Multi-wavelength Studies on Microquasars and AGNs Xue-Bing WU (wuxb@pku.edu.cn) (Dept. of Astronomy, Peking University)
Dept. of Astronomy, PKU 1960, Astronomy division in geophysics department; undergraduate program 1979, Postgraduate program 1998, CAS-PKU Beijing Astrophysics Center 2000, Department of Astronomy established (Chair: Prof. Jiansheng Chen) April 2008, 9 faculty members + 30 postgraduates + 40 undergraduates Cosmology & Galaxy formation: Jiansheng Chen, Zu-Hui Fan AGN & BH: Fukun Liu, Xue-Bing Wu Planet, Star & ISM: Xiao-Wei Liu, Eric Peng, Hua-Wei Zhang Particle Astrophysics: Ren-Xin Xu Astrophysics Technology: Jian Zhang Emeritus: Guojun Qiao, Xinji Wu & Yuefang Wu
Outline Introduction Broadband SED of Microquasars Radio/X-ray correlation of AGNs CO line width and M-σ relation of quasars Summary Main Collaborators: R. Wang (PKU), Z. Y. Li (PKU); M. Z. Kong(HNU); W. Cui (Purdue), Y.Q. Xue (Purdue)
Mirabel (2004) 1. Introduction BH systems at different scale: Common ingredients: BH, accretion disk, jet,...
Multi-wavelength study of Microquasars Radio: Jet IR: Companion Opt: Companion X-ray: Accretion, Jet Gamma-ray: Jet (Xue, Wu & Cui 2008, MNRAS, 384,440)
Multi-wavelength study of AGNs Radio: Jet IR: Torus, Host-G., Jet UV/Opt: Accretion, Jet, Host-G. X-ray: Accretion, Jet Gamma-ray: Jet
2. Broadband SED of Microquasars XTE J1550-564 H 1743-322 (Xue, Wu & Cui 2008)
Jet Emission Corbel et al. 2002 Xue, Wu & Cui 2008
Radio/X-ray correlation in Microquasars Gallo, Fender & Pooley (2003) Xue & Cui (2007) L R L 0.7 X
Radio/X-ray correlation in Microquasars Xue, Wu & Cui (2008, MNRAS) Xue & Cui (2007, A&A) XTE J1550-564 =>Radio/X-ray correlation is frequency dependent and probably evolving with time
3. Radio/X-ray correlation of AGNs BH: Mass (M) Accretion flow: X-ray emission(l X ) Jet: Radio emission(l R ) (+L X in some cases) Any common relationship among L R, L X and M?
A fundamental plane of black hole activity (Merloni, Heinz, & Di Matteo, 2003, MNRAS) Supermassive BHs Stellarmass BHs
Test with a uniform sample from multi-wavelength surveys Problems of previous studies non-uniform samples Our sample 1 a relatively uniform, low-z radio and X-ray emitting broad line AGN sample selected from SDSS(DR1)- RASS-FIRST surveys (Wang, Wu & Kong 2006, ApJ, 645,890) including 76 radio-loud and 39 radio-quiet AGNs Our sample 2 725 SDSS(DR5)-RASS-FIRST broad line AGNs, including 498 radio-loud and 227 radio-quiet AGNs (Li, Wu, & Wang 2008, ApJ, submitted)
AGN black hole mass estimates based on SDSS optical spectra Virial law (Kaspi et al. 2000, 2005) R-L Hβ relation (Wu et al. 2004, A&A) McLure -Jarvis (2002) relation
Weak/no correlation with M For radio-quiet sources: Different slopes
Difference between radio-loud and radio-quiet AGNs in the radio--x-ray correlation
lg F ν -α r Heinz (2004, MNRAS) Scaling relations for scale-invariant cooled jets (both Lr & Lx are from jets): -α x N( γ ) γ P lg ν For canonical synchrotron spectrum of p=2,α r =0.5,α x =1 Consistent with our results for radio-loud AGNs!
Check with a larger sample of 725 SDSS(DR5)- RASS-FIRST AGNs (Li, Wu & Wang 2008) α r from FIRST & GB6
Radio -X-ray correlation for different X-ray origins (Yuan & Cui 2005, ApJ) Steep slope Flat slope RL AGN RQ AGN Consistent with our results obtained with a uniform AGN sample! (Radio-quiet AGN has a shallower slope than radio-loud AGN)
4. CO line width and M-σ relation of quasars Physics of the black hole - bulge relation: Close tie between BH and galaxy formation & evolution Feedback scenario (Silk & Rees 1998; King 2003, 2005; ) Two-direction starburst feedback model: Xu, Wu & Zhao (2007 ApJ, 664,198); Xu & Wu (2007 ApJ, 667,92) M BH σ 4 Tremaine et al. (2002)
M - σ relation of quasars For quasars: direct measurement of σ is difficult; σ=fwhm([oiii])/2.35 is usually adopted (Nelson 2000; Shields et al. 2003); galaxy growth is contemporaneous with black hole growth up to z=2~3 (however, Woo et al. 2008)
PG quasars with measured σ Dasyra et al. (2006, ApJ) Long integration near IR H-band spectroscopy with VLT
SDSS J1148+ 5251 (z=6.42) Walter et al. (2004) High-z Quasars Hi-z quasars, outliers? CO molecular line detected for a number of hi-z quasars (Solomon & Vanden Bout 2005 ARA&A) CO line width as a surrogate for σ (Shields et al. 2006 ApJ, 641, 683) σ=fwhm(co)/2.35 (Shields et al. 2006)
High-z Quasars Can we use σ=fwhm(co)/2.35?(no) A test with CO detected 33 Seyfert galaxies (Wu 2007, ApJ, 657, 177) A better correlation using inclination-corrected line width CO molecular disk coplanar with the galaxy disk (Heckman et al. 1989) Wu (2007, ApJ)
High-z Quasars Assuming inclination ~15 o for hi-z quasars, we can re-estimate σ values using the inclinationcorrected CO line width and study the M - σ relation at Hi-z Small inclinations (~15 o ) are also probably needed to explain the narrowness of CO line of hi-z quasars compared with the submillimeter galaxies (SMG) (Greve et al. 2005; Carilli & Wang 2006) Wu (2007, ApJ) Carilli & Wang (2006,AJ)
5. Summary Multiwavelength data collected with powerful instruments are crucial to probe the physics nature of AGN and Microquasars. Radio/X-ray correlation in Microquasars may not be universal, reflecting a complex accretion-jet physics. BH fundamental plane of AGNs seems independent on the BH mass, and is different for radio-loud and radioquiet AGNs. This may be related to different origins of X-ray emissions. Inclination-corrected CO line width can be taken as a surrogate for the stellar velocity dispersion. M-σ relation of nearby quasars is consistent with the local one. However, it s too early to say too much on the M-σ relation at hi-z universe.