sunyaev-zeldovich effect
DESCRIPTION
SUNYAEV-ZELDOVICH EFFECT. OUTLINE. What is SZE What Can we learn from SZE SZE Cluster Surveys Experimental Issues SZ Surveys are coming: What do we do?. INTRODUCTION. Inverse Compton Scattering of CMB photons. Decrement in intensity below SZ null (218 GHz), increment above - PowerPoint PPT PresentationTRANSCRIPT
SUNYAEV-ZELDOVICH EFFECT
OUTLINE
What is SZE
What Can we learn from SZE
SZE Cluster Surveys
Experimental Issues
SZ Surveys are coming What do we do
INTRODUCTION
Inverse Compton Scattering of CMB photons
Decrement in intensity below SZ null (218 GHz) increment above
Small spectral distortion of CMB of order ~1 mk
Independent of redshift
kSZ EffectThe Doppler effect of line of sight cluster velocity -gt observed shift of the CMB spectrum
In the nonrelativistic limit the spectral signature of the kinetic SZE is a pure thermal distortion of magnitude of the CMB signal
SZE FOR ASTROPHYSICS
S
Cluster physicsndash measure integrated pressure
Peculiar velocities at high z
Cluster gas mass fraction ΩM
ndash clean measure of baryon gas mass
Hubble constant H(z)ndash combined with x-ray 1048774 DA(z)
Cluster surveysndash exploit redshift independencendash constrain ΩM ΩΛ σ8 w w(t)hellip
Cluster gas mass fraction ΩM
Since clusters collapse from large volumes of order 1000 Mpc3 the ratio of baryons to dark matter should be a reasonable approximation to the mix in the universe as a whole
Isothermal model
Constrain and rc with SZE integrate-gttotal gas mass
Total mass of the cluster can be estimated from X-ray or lensing measurements
Grego et al2001
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
OUTLINE
What is SZE
What Can we learn from SZE
SZE Cluster Surveys
Experimental Issues
SZ Surveys are coming What do we do
INTRODUCTION
Inverse Compton Scattering of CMB photons
Decrement in intensity below SZ null (218 GHz) increment above
Small spectral distortion of CMB of order ~1 mk
Independent of redshift
kSZ EffectThe Doppler effect of line of sight cluster velocity -gt observed shift of the CMB spectrum
In the nonrelativistic limit the spectral signature of the kinetic SZE is a pure thermal distortion of magnitude of the CMB signal
SZE FOR ASTROPHYSICS
S
Cluster physicsndash measure integrated pressure
Peculiar velocities at high z
Cluster gas mass fraction ΩM
ndash clean measure of baryon gas mass
Hubble constant H(z)ndash combined with x-ray 1048774 DA(z)
Cluster surveysndash exploit redshift independencendash constrain ΩM ΩΛ σ8 w w(t)hellip
Cluster gas mass fraction ΩM
Since clusters collapse from large volumes of order 1000 Mpc3 the ratio of baryons to dark matter should be a reasonable approximation to the mix in the universe as a whole
Isothermal model
Constrain and rc with SZE integrate-gttotal gas mass
Total mass of the cluster can be estimated from X-ray or lensing measurements
Grego et al2001
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
INTRODUCTION
Inverse Compton Scattering of CMB photons
Decrement in intensity below SZ null (218 GHz) increment above
Small spectral distortion of CMB of order ~1 mk
Independent of redshift
kSZ EffectThe Doppler effect of line of sight cluster velocity -gt observed shift of the CMB spectrum
In the nonrelativistic limit the spectral signature of the kinetic SZE is a pure thermal distortion of magnitude of the CMB signal
SZE FOR ASTROPHYSICS
S
Cluster physicsndash measure integrated pressure
Peculiar velocities at high z
Cluster gas mass fraction ΩM
ndash clean measure of baryon gas mass
Hubble constant H(z)ndash combined with x-ray 1048774 DA(z)
Cluster surveysndash exploit redshift independencendash constrain ΩM ΩΛ σ8 w w(t)hellip
Cluster gas mass fraction ΩM
Since clusters collapse from large volumes of order 1000 Mpc3 the ratio of baryons to dark matter should be a reasonable approximation to the mix in the universe as a whole
Isothermal model
Constrain and rc with SZE integrate-gttotal gas mass
Total mass of the cluster can be estimated from X-ray or lensing measurements
Grego et al2001
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
kSZ EffectThe Doppler effect of line of sight cluster velocity -gt observed shift of the CMB spectrum
In the nonrelativistic limit the spectral signature of the kinetic SZE is a pure thermal distortion of magnitude of the CMB signal
SZE FOR ASTROPHYSICS
S
Cluster physicsndash measure integrated pressure
Peculiar velocities at high z
Cluster gas mass fraction ΩM
ndash clean measure of baryon gas mass
Hubble constant H(z)ndash combined with x-ray 1048774 DA(z)
Cluster surveysndash exploit redshift independencendash constrain ΩM ΩΛ σ8 w w(t)hellip
Cluster gas mass fraction ΩM
Since clusters collapse from large volumes of order 1000 Mpc3 the ratio of baryons to dark matter should be a reasonable approximation to the mix in the universe as a whole
Isothermal model
Constrain and rc with SZE integrate-gttotal gas mass
Total mass of the cluster can be estimated from X-ray or lensing measurements
Grego et al2001
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
SZE FOR ASTROPHYSICS
S
Cluster physicsndash measure integrated pressure
Peculiar velocities at high z
Cluster gas mass fraction ΩM
ndash clean measure of baryon gas mass
Hubble constant H(z)ndash combined with x-ray 1048774 DA(z)
Cluster surveysndash exploit redshift independencendash constrain ΩM ΩΛ σ8 w w(t)hellip
Cluster gas mass fraction ΩM
Since clusters collapse from large volumes of order 1000 Mpc3 the ratio of baryons to dark matter should be a reasonable approximation to the mix in the universe as a whole
Isothermal model
Constrain and rc with SZE integrate-gttotal gas mass
Total mass of the cluster can be estimated from X-ray or lensing measurements
Grego et al2001
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Cluster gas mass fraction ΩM
Since clusters collapse from large volumes of order 1000 Mpc3 the ratio of baryons to dark matter should be a reasonable approximation to the mix in the universe as a whole
Isothermal model
Constrain and rc with SZE integrate-gttotal gas mass
Total mass of the cluster can be estimated from X-ray or lensing measurements
Grego et al2001
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Hubble constant H(z)
33 SZ distances vs redshift
Ho = 63 3 kmsMpc for M = 03 and = 07 fitting all SZE distances
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Constraining Dark Energy The observed cluster red-shift distribution in a survey is the co-moving volume per unit red-shift and solid angle dVdzd times the co-moving density of clusters ncl with masses above the survey detection limit Mlim
Majumdar2004
~1H(z) mass function
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
CLUSTER SURVEYS WITH SZE Create cluster catalogs independent (almost) of cosmology and redshift
Trace structure formation from z~2 or 3 to present day
Sample to study individual clusters to study cluster physics
Number density of clusters as a function of mass and redshift
Cluster Abundance
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Comoving volume element (left) and comoving number density (center) for twocosmologies (ΩM ΩΛ)=(03 07) (solid ) and (05 05) (dashed) (Middle) The normalization of the matter power spectrum was taken to be σ8=09 and the Press-Schechter mass function was assumed The lower set of lines in the middle panel correspond to clusters with mass greater than 1015 hminus1 Msun while the upper lines correspond to clusters with mass greaterthan 1014 hminus1 Msun
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Mass Limits of Observability
S(1+z)4 enhancement compared to usual flux limit
zgt 1 DA is slowly varying Te is higher
=gtlimiting mass of an SZ survey gently declines
Deep Surveys~10 clusters per square degree
Less Deep Surveys (all sky Plank Survey) ~ 1 cluster every few square degree
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
bull Small signal
bull Must make differential measurementsndash Synchronous offsets
bull Contaminationsndash Radio Point Sources (synchrotron)ndash Point sources in mmsubmm (Galactic and Extragalactic dust)ndash Primary anisotropies of the CMB
Experimental Challenge
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
SZE and PRIMARY CMB ANISOTROPY
Arc minute anisotropy dominated bydiffuse SZE except at λrsquos near SZE null
SZE requires small beam andormulti-frequency observations
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Point source removedlow resolution
Point source removedhigh resolution
Point source
Point Source Removal
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
SZE Foregrounds -- point sources
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Some SZ-Experiments
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
SZ Surveys are coming What should we doSimulations to study survey selection function and observable uncertainties
Plot of the matched filter noise Y as a function of filter scale c (core radius of a cluster matched to the filter) for different surveys as labeled The filter noise is generated by primary CMB anisotropy and instrumental noise Clusters lying above the curve of a particular experiment have SN gt 1
Bartlett2006
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
Integrated source counts at SN gt 5 for each survey are shown along with the simulation input counts (curve labeled ldquomass functionrdquo) Catalog completeness percentage (ratio of the experimental curve to the input mass function counts) is given in the inset The important point is that the surveys are not flux limited and are significantly incomplete even at 5 times their point source sensitivities
SZ Surveys are coming What should we do
Bartlett2006
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
SZ Surveys are coming What should we do
Photometric recovery in terms of integrated Compton Y parameter for SPT (left) and AMI (right) Compton Y values (in arcmin2) recovered by the matched filter are plotted against the input Y values taken from the simulation catalog Each point represents a single cluster detected at SN gt 5 The red dashed curve gives the equality line For SPT the characteristic scatter at fixed Ytrue is 40 Confusion with primary CMB anisotropy seriously compromises photometric recovery of the single frequency survey (chosen here as AMI)
Multiple frequency observation or a follow up in X-ray is necessary
Bartlett2006
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-
SUMMARY
CLUSTERS ARE GREAT
SZE is COOL
Howeverhellip
- Slide 1
- Slide 2
- Slide 3
- Slide 4
- Slide 5
- Slide 6
- Slide 7
- Slide 8
- Slide 9
- Slide 10
- Slide 11
- Slide 12
- Slide 13
- Slide 14
- Slide 15
- Slide 16
- Slide 17
- Slide 18
- Slide 19
- Slide 20
- Slide 21
-