New Particles from 21cm Absorption Josh Ruderman (NYU) @Moriond EW, - - PowerPoint PPT Presentation

Center for Cosmology and Particle Physics

Josh Ruderman (NYU) @Moriond EW, 3/20/2019

New Particles from 21cm Absorption

Maxim Pospelov, Josef Pradler, JTR, Alfredo Urbano, 1803.07048 (PRL) & w/ Siddharth Mishra-Sharma (to appear)

• FIRAS, astro-ph/9605054
• ARCADE2, 0901.0555

Ê Ê Ê Ê Ê Ê Ê Ê Ê

10-5 10-4 10-3 10-2 10-1 1 101 102 10-4 10-3 10-2 10-1 1 101 102 103

x = wêTCMB dnêdx @cm-3D

ARCADE2 FIRAS

TCMB = 2.73 K × (1 + z)

low energy frontier

• f the CMB

2

Rayleigh-Jeans Tail

Cosmic Microwave Background Spectrum

unmeasured

Ê

Ê Ê Ê Ê Ê Ê Ê Ê Ê

10-5 10-4 10-3 10-2 10-1 1 101 102 10-4 10-3 10-2 10-1 1 101 102 103

x = wêTCMB dnêdx @cm-3D

ARCADE2 FIRAS

new photons from dark photon oscillations

γd → γ

EDGES

(99% C.L.)

Bowman et. al. Nature 555, 67 (2018)

TCMB = 2.73 K × (1 + z)

2

Rayleigh-Jeans Tail

Cosmic Microwave Background Spectrum

unmeasured

λ = 21 cm

at z=17

Plan

• I. 21cm Primer
• II. 21cm Photons from Dark Photons

• I. 21cm Primer

now

21cm reionization epoch:

z ∼ 17

t ∼ 2 × 108 y

4

21cm Warmup

nt ns ≡ 3e−ω21/TS

5 1s

triplet singlet

γ

ω21 = 5.9 µeV

λ = 21 cm

f21 = 1.4 GHz

• hyperfine splitting of hydrogen 1s:

Ts 6= Tk

hydrogen kinetic temperature

• hydrogen spin temperature:

21cm Warmup

6

γCMB

γobs

z ∼ 17

Tγ

λobs = 21 cm × (1 + z)

λγ = 21 cm

• cosmological 21cm absorption/emission:
• absorption/emission intensity:

T21(z) = 32 mK r 1 + z 18 ✓ 1 − Tγ(z) Ts(z) ◆

hydrogen gas

Ts

101 102 103 1 101 102 103 104

z Ti @KD

T

k

∝ (1 + z)

2

Ts

Tγ ∝ 1 + z

warmup: no stars

A Brief History of Temperatures

time

7

— , CMB — , H kinetic — , H spin

Tγ

Tk

Ts

γ

γ

e−

e−

Compton decoupling

101 102 103 1 101 102 103 104

z Ti @KD

Wouthuysen-Field (WF) Effect: WF

Ts

X-ray heating

Tγ ∝ 1 + z

with stars

Ts → Tk

time

7

Lyman-α

T

k

∝ (1 + z)

2

A Brief History of Temperatures

— , CMB — , H kinetic — , H spin

Tγ

Tk

Ts

101 102 103 1 101 102 103 104

z Ti @KD

Tγ ∝ 1 + z

Ts

absorption!

with stars

time

7

T

k

∝ (1 + z)

2

A Brief History of Temperatures

EDGES target

T21 ∝ 1 − Tγ Ts

— , CMB — , H kinetic — , H spin

Tγ

Tk

Ts

Why is Cosmological 21cm Absorption Interesting?

• Rayleigh-Jeans tail of CMB at unmeasured energies
• baryon temperature at reionization epoch
• first stars of our Universe

probes: new arena to test particle physics! 8

1,000 3,000 5,000 Temperature, T (K)

a

50 60 70 80 90 100

c

• m

s.

• Frequency, (MHz)

s d l

• m

s.

–0.6 –0.4 –0.2

d

Temperature, T (K) 50 60 70 80 90 100

• Frequency, (MHz)

e

r.m.s. = 0.025 K 50 60 70 80 90 100

• e

s d l

• m

s.

–0.6 –0.4 –0.2

d

Temperature, T (K)

• m

s.

• Frequency, (MHz)

–0.2 0.2

b

50

• s

r z r i-

–0.2 0.2 Temperature, T (K)

b

r.m.s. = 0.087 K 50 60 70 80 90 100

d

• data

best fit absorption residuals (foregrounds only) residuals (foregrounds+absorption)

map frequency to redshift:

fobs = f21 1 + z

• Bowman et. al. Nature 555, 67 (2018)
• for updates see talk by Raul Monsalve last week at La Thuile 2019

9

m s.

• Frequency, (MHz)

EDGES

Experiment to Detect the Global Epoch of Reionization Signature

EDGES vs. Theory

10 12 14 16 18 20 22 24

• 1.2
• 1.0
• 0.8
• 0.6
• 0.4
• 0.2

0.0 0.2 z T21 @KD

• absorption: ~7σ
• extra absorption: ~4σ

EDGES

(99%)

max

max absorption:

1) 2) cools adiabatically

Tk

Ts ≈ Tk

(marginalized over astro uncertainties) ex) param Lyman-α and X-ray fluxes

astro uncertainties:

10

Other Global 21cm Experiments

PRIZM: 50-130 MHz

1806.09531

Marion Island, South Africa

SARAS2: 87.5-175 MHz

1710.01101

Gauribidanur Obs., India

LEDA: 30-85 MHz

Owens Valley, California

1709.09313

HYPERION: 30-120 MHz

Owens Valley, California

1501.01633

SCI-HI: 60-90 MHz

Guadalupe Island, Mexico

1311.0014

CTP: 60-80 MHz

1611.06062

Equinox Farm, Virginia

11

T21 ∝ 1 − Tγ Ts

Increasing 21cm Absorption with New Particle Physics

cool baryons

☹

DM DM H H

0.1 0.3 1 3 10 30 100 m [MeV] 3⇥106 105 3⇥105 104 3⇥104

• hT21i = 500 mK

Planck 2015 constraints SN1987A cooling SLAC Stellar (RG) BBN

Kovetz, Poulin, Gluscevic, Boddy, Barkana, Kamionkowski, 1807.11482

add photons

ninject

γ

& nCMB

(λ = 21 cm)

(easy!)

millicharged DM

(hard)

12

21cm Photons Injected by BSM Physics?

when to add photons:

z

~2000 20 15

EDGES injection window rapid absorption

γ

e−

e−

p+

p+

t ∼ 108 y

∼ 105 y

13

γ

• II. 21cm Photons

from Dark Photons

H

γobs

γd

γ

✏

H

λγd = 21 cm

z ∼ 17

(at )

14

Dark Photon

Sun

mwLSW

Coulomb Rydberg

Jupiter Earth

CMB HB RG

DPB

LSW

Cosmology

Thermal DM

non-Thermal DM

Haloscopes

AGN, SNR

ALPS-II

UWA

ADMX

Dish Antenna

ADMX-HF

ADMX Stückelberg anisotropic Non-zero FI-term Hidden Higgs HmHhªm˝'L S t ü c k e l b e r g i s

• t

r

• p

i c H l i n e L

• 18
• 15
• 12
• 9
• 6
• 3

3 6

• 15
• 12
• 9
• 6
• 3
• 15
• 12
• 9
• 6
• 3

@ D

1311.0029

21cm γd → γ

γd

γ

✏

mγd (log10 eV)

✏ (log10)

15

Dark Photon to Photon Oscillations

mγ(z) ≈ mγd

• resonant oscillations:
• rdinary photon

plasma mass

1 10 100 1000 104 10-14 10-13 10-12 10-11 10-10 10-9 10-8

z mΓ @eVD

21cm Γd absorbtion

mγ(z) = s 4πα ne(z) me

Pγd→γ ∼ (109 − 1013) ✏2

mγd ∼ 10−14 − 10−9 eV

γd

γ

✏

16

Ê

Ê Ê Ê Ê Ê Ê Ê Ê Ê

10-5 10-4 10-3 10-2 10-1 1 101 102 10-4 10-3 10-2 10-1 1 101 102 103 104

x = wêTCMB dnêdx @cm-3D

ARCADE2 FIRAS

γd

γd → γ

z < 500

EDGES

(99% C.L.)

γd

γd

a

Dark Photons from Dark Matter

ma = 10−3 eV

τa = 1.4 × 1012 y

mγd = 5 × 10−12 eV

✏ = 4 × 10−7

zres = 500

ex)

dark matter

γd

γ

✏

17

21cm Absorption with Extra Soft Photons

10 12 14 16 18 20 22 24

• 1.0
• 0.8
• 0.6
• 0.4
• 0.2

0.0 0.2

z T21 @KD

101 102 103 10-3 10-2 10-1 1 101 102

z »T21» @KD

EDGES band high z

EDGES EDGES

SM SM

γd → γ

γd → γ

resonance redshift (location varies with )

mγd

findER (DAPPER): llSat Testbed

• DAPPER will be placed in proximity to NASA’s Lunar
• ≥ ≥
• ≈ 7

ed

• e all

ent to be

DAPPER

(proposed satellite)

46 ≤ z ≤ 93

prediction: edge in high-z 21cm

18

Take Away

Ê

Ê Ê Ê Ê Ê Ê Ê Ê Ê

10-5 10-4 10-3 10-2 10-1 1 101 102 10-4 10-3 10-2 10-1 1 101 102 103

x = wêTCMB dnêdx @cm-3D

ARCADE2 FIRAS

EDGES

(99% C.L.)

γd → γ

ex) is EDGES seeing the effect of dark photons? 21cm at reionization probes the low energy frontier of the CMB Rayleigh-Jeans Tail