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Frontiers in Science #7 Co-evolution of Galaxies and Massive Black Holes in the Universe

Frontiers in Science #7 Co-evolution of Galaxies and Massive Black Holes in the Universe. Masayuki Akiyama (Astronomical Institute) 2009/11/25. Today’s lecture. Astronomy, Astrophysics : Big Picture, recent discoveries Astronomy methodology What are galaxies ?

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Frontiers in Science #7 Co-evolution of Galaxies and Massive Black Holes in the Universe

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  1. Frontiers in Science #7Co-evolution of Galaxies and Massive Black Holes in the Universe Masayuki Akiyama (Astronomical Institute) 2009/11/25

  2. Today’s lecture • Astronomy, Astrophysics : Big Picture, recent discoveries • Astronomy methodology • What are galaxies ? • Formation and evolution of galaxies and black holes • Future prospects

  3. Astronomy, Astrophysics : Big Picture We would like to understand our “origin”, where are we from ? Origin of the universe Origin of galaxies Origin of the solar system

  4. Astronomy, Astrophysics : Big Picture • Origin of the universe • What are “dark matter”, “Dark energy”. • Dark energy accelerate the expansion of the universe ! • Dark matter dominate the dynamics of galaxy groups • Dark energy dominate the dynamics of the current universe. • Overlapping particle physics. From http://www eso.org/~bleibund/papers/EPN/epn.html

  5. Astronomy, Astrophysics : Big Picture • Origin of the universe • What are “dark matter”, “Dark energy”. • Dark energy accelerate the expansion of the universe ! • Dark matter dominate the dynamics of galaxy groups • Dark energy dominate the dynamics of the current universe. • Overlapping particle physics. From http://map.gsfc.nasa.gov/media/080998/

  6. Astronomy, Astrophysics : Big Picture • 2. Origin of galaxies • First galaxies, reionization of the universe. • Growth histories of galaxies and super massive black holes • Physical interplay between galaxies and SMBHs ! From http://map.gsfc.nasa.gov/media/080998/

  7. The deepest image of the sky From http://www.spacetelescope.org/images/html/opo0428b.html

  8. Astronomy, Astrophysics : Big Picture • Origin of the solar system • Discovery of extra-solar planets ! • Search for “earth”-like planets around stars. • Search for biological marker in their light. • Overlapping earth science, biology in future. From http://keckobservatory.org/gallery/category/C2

  9. Astronomy, Astrophysics : Methodology How? • Basically we are “passive” • (of course we are active in research !)… • Receiving electromagnetic wave • Various wavelength covering • Radio – IR – Visible – UV – X-ray - Gamma-ray • (In future with gravitational wave ?) • Ground-based or Satellite • Depends on wavelength (= atmospheric transmittance and atmospheric emission) • Imaging or Spectroscopy • Imaging: deeper, color, shape, deeper than spe. • Spectroscopy: many “lines”, rich physical info.

  10. Astronomy, Astrophysics : Methodology How? http://www.naoj.org/Pressrelease/2004/06/01/index.html

  11. Ground-based telescope : Subaru telescope At the top of Mauna Kea in Hawaii

  12. Astronomy, Astrophysics : Methodology How? Radio Optical-NIR X-ray http://www.naoj.org/Pressrelease/2004/06/01/index.html

  13. Galaxies in the local universe • Local universe = around our Milky-Way galaxy (the Galaxy). • Our understanding of galaxies and SMBHs in the local universe. • Where are we ? • SMBHs at the centers of the galaxies.

  14. Where are we now ? Based on the observations of the distribution of hydrogen gas emission on sky, it is thought that Solar system belongs to a spiral galaxy like this and it is located in the middle of the disk-like structure.

  15. Super Massive Black Hole Milky-Way galaxy has 10^6 Msolar black hole at the center. How is it revealed ?

  16. Stellar motion at the center of the MW-galaxy From http://www.astro.ucla.edu/~ghezgroup/gc/pictures/index.shtml These images/animations were created by Prof. Andrea Ghez and her research team at UCLA and are from data sets obtained with the W. M. Keck Telescopes.

  17. Super Massive Black Hole in other galaxies ! From http://b50a.miz.nao.ac.jp/b_hole.html From http://www.ioa.s.u-tokyo.ac.jp/kisohp2/IMAGES/extragalactic.html Radio observation revealed 2.5x10^7 Msolar SMBH at the center of NGC4258

  18. M104 M(BH) = 10^8 Msolar

  19. M87 M(BH) = 10^9 Msolar

  20. Introduction SMBH-galaxy connection From STSci

  21. The relation holds for smaller systems ? HST/STIS observations of a star cluster G1 in the M31 (Andromeda galaxy). The velocity dispersion at the center is 30km/s and the black hole mass is estimated to be 18000Msolar. Gebhardt et al. 2005, ApJ, 634, 1093 Gebhardt et al. 2002, ApJ, 578, L41

  22. The mass ratio is M(galaxy-bulge) : M(BH) = 1000 : 1 The physical scale is, R(galaxy-bulge) ~ 10 kpc ~ 33,000 ly R(black-hole) ~ 10AU ~ 1.6x10^-6 ly R(black-hole dominate)~ 10-100pc ~ 33-330 ly

  23. Formation and Evolution • Formation and evolution of galaxies • = Statistical variation of physical properties as a function of cosmic time (redshift). • Basic understanding of the galaxy formation theory • Movie 1: structure formation in the cold-dark matter (CDM) universe • Movie 2: formation of a galaxy in the structure • Growth history of SMBHs.

  24. Formation and Evolution Formation and evolution of galaxies CDM model can explain the distribution of galaxies in the local universe Real galaxy distribution Simulated structure From 4d2u.nao.ac.jp From www.sdss.org

  25. Catch active SMBHs in the distant universe Some SMBHs actively accreting gas around them, they can be detected as “Active Galactic Nuclei” (“Quasar” is luminous sub population of AGNs). From http://www.nasa.gov/centers/goddard/news/topstory/2007/active_galaxy.html

  26. Catch active SMBHs in the distant universe This AGN-phase is thought to be the major growing-phase of the SMBHs. In the local universe the number is 1/1000 of the galaxies. From http://www.nasa.gov/centers/goddard/news/topstory/2007/active_galaxy.html

  27. Catch active SMBHs in the distant universe They can be found using strong X-ray or radio emission. Optical-NIR X-ray Radio http://www.naoj.org/Pressrelease/2004/06/01/index.html

  28. Catch active galaxies in the distant universe The distance (how far away from us = how far trace back the cosmic history) can be measured with “redshift” http://cas.sdss.org/dr7/pt/sdss/data/data.asp galaxies at 4-billion years ago galaxies in the local universe Wavelength (angstrom=0.1nm)

  29. SMBHs accretion history in the universe Number density of X-ray AGNs as a funtion of cosmic time (=redshift). Sample is divided by X-ray luminosity (brightness). Ueda, Akiyama et al. 2003, ApJ, 598, 886

  30. Estimate Black hole properties For each AGN, we can estimate properties of black holes using, Luminosity -> Mass accretion rate (growth rate) Line width (how fast the gas around BH is moving) -> Black hole mass

  31. Growth history of the SMBHs inferred from the number density Marconi et al. 2004, MNRAS, 351, 169

  32. Growth history of the SMBHs compared with that of galaxies Perez-Gonzalez et al. 2008, ApJ, 675, 234 Marconi et al. 2004, MNRAS, 351, 169

  33. Introduction: Importance of AGNs between z=1-3 Number density of X-ray AGNs Stellar mass density in galaxies • At z=1-3 Number density of AGNs ~10 times larger than in the local universe. Number density of galaxies ~10 times smaller than in the local universe. • Naïve argument: !! AGN should be 100 times more common among galaxies in the redshift range !! Ueda et al. 2003 Marchesini et al. 2008

  34. AGNs play more important role in distant galaxies K-selected 2<z<4 (~10billion years ago) galaxies from MOIRCS Deep Survey At 2<z<4,1/3 of the high stellar mass galaxies are detected in deep Chandra image (estimated hard X-ray luminosity L(2-10keV)=10^42-10^45erg/s, i.e. Seyferts and QSOs). Squares: X-ray selected galaxies Yamada, Kajisawa, Akiyama et al. 2009, ApJ, 699, 1354

  35. SMBH can be a key player Based on simple Cold-Dark-Matter galaxy formation model, more massive galaxies expected than observed. Formation of massive galaxies cannot be stopped without feed-back from AGNs (SMBHs growing process). Without AGN feedback With AGN feedback Without AGN feedback With AGN feedback Bower et al. 2006, MNRAS, 370, 645

  36. 近いFuture prospects 将来 From http://www.aoc.nrao.edu/evla/ From http://www.nro.nao.ac.jp/alma/J/photonews/index.html In the near future, new radio observatories, ALMA and E-VLA start observations. They can detect “gas” component of the distant galaxies. Such information is necessary to understand the galaxy evolution and SMBH growth in the cosmic history.

  37. 近いFuture prospects 将来 • What are the “seeds” of the SMBHs ? • Stellar mass black hole (~10Msolar) are too small http://chandra.harvard.edu/edu/formal/stellar_ev/

  38. Future Prospects Latter half of the 2010s will be a era of next generation “giants”. JWST6.5m (2013?) ＋ ground-based 30m telescope (2018?-). Low-background NIR deep imaging & spectroscopy with JWST and high-spatial resolution observation with 30m telescope with Adaptive Optics will resolve the physical properties of distant galaxies as we currently observe galaxies in the local universe.

  39. Why Astronomy Astrophysics ? We would like to understand our “origin”, where are we from ? Origin of the universe Origin of the galaxies Origin of the solar system If we do not explore these issues, why do human being need to exist ? I think…..

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