1 / 10

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:

raven-larsen
Download Presentation

Multi-frequency radio observations of BAL quasar 1045+352

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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;

More Related