Astrophysics Theory Review - INDICO (Indico) · 2011. 9. 26. · Evidence emerging for extra N ν?...

Astrophysics Theory Review

Kevork AbazajianUniversity of California, Irvine

SNAC 2011 - Virginia TechMonday, September 26, 2011

PDG, RPP 2004

Too Much of a Good Thing?

Experimental Motivation:

Monday, September 26, 2011

PDG, RPP 2004

Three Mass Differences




PDG, RPP 2004




“2+2”

δm2sol

δm2atm

δm2LSND

ν4ν3

ν1ν2


PDG, RPP 2004




“2+2”

δm2sol

δm2atm

δm2LSND

ν4ν3

ν1ν2

“3+1”

δm2atm

δm2sol

δm2LSND

ν1ν2ν3

ν4


Evidence for light sterile neutrinos?(extra relativistic degrees of freedom?)

Evidence from the Cosmic Microwave Background and Large Scale Structure:


The cosmological density perturbation spectrum

• Power spectrum of cosmological density fluctuations

• Primordial Harrison-Zeldovich:from scale invariance

– Natural solution to perturbation spectrum:self-similar evolution

• Predicted by inflation

P(k)

→

k →

P (k) = 〈|δk|2〉

P (k) ∝ k

P (k) ∝ kn

n ! 1


k →

P(k)

→

?

Perturbations enter horizon:

hori

zon

size

Matter Domination[δΦmat const]

Radiation Domination[δΦrad decays]


The Cosmic Microwave Background

WMAP 7 + high-l


CMB

SDSS w(p)

Measuring P(k)

SDSS Ly-α


Evidence emerging for extra Nν?

95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)

WM

AP5+

max

BCG+

H 0 (R

eid

et a

l.)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)

WM

AP5+

max

BCG+

H 0 (R

eid

et a

l.)W

MAP

7+BA

O+H

0 (Ko

mat

su e

t al.)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)

WM

AP5+

max

BCG+

H 0 (R

eid

et a

l.)W

MAP

7+BA

O+H

0 (Ko

mat

su e

t al.)

WM

AP7+

SDSS

LRG

(Ham

man

et a

l.)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)

WM

AP5+

max

BCG+

H 0 (R

eid

et a

l.)W

MAP

7+BA

O+H

0 (Ko

mat

su e

t al.)

WM

AP7+

SDSS

LRG

(Ham

man

et a

l.)W

MAP

7+AC

T+BA

O+H

0 (D

unkl

ey e

t al.)



95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)

WM

AP5+

max

BCG+

H 0 (R

eid

et a

l.)W

MAP

7+BA

O+H

0 (Ko

mat

su e

t al.)

WM

AP7+

SDSS

LRG

(Ham

man

et a

l.)W

MAP

7+AC

T+BA

O+H

0 (D

unkl

ey e

t al.)

Plan

ck A

LON

E Fo

reca

stMonday, September 26, 2011


95% CL Errors

PSCz

+ CM

B (H

anne

stad

200

1)

WM

AP1

(Cro

tty

et a

l.; P

ierp

aoli;

Han

nest

ad)

WM

AP3+

SDSS

+2dF

GRS+

H 0

(Han

nest

ad)

WM

AP3

+ SD

SS P

(k) +

Lyα

(Sel

jak

et a

l.)

WM

AP5+

BAO+

SN+H

0 (Ko

mat

su e

t al.)

WM

AP5+

max

BCG+

H 0 (R

eid

et a

l.)W

MAP

7+BA

O+H

0 (Ko

mat

su e

t al.)

WM

AP7+

SDSS

LRG

(Ham

man

et a

l.)W

MAP

7+AC

T+BA

O+H

0 (D

unkl

ey e

t al.)

Plan

ck A

LON

E Fo

reca

st

Yvonne W

ong Talk

...


Forecast Precision Cosmology: PLANCK

(Martin White)


Dependence of Indications for Nν>3 on Priors & Statistical evidence...Gonzales-Morales et al 2011

arxiv:1106.5052


The alpha-effect problem in r-process creation of the heavy elements

Evidence from Supernova r-process nucleosynthesis?


from G. FullerMonday, September 26, 2011

Rebec

ca S

urman Ta

lk...


Warm Dark Matter and Sterile Neutrinos as Dark Matter

Evidence from Cosmological Small-Scale Structure:


Warm Dark Matter and Sterile Neutrinos as Dark Matter

Evidence from Cosmological Small-Scale Structure:

WMAP7 + SDSS BAO + H0(Komatsu et al. 2010)

ΩDM = 0.227 ± 0.007


k →

P(k)

→

?


hori

zon

size



The Cosmological Matter Power Spectrum


k →

P(k)

→

?


hori

zon

size



The Cosmological Matter Power Spectrum

Dark matter....


What is the small scale clustering of dark matter?


What is the small scale clustering of dark matter?

The nature of dark matter...


How far into the small-scale regime can we measure?


How far into the small-scale regime can we measure?

WIMP CDM kc ~ 106 h /Mpc

(Zaldarriaga & Loeb 2006)Monday, September 26, 2011

The CDM Ansatz


Problems in Cold Dark Matter?Halo Substructure:satellite galaxies and sub-halos (Klypin et al 1999; Moore et al 1999)

Halo Cores and Densities: (Gilmore et al 2006; Kuzio de Naray 2008)

Void Galaxy abundances(Peebles 2001)

Angular Momentum Problem(Navarro & Benz 1991; Sommer-Larsen & Dolgov 2001)

Disk Dominated Galaxy Formation(Governato et al 2002)


Problems in Cold Dark Matter?Halo Substructure:satellite galaxies and sub-halos (Klypin et al 1999; Moore et al 1999)

Halo Cores and Densities: (Gilmore et al 2006; Kuzio de Naray 2008)

Void Galaxy abundances(Peebles 2001)

Angular Momentum Problem(Navarro & Benz 1991; Sommer-Larsen & Dolgov 2001)

Disk Dominated Galaxy Formation(Governato et al 2002)

Is the power spectrum different at small scales?Monday, September 26, 2011

keV Sterile Neutrinos

• Could be the Dark Matter (ms ~ 1 keV)(Dodelson & Widrow 1994; Shi & Fuller 1999; Abazajian, Fuller & Patel 2001)

• May Solve Several Potential Problems in the cold dark matter paradigm of Galaxy and Small Scale Structure Formation (e.g., Bode, Ostriker & Turok 2001)

• May provide pulsar kicks (Kusenko & Segre 1999)

• Enhances shock heating of the shock in Type II supernovae(Hidaka & Fuller 2006)


Subhalos and Dwarf Galaxies

CDMWDM

B. Moore


Dwarf Spheroidal Density Profiles from Radial Stellar Velocity Dispersion

• All dwarf spheroidals studied are consistent with NFW and cored profiles, except for UMi, “only consistent with cored profile” [Gilmore et al.,astro-ph/0608528]

• Constant core mass within stellar profile

CDM


Central densities of Dwarfs are too low relative to latest CDM results (Parry, Eke, Frenk, Okamoto 2011)


Sterile Neutrino Dark Matter Production

Γ(να → νs) ∼Γα(p)∆2(p) sin2 2θ

∆2(p) sin2 2θ + D2(p) + [∆(p) cos 2θ − V L(p) − V T (p)]2





Γα(p) ∼ G2F pT 4

∼ T 5





∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5





∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

D(p)2 ∼ T 10





∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10





H2=

8π

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10





H2=

8π

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10

Γ

H∼

T−9 High T

T 3 Low T



Γ/H

T (MeV)



H2=

8π

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10

Γ

H∼

T−9 High T

T 3 Low T



Γ/H

T (MeV)



H2=

8π

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10

Never in Equilibrium!!

Γ

H∼

T−9 High T

T 3 Low T


Sterile Neutrino Perturbation Evolution and Structure

z ∼ 1012

z ∼ 0T ∼ 10

12K

T ∼ 3 K

Growth


• SDSS 3D P(k) Main Galaxies (Tegmark et al 2003)• SDSS Lyman-alpha forest (McDonald et al 2005)• High-Resolution Lyman-alpha forest (Viel, Haehnelt & Springel 2004)• CMB: WMAP, ACBAR, CBI, VSA, BooMERANG-2K2

Where does the CDM ansatz fail?

Abazajian 2006



SDSS galaxy Pg(k)


Abazajian 2006



SDSS galaxy Pg(k)SDSS Ly-α forest PF (k)


Abazajian 2006



SDSS galaxy Pg(k)SDSS Ly-α forest PF (k)LUQAS (VLT) Ly-α forest PF (k)


Abazajian 2006



SDSS galaxy Pg(k)SDSS Ly-α forest PF (k)LUQAS (VLT) Ly-α forest PF (k)

Keck Ly-α forest PF (k)


Abazajian 2006


J. Shalf, Y. Zhang (UIUC) et al., GCCC

Lyman-α forest: Powerful & Challenging


http://zeus.ncsa.uiuc.edu:8080/lca_home_page.html

http://zeus.ncsa.uiuc.edu:8080/lca_home_page.html

http://zeus.ncsa.uiuc.edu:8080/GC3_Home_Page.html

http://zeus.ncsa.uiuc.edu:8080/GC3_Home_Page.html

J. Shalf, Y. Zhang (UIUC) et al., GCCC

Lyman-α forest: Powerful & Challenging

←the flux power spectrum→

λ (Å)


Lyman-alpha Forest Constraints on CDM

Seljak et al 2006: WMAP1 + SDSS Pg(k) + Lya + HR

All Depend on the McDonald et al. (2006) SDSS PF(k) Measurement

λFS < 54 kpc MFS < 107 Msun (Abazajian & Koushiappas 2006)

ms > 12.1 keVms > 12.1 keV

ms > 12.1 keV (SDSS PF(k) + VLT LUQAS data; Boyarsky et al 2008)

ms > 14 keV


SDSS Ly-α Constraints: Viel et al 2006 (unpublished)

Very high T0

~35000 K

WDM analysis


Turning an astrophysical signal into a constraint:The Dwarf galaxy count in the Milky Way

• Eventually, WDM is too much of a good thing, oversupression of the dwarf galaxy scale

• SDSS has found a large population of new dwarf galaxies in the MW local group

Polisensky & Ricotti (2011)


Astrophysical Constraints: CMB, Diffuse Photon Background, BBN, Type II Supernovae, Small Scale Structure, X-Ray…

sin22θ

ms[k

eV]

Abazajian, Fuller & Patel 2001


Radiative Decay in the X-ray

Γγ = 6.8× 10−33 sec−1

sin2 2θ

10−10

ms

1 keV

5

“νs”→ “να” + γ

Eγ =ms

2∼ 1 keV2 W+

1

l -l -

Pal & Wolfenstein 1981


Virgo Cluster: 1070 DM particles

Radiative Decay in the X-ray

Γγ = 6.8× 10−33 sec−1

sin2 2θ

10−10

ms

1 keV

5

“νs”→ “να” + γ

Eγ =ms

2∼ 1 keV2 W+

1

l -l -

Pal & Wolfenstein 1981


Upper Mass Limit: X-ray observations of Virgo

Abazajian, Fuller & Tucker 2001

ms = 4 keV ms = 5 keV


Chandra Deep Field: Milky Way Halo Limitsfrom the Unresoved X-ray Background

http://www.mpe.mpg.de/~mainieri/cdfs_pub/cdfs_col_940ks.jpghttp://www.mpe.mpg.de/~mainieri/cdfs_pub/cdfs_col_940ks.jpg

CDF-South Source Removal

Hickox & Markevitch 2006, 2007Monday, September 26, 2011

http://www.mpe.mpg.de/~mainieri/cdfs_pub/cdfs_col_940ks.jpg




The Soft X-ray Background

100.7 sec X-ray quantum calorimeter observation on sounding rocket flight from White Sands, NM

Using modern microcalorimetersResolution ~9 eV(McCammon et al., 2002)


Dark Matter Detection viasoft X-ray Quantum Calorimeters

(Abazajian et al, 2006; McCammon et al., 2002)

Sterile Neutrino Line(50x MW Predicted)


X-ray Constraint Summary

XMM Newton: The Virgo Cluster

ms < 6.3 keV

ms < 8.9 keV

Coma + Virgo Clusters:Boyarsky et al 2006

X-Ray Background:Boyarsky et al 2006

Andromeda Galaxy:Watson et al 2006

ms < 3.5 keV

Virgo Cluster:Abazajian et al 2001

ms < 8.2 keV

Chandra Deep Field:Abazajian et al. 2007

ms < 5.7 keV


The Detection of a WDM Sterile Neutrino?

ApJ 2010, arXiv:0912.0552v1

Text significance of 1.8 σ


The Detection of a WDM Sterile Neutrino?

ApJ 2010, arXiv:0912.0552v1

Text


Claimed νs line: unaddressed problems...

• One should see a line in the noise in a 0.2 keV resolution spectrum from 1 - 7 keV at this level of statistical significance (2.8 σ)

• Sulfur lines present in this region

• Method of subtraction of the background could be revealing this line (Mirabel & Nieto, arXiv:1003.3745)

• Willman 1 is consistent with harboring no dark matter, L&K must use the upper limit value of the Willman 1 halo mass to escape other bounds. (Wolfe et al 2009)


International X-ray Observatory


Sterile Neutrino Dark Matter Parameter Space Summary

Abazajian 2009

Pulsar Kicks


Summary

• There is a hint of evidence for extra relativistic degrees of freedom in the universe from a combination of CMB + LSS measurements

• Light sterile neutrinos may be necessary for r-process nucleosynthesis

• Cosmological small scale structure: dwarf galaxy abundance, central profile and density may be alleviated by warm dark matter like that of a sterile neutrino

• Current and future X-ray telescopes are sensitive to sterile neutrino dark matter decay

• Parameters similar to that needed for WDM sterile neutrinos may produce the observed high-velocity pulsar kicks


Astrophysics Theory Review - INDICO (Indico) · 2011. 9. 26. · Evidence emerging for extra N ν?...

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Transcript of Astrophysics Theory Review - INDICO (Indico) · 2011. 9. 26. · Evidence emerging for extra N ν?...