Gravitational lensing: surveys and studies with new instruments.
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Transcript of Gravitational lensing: surveys and studies with new instruments.
Gravitational lensing: surveys and studies with new
instruments
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
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+)
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)
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
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
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
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
CLASS survey separation histogram
SDSSseeing
UKIDSS seeing
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!
MUSCLES-1 and 2
Combination SDSS+UKIDSS(Jackson, Ofek & Oguri 2008)
Jackson, Ofek & Oguri 2009
MUSCLES-1 and 2
Combination SDSS+UKIDSS(Jackson, Ofek & Oguri 2008)
Jackson, Ofek & Oguri 2009
Studies of the central <100pc: core images
PMN1632-0033:Winn, Rusin & Kochanek 2003, 2004
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)
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
existing sensitivitylevels
e-Merlin
Currently: 1 radio lens/30; for standard BH and cuspparameters, should detect many more! -> determinethese parameters
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...