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

The Radio Sky

Matt Jarvis (not Steve Rawlings!)

University of Hertfordshire

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

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)

Redshift

ith cell, redshift zi

ΔΩ

Wilman et al. (2008)

Semi-Empirical eXtragalactic S3-SEX Simulation

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


FRI/II: unification, beaming, structures & spectra

FRI

FRII:

Hotspot:extended flux ratio fHS = 0.4[logL151 - 25.5] ± 0.15


L(60 μm)

‘normal’ galaxies

starbursts

• 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)


Two populations of star-forming galaxies

Clusters of galaxies

• 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, 1014-16 h-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

Redshift


Large-scale structure and biasing

• 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

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


S3-SEX Example Use

But what next?

From SKADS to Herschel, Spitzer and beyond?

3.5m primary

Launched in May 2009

Continuum capabilities from

70-550 microns

3.5m primary

Launched in April 2009

Continuum capabilities from

70-550 microns

A few surveys directly relevant to SKA science

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)

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

Herschel-ATLAS Dunne, Eales, Jarvis++

• Local(ish) Galaxies

• Planck synergies

• Efficient lens survey

• Rare object science

• Large-scale structure

• Clusters

• Galactic science

Aim is to survey

~550sq.deg with Herschel

at 110, 170, 250, 350 and

550mm. (600hrs allocated)







• Clusters


Aim is to survey


at 110, 170, 250, 350 and


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







• Clusters


Aim is to survey


at 110, 170, 250, 350 and


But for now we go from the SKADS radio simulation to predict what Spitzer and Herschel have and will see…

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.

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.


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)


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)


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


Mid-infrared redshift

distributions

Far-infrared redshift

distributions

Predictions for Herschel Surveys

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http://s-cubed.physics.ox.ac.uk/s3_saxObreschkow et al. 2009 (ApJ 703)

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

Obreschkow et al. 2009 (ApJ 698); Obreschkow et al. 2009 (ApJ 703)

HerMES; Oliver et al. 2010HerMES; Oliver et al. 2010

e-MERLIN + Goonhilly

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

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

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

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