PKS 0048-097

Last updated
PKS 0048-097
PKS 0048-097 SDSS.png
SDSS image of PKS 0048-097
Observation data (J2000.0 epoch)
Constellation Cetus
Right ascension 00h 50m 41.311s [1]
Declination −09° 29′ 05.210″ [1]
Redshift 0.634000 [1]
Heliocentric radial velocity 190,068 km/s [1]
Distance 6.073 Gly
Apparent magnitude  (V)16.22
Apparent magnitude  (B)16.39
Characteristics
Type Opt.var. BLLAC [1]
Other designations
6dF J0050413-092905, 2MASS J00504130-0929051, LEDA 2822375, OB -080, NVSS J005041-092906, PHL 0856, WMAP 077, VLSS J0050.6-0929, SDSS J005041.30-092905.1, FBQS J0050-0929, MRC 0048-097 [1]

PKS 0048-097 is a BL Lacertae object located in the western region of the Cetus constellation. The redshift of the object is (z) 0.635 based on measurement of emission lines, [2] estimating it to be 6 billion light-years from Earth. [1] It was first discovered by astronomers during the Parkes Observatory radio sources survey in 1966. [3] The source is known to be variable based on its flux density and is located northeast from NGC 246, a planetary nebula. [4] [5]

Contents

Description

PKS 0048-097 is optically violently variable. When observed during photometric monitoring on January 18 in 2001, the source fluctuated in brightness, increasing by 0.38 magnitudes within 45 minutes then decreasing its brightness before increasing once more. [6] In addition, the object has displayed several flaring periods with a large optical outburst occurring in June 2009. [7] It was noted to be in a moderate high optical state of 15.5 magnitudes with its energy distribution estimated to be from 1014 reaching up to 2.5 x 1015 Hz. [8] Long-term variations were observed via optical wavelengths of almost 3 magnitudes with a flickering period of 8 magnitude less than one week. [9] A near-infrared flaring period was detected in January 2011. [10]

The radio structure of PKS 0048-097 is compact. Based on observations, the source displays a radio spectrum with a turnover frequency at 10 GHz but becomes inverted to 22 GHz when its activity becomes minimum. [11] Imaging by Very Long Baseline Interferometry showed there is a jet towards the southeast direction with a position angle of 165°, a polarized jet component and a weakly polarized radio core. [12] Extended radio emission from the core is seen in the center of both a possible hotspot and a diffused structure. [13] Very Large Array observations found an extended secondary component holding a flux density of 0.05 ± 0.01 Jansky. [14]

PKS 0048-097 is classified as a polarization rotator. It has polarization variations occurring at the time scale of five years, which in turn, are associated with a component described as slow varying opposed to outbursts on short time scales. The polarization position angle is also noted as stable at 90° ± 1.5° without any signs of major amplitude changes in this eight year observation period. A rotation of 260° was reported, beginning before the outburst in 1974-75 and ending as soon the outburst reached a peak of 8 GHz. Further observations detected its spectrum elevating at all frequencies suggesting the outburst was broadband. [15]

The host galaxy of PKS 0048-097 is undetected, but is assumed to be an elliptical galaxy. [16] It has a faint companion located 2.5 arcseconds east from its nucleus appearing as both resolved and associated together with the source based on imaging. [17]

A quasi-periodicity modulation was found for PKS 0048–097. Based on light curve data observations, the periodicity is estimated between 350 and 600 days. The structure is also known to vary dramatically with its jet direction shifting in position angle from -160° south-westwards to +160° south-eastwards. [18]

References

  1. 1 2 3 4 5 6 7 "NED search results for PKS 0048-097". NASA/IPAC Extragalactic Database. Retrieved 2025-07-27.
  2. ↑ Landoni, M.; Falomo, R.; Treves, A.; Sbarufatti, B.; Decarli, R.; Tavecchio, F.; Kotilainen, J. (July 2012). "On the redshift of the bright BL Lacertae object PKS 0048-097". Astronomy & Astrophysics. 543: A116. arXiv: 1205.1215 . Bibcode:2012A&A...543A.116L. doi:10.1051/0004-6361/201219114. ISSN   0004-6361. Archived from the original on 2022-06-20.
  3. ↑ Shimmins, A. J.; Day, G. A.; Ekers, R. D.; Cole, D. J. (December 1966). "The Parkes catalogue of radio sources, declination zone 0° to -20°". Australian Journal of Physics. 19 (6): 837. Bibcode:1966AuJPh..19..837S. doi:10.1071/PH660837. ISSN   0004-9506.
  4. ↑ Ross, Hugh N. (May 1970). "Verification of Radio Variability of the Galaxy PKS 0048–09". Nature. 226 (5244): 431. Bibcode:1970Natur.226..431R. doi:10.1038/226431a0. ISSN   1476-4687. PMID   16057303.
  5. ↑ "PKS 0048-097". Frankfurt Quasar Monitoring. Retrieved 2025-07-27.
  6. ↑ Xie, G. Z.; Zhou, S. B.; Dai, B. Z.; Liang, E. W.; Li, K. H.; Bai, J. M.; Xing, S. Y.; Liu, W. W. (February 2002). "Photometric monitoring of 12 BL Lacertae objects". Monthly Notices of the Royal Astronomical Society. 329 (4): 689–699. Bibcode:2002MNRAS.329..689X. doi: 10.1046/j.1365-8711.2002.04952.x . ISSN   0035-8711.
  7. ↑ Wierzcholska, Alicja (August 2015). "Nine years of multi-frequency monitoring of the blazar PKS 0048-097: spectral and temporal variability". Astronomy and Astrophysics. 580: A104. arXiv: 1604.05642 . Bibcode:2015A&A...580A.104W. doi:10.1051/0004-6361/201525649. ISSN   0004-6361.
  8. ↑ Falomo, R.; Bouchet, P.; Maraschi, L.; Tanzi, E. G.; Treves, A. (December 1988). "Quasi-simultaneous Ultraviolet Optical and Infrared Observations of the BL Lacertae Object PKS 0048-09". The Astrophysical Journal. 335: 122. Bibcode:1988ApJ...335..122F. doi:10.1086/166910. ISSN   0004-637X.
  9. ↑ Lepine, J. R. D.; Braz, M. A.; Epchtein, N. (August 1985). "Near infrared and radio observations of active galactic nuclei". Astronomy and Astrophysics. 149: 351–356. Bibcode:1985A&A...149..351L.
  10. ↑ "NIR flaring of the blazar PKS0048-097". The Astronomer's Telegram. Retrieved 2025-07-27.
  11. ↑ Torniainen, I.; Tornikoski, M.; Teräsranta, H.; Aller, M. F.; Aller, H. D. (2005-06-01). "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.
  12. ↑ Gabuzda, D. C.; Pushkarev, A. B.; Cawthorne, T. V. (August 1999). "The lambda=6cm VLBI polarization structure of nine BL Lacertae objects". Monthly Notices of the Royal Astronomical Society. 307 (3): 725–736. Bibcode:1999MNRAS.307..725G. doi: 10.1046/j.1365-8711.1999.02683.x . ISSN   0035-8711.
  13. ↑ Cassaro, P.; Stanghellini, C.; Bondi, M.; Dallacasa, D.; della Ceca, R.; Zappalà, R. A. (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.
  14. ↑ Wardle, J. F. C.; Moore, R. L.; Angel, J. R. P. (April 1984). "The radio morphology of blazars and relationships to optical polarization and to normal radio galaxies". The Astrophysical Journal. 279: 93–111. Bibcode:1984ApJ...279...93W. doi:10.1086/161868. ISSN   0004-637X.
  15. ↑ O'Dea, C. P.; Dent, W. A.; Balonek, T. J.; Kapitzky, J. E. (November 1983). "2.7-GHz observations of four radio polarization rotators". The Astronomical Journal. 88: 1616–1625. Bibcode:1983AJ.....88.1616O. doi:10.1086/113451. ISSN   0004-6256.
  16. ↑ Kotilainen, Jari K.; Falomo, Renato; Scarpa, Riccardo (August 1998). "The host galaxies of BL Lac objects in the near-infrared". Astronomy and Astrophysics. 336: 479–489. arXiv: astro-ph/9805295 . Bibcode:1998A&A...336..479K. ISSN   0004-6361.
  17. ↑ Falomo, R. (November 1996). "Host galaxy and close environment of BL Lacertae objects". Monthly Notices of the Royal Astronomical Society. 283 (1): 241–250. doi: 10.1093/mnras/283.1.241 . ISSN   0035-8711.
  18. ↑ Kadler, M.; Hughes, P. A.; Ros, E.; Aller, M. F.; Aller, H. D. (2006-08-31). "A quasi-periodic modulation of the radio light curve of the blazar PKS B0048-097". Astronomy & Astrophysics. 456 (2): L1 –L4. arXiv: astro-ph/0605587 . doi:10.1051/0004-6361:200600026. ISSN   0004-6361.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.