gravitational lensing: surveys and studies with new instruments
TRANSCRIPT
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Gravitational lensing: surveys and studies with new
instruments
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Science: structure and evolution of galaxies
What is the overallprofile slope, andhow did it get that way?
How much blobby CDMstuff is there here?
What is the central profile, and whyis what goes on in the middle so importantfor the structure of the rest of the galaxy?
Image 3”=~20kpc
Mostly DMout here
mostlybaryonsin here
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Science: structure and evolution of galaxies
What is the overallprofile slope, andhow did it get that way?
How much blobby CDMstuff is there here?
What is the central profile, and whyis what goes on in the middle so importantfor the structure of the rest of the galaxy?
Image 3”=~20kpc
SLACS (Bolton+,Koopmans+) - isothermalconspiracy – hard to simulate over wide z range
Flux anomalies in CLASS radioquads (Mao&Schneider, Dalal&Kochanek – picture confused, some seen, notunderstood)
One central image seen ingalaxy-only lens (Winn+)
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Science: structure and evolution of galaxies
What is the overallprofile slope, andhow did it get that way?
How much blobby CDMstuff is there here?
What is the central profile, and whyis what goes on in the middle so importantfor the structure of the rest of the galaxy?
Image 3”=~20kpc
SLACS (Bolton+,Koopmans+) - isothermalconspiracy – hard to simulate over wide z range
Flux anomalies in CLASS radioquads (Mao&Schneider, Dalal&Kochanek – picture confused, some seen, notunderstood)
One central image seen ingalaxy-only lens (Winn+)
Need more statistics (>80)particularly at high redshift Need more statistics (>7)
especially lenses with long-fluxes
Need morestatistics (>1)
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Science: structure and evolution of galaxies
What is the overallprofile slope, andhow did it get that way?
How much blobby CDMstuff is there here?
What is the central profile, and whyis what goes on in the middle so importantfor the structure of the rest of the galaxy?
Image 3”=~20kpc
SLACS (Bolton+,Koopmans+) - isothermalconspiracy – hard to simulate over wide z range
Flux anomalies in CLASS radioquads (Mao&Schneider, Dalal&Kochanek – picture confused, some seen, notunderstood)
One central image seen ingalaxy-only lens (Winn+)
Need more statistics (>80)particularly at high redshift Need more statistics (>7)
especially lenses with long-fluxes
Need morestatistics (>1)
More lenses of all types (LSST,Pan-STARRS,JDEM,SKA.....) Substructure-friendly lenses
e-MERLIN, LSST,SKA....
e-MERLIN onexisting lenses
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Science: structure and evolution of galaxies
What is the overallprofile slope, andhow did it get that way?
How much blobby CDMstuff is there here?
What is the central profile, and whyis what goes on in the middle so importantfor the structure of the rest of the galaxy?
Image 3”=~20kpc
SLACS (Bolton+,Koopmans+) - isothermalconspiracy – hard to simulate over wide z range
Flux anomalies in CLASS radioquads (Mao&Schneider, Dalal&Kochanek – picture confused, some seen, notunderstood)
One central image seen ingalaxy-only lens (Winn+)
Need more statistics (>80)particularly at high redshift Need more statistics (>7)
especially lenses with long-fluxes
Need morestatistics (>1)
More lenses of all types (LSST,Pan-STARRS,JDEM,SKA.....) Substructure-friendly lenses
e-MERLIN, LSST,SKA....
e-MERLIN onexisting lenses
This talk, section 1Section 2
Also: given cosmological model, z/separation statistics giveparameters for galaxy evolution models
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Discovery of new lenses:
short-term: efficient use of existing surveys (SL2S, COSMOS,UKIDSS/MUSCLES....)
long-term: big new instruments (e.g. LSST, JDEM, SKA...)
Faure et al.2008 Jackson 2008
Cabanac et al. 2008
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SQLS (SDSS quasar lens survey)
Major optical quasar survey to date: SQLS (Sloan quasars)
Inadaet al. 2005
Inadaet al.2004
Inada et al. 2008
~25 lenses
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CLASS survey separation histogram
SDSSseeing
UKIDSS seeing
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Muscles survey selection
77000 Sloan quasars (to DR5)UKIDSS to date -> 10000inspect visually for extensions (not necessarily the same colour)150 candidates
Detects all (6) known quasar lenses!
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MUSCLES-1 and 2
Combination SDSS+UKIDSS(Jackson, Ofek & Oguri 2008)
Jackson, Ofek & Oguri 2009
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MUSCLES-1 and 2
Combination SDSS+UKIDSS(Jackson, Ofek & Oguri 2008)
Jackson, Ofek & Oguri 2009
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Studies of the central <100pc: core images
PMN1632-0033:Winn, Rusin & Kochanek 2003, 2004
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Attempts to detect in galaxy-only
lenses have been unsuccessful due
to limited sensitivity....
Recent HSA (VLA+GB+VLBA+Arecibo) observations of CLASS B1030+074 (Zhang et al. 2007)
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Other scales: 2. The central 10pc
Recent HSA (VLA+GB+VLBA+Arecibo) observations of CLASS B1030+074 (Zhang et al. 2007)
(Lack of) central image constrainsthe steepness of the central partof the potential.
Steeper central profile or large BHgives weaker central image
Interesting constraints await e-Merlin
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existing sensitivitylevels
e-Merlin
Currently: 1 radio lens/30; for standard BH and cuspparameters, should detect many more! -> determinethese parameters
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Summary
need larger samples of both - quasar-galaxy lenses - galaxy-galaxy lenses
to contribute to studies of - central potentials – BHs, cusps... - substructure via flux anomalies or direct mapping - mass profiles – how do they get like that? - statistics – parametrised galaxy evolution
Short term: use existing surveys to maximum (UKIDSS, COSMOS,SDSS,SL2S) -> dozens of lensesMedium term: studies of existing lenses (e-MERLIN,EVLA...), new surveys (PanSTARRS) -> hundreds of lensesLong term: LSST, JDEM, SKA.... -> thousands of lenses, ultimate statistics, galaxy evolution...