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Multi-frequency radio observations of BAL quasar
1045352
Magdalena Kunert-Bajraszewska
Torun Centre for Astronomy, N. Copernicus
University
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Features of BAL quasars

• very broad, blue-shifted absorption lines
  arising from
• - high-ionization transitions e.g. CIV
  l1549 ? HiBAL quasars
• - low-ionization transitions e.g. MgII
  l2800 ? LoBAL quasars
• -lack of radio emission, only radio-quiet
  objects
• - orientation hypothesis
• - all quasars have BAL region
• - the BAL features are visible along a
  particular line of sight,
• e.g. line of sight skimming the edge
  of the accretion disk or torus
• (Weymann et al., 1991, Elvis 2000)
• - the line of sight intersects an
  outflow or wind from the accretion
• disk (Murray et al., 1995)

(until 1997!)
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Radio-loud BAL quasars

• discoveries of radio-loud BAL quasars Becker et
  al., 1997 Becker et al., 2000
• 
  Menou et
  al., 2001 Brotherton et al., 1998

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Radio-loud BAL quasars

• BAL quasars as young or recently refuelled
  quasars

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BAL quasar 1045352
It is a HiBAL quasar. Willott et al.,
2002, MNRAS, 331, 435
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BAL quasar 1045352
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BAL quasar 1045352
- one of the most radio-luminous BAL quasars
logL 27.65 W Hz-1
1.4 GHz
log(R)(total) 5.2 (4.4) log(R)(core) 4.0
(3.2)
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Orientation of 1045352
log(Rv)log(Lcore) 0.4Mv 13.69 Wills
Brotherton, 1995, ApJ, 448, L81
5 GHz
log(Rv) 3.2
q 20
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Submillimetre emission 1045352
- hyperluminous infrared quasar (Willott et al.,
2002, MNRAS, 331, 435)
gt40
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BAL quasar 1045352
Summary

• it is a compact, young CSS object and it is
  consistent with
• the theory of BAL quasar evolution
• its radio emission is boosted
• the angle between the line of sight and the jet
  axis is very
• small, 20
• the submillimetre flux is dominated by
  synchrotron emission,
• the large dust mass does not coexist with BAL
  phenomenon
• - the radio structure can indicates intermittent
  activity