Astronomy:QSO B0738+313

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QSO B0738+313
QSO B0728+313 imaged by SDSS.
Observation data (J2000.0 epoch)
ConstellationGemini
Right ascension 07h 41m 10.70s[1]
Declination+31° 12′ 00.22″[1]
Redshift0.630995[1]
Helio radial velocity189,186 km/s[1]
Distance5.729 Gly
Apparent magnitude (V)16.89
Apparent magnitude (B)17.02
Characteristics
TypeOpt.var; LPQ Sy1
Other designations
SDSS J074110.70+311200.2, 2MASS J07411070+3112002, KODIAQ J074110+311200, OI +363, NVSS J074110+311200, CRATES J0741+3112, TXS 0738+313, CoNFIG 005, IERS B0738+313, WMAP 107[1]

QSO B0738+313 or B2 0738+313, is a quasar located in the constellation of Gemini. It has a redshift of (z) 0.630[1] and it was first discovered as an astronomical radio source in 1968 by astronomers who designated it as OI 363.[2] The object has a radio spectrum appearing as flat making it a flat spectrum radio source but also a gigahertz-peaked spectrum source.[3][4]

Description

QSO B0738+313 is classified as a core-dominated radio-loud quasar with an X-ray luminosity of L0.1-10 KeV ~ 45 erg s-1. However, the polarization level of the object is low.[5][6] When observed by astronomers during R-band monitoring for four nights, its light curve was described as clear and almost sinusoidal with a few variations occurring on 21 January and 22 December 2006.[5] In its spectrum, the quasar displays two dampened Lyman-alpha absorption-line systems located at redshifts of (z) 0.0912 and (z) 0.2212, making these the lowest known absorption-line systems of its kind.[7][8] Two other faint companions were found, although not relating to the quasar.[9][10]

The quasar has a compact radio structure. When imaged with the Very Long Baseline Array at 15 GHz, it has two strong components. The first component is found weakly polarized at 0.5% with an inverted spectrum, while the other is polarized by around 1.5%. There are also weak and diffused radio lobes on each side of a much stronger radio component.[4] Very Long Baseline Interferometry imaging at six centimeters showed the structure has an unresolved radio core, a small surface brightness radio emission surrounding the source and a jet located in north-south which extends by 5 milliarcseconds.[11] This jet also displays a sharp bend at 45° towards the south-west direction with a knot at its bend.[6][12]

X-ray jet

An X-ray jet was discovered in QSO B0738+313 by Chandra X-ray observatory in March 2003.[6][13] Based on results, the X-ray jet has an extent of 200 kiloparsecs and is narrow. Observations also showed the X-ray jet is curving as well, which then follows the path of a radio structure south of the quasar and terminating at a hotspot located within the southernmost part of a radio lobe.[6] As it moves further from the core, the jet emission becomes fainter.[14] Astronomers found the X-ray emission is centered strongly towards the jet's direction, 3.8 arcseconds south from the radio core suggesting location of innermost components of the jet.[6]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "NED search results for QSO B0738+313". https://ned.ipac.caltech.edu/byname?objname=B0738+31&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Thompson, J. R.; Kraus, J. D.; Andrew, B. H. (October 1968). "Optical Identifications of Ohio Radio Sources with Peculiar Spectra". The Astrophysical Journal 154: L1. doi:10.1086/180255. ISSN 0004-637X. Bibcode: 1968ApJ...154L...1T. https://adsabs.harvard.edu/full/1968ApJ...154L...1T. 
  3. ↑ Andrew, B. H.; Kraus, J. D. (January 1970). "Radio Sources with Flat Spectra" (in en). The Astrophysical Journal 159: L45–L50. doi:10.1086/180475. ISSN 0004-637X. Bibcode: 1970ApJ...159L..45A. https://articles.adsabs.harvard.edu/pdf/1970ApJ...159L..45A. 
  4. ↑ 4.0 4.1 Stanghellini, C.; Dallacasa, D.; O'Dea, C. P.; Baum, S. A.; Fanti, R.; Fanti, C. (2001-10-01). "VLBA observations of GHz-Peaked-Spectrum radio sources at 15 GHz" (in en). Astronomy & Astrophysics 377 (2): 377–388. doi:10.1051/0004-6361:20011101. ISSN 0004-6361. Bibcode: 2001A&A...377..377S. https://www.aanda.org/articles/aa/pdf/2001/38/aa1554.pdf. 
  5. ↑ 5.0 5.1 Goyal, A.; Gopal-Krishna; Wiita, P. J.; Anupama, G. C.; Sahu, D. K.; Sagar, R.; Joshi, S. (August 2012). "Intra-night optical variability of core dominated radio quasars: the role of optical polarization" (in en). Astronomy and Astrophysics 544: A37. doi:10.1051/0004-6361/201218888. ISSN 0004-6361. Bibcode: 2012A&A...544A..37G. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Siemiginowska, Aneta; Stanghellini, Carlo; Brunetti, Gianfranco; Fiore, Fabrizio; Aldcroft, Thomas L.; Bechtold, Jill; Elvis, Martin; Murray, Stephen S. et al. (October 2003). "Chandra Discovery of an X-Ray Jet and Extended X-Ray Structure in the z = 0.63 Quasar B2 0738+313". The Astrophysical Journal 595 (2): 643–655. doi:10.1086/377369. ISSN 0004-637X. Bibcode: 2003ApJ...595..643S. https://iopscience.iop.org/article/10.1086/377369/fulltext/. 
  7. ↑ Lane, W. M.; Briggs, F. H.; Smette, A. (March 2000). "Detection of Warm and Cold Phases of the Neutral ISM in a Damped Lyα Absorber" (in en). The Astrophysical Journal 532 (1): 146–151. doi:10.1086/308578. ISSN 0004-637X. Bibcode: 2000ApJ...532..146L. https://ui.adsabs.harvard.edu/abs/2000ApJ...532..146L/abstract. 
  8. ↑ Rao, Sandhya M.; Turnshek, David A. (June 1998). "Discovery of z = 0.0912 and z = 0.2212 Damped Lyα Absorption-Line Systems Toward the Quasar OI 363: Limits on the Nature of Damped Lyα Galaxies" (in en). The Astrophysical Journal 500 (2): L115–L119. doi:10.1086/311411. ISSN 0004-637X. Bibcode: 1998ApJ...500L.115R. https://ui.adsabs.harvard.edu/abs/1998ApJ...500L.115R/abstract. 
  9. ↑ Hutchings, J. B. (October 1992). "[O IIand Continuum Structure in Radio-Loud QSOs to Z = 0.9"] (in en). The Astronomical Journal 104: 1311. doi:10.1086/116320. ISSN 0004-6256. Bibcode: 1992AJ....104.1311H. https://articles.adsabs.harvard.edu/pdf/1992AJ....104.1311H. 
  10. ↑ Torniainen, I.; Tornikoski, M.; Teräsranta, H.; Aller, M. F.; Aller, H. D. (June 2005). "Long term variability of gigahertz-peaked spectrum sources and candidates" (in en). Astronomy and Astrophysics 435 (3): 839–856. doi:10.1051/0004-6361:20041886. ISSN 0004-6361. Bibcode: 2005A&A...435..839T. https://www.aanda.org/articles/aa/pdf/2005/21/aa1886-04.pdf. 
  11. ↑ Stanghellini, C.; O'Dea, C. P.; Baum, S. A.; Dallacasa, D.; Fanti, R.; Fanti, C. (September 1997). "A VLBI study of GHz-peaked-spectrum radio sources. I. VLBI images at 6cm." (in en). Astronomy and Astrophysics 325: 943–953. ISSN 0004-6361. Bibcode: 1997A&A...325..943S. https://articles.adsabs.harvard.edu/pdf/1997A%26A...325..943S. 
  12. ↑ Kellermann, K. I.; Vermeulen, R. C.; Zensus, J. A.; Cohen, M. H. (April 1998). "Sub-Milliarcsecond Imaging of Quasars and Active Galactic Nuclei" (in en). The Astronomical Journal 115 (4): 1295–1318. doi:10.1086/300308. ISSN 0004-6256. Bibcode: 1998AJ....115.1295K. https://ui.adsabs.harvard.edu/abs/1998AJ....115.1295K/abstract. 
  13. ↑ Siemiginowska, Aneta; Stanghellini, Carlo; Brunetti, Gianfranco; Aldcroft, Tom L.; Bechtold, Jill; Elvis, Martin; Harris, D. E. (2003-10-01). "Discovery of X-ray jets in GPS sources". New Astronomy Reviews. The physics of relativistic jets in the CHANDRA and XMM era 47 (6): 467–469. doi:10.1016/S1387-6473(03)00073-3. ISSN 1387-6473. Bibcode: 2003NewAR..47..467S. https://www.sciencedirect.com/science/article/pii/S1387647303000733. 
  14. ↑ Siemiginowska, Aneta; Aldcroft, Thomas L.; Bechtold, Jill; Brunetti, Gianfranco; Elvis, Martin; Stanghellini, Carlo (2003). "X-ray Emission from Gigahertz Peaked/Compact Steep Spectrum Sources". Publications of the Astronomical Society of Australia 20 (1): 113–117. doi:10.1071/as02052. ISSN 1323-3580. Bibcode: 2003PASA...20..113S. https://adsabs.harvard.edu/full/2003PASA...20..113S. 



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