fmos & lofar? will percival matt jarvis steve rawlings dave bonfield + other members of the...
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![Page 1: FMOS & LOFAR? Will Percival Matt Jarvis Steve Rawlings Dave Bonfield + other members of the LOFAR cosmology working group Will Percival Matt Jarvis Steve](https://reader035.vdocuments.us/reader035/viewer/2022062806/5697bfde1a28abf838cb23f8/html5/thumbnails/1.jpg)
FMOS & LOFAR?FMOS & LOFAR?
Will Percival
Matt Jarvis
Steve Rawlings
Dave Bonfield
+ other members of the LOFAR cosmology working group
Will Percival
Matt Jarvis
Steve Rawlings
Dave Bonfield
+ other members of the LOFAR cosmology working group
Oxford FMOS meeting, June 23Oxford FMOS meeting, June 23rdrd 2009 2009Oxford FMOS meeting, June 23Oxford FMOS meeting, June 23rdrd 2009 20091/10
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LOFARLOFAR
LOFAR will be the fastest survey telescope in the world.
Able to detect Milky Way-type galaxies up to z~3, and SCUBA-type galaxies at z>6
Now being built in Netherlands. UK joined along with Germany. 1st in the new generation of powerful
radio telescopes. Operates at 30-80MHz and 120-
240MHz Free of any dust obscuration
LOFAR will be the fastest survey telescope in the world.
Able to detect Milky Way-type galaxies up to z~3, and SCUBA-type galaxies at z>6
Now being built in Netherlands. UK joined along with Germany. 1st in the new generation of powerful
radio telescopes. Operates at 30-80MHz and 120-
240MHz Free of any dust obscuration
![Page 3: FMOS & LOFAR? Will Percival Matt Jarvis Steve Rawlings Dave Bonfield + other members of the LOFAR cosmology working group Will Percival Matt Jarvis Steve](https://reader035.vdocuments.us/reader035/viewer/2022062806/5697bfde1a28abf838cb23f8/html5/thumbnails/3.jpg)
All Sky Survey– 20,000 sq.degree survey at 15, 30, 60, 120, 200MHz to 10, 2, 0.75, 0.1, 0.2mJy–1000 sq.degree survey at 200MHz to 0.065mJy (Cluster relics/haloes, starburst galaxies)
Deep Survey–3000 sq.deg at 30 & 60MHz to 0.7 & 0.25mJy–550 sq.deg at 120MHz to 0.025mJy –360 sq.deg.at 200MHz to 0.016mJy (distant starbursts, AGN, clusters…)–choose blank field regions with the best degree-scale multi-wavelength data
Ultra-Deep Survey–71 sq. deg. at 150MHz to 0.0062mJy (confusion limited at sub-arcsec resolution) very high-z starbursts, RQ-AGN, …
All Sky Survey– 20,000 sq.degree survey at 15, 30, 60, 120, 200MHz to 10, 2, 0.75, 0.1, 0.2mJy–1000 sq.degree survey at 200MHz to 0.065mJy (Cluster relics/haloes, starburst galaxies)
Deep Survey–3000 sq.deg at 30 & 60MHz to 0.7 & 0.25mJy–550 sq.deg at 120MHz to 0.025mJy –360 sq.deg.at 200MHz to 0.016mJy (distant starbursts, AGN, clusters…)–choose blank field regions with the best degree-scale multi-wavelength data
Ultra-Deep Survey–71 sq. deg. at 150MHz to 0.0062mJy (confusion limited at sub-arcsec resolution) very high-z starbursts, RQ-AGN, …
LOFAR surveysLOFAR surveys
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LOFAR deep redshift distributionLOFAR deep redshift distribution
LOFAR 10σ sources expected in deep survey (550deg2) cut to 300deg2 survey assume we can remove z<0.4 galaxies with photometric (SDSS?) selection gives ~1x106 SF
galaxies with0.5<z<1.7
1.9x106 other sources (including 0.4<z<0.5 SF gals)
gives a “redshift completeness” of 0.36
pessimistic as wouldalso get z for some AGN + extra photo-z selection. Also can useluminosity to favor SFgalaxies
LOFAR 10σ sources expected in deep survey (550deg2) cut to 300deg2 survey assume we can remove z<0.4 galaxies with photometric (SDSS?) selection gives ~1x106 SF
galaxies with0.5<z<1.7
1.9x106 other sources (including 0.4<z<0.5 SF gals)
gives a “redshift completeness” of 0.36
pessimistic as wouldalso get z for some AGN + extra photo-z selection. Also can useluminosity to favor SFgalaxies
FMOS redshift limits
SF galaxies
FRIRQ AGN
Wilman et al 2008
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Plot explanation: cosmological constraintsPlot explanation: cosmological constraints
Fisher matrix predictions for cosmological constraints from BAO and from redshift-sapce distortions
Fisher matrix predictions for cosmological constraints from BAO and from redshift-sapce distortions
Radial BAOAngular BAOz-space distortions
lower = better
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Redshift completenessRedshift completeness
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets effect of sub-sampling by a factor e shown below
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets effect of sub-sampling by a factor e shown below
big gains until e~0.5, then diminishing returns, particularly for redshift-space distortions
big gains until e~0.5, then diminishing returns, particularly for redshift-space distortions
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Galaxy selection?Galaxy selection?
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets assume fiducial e=0.36 where to pre-select galaxies – ie put these galaxies in different redshift bins
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets assume fiducial e=0.36 where to pre-select galaxies – ie put these galaxies in different redshift bins
high number of high redshift galaxies helps high number of high redshift galaxies helps
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Volume vs number densityVolume vs number density
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets compare with oversampling by a factor of 2 or 4, covering a smaller area
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets compare with oversampling by a factor of 2 or 4, covering a smaller area
definitely do not want to decrease survey area definitely do not want to decrease survey area
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Comparison with other surveysComparison with other surveys
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets assume can remove z<0.4 galaxies from photometric redshifts leaves e=0.36 SF galaxy fraction in 0.z<z<1.7 pessimistic as can get redshifts for some AGN
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets assume can remove z<0.4 galaxies from photometric redshifts leaves e=0.36 SF galaxy fraction in 0.z<z<1.7 pessimistic as can get redshifts for some AGN
![Page 10: FMOS & LOFAR? Will Percival Matt Jarvis Steve Rawlings Dave Bonfield + other members of the LOFAR cosmology working group Will Percival Matt Jarvis Steve](https://reader035.vdocuments.us/reader035/viewer/2022062806/5697bfde1a28abf838cb23f8/html5/thumbnails/10.jpg)
Things look better with larger bins …Things look better with larger bins …
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets assume can remove z<0.4 galaxies from photometric redshifts leaves e=0.36 SF galaxy fraction in 0.z<z<1.7 pessimistic as can get redshifts for some AGN
take SF galaxy distribution (predicted 10σ LOFAR sources) 0.5<z<1.7, 300deg2 baseline FMOS survey has ~600 000 targets assume can remove z<0.4 galaxies from photometric redshifts leaves e=0.36 SF galaxy fraction in 0.z<z<1.7 pessimistic as can get redshifts for some AGN
![Page 11: FMOS & LOFAR? Will Percival Matt Jarvis Steve Rawlings Dave Bonfield + other members of the LOFAR cosmology working group Will Percival Matt Jarvis Steve](https://reader035.vdocuments.us/reader035/viewer/2022062806/5697bfde1a28abf838cb23f8/html5/thumbnails/11.jpg)
conclusionsconclusions
300deg2 FMOS survey means close to cosmic variance limit
To optimise science return need to increase high-z galaxy distribution
LOFAR deep selection can provide a sample of star-forming galaxies with a sampling return of 0.36, just removing z<0.4 galaxies
would also pick up redshifts for some of the AGN so e=0.5-0.6 probably more realistic
300deg2 FMOS survey means close to cosmic variance limit
To optimise science return need to increase high-z galaxy distribution
LOFAR deep selection can provide a sample of star-forming galaxies with a sampling return of 0.36, just removing z<0.4 galaxies
would also pick up redshifts for some of the AGN so e=0.5-0.6 probably more realistic