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X-ray to Radio Mapping of the Virtual Cosmos by GCD+

X-ray to Radio Mapping of the Virtual Cosmos by GCD+. Daisuke Kawata, Chris B. Brook, Tim W. Connors, and Brad K. Gibson Centre for Astrophysics and Supercomputing, Swinburne University of Technology. Direct and quantitative comparison. The Physics of Galaxy Formation and Evolution.

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X-ray to Radio Mapping of the Virtual Cosmos by GCD+

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  1. X-ray to Radio Mapping of the Virtual Cosmos by GCD+ Daisuke Kawata, Chris B. Brook, Tim W. Connors, and Brad K. Gibson Centre for Astrophysics and Supercomputing,Swinburne University of Technology

  2. Direct and quantitative comparison The Physics of Galaxy Formation and Evolution Synthesized multi-wavelength spectrumincluding information about structure Numerical Simulations of Galaxy Formation can follow chemo-dynamical evolution of gas and stellar components of galaxies 1. Introduction The Virtual Observatoryoffers multi-wavelength (X-ray to radio) observational data

  3. GCD+: Galactic Chemo-Dynamics Code(Kawata & Gibson 03) 3D vector/parallel tree N-body/SPH codetaking into account the complex dynamical and chemical evolutions in forming galaxy self-consistently DM, Gas, Star formation, SNe Feedback, and Metal Enrichment Cosmological Simulations by GCD+ Virtual Cosmos offers physical condition and chemical conposition of gas and stellar components at various redshift and environments plasma model, population synthesis, K-correction, etc. Synthesized spectrum from gas and stars + absorption by IGM and ISM including dust + re-emission from dust Self-consistent X-ray to radio mapping of Virtual Cosmos

  4. 2. Brief Introduction of GCD+3D vector/parallel tree N-body/SPH code DM and Stars•••Tree N-body code Gas ••• Smoothed Particle Hydrodynamics (SPH) + Radiative Cooling(MAPPINGSIII: Sutherland & Dopita) depends on metallicity + Star Formation SFR ∝ ρ1.5 (ρg ＞ 2 x10-25 g/cm3) IMF: Salpeter type + SNe FeedbackSNeII and SNeIa + Metal Enrichment SNe II, SNeIa, and intermediate mass starsH,He,C,N,O,Ne,Mg,Si, and Fe

  5. 3. Cosmological Simulation Model follows the evolution of large scale structures as well as the galaxy formation process, including gas dynamics and star formation DM density map I band image standard ΛCDM (Ω0=0.3, λ0=0.7, h=0.7, Ωb=0.019h-1,σ8=0.9

  6. Multi-Resolution Cosmological Simulation (grafic2: Bertschinger 01) Highest Resolution Region: mDM=2x105M, εDM=0.14 kpc, mgas=3x104M , εgas=0.08 kpc snap shot @ z = 5.45 J band image face-on edge-on 5kpc = 0.83” Mvir = 6x109MVmax = 65 km/s

  7. Comparison of apparent size and magnitude relation with observations Good agreement with HDF and 2df galaxies= reliable cosmologicalsimulation High-z (z>5) galaxies whichshould be detectable byJWST predicted size of these galaxies < diffraction limit?

  8. gas stars ４. Analysis derive both X-ray/Optical properties withminimum assumption Synthetic R-band image + X-ray contours

  9. fake X-ray Spectrum using XSPEC vmekal plasma model + XMM EPN response function Synthetic X-ray Spectrum with XMM response function Fit the spectrum using XSPEC vmekal model  Lx,Tx,(Fe/H)x,(O/H)x… X-ray properties Distribution of gas particles (ρ,T,ZO,Mg,Si,Fe…)

  10. Population SynthesisSSPs: Kodama & Arimoto97 Synthetic Optical/NIR Spectrum X-ray Spectrum with XMM response function  Luminosities and colours (MB, VK) Optical properties Distribution of star particles (age,ZO,Mg,Si,Fe…)

  11. Current Status Wavelength Telescope Properties of high-z galaxies Kawata, Gibson w/Windhorst (ASU) optical HST, JWST Previous Slides Dynamics of high-z galaxies Kawata, Gibson Radio (redshifted 21cm) SKA, LOFAR Tomorrow XMM, ChandraGrand+Spaceoptical telescopes Formation of elliptical galaxies Kawata, Gibson X-ray/optical Sec. 5 Formation of Milky Way Brook, Kawata, Gibson w/Flynn (Tuorla) Hipparcos,(RAVE), GAIA optical(astrometry) Sec. 6 Parkes(HIPPASS),ATCA, Southernoptical telescopes SMC and Magellanics Stream Connors, Kawata, Gibson radio,optical Near future…

  12. 5. An X-ray/Optical Study of Elliptical Galaxy Formationin CDM Universe 5.1. Introduction Coma B-R Elliptical Galaxies optical: stellar properties X-ray: gas properties R Any successful galaxy formationscenario must explain bothobserved X-ray and optical properties. Using self-consistent numericalsimulations, we are attemptingto construct such models forelliptical galaxies. 1 10 Cluster & groupXue & Wu (00)

  13. 5.2. Cosmological Simulation Model High Resolution Region: mDM=4x108M, εDM=4.3kpc, mg=5.9x107M , εDM=2.3kpc Target galaxy Largest galaxy in the simulation volume Mvir=2x1013M NGC4472 (Virgo elliptical) 3 Different Modelsmodel A: adiabatic model model B: cooling + weak feedbackmodel C: cooling + strong feedback

  14. 5.3. Results model A: adiabatic model (no cooling = no star formation)model B: with cooling and minimum SNe feedback model C: with cooling and 100 times stronger feedback 5.3.1 LxTx relation adiabatic simulation of clusters (Muanwong et al. 01) extrapolation of cluster relation(Edge et al. 91) Adiabatic model (model A) incompatible with datahigher Lx and lower Tx model A Inclusion of cooling leads to lower Lx and higher Tx consistent with observed Lx and Tx for NGC4472(models B&C) model C model B ellipticals (Matsushita et al. 00) consistent with simulations of Pearceet al. (00), Muanwong et al. (01)

  15. Semi-cosmological galaxy formation model advantage: less computational costs = can achieve higher resolutiondisadvantage: not exactly follow the cosmological evolution, e.g., might underestimate later accretion of the gas and satellite dwarf galaxies update to full cosmological simulation in near future

  16. 5.3.3. Optical properties ColourMagnitute relation Coma ellipticals (Bower et al. 1992) Problem!: An excessive popuation of young stars result due to cooling flow. Colours aretoo blue, regardless of feedback. model C model B Double check in both X-ray and optical properties gives stronger constraints on the theoretical models

  17. 6. Self-consistent modeling of Milky Way formationBrook, Kawata, Gibson, Flynn GAIA (also RAVE by UK Schmidt) Astrometry, radial velocities, and chemical composition for more than 1 billion stars within 10 kpc Chemo-dynamical modeling of formation and evolution of Milky Way templates of Milky Way like galaxies with different formation histories, such as major and minor merger history, to extract useful information from such huge data set. what observational signatures tell what formation history. The detailed formation history of Milky Way

  18. Galactic Halo Stars in Phase Space: A Hint ofSatellite Accretion?Brook, Kawata, Gibson, & Flynn (2003, ApJL in press) disrupted satellite which is identified at z=0.5 gas particles Solar neighbourhood stars Chiba & Beers (00) eccentricity Traditional interpretation: sign of rapid collapse (Eggen et al. 62)

  19. Phase Space properties Observation Simulation field stars disrupted satellite stars with low [Fe/H] and high e Identical phase space distribution Observed low [Fe/H]/high-e stars concentration can be explained bythe recent accretion of high-e orbit satellite.= alternative explanation from “rapid collapse” scenario

  20. 7. Conclusion GCD+ can provide observable values from numerical simulations. = equivalent data to what the Virtual Observatory offers. Ultimate Goal The Virtual Observatory for Virtual Cosmos Quantitative comparison between GCD+ VO for VC and VO in multi-wavelength regimeshould be exciting for studies of galaxy formation and evolution The Virtual Observatory is great for our science!

  21. Contribution to the Theory Virtual Observatory (plan) Public GCD+ VO for VC, using the same interface as VC black box (= reducing process in observation) store: the raw dataphysical and chemical data for DM, gas, star particlesanalysis codesynthesized image and spectrum similar interface to VO Image, spectrumluminosity function requests user looks great and all cosmological simulators can follow this with minimum amount of effort (probably), however…

  22. Problem: There is no perfect theoretical model.i.e.we can create lots of different virtual cosmos Therefore, the VO for VC should be provided with the descriptionof modeling.  unified format for such description and classification of modeling would be also important. Interface allow to chose whose which modele.g., GCD+ no feedback model or with strong feedback model If all (cosmological) simulators follow this sort of idea, what is the benefit?for simulator who knows differences between the codes easy to compare with the results from other code  reduce the bugsforobserver or other theoretician helpful to understand their observation and/or analytic model confused by lots of different model? show the idea how to chose the model (whose one is the best, in which case?) or enquiry to prepare this, regular meeting and comparisons among the simulator are necessarily…

  23. 5.3.3. Optical properties ColourMagnitute relation Coma ellipticals (Bower et al. 1992) Problem!: An excessive popuation of young stars result due to cooling flow. Colours aretoo blue, regardless of feedback. ignore young stars(age<8 Gyr) model C If the contribution of these young stars is ignored, the observed colour is recovered. model B Young stars formed in later cooling might have a bottom-heavy IMF?(Fabian et al. 1987; Mathews & Brighenti 1999)and/orExtra heating source (AGN?) to suppress star formation, but then the LxTx relation and Lx-(Fe/H)x must be checked again.

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