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Multi-frequency radio observations of BAL quasar 1045+352

Multi-frequency radio observations of BAL quasar 1045+352. Magdalena Kunert-Bajraszewska. Toruń Centre for Astronomy, N. Copernicus University. Features of BAL quasars. very broad, blue-shifted absorption lines arising from:

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Multi-frequency radio observations of BAL quasar 1045+352

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  1. Multi-frequency radio observations of BAL quasar 1045+352 Magdalena Kunert-Bajraszewska Toruń Centre for Astronomy, N. Copernicus University

  2. Features of BAL quasars • very broad, blue-shifted absorption lines arising from: • - high-ionization transitions e.g. CIVl1549  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!)

  3. compact objects! wide range of orientation! FIRST J101614.3+520916 J1312+2319 VLA 1.4 GHz EVN 1.6 GHz compact BAL quasar first known BAL+FRII quasar Jiang & Wang, 2003, A&A, 397, L13 Gregg et al., 2000, ApJ, 544, 142 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

  4. „unification by time” Becker et al., 2000; Gregg et al., 2000 • evolutionary sequence: • compact BAL QSO  LoBAL+FRII  HiBAL+FRII < 105 years ! Radio-loud BAL quasars • BAL quasars as young or recently refuelled quasars;

  5. BAL quasar 1045+352 It is a HiBAL quasar.Willott et al., 2002, MNRAS, 331, 435

  6. MERLIN 5 GHz VLBA 1.7 GHz 2.1 kpc NE NW ~104 yr SE SW VLBA 5 GHz VLBA 8.4 GHz BAL quasar 1045+352

  7. radio-loudness parameter (Stocke et al., 1992): • definition: log(R*) > 1  radio-loud object log(R*)=log(f5GHz) – log(f2500Å) BAL quasar 1045+352 - 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)

  8. Orientation of 1045+352 log(Rv)=log(Lcore) + 0.4Mv – 13.69 Wills & Brotherton, 1995, ApJ, 448, L81 5 GHz log(Rv) ~ 3.2 q ~ 20°

  9. 30 GHz flux density measured with OCRA-p (Toruń 32-m telescope) • S=69mJy +/- 7 mJy, a = -1.01 30 GHz 4.85 GHz log S radio emission 1.25 mm Haas et al., 2006 850 mm and 450 mm Willott et al., 2002 log v Submillimetre emission 1045+352 - hyperluminous infrared quasar (Willott et al., 2002, MNRAS, 331, 435) >40%

  10. BAL quasar 1045+352 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;

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