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Cosmic Microwave Background as the Backlight: Mapping Hot Gas in the Universe with the Sunyaev-Zeldovich Effect Eiichiro Komatsu (Max-Planck-Institut fr Astrophysik) Physikalisches Kolloquium, Universitt Bonn 6. Dezember, 2019 Sky in

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Cosmic Microwave Background as the Backlight: Mapping Hot Gas in the Universe with the Sunyaev-Zeldovich Effect

Eiichiro Komatsu (Max-Planck-Institut für Astrophysik) Physikalisches Kolloquium, Universität Bonn

  • 6. Dezember, 2019
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Sky in Optical (~0.5μm)

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Sky in Microwave (~1mm)

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Light from the fireball Universe filling our sky (2.7K) The Cosmic Microwave Background (CMB)

Sky in Microwave (~1mm)

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410 photons per cubic centimeter!!

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Spectrum of CMB = Planck Spectrum

4K Planck Spectrum 2.725K Planck Spectrum 2K Planck Spectrum Rocket (COBRA) Satellite (COBE/FIRAS) Rotational Excitation of CN Ground-based Balloon-borne Satellite (COBE/DMR)

3mm 0.3mm 30cm 3m

Brightness Wavelength

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Basak, Prunet & Benumbed (2008)

δTintrinsic(ˆ n)

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Basak, Prunet & Benumbed (2008)

δTlensed(ˆ n) = δTintrinsic(ˆ n + rφ)

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Planck Collaboration From full-sky temperature maps to…

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A full-sky lensing potential map! Planck Collaboration

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Mroczkowski et al. (2019)

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Mroczkowski et al. (2019)

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Mroczkowski et al. (2019) Reduced intensity at low frequencies Enhanced intensity at high frequencies

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Mroczkowski et al. (2019) Reduced intensity at low frequencies Enhanced intensity at high frequencies

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Mroczkowski et al. (2019) Reduced intensity at low frequencies Enhanced intensity at high frequencies

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Mroczkowski et al. (2019) Reduced intensity at low frequencies Enhanced intensity at high frequencies

Sunyaev-Zeldovich (SZ) Effect (Sunyaev & Zeldovich 1972)

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Where is a galaxy cluster?

Subaru image of RXJ1347-1145 (Medezinski et al. 2010) http://wise-obs.tau.ac.il/~elinor/clusters

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Where is a galaxy cluster?

Subaru image of RXJ1347-1145 (Medezinski et al. 2010) http://wise-obs.tau.ac.il/~elinor/clusters

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Subaru image of RXJ1347-1145 (Medezinski et al. 2010) http://wise-obs.tau.ac.il/~elinor/clusters

Visible

Ground-based Telescope (Subaru)

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Hubble image of RXJ1347-1145 (Bradac et al. 2008)

Visible

Hubble Space Telescope

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Chandra X-ray image of RXJ1347-1145 (Johnson et al. 2012)

X-ray

Chandra Space Telescope

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Chandra X-ray image of RXJ1347-1145 (Johnson et al. 2012) ALMA Band-3 Image of the Sunyaev-Zel’dovich effect at 92 GHz (Kitayama et al. 2016)

Microwave!

Atacama Millimeter and Submillimeter Array (ALMA)

1σ=17 μJy/beam =120 μKCMB 5” resolution (World record)

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Multi-wavelength Data

Optical:

  • 102–3 galaxies
  • velocity dispersion
  • gravitational lensing

X-ray:

  • hot gas (107–8 K)
  • spectroscopic TX
  • Intensity ~ ne2L

IX = Z dl n2

eΛ(TX)

SZ [microwave]:

  • hot gas (107-8 K)
  • electron pressure
  • Intensity ~ neTeL

ISZ = gν σT kB mec2 Z dl neTe

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Multi-wavelength Astrophysics Rocks!

  • One electromagnetic wavelength tells only a limited

story!

  • The X-ray intensity measures the electron density

(squared)

  • The SZ intensity measures the electron pressure
  • How do they the compare?

IX = Z dl n2

eΛ(TX)

ISZ = gν σT kB mec2 Z dl neTe

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SZ X-ray

They are similar, but not quite the same

Interesting! This is the first time to compare SZ and X-ray images at a comparable angular resolution!

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SZ X-ray

Let’s subtract a smooth component

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Let’s subtract a smooth component

SZ X-ray Ueda et al. (2018)

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SZ X-ray

Gas density is stirred (“sloshed”), but no change in pressure! => First, direct evidence that sloshed gas motion is sub-sonic

Let’s subtract a smooth component

Ueda et al. (2018)

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Hubble image of RXJ1347-1145 (Bradac et al. 2008)

Visible

Hubble Space Telescope

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Contours: Mass map from lensing!

SZ X-ray Ueda et al. (2018)

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Contours: Mass map from lensing!

SZ X-ray

Gas stripping?

Ueda et al. (2018)

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Déjà vu?

  • Dark matter is collisionless!

Clowe et al. (2006) Mass map from lensing data Gas map from X-ray data

σDM/m < 5 h−1 cm2 g−1 (95% CL)

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SZ X-ray

New constraint on the self- interaction strength of DM

Ueda et al. (2018)

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Kitayama et al., submitted on November 22

One more cluster!

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Kitayama et al., submitted SZ X-ray

SZ and X-ray images look more alike than the previous cluster

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SZ X-ray

Let’s subtract a smooth component

Kitayama et al., submitted

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SZ X-ray

  • Structures in the X-ray residual image indicate

that gas is pushed by jets from the central galaxy

  • Once again, no structure in the SZ residual!

The gas motion is sub-sonic Kitayama et al., submitted

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SZ + X-ray = Thermometer

  • SZ gives the electron pressure, while X-ray gives

the electron density

  • Combination = Electron temperature!
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Deeply cooling core?

Kitayama et al., submitted

  • Temperature

continues to fall towards the center

  • Highly unusual: In
  • ther clusters,

temperature stabilises in the core

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Deeply cooling core?

  • Entropy of gas also

continues to fall towards the center

  • Highly unusual also:

In other clusters, entropy stabilises in the core, or the slope is more like r1.2

Kitayama et al., submitted Entropy S t e a d y

  • s

t a t e c

  • l

i n g !

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Full-sky SZ Map

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Full-sky Thermal Pressure Map

North Galactic Pole South Galactic Pole Planck Collaboration

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We can simulate this in (super)computers

arXiv:1509.05134

  • Volume: (896 Mpc/h)3
  • Cosmological hydro (P-GADGET3) with star formation

and AGN feed back

  • 2 x 15263 particles (mDM=7.5x108 Msun/h)

[MNRAS, 463, 1797 (2016)]

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Dolag, EK, Sunyaev (2016)

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  • “The local universe simulation” reproduces the
  • bserved structures pretty well
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1-point PDF fits!! Dolag, EK, Sunyaev (2016)

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2-point statistics (Power Spectrum) fits!! Dolag, EK, Sunyaev (2016) small scale large scale

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Simple Interpretation

  • Randomly-distributed point sources

= Poisson spectrum = ∑i(fluxi)2 / 4π wavenumber, l Cl [not “l2Cl”]

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Simple Interpretation

  • Extended sources = the power

spectrum reflects intensity profiles Cl [not “l2Cl”] wavenumber, l

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Wavenumber, l l(l+1)Cl/2π [μK2]

>2x1015 Msun >1015 Msun >5x1014 Msun >5x1013 Msun Adding smaller clusters

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Tomography of all hot gas pressure in the Universe!

  • The SZ map does not tell us redshifts (or distances

from us)

  • By cross-correlating the SZ map with galaxies with

known redshifts, we can identify the amount of gas pressure as a function of redshifts (distances)

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Auto 2-point Correlation

TCMB(1) x TCMB(2) ngal(1) x ngal(2) CMB Galaxies 1 2 1 2

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CMB Galaxies TCMB(1) x ngal(2) ngal(1) x TCMB(2) 1 2 1 2

Cross 2-point Correlation

TCMB(1) x TCMB(2) ngal(1) x ngal(2)

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Tomography of Pressure

Chiang, Makiya et al., to be submitted

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Near Future? CCAT-prime

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Frank’s slide from the Florence meeting

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  • CCAT-prime: 6-m telescope on Cerro Chajnantor

(5600 m)

  • Germany makes great

telescopes!

  • Design study completed, the contract signed by “VERTEX

Antennentechnik GmbH”, and the construction

has begun

A Game Changer

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Frank’s slide from the Florence meeting

Cornell U. + German consortium + Canadian consortium + …

First light: 2021

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CCAT-prime Collaboration

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Summary

  • New results on the SZ effect, from small to large:
  • 1. Highest angular resolution images of the SZ effect by

ALMA - opening up a new study of cluster astrophysics via pressure fluctuations and “thermometer”

  • 2. Computer simulations are able to reproduce the low-
  • rder statistics (1-point and 2-point PDF) of pressure

fluctuations in the Universe. We (roughly) understand how gas works in the Universe

  • 3. Tomography of gas pressure! This is the thermal

history of the whole Universe

  • 4. Near future: CCAT-prime to more cleanly

separate dust emission from the SZ effect

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SZ Maps by ALMA

Thank you Time Allocation Committee (TAC)! 8.1 hours with 7-m array 3.2 hours with 12-m array 5.6 hours with 7-m array 2.6 hours with 12-m array