A ``Multimessenger'' Approach to Substructure...
Transcript of A ``Multimessenger'' Approach to Substructure...
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
A “Multimessenger” Approach toSubstructure Lensing
Chuck Keeton
July 22, 2009
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Substructure lensing
Past.
I Mao & Schneider 1998: connect flux ratios and substructure
I Metcalf & Madau 2001, Chiba 2002: propose to test CDM
I Dalal & Kochanek 2002: constrain substructure mass fraction
Present/future.
I New observables.
I Can we learn more about substructure?
I Is there really a population of clumps?
I Can we constrain its: mass function? spatial distribution?redshift evolution?
I What does it reveal about dark matter?
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Flux ratio anomalies
without clump with clump
Flux ratio anomalies are hard to miss, and hard to misinterpret.(CRK, Gaudi & Petters 2003, 2005; Congdon & CRK 2005; Yoo et al. 2005, 2006)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
B1555+375
Marlow et al. (1999)
Smooth models generically predict A−B ≈ 0. (CRK, Gaudi & Petters 2005)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
B2045+265
Fassnacht et al. (1999)
Smooth models predict A−B + C ≈ 0. (CRK, Gaudi & Petters 2003)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Flux ratios and substructure
Dalal & Kochanek (2002): constrain substructure mass fraction
0.001 0.01 0.1 1
Single-wavelength flux ratios reveal∫m
dN
dmdm
but say little about dN/dm itself.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Finite source effects
Flux perturbation depends on size of subhalo relative to size ofsource. (Dobler & CRK 2006)
-2
-1
0
1
2
-2 -1 0 1 2
a = 1.2
-2
-1
0
1
2
-2 -1 0 1 2
a = 1.2
-2
-1
0
1
2
-2 -1 0 1 2
a = 1.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 1.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 1.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 1.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 1.2
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Finite source effects
Flux perturbation depends on size of subhalo relative to size ofsource. (Dobler & CRK 2006)
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.8
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.8
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.8
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.8
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.8
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.8
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.8
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Finite source effects
Flux perturbation depends on size of subhalo relative to size ofsource. (Dobler & CRK 2006)
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.4
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.4
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.4
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.4
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.4
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.4
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.4
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Finite source effects
Flux perturbation depends on size of subhalo relative to size ofsource. (Dobler & CRK 2006)
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.2
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.2
-2
-1
0
1
2
-2 -1 0 1 2
a = 0.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.2
-6
-4
-2
0
2
4
6
-6 -4 -2 0 2 4 6
a = 0.2
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Finite source effects(Dobler & CRK 2006)
-2
-1.5
-1
-0.5
0
0.5
1
1.5
2
-2 -1.5 -1 -0.5 0 0.5 1 1.5 2-2
-1.5
-1
-0.5
0
0.5
1
1.5
2
-2 -1.5 -1 -0.5 0 0.5 1 1.5 2-2
-1.5
-1
-0.5
0
0.5
1
1.5
2
-2 -1.5 -1 -0.5 0 0.5 1 1.5 2 1
1.5
2
2.5
3
3.5
4
4.5
5
5.5
6
6.5
0.001 0.01 0.1 1 10
1
1.2
1.4
1.6
1.8
2
2.2
2.4
2.6
0.001 0.01 0.1 1 10 1.1
1.2
1.3
1.4
1.5
1.6
1.7
1.8
1.9
2
2.1
0.001 0.01 0.1 1 10
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Multiwavelength flux ratios
Heuristically, each wavelength probes substructure above somemass threshold:
δµ(λ) ∼∫ mhi
m(Rsrc(λ))
mdN
dmdm
Plus, useful “resonance” if Rein(m) ≈ Rsrc.
Many possibilities:
I radio
I mid-IR (Chiba et al. 2005, Poindexter et al. 2007, Minezaki et al. 2009, Fadely & CRK)
I optical emission lines (Moustakas & Metcalf 2003, Metcalf et al. 2004, CRK et al. 2006, Sluse et
al. 2007, Sugai et al. 2007, Eigenbrod et al. 2008)
I optical continuum
I X-ray (Blackburne et al. 2006, Pooley et al. 2006, 2007, 2009, Kochanek et al. 2007, Morgan et al. 2008,
Chartas et al. 2009, Dai et al. 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass “threshold”
Band corresponds to range of redshifts in current sample.
1 100 104 106 108M HMsunL
1017
1018
1019
1020
1021
Rein HcmL
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Milli-imagesMG 2016+112, Koopmans et al. (2002)
Center at RA 20 19 18.04171 DEC 11 27 11.3350
BOTH: 2016+112 IPOL 4984.990 MHZ 2016R3U804K.ICLN02.2PLot file version 2 created 01-NOV-2000 16:54:49
Grey scale flux range= 0.000 6.000 MilliJY/BEAMCont peak flux = 6.6350E-03 JY/BEAM Levs = 1.410E-04 * (-3, 3, 5, 10, 20)
Mill
iAR
C S
EC
MilliARC SEC100 50 0 -50 -100
50
40
30
20
10
0
-10
-20
-30
Center at RA 20 19 18.18469 DEC 11 27 14.5700
BOTH: 2016+112 IPOL 4984.990 MHZ 2016R3U804K.ICLN.2PLot file version 1 created 01-NOV-2000 17:02:38
Grey scale flux range= 0.000 6.000 MilliJY/BEAMCont peak flux = 6.0946E-03 JY/BEAM Levs = 1.410E-04 * (-3, 3, 5, 10, 20)
Mill
iAR
C S
EC
MilliARC SEC30 20 10 0 -10 -20 -30 -40
30
20
10
0
-10
-20
-30
-40
Center at RA 20 19 17.97967 DEC 11 27 13.0600
BOTH: 2016+112 IPOL 4984.990 MHZ 2016R3U804K.ICLN01.2PLot file version 1 created 01-NOV-2000 17:01:09
Grey scale flux range= 0.000 6.000 MilliJY/BEAMCont peak flux = 5.9581E-03 JY/BEAM Levs = 1.410E-04 * (-3, 3, 5, 10, 20)
Mill
iAR
C S
EC
MilliARC SEC40 30 20 10 0 -10 -20 -30
30
20
10
0
-10
-20
-30
-40
B2B1
C2
C13C12C11
A1A2
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Milli-imagesB0128+437, Biggs et al. (2004)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Milli-imagesMG J0414+0534, Trotter et al. (2000)
Mill
iAR
C S
EC
MilliARC SEC200 150 100 50
500
480
460
440
420
400
380
360
340
320
Mill
iAR
C S
EC
MilliARC SEC-500 -550 -600 -650
2000
1950
1900
1850
Mill
iAR
C S
EC
MilliARC SEC100 50 0 -50 -100
100
50
0
-50
-100
Mill
iAR
C S
EC
MilliARC SEC-1850 -1900 -1950 -2000
400
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p
q
s
r
s
r
qp
r
sp
q
sr
q
p
A2
A1
B
C
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Gravitational imaging
Vegetti & Koopmans (2009ab): clumps & 108M� visibly perturbEinstein ring images (a la SLACS)
(my illustration)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Time delay millilensing
(CRK & Moustakas 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Time delay millilensing
(CRK & Moustakas 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Time delay millilensing
(CRK & Moustakas 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Time delay millilensing
(CRK & Moustakas 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Time delay millilensing
(CRK & Moustakas 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Random time delays
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Scalings
σt ∝
(fs
⟨m2⟩
〈m〉
)1/2
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
RX J1131−1231Morgan et al. (2006): M2 (2.2± 1.6 d) M1 (9.6± 2.0 d) S1.
Smooth models predict M1 leads M2.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
RX J1131−1231Morgan et al. (2006): M2 (2.2± 1.6 d) M1 (9.6± 2.0 d) S1.
But substructure can reverse that ordering. (CRK & Moustakas 2009)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Summary of observables
I radio flux ratios
I multiwavelength flux ratios
I milli-images
I gravitational imaging
I time delays
I . . . ?
They probe different aspects of the subhalo population . . .but how, exactly?
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Lensing with stochastic substructure
Can we develop a general theory of substructure lensing?
1. Improve substructure modeling:I fasterI richer — broader substructure modelsI better — understanding of systematic uncertainties
2. Develop general insights:I how is information about substructure encoded in lensing
observables?I what are the “reduced observables” we can/should aim to
measure?
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Framework
Lensing potential from 2-d Poisson equation:
∇2φ = 2κ = 2Σ
Σcrit
Time delay:
τ(x;u) =1 + zlc
DlDs
Dls
[12|x− u|2 − φ(x)
]Fermat’s principle ∇xτ = 0 gives lens equation:
u = x−α(x) where α(x) = ∇φ(x)
Distortions/magnifications:
M =(∂u
∂x
)−1
=[
1− φxx −φxy−φxy 1− φyy
]−1
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Characterizing substructure effects
Can express observables in terms of
potential φ
deflection αx =∂φ
∂x
αy =∂φ
∂y
convergence κ =12
(∂2φ
∂x2+∂2φ
∂y2
)shear γc =
12
(∂2φ
∂x2− ∂2φ
∂y2
)γs =
∂2φ
∂x∂y
Formally, we need to know the (joint) probability distribution ofΦ = {φ, αx, αy, κ, γc, γs} at all image positions.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Deflection
αx =∂φ
∂xαy =
∂φ
∂y
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Convergence
κ =12
(∂2φ
∂x2+∂2φ
∂y2
)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Shear
γc =12
(∂2φ
∂x2− ∂2φ
∂y2
)γs =
∂2φ
∂x∂y
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Use polar coordinates (ri, θi) centered on an image:
φ =∑i
mi
πln ri[
αxαy
]= −
∑i
mi
πri
[cos θisin θi
][γcγs
]= −
∑i
mi
πr2i
[cos 2θisin 2θi
](Small corrections for any clump that overlaps line of sight.)
Can we just use the Central Limit Theorem?
No: variances diverge.
Trouble caused by clump(s) closest to image. If we can handlethose, we can use CLT on the bulk of the remaining population.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Use polar coordinates (ri, θi) centered on an image:
φ =∑i
mi
πln ri[
αxαy
]= −
∑i
mi
πri
[cos θisin θi
][γcγs
]= −
∑i
mi
πr2i
[cos 2θisin 2θi
](Small corrections for any clump that overlaps line of sight.)
Can we just use the Central Limit Theorem?No: variances diverge.
Trouble caused by clump(s) closest to image. If we can handlethose, we can use CLT on the bulk of the remaining population.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Local analysis: Uniform spatial distribution
Goal: find probability distributions for most extreme shear,deflection, and potential.
Work through uniform case analytically for illustration.
px(x) =κs
N 〈m〉
(Over some large but finite area such that∫px(x) d2x = 1.)
Polar coordinates (ri, θi) centered on an image. Shear strength:
γi =mi
πr2i
What is the probability distribution for the largest shear?
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Probability that the shear from clump i is bigger than γ:
Pi(>γ) =∫miπr2i
>γ
px(xi) pm(mi) d2xi dmi
=1
N 〈m〉
∫dm pm(m)
∫dθ
∫ ( mπγ )1/2
0
dr r κs
=1
N 〈m〉
∫dm pm(m)× 2π × 1
2
(m
πγ
)κs
=κsNγ
Probability that all shears are smaller than γ:
Pall(<γ) =(
1− κsNγ
)N→ exp
(−κsγ
)for N →∞
This is the cumulative probability distribution for γmax.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Deflection strength:
αi =mi
πri
What is the probability distribution for the largest deflection?
Probability that the deflection from clump i is bigger than α:
Pi(>α) =∫miπri
>α
px(xi) pm(mi) d2xi dmi
=1
N 〈m〉
∫dm pm(m)
∫dθ
∫ mπα
0
dr r κs
=κs
Nπα2
⟨m2⟩
〈m〉
Probability that all deflections are smaller than α:
Pall(<α) =
(1− κs
Nπα2
⟨m2⟩
〈m〉
)N→ exp
(− κsπα2
⟨m2⟩
〈m〉
)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Local analysis: Power law spatial dist’n
Substructure population: κs ∝ rη−2 with 0 < η ≤ 2.
Taylor series expansions for large local shear/deflection:
P (<γ) = 1− κs,img
γ
+κs,img
γ2
[κs,img
2−⟨m2⟩
〈m〉(η − 2)2
8πr2img
]+O
(γ−3
)P (<α) = 1−
⟨m2⟩
〈m〉κs,img
πα2
+κs,img
2π2α4
[⟨m2⟩2
〈m〉2κs,img −
⟨m4⟩
〈m〉(η − 2)2
4πr2img
]+O
(α−6
)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Local shear
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix meff =⟨m2⟩/ 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
Theory.
0
0.2
0.4
0.6
0.8
1
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
PD
F
shear
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Local shear
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
0
0.2
0.4
0.6
0.8
1
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
PD
F
shear
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Local deflection
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix meff =⟨m2⟩/ 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
Theory.
0
0.2
0.4
0.6
0.8
1
0 0.005 0.01 0.015 0.02 0.025
PD
F
deflection (arcsec)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Local deflection
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
0
0.2
0.4
0.6
0.8
1
0 0.005 0.01 0.015 0.02 0.025
PD
F
deflection (arcsec)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Local potential
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix meff =⟨m2⟩/ 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
0
0.2
0.4
0.6
0.8
1
-0.006 -0.005 -0.004 -0.003 -0.002 -0.001 0 0.001 0.002
PD
F
potential (arcsec^2)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Spatial distribution: Local shear
κs ∝ rη−2 and dN/dm ∝ m−1.9 with q = 100.Isothermal (η = 1), steeper (η = 0.5), and shallower (η = 1.5).
0
0.2
0.4
0.6
0.8
1
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
PD
F
shear
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Spatial distribution: Local deflection
κs ∝ rη−2 and dN/dm ∝ m−1.9 with q = 100.Isothermal (η = 1), steeper (η = 0.5), and shallower (η = 1.5).
0
0.2
0.4
0.6
0.8
1
0 0.005 0.01 0.015 0.02 0.025
PD
F
deflection (arcsec)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Spatial distribution: Local potential
κs ∝ rη−2 and dN/dm ∝ m−1.9 with q = 100.Isothermal (η = 1), steeper (η = 0.5), and shallower (η = 1.5).
0
0.2
0.4
0.6
0.8
1
-0.006 -0.005 -0.004 -0.003 -0.002 -0.001 0 0.001 0.002
PD
F
potential (arcsec^2)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Long-range analysis
Can use Central Limit Theorem ⇒ need to know variance.
Illustrate with deflection:
αx =∑i
αxi
Variance:
var(αx) =⟨α2x
⟩− 〈αx〉2
=∑i
∑j
〈αxiαxj〉 −
(∑i
〈αxi〉
)2
=∑i
⟨α2xi
⟩+∑i
∑j 6=i
〈αxi〉 〈αxj〉 −(N 〈αxi〉
)2
= N⟨α2xi
⟩−N 〈αxi〉2
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
〈αxi〉 =1
N 〈m〉
∫dmi pm(mi)
∫d2xi κs(xi)
mi cos θiπri⟨
α2xi
⟩=
1N 〈m〉
∫dmi pm(mi)
∫d2xi κs(xi)
(mi cos θπri
)2
Note
N 〈αxi〉2 ∼ O(
1N
)Thus
var(αx) ≈ N⟨α2xi
⟩=
⟨m2⟩
〈m〉
∫d2xi κs(xi)
(cos θπri
)2
Similar analysis for all quantities.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Local vs. total: Shear
κs ∝ r−1 and dN/dm ∝ m−1.9 with q = 100.
0
0.2
0.4
0.6
0.8
1
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
PD
F
shear
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Local vs. total: Deflection
κs ∝ r−1 and dN/dm ∝ m−1.9 with q = 100.
0
0.2
0.4
0.6
0.8
1
0 0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 0.045
PD
F
deflection (arcsec)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Local vs. total: Potential
κs ∝ r−1 and dN/dm ∝ m−1.9 with q = 100.
0
0.2
0.4
0.6
0.8
1
-0.4 -0.3 -0.2 -0.1 0 0.1 0.2 0.3 0.4 0.5
PD
F
potential (arcsec^2)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Total shear
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix meff =⟨m2⟩/ 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
0
0.2
0.4
0.6
0.8
1
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
PD
F
shear
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Total deflection
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix meff =⟨m2⟩/ 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
0
0.2
0.4
0.6
0.8
1
0 0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 0.045
PD
F
deflection (arcsec)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Mass function: Total potential
κs ∝ r−1 and dN/dm ∝ m−1.9.
Fix meff =⟨m2⟩/ 〈m〉. Vary q = mhi/mlo = 1, 10, 100, 1000.
0
0.2
0.4
0.6
0.8
1
-0.015 -0.01 -0.005 0 0.005 0.01 0.015 0.02
PD
F
potential (arcsec^2)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Spatial distribution: Total shear
κs ∝ rη−2 and dN/dm ∝ m−1.9 with q = 100.Isothermal (η = 1), steeper (η = 0.5), and shallower (η = 1.5).
0
0.2
0.4
0.6
0.8
1
0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 0.16 0.18
PD
F
shear
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Spatial distribution: Total deflection
κs ∝ rη−2 and dN/dm ∝ m−1.9 with q = 100.Isothermal (η = 1), steeper (η = 0.5), and shallower (η = 1.5).
0
0.2
0.4
0.6
0.8
1
0 0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 0.045
PD
F
deflection (arcsec)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Spatial distribution: Total potential
κs ∝ rη−2 and dN/dm ∝ m−1.9 with q = 100.Isothermal (η = 1), steeper (η = 0.5), and shallower (η = 1.5).
0
0.2
0.4
0.6
0.8
1
-0.4 -0.3 -0.2 -0.1 0 0.1 0.2 0.3 0.4 0.5
PD
F
potential (arcsec^2)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Lensing Complementarity
Einstein radius, Rein ∝ m1/2. Scaled distance, r̂ = r/Rein.
observable mnemonic mass scale spatial scale
magnifications δµ ∼ 1/r̂2∫m dN
dm dm quasi-local
positions δx ∼ Rein/r̂⟨m2⟩/ 〈m〉 intermediate
time delays δt ∼ R2ein ln r̂
⟨m2⟩/ 〈m〉 long-range
Different observables contain different information about theclump population.
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Outlook
what how reduced observables
mass function combine∫m (dN/dm) dm
observables and⟨m2⟩/ 〈m〉
low-mass cutoff multiwavelength∫m (dN/dm) dm for
(e.g., WDM) flux ratios different thresholds
spatial time delays something likedistribution
∫r−n κs(x) d2x
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Outlook
Radio quads.
I radio loud: 9 — 3 currently have milli-images
I radio quiet: &20 — doable with EVLA and e-MERLIN?(N. Jackson, O. Wucknitz)
Multiwavelength (optical/IR).
I Others: 4 quads + 1 double published
I Fadely: 1 quad + 5 doubles now, 2 quads + 8 doubles soon
Quad time delays. (Congdon et al. ApJ submitted)
I 7 known currently; more and better measurements to come. . .
I 1 with clear evidence for substructure
I 4 with “anomalies”
Gravitational imaging: &100 SLACS lenses. (S. Vegetti et al.)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Outlook
Wide-field time-domain surveys will yield thousands of new lenses:Pan-STARRS, DES, LSST, SKA, . . .
Dream:
I Clean sample of ∼100 quads.
I Radio/mid-IR photometry: multiwavelength flux ratios.
I Radio interferometry: milli-images.
I Optical/near-IR monitoring: precise time delays.(Also microlensing and AGN structure.)
The Observatory for Multi-Epoch Gravitational lens Astrophysics(OMEGA)! (L. Moustakas et al.)
Observables
Flux ratios
Multiwavelength
Milli-images
Grav. imaging
Time delays
Recap
Theory
Framework
Local
Long-range
Local vs. total
Total
Complementarity
Outlook
Outlook
Wide-field time-domain surveys will yield thousands of new lenses:Pan-STARRS, DES, LSST, SKA, . . .
Dream:
I Clean sample of ∼100 quads.
I Radio/mid-IR photometry: multiwavelength flux ratios.
I Radio interferometry: milli-images.
I Optical/near-IR monitoring: precise time delays.(Also microlensing and AGN structure.)
The Observatory for Multi-Epoch Gravitational lens Astrophysics(OMEGA)! (L. Moustakas et al.)