Exploring Junctions of Filamentary Structure with SUZAKU Hajime Kawahara (TMU)

Slides:

Advertisements

Similar presentations

Florent Rostagni 1.  Context  Sample  Algorithm for detection and classification  Star formation  X-ray – optical study  Perspectives - Conclusion.

Advertisements

Dark Energy BAO Intensity Mapping T. Chang, UP, J. Peterson, P. McDonald PRL 100, (March 5, 2008) UP, L. Staveley-Smith, J. Peterson, T. Chang arXiv:

Front X-ray Studies of Galaxies and Galaxy Systems Jesper Rasmussen Ph.D. Defence Astronomical Observatory, Univ. of Copenhagen 17th March 2004.

Is there a correlation between the presence of bent radio sources and the X-ray environment ? Oozeer N HartRAO 2010 South African SKA Postgraduate Bursary.

Deep Chandra and XMM-Newton Observations of NGC 4472 R. P. Kraft, S. W. Randall, W. R. Forman, P. E. J. Nulsen, C. Jones, A. Bogdan, M. J. Hardcastle,

The Radio/X-ray Interaction in Abell 2029 Tracy Clarke (Univ. of Virginia) Collaborators: Craig Sarazin (UVa), Elizabeth Blanton (UVa)

24-28 October 2005 Elena Belsole University of Bristol Distant clusters of Galaxies Ringberg Workshop X-ray constraints on cluster-scale emission around.

X-ray and Radio AGN in Coma Cluster Progenitors Quyen Nguyen Hart University of Colorado at Boulder, Center for Astrophysics and Space Astronomy Collaborators.

Galaxies Cluster formation : Numerical Simulations and XMM Observations JL Sauvageot *, Elena Belsole *,R.Teyssier *, Herve Bourdin + Service d'Astrophysique.

Hamburg, 18 September 2008 LOFAR Wokshop1/44 Thermal and non-thermal emission from galaxy clusters: X-ray and LOFAR observations Chiara Ferrari Observatoire.

Swift/BAT Hard X-ray Survey Preliminary results in Markwardt et al ' energy coded color.

Dark Halos of Fossil Groups and Clusters Observations and Simulations Ali Dariush, Trevor Ponman Graham Smith University of Birmingham, UK Frazer Pearce.

Taotao Fang UC Berkeley Collaborator: R. Croft, W. Sanders, J. Houck, R. Dave, N, Katz, D. Weinberg, L. Hernquist Soft X-ray Emission from the Warm-Hot.

15 The Milky Way More than just a candy bar.. 15.

Evolution of Luminous Galaxy Pairs out to z=1.2 in the HST/ACS COSMOS Field Jeyhan Kartaltepe, IfA, Hawaii Dave Sanders, IfA, Hawaii Nick Scoville, Caltech.

Searching for the large-scale hot gaseous Galactic halo --Observations confront theories Yangsen Yao in collaboration with Michael A. Nowak Q. Daniel Wang.

Molecular Hydrogen in the outer filaments surrounding NGC 1275 Nina Hatch CS Crawford, RM Johnstone, AC Fabian IOA, Cambridge.

HI in Galaxies at Redshifts 0.1 to 1.0: Current and Future Observations Using Optical Redshifts for HI Coadding Deep Surveys of the Radio Universe with.

Calibration of the SDSS Spectroscopic Line Width Scaling Relations Calibration of the SDSS Spectroscopic Line Width Scaling Relations Barbara Catinella.

Suzaku search for evidence of sterile neutrinos in the X-ray spectra of dwarf spheroidal galaxies Michael Loewenstein, Alexander Kusenko (UCLA), Peter.

Evolution of Luminous Galaxy Pairs out to z=1.2 in the HST/ACS COSMOS Field Jeyhan Kartaltepe, IfA, Hawaii Dave Sanders, IfA, Hawaii Nick Scoville, Caltech.

The Evolution of X-ray Luminous Groups Tesla Jeltema Carnegie Observatories J. Mulchaey, L. Lubin, C. Fassnacht, P. Rosati, and H. Böhringer.

Inflation, Expansion, Acceleration Two observed properties of the Universe, homogeneity and isotropy, constitute the Cosmological Principle Manifest in.

Dynamical state and star formation properties of the merging galaxy cluster Abell 3921 C. Ferrari 1,2, C. Benoist 1, S. Maurogordato 1, A. Cappi 3, E.

How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray.

Luminosity and Mass functions in spectroscopically-selected groups at z~0.5 George Hau, Durham University Dave Wilman (MPE) Mike Balogh (Waterloo) Richard.

X-ray Surveys with Space Observatory Khyung Hee University Kim MinBae Park Jisook.

The Evolution of Quasars and Massive Black Holes “Quasar Hosts and the Black Hole-Spheroid Connection”: Dunlop 2004 “The Evolution of Quasars”: Osmer 2004.

Wide Field Imagers in Space and the Cluster Forbidden Zone Megan Donahue Space Telescope Science Institute Acknowledgements to: Greg Aldering (LBL) and.

1 st Subaru Intl. Conference Subaru Weak Lensing Study of Merging Clusters of Galaxies Reference: Okabe & Umetsu 2008, PASJ in press (astro-ph/ )

Suzaku, XMM-Newton and Chandra Observations of the Central Region of M 31 Hiromitsu Takahashi (Hiroshima University, Japan) M. Kokubun, K. Makishima, A.

Summary(3) -- Dynamics in the universe -- T. Ohashi (Tokyo Metropolitan U) 1.Instrumentation for dynamics 2.Cluster hard X-rays 3.X-ray cavities 4.Dark.

The Warm-hot Gaseous Halo of the Milky Way Smita Mathur The Ohio State University With Anjali Gupta, Yair Krongold, Fabrizio Nicastro, M. Galeazzi.

1 The XENIA mission The XENIA mission Cosmic chemical evolution of baryons Dieter H. Hartmann C. Kouveliotou, M. C. Weisskopf, J.W. den Herder, L. Piro,

Feb/19/2008 A Demography of Galaxies in Galaxy Clusters with the Spectro-photometric Density Measurement. Joo Heon Yoon 윤주헌 Sukyoung Yi 이석영 Yoon et al.

Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.

A look at XMM slew data Richard Saxton, Andrew Read, Michael Freyberg, Bruno Altieri, Puri Munuera.

Chandra Observation of the Failed Cluster Candidate K. Hayashida, H. Katayama (Osaka University), K. Mori (Penn State University), T.T. Takeuchi.

MASS-TO-LIGHT FUNCTION: from Galaxies to Superclusters MASS-TO-LIGHT FUNCTION: from Galaxies to Superclusters Celebrating Vera Rubin Neta A. Bahcall Princeton.

Wide-field Weak Lensing Mass Reconstructions of Merging Galaxy Clusters Brett Ragozzine, Douglas Clowe Ohio University, Department of Physics & Astronomy,

Main-Cluster XIS0XIS1XIS3 Weighted mean Chandra Figure 2 : XIS spectra of the main-cluster XIS keV Main-Cluster Sub-Cluster Search for Bulk Motion.

X-ray Astronomy School 2002 Clusters of Galaxies (and some Cosmology) Scientific and Data Analysis Issues Keith Arnaud NASA/GSFC and UMCP.

USING LOW POWER RADIO GALAXIES AS BEACONS FOR CLUSTERS AT 1

Group Evolution Multi-wavelength Survey (GEMS) Duncan A. Forbes Centre for Astrophysics & Supercomputing, Swinburne University.

The morphology of clusters of galaxies: the cluster-galaxy connection Irini Sakelliou Birmingham : T. Ponman MPIA : S. Falter, V. Smolcic, E. Bell MPE.

25s detection of the Sy1 galaxy NGC3516 The Palermo BAT survey project Application to a sample of SDSS LINERs V. La Parola, A.Segreto, G. Cusumano, V.

Luminous Red Galaxies in the SDSS Daniel Eisenstein ( University of Arizona) with Blanton, Hogg, Nichol, Tegmark, Wake, Zehavi, Zheng, and the rest of.

T. Ohashi (Tokyo Metropolitan University)

The Formation and Evolution of Galaxies Michael Balogh University of Waterloo.

Rapture of the Deep Sky Mel Ulmer Dept of Physics & Astronomy Northwestern University This talk posted on

Exploring an evidence of supermassive black hole binaries in AGN with MAXI Naoki Isobe (RIKEN, ) and the MAXI

KASI Galaxy Evolution Journal Club A Massive Protocluster of Galaxies at a Redshift of z ~ P. L. Capak et al. 2011, Nature, in press (arXive: )

Compact groups of galaxies: small, dense, elusive by: E. Pompei - European Southern Observatory A. Iovino - Osservatorio astronomico di Brera-Milano V.

The XMM Distant Cluster Project: Survey limits and Pilot Survey Georg Lamer A. Schwope, V. Hambaryan, M. Godolt (AIP) H. Böhringer, R. Fassbender, P. Schücker,

Combine Observations of Galaxy Clusters to Constrain Cosmological Parameters Heng Yu ( 余恒 ) & Zong-Hong Zhu Beijing Normal University

Eugenio Ursino on behalf of the UM Astrophysics Group University of Miami, USA Looking for the Missing Baryons.

W.Becker 1, M.C.Weisskopf 2, Z.Arzoumanian 3, D.Lorimer 4, F.Camilo 5, R.F.Elsner 2, G.Kanbach 1, O.Reimer 6, D.A.Swartz 2, A.F.Tennant 2, S.L.O’Dell 2.

Ewan O’Sullivan (SAO) thanks to: J. Vrtilek, L. David, S. Giacintucci, S. Raychaudhury, A. Zezas, and others.

Wide-field Infrared Survey Explorer (WISE) is a NASA infrared- wavelength astronomical space telescope launched on December 14, 2009 It’s an Earth-orbiting.

Color Magnitude Diagram VG. So we want a color magnitude diagram for AGN so that by looking at the color of an AGN we can get its luminosity –But AGN.

New XMM-Newton deep Survey in the Lockman Hole Vincenzo Mainieri MPE Workshop on AGN Surveys, Puebla, June 23- July 11, 2003 Guenther Hasinger Hans Boehringer.

Galaxy Group Studies in Future Jubee Sohn.

Virgo cluster survey with MXT

DIFFUSE RADIO SOURCES in GROUPS and POOR CLUSTERS

Mapping the Universe With radio galaxies and quasars.

The XENIA mission Cosmic chemical evolution of baryons

Search for Bulk Motion in A2256 with Suzaku and ASTRO-H

2XMMp clusters in the SDSS

Core of Coma Cluster (optical)

THE OUTSKIRTS OF THE NGC 5044 GROUP

Presentation transcript:

Exploring Junctions of Filamentary Structure with SUZAKU Hajime Kawahara (TMU)

~ 80 % of Baryons is still missing Stars in Galaxies ~ 10 % Hot gases in Galaxy Clusters ~ 10 %

FOV is so small 70 Mpc Simulated Universe ( Takei+ 2011) Galaxy clusters Detectable by Low sensitivity sky surveys Field of View of High sensitivity Satellites

Suzaku search for emission from missing baryons Nearby of a massive cluster Akamatsu+2011 Middle of two massive clusters Mitsuishi+2011 No missing baryon was found.

SDSS galaxy map

RA DEC Points: SDSS spectroscopic galaxies Curves: DisPerSE : filament extractor Sousbie 2011, Sousbie, Pichon, & Kawahara 2011 Points: SDSS spectroscopic galaxies Curves: DisPerSE : filament extractor Sousbie 2011, Sousbie, Pichon, & Kawahara 2011 Kawahara+ApJL 2011 z

Massive Cluster A2142 Rosat All Sky Survey

The referee might need courage to accept the observation of “blank fields” $ 30 billion (total)/ 5 years x 80 ksec = $ million for “blank field” ! Thank you very much for accepting

Massive Cluster A2142 Rosat All Sky Survey

Kawahara, Yoshitake, Nishimichi & Sousbie ApJL, 727, L38 (2011) X-ray Brightness keV (10 4 cnt/s/cm2/sr) Hardness Ratio H= ,S= keV Optical image (DSS)

−0.11 (STAT) ±0.05 (SYS) keV (STAT) ±0.28 (SYS) keV Merging group Suzaku J

Anderson kpc redshift Bullet cluster Suzaku J A1750 A2142 A1758

Massive Cluster A2142 Merging Galaxy Group Suzaku J keV 1.6 keV Suzaku J is not WHIM ( < 1 keV ) But was Missing Baryon

In 2011 (Suzaku AO-6 period)

How to select the targets ? In 2011 (AO6) DisPerSe + SDSS DR7 3D Structure X-ray Map (RASS) BCG like galaxy

Sekiya, HK + in prep Junction 1 Junction 2 Junction 3 T ~ 0.7 keVT ~ 1.3 keV T ~ 0.7 keV ? Preliminary results of 3 new junctions Hardness Ratio (0.5-1 & 1-5 keV)

XMM If observing good positions, even current satellites can glance the low-T missing world of the Universe Star: major merger Conclusions local universe ROSAT Chandra