Conference Summary

1. Sorry, covering oral talks only… Conference Summary [SOC] Andrzej Zdziarski, Yasuo Tanaka, Ramesh Narayan, Richard Mushotzky, Felix Mirable,Jeff McClintock, Karen Leighly, Katsuji Koyama, Rob Fender, Chris Done, Thomas Boller, Roger Blandford, Kazuo Makishima These members have agreed to serve as the international advisory committee for the Grand-in-Aid for a Priority Research Area “New Development in BH Astronomy”

2. 《1》 Galactic BHB & ULX/IMBH [Q1A] Three basic issues of the WS [S.Mineshige] • Comparative study of various BHs; BHB-ULX-AGN • Beyond the standard accretion disk. • Formation and evolution of BHs. [Q1B] Have we understood BHB state classifications? • Spectra and variability --> mostly OK[R.Remillard, C.Done, A.Kubota]; low/hard state, high/soft/standard state, and….. • Compton dominated (very high, or anomalous) state • Slim disk may apply to some BHB in the outbutst peaks[A.Kubota], ULXs[A.Kubota, K.Ebisawa], and NLSy1[T.Kawaguchi]. [Q1C] Do we see phenomena on dynamical t.s.? • Yes, at last: msec flares from Cyg X-1[M.Gierlinski]; spectral changes across “shots” in Cyg X-1 and NLS1s [H.Negoro] • The 102-3 sec X-ray, K-band[A.Eckart],and radio[M.Miyoshi]flare from Sgr A* may be, too.

3. [Q1D] Are ULXs and the M82 X-1 IMBHs? • Yes, they are: From luminosity[A.Kubota, R.Mushotzky, T.Tsuru], QPO frequency[R.Moshotzky], close similarity to Galactic microQSOs that are not beamed toward us[A.Kubota], and lack of evidence for strong beaming[Mushotzky]. • IMBHs may form in dense stellar clusters[J.Makino], and/or as endpoints of pop-III stars [Y.Taniguchi] • At least some ULXs, with a very cool disk component, are likely to be so[J.Miller, A.Kong, R. Di Stefano]. However: • Unlikely: From evolutionary viewpoint, binary formation, fueling etc: the Cartwheel galaxy --> cannot invoke metal-poor 1st generation star[A. King]. • ULXs may instead be mildly beamed and mildly super-Eddington[A. King]. • Super-Eddington luminosity may be possible[F.Meyer]. • They may represent the highest-M and highest M-dot end of HMXBs[M.Gilfanov, K.Ebisawa].

4. GRO 1655-40 [Q1D] continued. --- Future work TBD 1. Examine the degree of X-ray beaming in XRBs. SS433 --> is there any evidence for radiation anisotropy besides relativistic Doppler with 0.26c? microQSOs: is there any evidence of X-ray bemaing? 2. Study the evolution of the most massive stars. 3. Search for transitions between Compton and standard-disk states. [Q1F] Is the “too hot disk” due to Kerr disk or slim disk? • Slim disk preferred[K.Ebisawa]. • GRO1655-40 and LMC X-3; they have very similar parmeters, but their disk temperatures are much different -- a hidden variable?

5. 《2》 Jets &Theoretical/Numerical [Q2A] Is the hard X-ray emission from BHB significantly contributed by jets? • Yes: because jets can do everything a corona can[H.Falcke]. • A good analogy between microQSOs and AGNs[F.Mirabel]. • Jets are ubiquitous, particularly at low mdot[A. Celotti]. • Low-mdot AGNs; tight Lr-Lx correlation[H.Falcke, E.Gallo]. However: • Hard X-rays in low-state BHBs must be disk-dominated, because the high-energy cutoff is too abrupt for a synchrotron break[A.Zdziarski]. • Disk-dominated AGN (Syferts, radio-quiet QSOs) and jet-dominated ones (radio-loud QSOs and Blazars) show distinct multi-band SEDs. A definite answer--> X-ray polarimetry[T. Takahashi, T.Tanimori]

6. [Q2B] Do we have a good understanding of stellar-mass BH formation? --> Probably No. • “BH formation in the dark”[F.Mirabel]. [Q2C] Which radiatively inefficient flow do we expect? • ADAF, ADIOS, CDAF, ETC, some realized in simulation[I.Igmenshuchev]; JDAF [H.Falcke]. Butno distinction yet. [Q2D] Is the BH spin related with jet activity? • AGN fundamental plane {Lr, Lx, mass}[E.Gallo]apparently rules out the freedom for a 3rd parameter, but the scatter around the plane may be due to the BH spin. • Disks around Kerr BHs are more strongly mangetized[J.Krolik]. • Jets emanating from ergo sphere around a Kerr BH[S.Koide]. General consensus:(Prograde) BH spin enhances jets. But:To what extent the jet activity depends on the BH spin? Then:How to observationally prove the jest vs. BH spin correlation?

7. [Q2F] Are magnetic fields essential in accretion? • Yes; to specify viscosity in non ad-hoc way; Good-bye to Alpha[I.Igumenshchev, J.Hawley, R.Matsumoto, J. Krolik, S.Koide];. • Beta>1 in disk and beta<1 in corona[J.Hawley], or the other way around when considering cooling[R.Matsumoto]. Consensus : Simple hydro calculation is inadequate. But: How to quantify the MHD simulation results? Comparing Mdot[R.Matsumoto, J.Krolik]--> calculate emissivity. [Q2E] Are jets leptonic or hadronic? • Still an open question[A.Celloti]. • Hadronic flow may be needed to transport energy[T. Takahashi]. [Q2G] Are jets magnetically-driven of pressure driven? • Jets are pressure driven (along the minimum-B region) but magnetically collimated[J.Hawley, answering to Q from S.Koide].

8. 《3》 SMBHs & BH formation/evolution Direct imaging [H.Hirabayashi, M.Miyoshi] [3A] Various efforts of probing SMBHs Dynamical[A.Eckert] Sgr A* M=3.6e6 Msun Spectroscopic [M.Kishimoto] SMBH Evidence, Mass, Mdot, Spin Environment,Fueling mechnanism, Outflow, etc Historical echo[K.Koyama] Time variation [P.Uttley, A.Eckart] New technology is important

9. [3B] Formation mechanism of SMBHs numerical observational The long-lasting issue since the Rees’s work [J.Makino]Runaway stellar mergers --> IMBHs --> Growth due to accretion --> Mergers in the GC region --> SMBHs [Y.Taniguchi]Pop III star (z~25) --> IMBH (~100 Msun) --> Growth of SMBH (z~8) --> Magorrian phase [W.Duschl]Galaxy-galaxy merger --> SMBHs and fueling [M.Umemura]ULIRG -> photon drag --> fueling and growth of SMBH-- > QSO --> BH-mass vs. bulge correlation theoretical theor+num ☆ What provides seed BHs? Pop III or runaway stellar mergers? ☆ Does the seed BH grow via accretion? If so, how to fuel it, and how the object appear observationally? ☆ Does the seed BH grow via mergers? If so, any evidence? How to extract angular momentum-- via GW, or by launching helical Alfven waves?

10. [3C] Solution to the CXB puzzle [Y.Ueda] • ASCA deep survay + opt.ID + Chandra.. • Major contributor to CXB; Lx~1043.8, z~0.6 Then: • Are the results consistent with general scenario of AGN formation and evolution? • Future hard X-ray deep survey, with ASTRO-E2 HXD to be launched in Jan/Feb. 2005

11. Ton S180 with ASCA [Q4C] How to interpret the pronounced variability? 《4》NLS1s & Key Evidence & GRB Consensus: low-M and high-mdot AGNs, but mysterious [Th.Boller, K.Leighly, Y.Tanaka, H.Negoro, M.Guzainazzi] [Q4A] What produces the soft excess? • A standard disk model can reproduce spectral shape, but too hot, and the apparent disk radius changes with kT kept constant. • Compton [e.g.,Vaughan et al], or slimm disk [e.g.Mineshige]? • PL×exponential -- Comptonized (VH) state [M.Murashima]? [Q4B] The nature of Γ〜2.5 PLwith a sharp Fe-K edge? • The PL slope close to those seen in H or VH state of BHB. • The edge feature unlikely to be reflection (no Fe-K emission line); due to partial covering with Fe-rich matter [Tanaka]? • Complex spectral changes [M.Guzainazzi] • Spectral changes across the shot -- similar to Cyg X-1 [H.Negoro] • QPO-like behavior of periods ~104-5 sec [Q4D] How about optical properties? [K.Leighly]

12. [Q4E] What is the current status of the Fe-K lines? • The broad Fe-K line, discovered with ASCA, appears to be robust, but is less variable than the continuum [K.Iwasawa]. • The lime profile may be explained as relativistic broadening in accretion disks, but models are important [K. Beckwith]. • The lack of line variability may be explained by a Kerr disk + a ring-shaped source above it with varying heitht [G.Miniutti]. But: what is the reality of the “illuminating ring” ? [Q4F] Other key physical evidence for BHs • Are BHCs really BHs? --> Yes! Based on Type I butsts, quiescence luminosity, spectral color, etc. [R.Narayan]. • Search for MeV thermal signals vua pion production [T.Tanimori] [GRB] [N,Kawai, A.Beloborov, K.Nommoto] • Wonderful coordination among HETE-2, robotic telescopes, and theories.

13. Thank all the conference participants, including the invited speakers in particular. Our knowledge horizon has expanded and swallowed all of us! Thank LOC S. Mineshige, T. Tanimori, T. Tsuru, H. Matsumoto, H. Kubo, K. Miuchi, Secretaries andGraduate Studentsat Yukawa Institute and Cosmic-Ray Laboratory of Kyoto University