1. 9/17/2018
Cosmology from Space
Max Tegmark, MIT

2. 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

3. 9/17/2018
What have we learned?

4. 9/17/2018
OUR PLACE IN SPACE

5. 9/17/2018
DSE

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OUR PLACE IN TIME

7. 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)

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Formation movies

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EVIDENCE?

10. 9/17/2018
What we’ve learned about the cosmic expansion history from SN Ia
Riess et al, astro-ph/

11. 9/17/2018
2008:
Nolta et al 2008, arXiv:

12. Cmbgg OmOl
9/17/2018

13. 4%
21%
75%
Cmbgg OmOl
Using WMAP3 + SDSS LRGs:
9/17/2018

14. Cmbgg OmOl
430
386
13.8
9/17/2018

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

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

17. 9/17/2018

18. 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?

19. 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

20. 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?

21. 9/17/2018
How did it all begin?

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

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

24. 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

25. 9/17/2018 ?
(Graphics fromWMAP team)

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

27. History
9/17/2018

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

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

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

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

32. Guth 1981, PRD, 23, 347

33. Guth 1981, PRD, 23, 347

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

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

40. CMB polarization missions
Dark Energy missions

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

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

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

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

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

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

47. Cmbgg OmOl
9/17/2018
CMB +
LSS

48. Cmbgg OmOl
9/17/2018
CMB +
LSS

49. Cmbgg OmOl
9/17/2018
CMB +
LSS

50. Cmbgg OmOl
9/17/2018
CMB +
LSS

51. Cmbgg OmOl
9/17/2018
CMB +
LSS

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

53. 9/17/2018

54. 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)

55. 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?

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

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

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

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

60. Cmbgg OmOl
9/17/2018

61. Cmbgg OmOl
9/17/2018

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

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

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

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

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

67. 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

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

69. 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)

70. 9/17/2018