PKS 0537-441

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PKS 0537-441
Image of PKS 0537-441.jpg
The blazar PKS 0537-441
Observation data (J2000.0 epoch)
Constellation Pictor
Right ascension 05h 38m 50.361s
Declination −44° 05′ 08.939″
Redshift 0.896000
Heliocentric radial velocity 268,614 km/s
Distance 7.335 Gly
Apparent magnitude  (V)16.48
Apparent magnitude  (B)15.77
Characteristics
Type Blazar, BL Lac
Other designations
LEDA 2824444, IRAS F05373-4406, WMAP 148, 4FGL J0538.8-4405, 2E 1488, Cul 0537-441

PKS 0537-441 is a blazar [1] located in the constellation of Pictor. It has a redshift of 0.896 [2] and was discovered in 1973 by an American astronomer named Olin J. Eggen, who noted it as a luminous quasar. [3] This is a BL Lacertae object in literature because of its featureless optical spectra [4] [5] as well as both a possible gravitational microlensing [6] and a gravitationally lensed candidate. [7] Its radio source is found compact and is characterized by a spectral peak in the gigahertz range, making it a gigahertz-peaked spectrum source (GPS). [8]

Contents

Description

PKS 0537-441 is found violently variable on the electromagnetic spectrum at all frequencies, [9] and is a source of gamma ray emission. [10] [11] Between December 2004 and March 2005, it underwent intense activity showing more than 4 magnitudes in a V filter in 50 days and 2.5 in 10 days. [12] PKS 0537-441 is also known to display two flaring episodes, one in July 2009 and one in March 2010, with its gamma ray luminosity in the 0.1-100 GeV energy range reaching a peak value (2.6 x 1048 erg s−1) on 3-d timescales at the end of the month. [13] During its variability, PKS 0537-441 shows signs of both flux and color index variability on timescales. [14]

PKS 0537-441 contains a radio structure. The source is found to be core dominated on arcsecond scales with a secondary bright component separated by 7".2 at a 305° positional angle (PA). However, according to 2.3 GHz observations conducted by the Southern Hemisphere VLBI Experimental program (SHEVE), the radio structure has a 4.2 Jansky core with a measured diameter of 1.1 mas. There is a jetlike component, confirmed to be an asymmetric core-jet structure according to a 5 GHz Very-long-baseline interferometry imaging. This component is located north of the compact core. [15]

PKS 0537-441 shows gamma ray and optical oscillations. During its high state between August 2008 and 2011, the periodogram of its gamma ray light curve displays a peak reaching T0 ~ 280 days with significance of 99.7%. [16] A broad magnesium ionized emission line was also discovered at redshift (z) 0.885, implied to be a mini low ionization broad absorption-line quasar. This speculates PKS 0537-441 might be a binary quasar. [17]

References

  1. ↑ Pian, E.; Falomo, R.; Hartman, R. C.; Maraschi, L.; Tavecchio, F.; Tornikoski, M.; Treves, A.; Urry, C. M.; Ballo, L.; Mukherjee, R.; Scarpa, R.; Thompson, D. J.; Pesce, J. E. (2002-09-01). "Broad-band continuum and line emission of the gamma-ray blazar PKS 0537-441". Astronomy and Astrophysics. 392 (2): 407–415. arXiv: astro-ph/0207355 . Bibcode:2002A&A...392..407P. doi:10.1051/0004-6361:20020881. ISSN   0004-6361.
  2. ↑ Li, Xiao-Pan; Luo, Yu-Hui; Zhang, Li; Yang, Cheng; Yang, Hai-Tao; Cai, Yan (2016-10-14). "SimultaneousSwiftand Rapid Eye Mount telescope observations of the blazar PKS 0537–441". Monthly Notices of the Royal Astronomical Society. 464 (4): 3972–3990. doi: 10.1093/mnras/stw2652 . ISSN   0035-8711.
  3. ↑ Eggen, O. J. (November 1973). "A Very Large Light Pulse from the Object Identified with PKS 0537-441". The Astrophysical Journal. 186: L1. doi:10.1086/181344. ISSN   0004-637X.
  4. ↑ Bechtold, Jill; Dobrzycki, Adam; Wilden, Brenda; Morita, Miwa; Scott, Jennifer; Dobrzycka, Danuta; Tran, Kim-Vy; Aldcroft, Thomas L. (June 2002). "A Uniform Analysis of the Lyα Forest at z = 0–5. III. Hubble Space Telescope Faint Object Spectrograph Spectral Atlas" . The Astrophysical Journal Supplement Series. 140 (2): 143–238. arXiv: astro-ph/0111486 . doi:10.1086/342489. ISSN   0067-0049.
  5. ↑ Tanzi, E. G.; Barr, P.; Bouchet, P.; Chiappetti, L.; Cristiani, S.; Falomo, R.; Giommi, P.; Maraschi, L.; Treves, A. (December 1986). "Multifrequency observations of the Blazar PKS 0537-441 in a moderately active state". The Astrophysical Journal. 311: L13. doi:10.1086/184789. ISSN   0004-637X.
  6. ↑ Surpi, G. C.; Romero, G. E.; Vucetich, H. (1996-10-01). "The Gravitational Microlensing Scenario for PKS 0537--441". Revista Mexicana de Astronomía y Astrofísica. 32: 153–159. Bibcode:1996RMxAA..32..153S. ISSN   0185-1101.
  7. ↑ Stickel, M.; Fried, J. W.; Kuehr, H. (1988-11-01). "PKS 0537-441 : a gravitationally lensed blazar ?". Astronomy and Astrophysics. 206: L30 –L33. Bibcode:1988A&A...206L..30S. ISSN   0004-6361.
  8. ↑ 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. doi:10.1051/0004-6361:20041886. ISSN   0004-6361.
  9. ↑ Pian, E.; Romano, P.; Treves, A.; Ghisellini, G.; Covino, S.; Cucchiara, A. (July 2007). "Simultaneous Swift and REM Monitoring of the Blazar PKS 0537-441 in 2005". The Astrophysical Journal. 664: 106–116. arXiv: 0704.0958 . doi:10.1086/518469.
  10. ↑ Cannon, A. (2010-04-01). "Fermi LAT detection of increasing gamma-ray activity of blazars PKS 0537-441 and PKS 0301-243". The Astronomer's Telegram. 2591: 1. Bibcode:2010ATel.2591....1C.
  11. ↑ Lucarelli, F.; Striani, E.; D'Ammando, F.; Verrecchia, F.; Pittori, C.; Tavani, M.; Vercellone, S.; Del Monte, E.; Donnarumma, I.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Pacciani, L.; Soffitta, P.; Costa, E. (2010-02-01). "AGILE detects enhanced gamma-ray emission from the blazar PKS 0537-441". The Astronomer's Telegram. 2454: 1. Bibcode:2010ATel.2454....1L.
  12. ↑ Dolcini, A.; Covino, S.; Treves, A.; Palazzi, E.; Pian, E.; Molinari, E.; Chincarini, G.; Zerbi, F. M.; Rodonó, M.; Testa, V.; Tosti, G.; Vitali, F.; Antonelli, L. A.; Conconi, P.; Cutispoto, G. (2005-11-15). "Multiband photometry of the blazar PKS 0537-441: a major active state in December 2004–March 2005". Astronomy & Astrophysics. 443 (3): L33 –L36. arXiv: astro-ph/0510358 . doi:10.1051/0004-6361:200500198. hdl: 10550/16804 . ISSN   0004-6361.
  13. ↑ D’Ammando, F.; Antolini, E.; Tosti, G.; Finke, J.; Ciprini, S.; Larsson, S.; Ajello, M.; Covino, S.; Gasparrini, D.; Gurwell, M.; Hauser, M.; Romano, P.; Schinzel, F.; Wagner, S. J.; Impiombato, D. (2013-03-30). "Long-term monitoring of PKS 0537−441 with Fermi–LAT and multiwavelength observations". Monthly Notices of the Royal Astronomical Society. 431 (3): 2481–2492. arXiv: 1302.5439 . doi: 10.1093/mnras/stt344 . ISSN   1365-2966.
  14. ↑ Li, Xiaopan; Zhang, Li; Luo, Yuhui; Wang, Lisha; Zhou, Li (2015-04-02). "Colour variation of the BL Lacertae object PKS 0537–441". Monthly Notices of the Royal Astronomical Society. 449 (3): 2750–2758. doi: 10.1093/mnras/stv563 . ISSN   1365-2966.
  15. ↑ Shen, Z.Q.; Wan, T.S.; Moran, J.M.; Jauncey, D.L.; Reynolds, J.E.; Tzioumis, A.K.; Gough, R.G.; Ferris, R.H. (April 1998). "A 5 GHz Southern Hemisphere VLBI Survey Of Compact Radio Sources. II". The Astronomical Journal. 115: 1357–1370. arXiv: astro-ph/9803104 . doi:10.1086/300284.
  16. ↑ Sandrinelli, A.; Covino, S.; Treves, A. (2016-03-11). "Gamma Ray And Optical Oscillations In PKS 0537–441". The Astrophysical Journal. 820 (1): 20. arXiv: 1512.08801 . doi: 10.3847/0004-637x/820/1/20 . ISSN   0004-637X.
  17. ↑ Heidt, J.; Jäger, K.; Nilsson, K.; Hopp, U.; Fried, J. W.; Sutorius, E. (August 2003). "PKS 0537-441: Extended [O II] emission and a binary QSO?" (PDF). Astronomy & Astrophysics. 406 (2): 565–577. doi:10.1051/0004-6361:20030804. ISSN   0004-6361.
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