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The Radio Sky

The Radio Sky. Matt Jarvis (not Steve Rawlings!) University of Hertfordshire. Semi-Empirical eXtragalactic S 3 -SEX Simulation. Starting point: a z=0 ( δρ / ρ ) DM linear theory dark matter density field defined on a 550x550x1500 grid of 5 Mpc/h cells

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The Radio Sky

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  1. The Radio Sky Matt Jarvis (not Steve Rawlings!) University of Hertfordshire

  2. Semi-Empirical eXtragalactic S3-SEX Simulation Starting point: a z=0 (δρ/ρ)DM linear theory dark matter density field defined on a 550x550x1500 grid of 5 Mpc/h cells Cosmology: H0=70 km/s/Mpc, ΩM=0.3, ΩΛ=0.7, σ8=0.74, BAO P(k) Wilman et al. (2008) - MNRAS

  3. Semi-Empirical eXtragalactic S3-SEX Simulation Redshift ΔΩ ith cell, redshift zi In the ith cell, for each source population: • Poisson sample the LF at L > Li •In the limit (δρ/ρ)→0, (δn/n) → b(z)G(z)(δρ/ρ) (i.e. a linear bias model) Wilman et al. (2008)

  4. Continuum source populations • Radio-quiet AGN: Hard X-ray AGN LF (Ueda et al. 2003) + X-ray:radio relation (Brinkmann et al. 2000) • FRI radio sources: Willott et al. (2001) 151 MHz LF • FRII radio sources: Willott et al. (2001) 151 MHz LF • Normal star-forming galaxies:Yun et al. (2001) 1.4 GHz LF (low-L component) + PLE • Starburst galaxies: Yun et al. (2001) 1.4 GHz LF (high-L component) + PLE Wilman et al. (2008)

  5. FRI FRI/II: unification, beaming, structures & spectra FRII: Hotspot:extended flux ratio fHS = 0.4[logL151 - 25.5] ± 0.15 Wilman et al. (2008)

  6. Two populations of star-forming galaxies L(60 μm) • Radio LF of IRAS-selected galaxies from Yun,Reddy & Condon (2001) • Double Schechter-fn fit representing normal galaxies and starbursts • We assume LF flattens below L1.4 GHz = 1020.7 W/Hz and integrate down to 1018 W/Hz (SFR ~ 10-3 M/yr) starbursts ‘normal’ galaxies Wilman et al. (2008)

  7. Clusters of galaxies Redshift Wilman et al. (2008) • Each 5 h-1 Mpc cell has mass 1013 h-1 M → resolution to identify cluster-mass haloes • Smooth density field on a range of mass scales, 1014-16h-1 M, and search for islands of overdense cells with (δρ/ρ) > 1.66/G(z) • Discreteness of grid and lack of filter-edge interpolation → ‘quantised’ cluster masses

  8. Large-scale structure and biasing Each population assigned a halo mass which reflects large-scale clustering which is then used to compute b(z) N.B. We are not directly populating galaxy-sized haloes • Radio-quiet quasars: Mhalo = 3E12/h M • FRI radio sources: Mhalo = 1E13/h M • FRII radio sources: Mhalo = 1E14/h M • Normal star-forming galaxies: Mhalo = 1E11/h M • Starburst galaxies: Mhalo = 5E13/h M Wilman et al. (2008)

  9. S3-SEX Example Use

  10. But what next?

  11. From SKADS to Herschel, Spitzer and beyond? 3.5m primary Launched in May 2009 Continuum capabilities from 70-550 microns

  12. A few surveys directly relevant to SKA science 3.5m primary Launched in April 2009 Continuum capabilities from 70-550 microns

  13. A few surveys directly relevant to SKA science • Herschel Multi-tiered Extragalactic Survey (HerMES, 900hours) • PACS evolutionary probe (PEP, 650 hours) • Herschel-ATLAS (600 hours) • Great Observatories Origins Deep Survey: far infrared imaging with Herschel (363 hours) • The Herschel Lensing Survey (292 hours)

  14. HerMES+PEP(the usual deep fields) GOODS North / HDF North GOODS South CDFS ECDFS Lockman wide & deep Extended Groth Strip Bootes XMM/VVDS SWIRE fields (EN1, EN2, ES1) Spitzer-FLS AKARI SEP Courtesy of S. Oliver

  15. Herschel-ATLAS Dunne, Eales, Jarvis++ Aim is to survey ~550sq.deg with Herschel at 110, 170, 250, 350 and 550mm. (600hrs allocated) • Local(ish) Galaxies • Planck synergies • Efficient lens survey • Rare object science • Large-scale structure • Clusters • Galactic science

  16. Herschel-ATLAS Dunne, Eales, Jarvis++ Aim is to survey ~550sq.deg with Herschel at 110, 170, 250, 350 and 550mm. (600hrs allocated) • Local(ish) Galaxies • Planck synergies • Efficient lens survey • Rare object science • Large-scale structure • Clusters • Galactic science These will all be completed by 2012, so we can use them (and other wavelength surveys) to feed into the SKA sky simulations and give us a better picture of the SKA-sky

  17. Herschel-ATLAS Dunne, Eales, Jarvis++ Aim is to survey ~550sq.deg with Herschel at 110, 170, 250, 350 and 550mm. (600hrs allocated) • Local(ish) Galaxies • Planck synergies • Efficient lens survey • Rare object science • Large-scale structure • Clusters • Galactic science But for now we go from the SKADS radio simulation to predict what Spitzer and Herschel have and will see…

  18. Wilman, Jarvis et al. • Baseline model • Starbursts follow FIR-radio correlation of Yun, reddy, Condon • AGN given distribution in torus emission according Poletta et al. and CLUMPY models of Nenkova et al. • FIR emission assigned scaled with L(AGN) and according to Grimes et al.

  19. Wilman, Jarvis et al. • Baseline model • Starbursts follow FIR-radio correlation of Yun, Reddy, Condon • AGN given distribution in torus emission according Poletta et al. and CLUMPY models of Nenkova et al. • FIR emission assigned scaled with L(AGN) and according to Grimes et al.

  20. Wilman, Jarvis et al. • Modification 1 • Starbursts follow FIR-radio correlation of Yun, reddy, Condon • Evolution was PLE in a E-dS Cosmology. • Use new prescription of PLE in L-Cosmology for the 70um population (Huynh et al. 2007)

  21. Wilman, Jarvis et al. • Modification 1 • Starbursts follow FIR-radio correlation of Yun, reddy, Condon • Evolution was PLE in a E-dS Cosmology. • Use new prescription of PLE in L-Cosmology for the 70um population (Huynh et al. 2007)

  22. Wilman, Jarvis et al. • Modification 2 • New evidence suggests that higher-redshift sources have cooler SEDs (e.g. Symeonidis et al. 2009) (peak of the thermal dust emission moves to longer wavelengths) • Results in a very slight modification in the FIR-radio relation

  23. Mid-infrared redshift distributions

  24. Far-infrared redshift distributions

  25. Predictions for Herschel Surveys

  26. HerMES; Oliver et al. 2010 H-ATLAS; Clements, Rigby, et al. 2010

  27. http://s-cubed.physics.ox.ac.uk/s3_sax Obreschkow et al. 2009 (ApJ 703)

  28. http://s-cubed.physics.ox.ac.uk/s3_sax DeLucia2006a-simulation boxes with HI and H2 properties Mock observing cone with HI and CO emission lines HerMES; Oliver et al. 2010 HerMES; Oliver et al. 2010 Obreschkow et al. 2009 (ApJ 698); Obreschkow et al. 2009 (ApJ 703)

  29. e-MERLIN + Goonhilly e-MERLIN plus Goonhilly needed to recover correct CO PA at z=4 (Heywood et al. 2011)

  30. Summary • We have a multi-frequency radio survey from the SKADS • We have expanded this simulation to far- and mid-infrared wavelengths • Our final simulation fits the current constraints very well from 24um through to 850um • This will be tested with Herschel over the next few years • Any departure from our predictions may have a direct impact on the radio frequency simulations, allowing us to refine the SKA simulation as time goes on • We plan to further extend this simulation to the optical and near-IR over the next few months • Use new surveys at these wavelengths to aid in producing the best large-area sky simulation for the SKA and other surveys in the SKA era. • Johnston-Hollitt working on incorporating diffuse radio emission from clusters properly

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