliarcseconds from the radio core and orientated at a position angle of 130° by southeast direction.[9][12] The jet structure is mainly complex with an outer component that broadens upon reaching a distance of four milliarcseconds. There are three other components and a compact radio core which displays signs of polarization.[13] A hotspot feature with a flat index spectrum is also present.[14] Another component is found west from the core with an elongated appearance. Faint radio emission is also surrounding it, indicating a halo feature is present.[12] A 456-day optical period is suggested for the galaxy, which might be accounted for by either a binary black hole or a helical jet.[15]
References
- 1 2 3 4 5 6 7 8 "NED Search results for OQ 530". NASA/IPAC Extragalactic Database. Retrieved 2025-11-23.
- ↑ Tagliaferri, G.; Ravasio, M.; Ghisellini, G.; Giommi, P.; Massaro, E.; Nesci, R.; Tosti, G.; Aller, M. F.; Aller, H. D.; Celotti, A.; Maraschi, L.; Tavecchio, F.; Wolter, A. (2003-03-01). "The BL Lacertae objects OQ 530 and S5 0716+714 - Simultaneous observations in the X-rays, radio, optical and TeV bands". Astronomy & Astrophysics. 400 (2): 477–486. arXiv:astro-ph/0301117. Bibcode:2003A&A...400..477T. doi:10.1051/0004-6361:20021916. ISSN 0004-6361.
- ↑ Barbieri, C.; Cristiani, S.; Romano, G. (April 1982). "A study of some compact extragalactic objects". The Astronomical Journal. 87: 616. Bibcode:1982AJ.....87..616B. doi:10.1086/113136. ISSN 0004-6256. Archived from the original on 2024-09-03.
- ↑ Zhang, Bing-Kai; Dai, Ben-Zhong; Zhang, Li; Cao, Zhen (2010-06-22). "Multi-band optical variability of BL Lac object OQ 530". Research in Astronomy and Astrophysics. 10 (7): 653–662. Bibcode:2010RAA....10..653Z. doi:10.1088/1674-4527/10/7/004. ISSN 1674-4527.
- 1 2 Miller, H. R. (July 1978). "1418+54: a new, violently variable BL Lacertae object". The Astrophysical Journal. 223: L67 – L70. Bibcode:1978ApJ...223L..67M. doi:10.1086/182730. ISSN 0004-637X.
- ↑ Carini, M. T.; Miller, H. R.; Goodrich, B. D. (August 1990). "The timescales of the optical variability of blazars. I - OQ 530". The Astronomical Journal. 100: 347. Bibcode:1990AJ....100..347C. doi:10.1086/115518. ISSN 0004-6256. Archived from the original on 2024-09-03.
- ↑ Ghosh, K. K.; Ramsey, B. D.; Sadun, A. C.; Soundararajaperumal, S. (March 2000). "Optical Variability of Blazars". The Astrophysical Journal Supplement Series. 127 (1): 11–26. Bibcode:2000ApJS..127...11G. doi:10.1086/313313. ISSN 0067-0049.
- ↑ G., Abraham, R.; M., McHardy, I.; S., Crawford, C. (October 1991). "Optical imaging of BL Lac host galaxies". Monthly Notices of the Royal Astronomical Society. 252. doi:10.1093/mnra (inactive 23 November 2025). ISSN 0035-8711. Archived from the original on 2022-11-07.
{{cite journal}}: CS1 maint: DOI inactive as of November 2025 (link) CS1 maint: multiple names: authors list (link) - 1 2 Massaro, E.; Mantovani, F.; Fanti, R.; Maesano, M.; Montagni, F.; Nesci, R.; Sclavi, S.; Tosti, G.; Venturi, T. (2004-09-01). "VLBI imaging and optical variability of the BL Lac object OQ 530 (B1418+546)" (PDF). Astronomy & Astrophysics. 423 (3): 935–942. Bibcode:2004A&A...423..935M. doi:10.1051/0004-6361:20040353. ISSN 0004-6361.
- ↑ "OQ 530". Frankfurt Quasar Monitoring. Retrieved 2025-11-23.
- ↑ Wurtz, Ron; Stocke, John T.; Yee, H. K. C. (March 1996). "The Canada-France-Hawaii Telescope Imaging Survey of BL Lacertae Objects. I. Properties of the Host Galaxies". The Astrophysical Journal Supplement Series. 103: 109. Bibcode:1996ApJS..103..109W. doi:10.1086/192271. ISSN 0067-0049.
- 1 2 P., Cassaro; C., Stanghellini; M., Bondi; D., Dallacasa; R., della Ceca; A., Zappalà, R. (November 1999). "Extended radio emission in BL Lac objects. I. The images". Astronomy and Astrophysics Supplement Series. 139 (3): 601–616. arXiv:astro-ph/9910209. Bibcode:1999A&AS..139..601C. doi:10.1051/aas:1999511. ISSN 0365-0138.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ↑ Gabuzda, D. C.; Pushkarev, A. B.; Cawthorne, T. V. (1999). "1999MNRAS.307..725G Page 725". Monthly Notices of the Royal Astronomical Society. 307 (3): 725. Bibcode:1999MNRAS.307..725G. doi:10.1046/j.1365-8711.1999.02683.x. Retrieved 2025-11-23.
- ↑ Baghel, Janhavi; Kharb, P; Hovatta, T; Gulati, S; Lindfors, E; S., Silpa (2023-10-17). "A Kpc-scale radio polarization study of PG BL Lacs with the uGMRT". Monthly Notices of the Royal Astronomical Society. 527 (1): 672–688. doi:10.1093/mnras/stad3173. ISSN 0035-8711.
- ↑ Liu, Yi; Li, Juan; Fan, Jun-Hui (June 2007). "A Possible 456-Day Optical Period of OQ 530". Chinese Journal of Astronomy and Astrophysics. 7 (3): 380–388. Bibcode:2007ChJAA...7..380L. doi:10.1088/1009-9271/7/3/07. ISSN 1009-9271.
