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

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) = 〈|δk|2〉

P (k) ∝ k

P (k) ∝ kn

Perturbations enter horizon:

Matter Domination[δΦmat const]

Radiation Domination[δΦrad decays]

The Cosmic Microwave Background

WMAP 7 + high-l

SDSS w(p)

Measuring P(k)

SDSS Ly-α

Evidence emerging for extra Nν?

95% CL Errors

t al.)

95% CL Errors

t al.)

H 0 (R

95% CL Errors

t al.)

H 0 (R

t al.)

95% CL Errors

t al.)

H 0 (R

t al.)

95% CL Errors

t al.)

H 0 (R

t al.)

95% CL Errors

t al.)

H 0 (R

t al.)

stMonday, September 26, 2011

95% CL Errors

t al.)

H 0 (R

t al.)

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

urman Ta

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

The Cosmological Matter Power Spectrum

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?

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

“3+1”

δm2atm

δm2sol

δm2LSND

ν1ν2ν3

Heavier Sterile Neutrinos:Sterile Neutrino Dark Matter

∼ 1 eV

∼ 1 keV

∼ 0.01 eV

|να〉 = cos θ|νa〉 + sin θ|νb〉

|νs〉 = − sin θ|νa〉 + cos θ|νb〉(sin2 2θ ∼ 10−7)

Dark Matter:Dodelson & Widrow 1993Shi & Fuller 1999

“3+1”

δm2atm

δm2sol

δm2LSND

ν1ν2ν3

Heavier Sterile Neutrinos:Sterile Neutrino Dark Matter

∼ 1 eV

∼ 1 keV

∼ 0.01 eV

|να〉 = cos θ|νa〉 + sin θ|νb〉

|νs〉 = − sin θ|νa〉 + cos θ|νb〉

“Warm” Dark Matter

(sin2 2θ ∼ 10−7)

Dark Matter:Dodelson & Widrow 1993Shi & Fuller 1999

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

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

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10

T−9 High T

T 3 Low T

T (MeV)

3Gρ ∼ T 4

∆2∼ p−2

∼ T−2Γα(p) ∼ G2

F pT 4∼ T 5

[V T ]2 ∼ T10D(p)2 ∼ T 10

T−9 High T

T 3 Low T

T (MeV)

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!!

T−9 High T

T 3 Low T

Sterile Neutrino Perturbation Evolution and Structure

z ∼ 1012

z ∼ 0T ∼ 10

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

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)

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

Abazajian, Fuller & Patel 2001

Radiative Decay in the X-ray

Γγ = 6.8× 10−33 sec−1

sin2 2θ

10−10

“νs”→ “να” + γ

Eγ =ms

2∼ 1 keV2 W+

l -l -

Pal & Wolfenstein 1981

Γγ = 6.8× 10−33 sec−1

sin2 2θ

10−10

“νs”→ “να” + γ

Eγ =ms

2∼ 1 keV2 W+

l -l -

Virgo Cluster: 1070 DM particles

Γγ = 6.8× 10−33 sec−1

sin2 2θ

10−10

“νs”→ “να” + γ

Eγ =ms

2∼ 1 keV2 W+

l -l -

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

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

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)

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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