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: - high-ionization transitions e.g. CIV 1549 HiBAL quasars - low-ionization transitions e.g. MgII 2800 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!)

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

compact objects! wide range of orientation!

J1312+2319FIRST J101614.3+520916

first known BAL+FRII quasarGregg et al., 2000, ApJ, 544, 142

VLA 1.4 GHz

EVN 1.6 GHz

compact BAL quasar

Jiang & Wang, 2003, A&A, 397, L13

Radio-loud BAL quasars

„unification by time”

Becker et al., 2000; Gregg et al., 2000

-BAL quasars as young or recently refuelled quasars;

< 105 years !

-evolutionary sequence: compact BAL QSO LoBAL+FRII HiBAL+FRII

BAL quasar 1045+352

It is a HiBAL quasar. Willott et al., 2002, MNRAS, 331, 435

BAL quasar 1045+352VLBA 1.7 GHzMERLIN 5 GHz

NE

SWSE

NW

VLBA 5 GHz VLBA 8.4 GHz

2.1 kpc

~104 yr

BAL quasar 1045+352

- one of the most radio-luminous BAL quasars: logL =27.65 W Hz-1;

log(R*)(total) ~ 5.2 (4.4)log(R*)(core) ~ 4.0 (3.2)

1.4 GHz

- radio-loudness parameter (Stocke et al., 1992):

definition: log(R*) > 1 radio-loud object

log(R*)=log(f5GHz) – log(f2500Å)

Orientation of 1045+352

log(Rv)=log(Lcore) + 0.4Mv – 13.69 Wills & Brotherton, 1995, ApJ, 448, L815 GHz

log(Rv) ~ 3.2

~ 20°

Submillimetre emission 1045+352

- 30 GHz flux density measured with OCRA-p (Toruń 32-m telescope)

S=69mJy +/- 7 mJy, = -1.01 30 GHz

4.85 GHzlo

g S

log v

850 m and 450 m Willott et al., 2002

1.25 mm Haas et al., 2006

radio emission

- hyperluminous infrared quasar (Willott et al., 2002, MNRAS, 331, 435)

>40%

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;