9/17/2018 Cosmology from Space Max Tegmark, MIT

THE COSMIC SMÖRGÅSBORD Smorgasbord 9/17/2018 Hinshaw, Wandelt Galaxy surveys Microwave background Supernovae Ia THE COSMIC SMÖRGÅSBORD Gravitational lensing Big Bang nucleosynthesis Abazajian Galaxy clusters Neutral hydrogen tomography Lyman  forest

9/17/2018 What have we learned?

9/17/2018 OUR PLACE IN SPACE

9/17/2018 DSE

9/17/2018 OUR PLACE IN TIME

Fluctuation generator 9/17/2018 Brief History of our Universe Fluctuation generator Fluctuation amplifier Hot Dense Smooth 400 Cool Rarefied Clumpy (Graphics from Gary Hinshaw/WMAP team)

9/17/2018 Formation movies

9/17/2018 EVIDENCE?

9/17/2018 What we’ve learned about the cosmic expansion history from SN Ia Riess et al, astro-ph/0611572

9/17/2018 2008: Nolta et al 2008, arXiv:0803.0593

Cmbgg OmOl 9/17/2018

4% 21% 75% Cmbgg OmOl Using WMAP3 + SDSS LRGs: 9/17/2018

Cmbgg OmOl 430 386 13.8 9/17/2018

Cosmological Parameters 9/17/2018 Cosmological data 4% 75% 21% Cosmological Parameters

Cosmological Parameters 9/17/2018 Cosmological data 4% 75% 21% Cosmological Parameters ARE WE DONE?

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Cosmological Parameters 9/17/2018 Cosmological data 4% 75% 21% Cosmological Parameters Why these particular values? ? Nature of dark matter? Fundamental theory Nature of dark energy? Nature of early Universe?

Four roads to dark matter: catch it, infer it, make it, weigh it 9/17/2018 Production: Direct: Indirect: Gravitational: Dermer, Kusenko, … GLAST launched 6/11-08 Wandelt Planck launch scheduled for December 2008 21 cm tomography coming

Cosmological Parameters 9/17/2018 Cosmological data 4% 75% 21% Cosmological Parameters Why these particular values? ? Nature of dark matter? Fundamental theory Nature of dark energy? Nature of early Universe?

9/17/2018 How did it all begin?

Herman, Gamow & Alpher, 1940’s 9/17/2018 Herman, Gamow & Alpher, 1940’s

Arno Penzias & Robert Wilson 1965 9/17/2018 Arno Penzias & Robert Wilson 1965

100dpi Other people associated with MIT who worked on COBE: 9/17/2018 Other people associated with MIT who worked on COBE: Chuck Bennett, Ed Cheng, Steve Meyer, Rai Weiss & Ned Wright

9/17/2018 ? (Graphics fromWMAP team)

History 9/17/2018 (Figure from Wayne Hu) (Figure from WMAP team)

History 9/17/2018

History 9/17/2018 CMB Foreground-cleaned WMAP map from MT, de Oliveira-Costa & Hamilton, astro-ph/0302496

Q: How see through this wall? History 9/17/2018 Q: How see through this wall?

Q: How see through this wall? A: With gravitational waves! History 9/17/2018 Q: How see through this wall? A: With gravitational waves!

Cmbgg OmOl 9/17/2018 CMB + LSS (Figure from Matias Zaldarriaga)

Guth 1981, PRD, 23, 347

Guth 1981, PRD, 23, 347

SN Ia+CMB+LSS constraints Yun Wang & MT, PRL 92, 241302

tot Q, ns, , r, nt (Multi-field caveat) , w

CMB polarization missions Dark Energy missions

Why should you believe this? 9/17/2018 Why should you believe this?

Boom zoom 9/17/2018 Guth & Kaiser 2005, Science

Cmbgg OmOl How flat is space? 9/17/2018 closed flat open

Cmbgg OmOl How flat is space? 9/17/2018

Cmbgg OmOl How flat is space? 9/17/2018 Somewhat.

Cmbgg OmOl How flat is space? 9/17/2018 tot=1.003

Cmbgg OmOl 9/17/2018 CMB + LSS

Cmbgg OmOl 9/17/2018 CMB + LSS

Cmbgg OmOl 9/17/2018 CMB + LSS

Cmbgg OmOl 9/17/2018 CMB + LSS

Cmbgg OmOl 9/17/2018 CMB + LSS

+ CMB LSS Cmbgg OmOl CMB polarization + SDSS: n=0.008, r=0.01 9/17/2018 CMB + LSS

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So is CMBpol satellite worthwhile? 9/17/2018 So is CMBpol satellite worthwhile? SKEPTIC: COUNTER: Won’t find anything, 1: Inflation energy could be anywhere from 103 to 1016 GeV, so very unlikely that ~1016 and hence detectable. This ignores that we’ve measured Q~10-5. Either we had classic (slow-rolling scalar field) inflation, in case we’ll see it, or we didn’t, and all bets are off. Also, GUT scale natural candidate for new physics. Won’t find anything, 2: There are theoretical arguments against high energy inflation (hard for to roll many Planck units). There are are counterexamples, like N-flation. Moreover, there are theoretical arguments against low energy inflation (landscape ns problem). Will be killed by foregrounds and systematics. These are very serious challenges, but detailed studies suggest that they can be overcome, just as they have so far. Going to space helps enormously! Very focused mission (as opposed to serving broader astrophysical community) CMB maps have proven useful for research on Galactic structure, ISM, Galactic B-field, cluster SZ effect, etc. Technology not ready Far along, can be ready on time as long as ball not dropped (see Weiss report)

Cosmological Parameters 9/17/2018 Cosmological data 4% 75% 21% Cosmological Parameters Why these particular values? ? Nature of dark matter? Map our universe! Fundamental theory Nature of dark energy? Nature of early Universe?

Physics with neutral hydrogen tomography 9/17/2018 Physics with neutral hydrogen tomography

CMB History Our observable universe Last scattering surface 9/17/2018 Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496 Last scattering surface

LSS 21cm tomography Our observable universe Last scattering surface 9/17/2018 Our observable universe LSS Last scattering surface 21cm tomography

Last scattering surface The time frontier 9/17/2018 LSS Last scattering surface 21cm tomography

Cmbgg OmOl 9/17/2018

Cmbgg OmOl 9/17/2018

LSS 21cm tomography (A. Klypin) The scale frontier (Q. Shafi) 9/17/2018 (A. Klypin) LSS The scale frontier (Q. Shafi) 21cm tomography

The sensitivity frontier 9/17/2018 FFTT The sensitivity frontier Tegmark & Zaldarriaga 2008

LSS 21cm tomography Our observable universe Last scattering surface 9/17/2018 Our observable universe LSS Last scattering surface 21cm tomography

Our observable universe 9/17/2018 Our observable universe LSS Spatial curvature: WMAP+SDSS: tot= 0.01 Planck: tot= 0.003 21cm: tot=0.0002 Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 21cm tomography

Our observable universe 9/17/2018 Our observable universe LSS Spectral index running: Planck:  =0.005 21cm =0.00017 2-potential: 0.0007 4-potential: 0.008 Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 21cm tomography

Our observable universe Neutrino mass: WMAP+SDSS: m <0.3 eV +LyF: m <0.17 eV Oscillations m>0.04 eV Future lensing: m~0.03 eV 21cm: m=0.007 eV 9/17/2018 Our observable universe LSS Final punchline: we’ll be talking lots at this meeting about fascinating physics we’ve learned from current cosmology data. But let’s not become complacent and lose sight of small a fraction of our universe we’ve mapped, and how much better we can do if we map the rest. Mao, MT, McQuinn, Zahn & Zaldarriaga 2008 21cm tomography

Advantages of deploying radio array here: Boom zoom 9/17/2018 Advantages of deploying radio array here: No ionosphere Shielding from terrestial radio noise

LARC LARC: Lunar Array for Radio Cosmology Boom zoom 9/17/2018 LARC: Lunar Array for Radio Cosmology Participants: MIT, Harvard, Washington, Berkeley, JPL, NRAO PI: Jacqueline Hewitt, MIT LARC Also DALI (Joe Lazio et al)

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