1 / 31

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

mathilda-sean
Télécharger la présentation

The Radio Sky

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related