Center for Astrophysics Third International ASTROD Symposium on Laser Astrodynamics, Space Test of Relativity and Gravitational-Wave Astronomy Beijing, China, July 14 - 16, 2006 Supermassive black hole mass J.H. Fan, J.S. Zhang Center for Astrophysics Guangzhou University

Outline Introduction Method Discussion Summary

INTRODUCTION Observations show that some sources with particular observational properties RBLs LBLs 1) BL Lacertae objects--BLs, XBLs HBLs 2) Flat Spectrum Radio Quasars—FSRQs

What is a BL Lac Object? RBLs LBLs BL Lacertae objects XBLs HBLs From surveys there are radio selected BL lacertae objects and X-ray selected objects. From SED, BL Lacertae objects can be divided into HBL (high-energy peaked ) and LBLs ( low-energy peaked (LBL) respectively (Giommi & Padovani 1994; Padovani & Giommi 1995).

What is an FSRQ? Confusion Optically violently variable quasars--OVVs, (m>1.0m) ( Penston & Cannon,1970) Kinman (1975) OVVs tend to have steep optical spectra and be associated with compact variable radio sources which have flat radio spectra at GHz frequencies. Highly polarized quasars--HPQs ( p>3.0%), (Moore and Stockman 1981, ApJ, 243 ) , 45% Core-dominated quasars--CDQs ( R = Lc/Le > 1.0) ….etc Confusion

INTRODUCTION Objects with one of the above properties BLAZARS The term “blazar” was coined, half in jest, by Ed Speigel at the first conference on BL Lac objects in Pittsburg. BLAZARS (BL Lacs and FSRQs) extragalactic objects with rapid variability, high luminosity, high and variable polarization, or superluminal motions.

AGN Model 窄线区 宽线区 喷流 黑洞 吸积盘 =(,) Fob=pFin Standard Model for Blazar 活动星系核的标准模型

Supermassive BH There a super-massive black hole at the center with an accretion disk surrounding the black hole. The charged particles within the accretion disk are ejected at near the speed of light, forming two relativistic jets perpendicular to the plane of the accretion disk. The central black hole is the central engine. It plays an important role on the emission of blazars.

BL & FSRQs Similarity??? Difference ???

Relationship between BLs and FSRQs 1. Gravitational Effect, BLs are the gravitational images of FSRQs 2. Evolution. FSRQs with emission line evolve into BLs 3. Different Classes 4. Different angles to the line of sight 5. Other… Nobody can ignore the difference and similarity between BL and FSRQs.

Their relationship has drawn much attention (e.g., Sambruna et al. 1996; Fan 2002;Ciaramella et al.2004) The central black hole is very important, we try to determine the black hole masses, and investigate the difference of BH masses between them.

Mass Determination The broad-line width technique (Wandel & Yahil 1985) Based on the assumption that Hβline velocity widths are gravitationally induced and orbit with Keplerian velocities. Using the Hβluminosity to estimate the distance of the broad-line region (BLR) from the central source.

Mass Determination 2. The reverberation mapping technique (e.g. Wandel et al. 1999) The size of the broad line region (BLR) can be measured from the time delay between the flux variations of the continuum and the emission lines of AGNs. The black hole mass is then estimated using the Virial theorem from the BLR size and the characteristic velocity (determined by the full width at half-maximum (FWHM) of the emission line). So far, reverberation studies have yielded the black hole masses of about 20 Seyfert 1 galaxies and 17 nearby bright quasars.

Our considerations *: The above methods are good for the nearby objects since we want to do observation of their emission clouds’ motion. For high redshift sources, they are not valid. 1 The central black hole masses of high redshift. Blazars have high redshifts. 2. Difference in BH masses between BL and FSRQs 3. We choose gamma-ray loud blazars

New Method--astro-ph/0503699

Considerations The -ray observations suggest that the -rays are strongly boosted -ray emission suggests that the optical depth of - pair production should not be larger than unity. The observed short-time scale gives some information about the size of -ray emitting region. The -ray emissions are from a cone with a solid angle Ω

Equation—1 Based on a paper by Becker & Kafatos(1995)

Equation-2 Based on the time Scale T is in Days

Equation-3 Based on the beamed and unisotropic -ray Luminosity

Variables

Observations

Equation-4 Based on the minimum of Equation 1

Equations ………….. Eq (A) …………….. Eq (B) ……….. Eq (C) ………….. Eq (D)

Sample 23 -ray loud blazars 11 BLs 12 FSRQs

Calculation Results

Mass Distribution for BL (solid line) and FSRQs (dotted line)

Results log M|BL= (8.13+/-0.46) solar masses log M|Q = (8.06+/-0.54) solar masses

Comparison For 0420-014 1. Log M = 8.0--- 8.2 Our Results Log M = 9.0 Woo & Urry 2002, ApJ

Comparison For 3C 273 1. Log M = 7.90--- 8.07 Our Results Wang et al. 1996, ApJ

Comparison For 3C 279 1. Log M = 7.6---8.0 Our result Log M = 8.43 Woo & Urry 2002, ApJ Log M = 8.4 Xie et al. 2005, PASJ

Comparison For 1510-089 1. Log M = 8.40--- 8.6 Our Results Woo & Urry, 2002, ApJ Log M = 8.1 Xie et al. 2005, PASJ

Conclusions 1. Masses are in the range of 10^(7-9) solar masses. Our results are consistent with others’. The is no BH mass difference between BL and FSRQS BH Masses do not play an important role in the evolution between BLs and FRSQs if there is an evolution from FSRQs to BLs Or there is no evolution between BLs and FSRQs.

Thanks a lot

M87 3*109 Yuan Y.F. et al. 2005, in this proceeding NGC Kalpha to estimate mass (Yuan Y.F. et al. 2005, in this proceeding)