1. Radio-loud quasars in SDSS DR3
WEI-HAO BIAN (1, 2) , YAN-MEI CHEN (1 ), CHEN HU (3, 1), AND JIAN-MIN WANG(1)
(1) Key Laboratory for Particle Astrophysics, IHEP
(2) Department of Physics, Nanjing Normal University
(3) NAOC

2. Outline 1. Background: Lradio, MBH-σ* relation, SDSS 2. Sample
3. Measurements of MBH, σ*
4. MBH-σ* relation for RL and RQ quasars
5. Lradio dependence on MBH, Lbol/LEdd

3. 1.Background Origin of L_radio FRI Sy+LINER BLRG PG Q RL Q
Total radio luminosity
409 AGNs (169 S+169 Q+107RG+4 BL )
Xu C, et al., 1999, AJ, 118, 1169
Sikora, et al., astro-ph/
Total L_radio

4. Laor , 2000, ApJ, 543, L111
PG Q
Woo & Urry, 2002, ApJ, 581, L5
747 QSOs, 0<z<2.5

5. Ho, L. C. 2002, ApJ, 564, 120
Nuclea L_radio
Sikora et al. 2007, astro-ph/
Total L_radio

6. MBH-σ* relation
Bian & Zhao, MNRAS, 2004, 347, 607

7. SDSS
(1) ugriz, A, 3”, resolution (York et al. 2000)
(2)DR3: 1360 sq. deg. (Abazajian et al. 2003)
multidimensional SDSS color space. (Richards et al. 2002)
(3) 46,420 quasars in SDSS DR3 (Schneider et al. ‘03) Mi < -22 (70, 0.3, 0.7, -0.5)
(4) ROSAT, FIRST, NVSS, 2MASS

8. 2. RL and RQ Sample FIRST: 20 cm, peak flux density, α=-0.5
Radio loudness: f_5GHz/f_B, rest frame, k correction, R=10
z < 0.83: Hβ, [OIII], N=9573
914 detected by FIRST(598 RL+ 316 RQ), 7846 under flux limit (5721 RQ), 993 not covered by FIRST
SDSS spectral fitting => MBH

9. Methods: Galactic extinction: optical. IR Fe II: optical, UV
continuum: power law
Balmer continuum
Two sets of two-Gaussians: [O III] 4959, 5997
Three-Gaussians for Hβ 4861: NLR contribution

10. EW ([O III]) > 1.5A, σEW/EW<100% (luminosity bias)
RQ Total sample: 3466
RL sample: 306 with R, L_radio
RQ sample: 181 with R, L_radio

11. 3. MBH,σ*
f=0.75

12. 4. MBH-σrelation for RL+RQ QSOs
bad relation
RQ,RL
Uncertainties
0.5 dex
0.2 dex
optical continuum beaming effect
orientation of BLRs. Rc0.1

14. Luminosity bias: Monte Carlo trials
Mgal(i)
MBH(i,j)
L(i,j,k)
Galaxy mass function
QSOs luminosity function (Boyle et al., 2000)
(1)For samples, for different redshift bins, mean luminosity;
(2)Form QSOs luminosity function, choose L_cut, to make the mean luminosity of the kept QSOs (L > L_cut ) equal to the observed mean luminosity in different redshift bin.

16. 5.Lradio – Lbol/LEdd+MBH
Lacy, 2001, ApJ, 551, L17

17. Some comments
Radio luminosity: total/nuclear, FSQ,SSQ, FRI, FRII, BLRG, lobe-dominated QSOs
High z radio-quiet QSOs, radio-loud QSOs
Morphology difference: spiral RL, ellip RQ?
radio loud AGNs with larger SMBH, small SMBH?
NLS1s? Intermediate black hole?
Optical-select, radio-slect, X-select samples ??
complete sample!
Origins of L_radio, L_x, L_opt , jet, corona, ADAF, AD, AGN or starburst? FRI: Torus? infrared
Bimodality of radio loudness: sample, z, M_BH, metal

18. Thank you

20. 6. Lradio – Lx+MBH

21. Wang et al., 2006, ApJ, 645, 890
Weak dependence on M_BH
Gallo et al., 2003, MNRAS, 344, 60
Index: 0.7