planck limpatto sulla cosmologia alessandro melchiorri
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PLANCKLrsquoIMPATTO SULLA COSMOLOGIA
ALESSANDROMELCHIORRI
PLANCKROMA1
Paolo de Bernardis (Roma1)Erminia Calabrese (Roma1) (PhD)Silvia Masi (Roma1)Alessandro Melchiorri (Roma1) Luca Pagano (Roma1) (PhD)Francesco Piacentini
Francesco De Bernardis (PhD)Silvia Galli (PhD)Giulia Gubitosi (PhD)Matteo Martinelli (PhD)Stefania Pandolfi (PhD)Marcella Veneziani (ass ric)
Laureandi MagistraleMaria ArchidiaconoPaolo FermaniElena GiusarmaAndrea MaselliEloisa MenegoniMarco Ruzza
(Analisi Dati e Implicazioni Cosmologiche)
PLANCKROMA2
Grazia De TroiaMarina MigliaccioPaolo NatoliNicola VittorioGiancarlo de Gasperishellipe altro
hellipin collaborazione con
2121 )12(
2
1
PCT
T
T
T
Current status of CMB observations
Temperature Angular spectrum varies withtotbchns hellip
We can measure cosmological parameters with CMB
How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model(Ωbh2 Ωmh2 h ns τ Σmν )
PARAMETERESTIMATES
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
PLANCKROMA1
Paolo de Bernardis (Roma1)Erminia Calabrese (Roma1) (PhD)Silvia Masi (Roma1)Alessandro Melchiorri (Roma1) Luca Pagano (Roma1) (PhD)Francesco Piacentini
Francesco De Bernardis (PhD)Silvia Galli (PhD)Giulia Gubitosi (PhD)Matteo Martinelli (PhD)Stefania Pandolfi (PhD)Marcella Veneziani (ass ric)
Laureandi MagistraleMaria ArchidiaconoPaolo FermaniElena GiusarmaAndrea MaselliEloisa MenegoniMarco Ruzza
(Analisi Dati e Implicazioni Cosmologiche)
PLANCKROMA2
Grazia De TroiaMarina MigliaccioPaolo NatoliNicola VittorioGiancarlo de Gasperishellipe altro
hellipin collaborazione con
2121 )12(
2
1
PCT
T
T
T
Current status of CMB observations
Temperature Angular spectrum varies withtotbchns hellip
We can measure cosmological parameters with CMB
How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model(Ωbh2 Ωmh2 h ns τ Σmν )
PARAMETERESTIMATES
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
2121 )12(
2
1
PCT
T
T
T
Current status of CMB observations
Temperature Angular spectrum varies withtotbchns hellip
We can measure cosmological parameters with CMB
How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model(Ωbh2 Ωmh2 h ns τ Σmν )
PARAMETERESTIMATES
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Current status of CMB observations
Temperature Angular spectrum varies withtotbchns hellip
We can measure cosmological parameters with CMB
How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model(Ωbh2 Ωmh2 h ns τ Σmν )
PARAMETERESTIMATES
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Temperature Angular spectrum varies withtotbchns hellip
We can measure cosmological parameters with CMB
How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model(Ωbh2 Ωmh2 h ns τ Σmν )
PARAMETERESTIMATES
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
How to get a bound on a cosmological parameter
DATA
Fiducial cosmological model(Ωbh2 Ωmh2 h ns τ Σmν )
PARAMETERESTIMATES
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Dunkley et al 2008
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Blu Dati attualiRosso Planck
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
F De Bernardis E Calabrese P de Bernardis S Masi AM 2009
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Next experiment for measuring neutrino mass KATRIN eVm 90
eVm 66
eVm 66
Current limits from laboratory
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Like
lihoo
d
GG0
Constraints on Newtonrsquos constant
S Galli A Melchiorri G Smoot O Zahn arxiv09051808
51 0 GG
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
When the luminous source is the CMB the lensing effect essentially re-maps the temperature field according to
unlensed lensed
CMB Temperature Lensing
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
We phenomenologically uncoupled weak lensing from primary anisotropies by introducing a new parameter AL that scales the
lensing potential such as
bull AL=0 corresponds to a theory ignoring lensingbull AL=1 corresponds to the standard weak lensing scenario
Analysis Method
AL can also be seen like a fudge parameter controlling the amount of smoothing of the peaks In fact in this figure we can see that the curves with increasingly smoothed peak structures correspond to analysis with increasingly values of AL (0 1 3 6 9)
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Planck
Letting the lensing parameter vary the obtained constraints are
Future constraints
HFI 143 GHz Channelbull fsky =1bull θ=7rsquo bull NoiseVar=3410-4 μK2
bull fiducial model with ACBAR+WMAP3 best fit parameters
E Calabrese A Slosar A Melchiorri G Smoot O Zahn PRD 2008
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Calabrese Martinelli AM Pagano 2009
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
CMB POLARIZATION
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
Fluctuation and GW generator
Fluctuation amplifier
But GW dissipatorhellip
Hot Dense SmoothCool Rarefied
Clumpy
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
On this map we see 100000 horizons at z=1000hellip 32tta
ctdhor
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
2121 )12(
2
1
PCT
T
T
T
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
SCALAR
+
TENSOR
=
We measure thesum of the two spectraIf GW are present thislowers the amplitudeof the peakDegeneracy with other Parameters
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
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- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
kMpckS
T
A
Ar
10170
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
- 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
- Slide 22
- Slide 23
- Slide 24
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- Slide 31
- Slide 32
- Slide 33
- Slide 34
-
CMB Polarizationbull Polarization is described by Stokes-Q and -Ubull These are coordinate dependent bull The two dimensional field is described by a gradient of a scalar (E) or curl of a pseudo-scale (B)
Grad (or E) modes
Curl (or B) modes
Temperature map T ( ˆ n )
Polarization map P( ˆ n ) E B
(density fluctuations have no handness so no contributionto B-modes) B-Modes=Gravity Waves
Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
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Several inflationarymodels predicta sizable GW background(rgt001) if nlt1
Pagano Cooray MelchiorriAnd Kamionkowsky JCAP 08
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