1. The Einstein Inflation Probe: Mission Concept Study Gary Hinshaw, NASA/GSFC May 12, 2004 Beyond Einstein @ SLAC

2. “Einstein's equations didn't have a solution that described a universe that was unchanging in time. … he fudged the equations by adding a term called the cosmological constant... The repulsive effect of the cosmological constant would balance the attractive effect of matter and allow for a universe that lasts for all time.” ---Stephen Hawking ALBERT EINSTEIN TIME MAGAZINE “PERSON OF THE CENTURY” 1916: Einstein Shows How Gravity Works Einstein applied the General Theory of Relativity to the Universe as a whole: Future collapse or expand forever Static Universe (Einstein’s requirement)

3. The Evolution of the Universe Early universe remarkably uniform, Current universe is not… HOW DID THIS HAPPEN? Inflation?... Cyclic model?... (Beyond Einstein)

4. Beyond Einstein - The Einstein Probes NASA/NSF/DOE are planning a line of 3 “Einstein Probe” missions: –A mission to study the dark energy, jointly with DOE, the “Joint Dark Energy Mission” (JDEM) a.k.a. SNAP. –A survey mission to find black holes in the nearby universe, the “Black Hole Finder”. –A mission to measure the polarization of the CMB to search for gravity waves from inflation, the “Inflation Probe” or CMBPOL. NASA issued an AO soliciting mission concept studies for each of these missions. In November 2003, several groups were selected to undertake studies. Three groups will study the Inflation Probe mission. Their goals are to define the mission requirements for sensitivity, sky coverage, angular resolution, frequency coverage, and the key experimental technologies.

5. The Concept Study Team Chuck Bennett (GFSC) Mark Devlin (U. Penn) Dale Fixsen (GSFC) Gary Hinshaw (GSFC, PI) Wayne Hu (U. Chicago) Kent Irwin (NIST/Boulder) Norm Jarosik (Princeton) Alan Kogut (GSFC) Arthur Kosowsky (Rutgers) Michele Limon (GSFC) Steve Meyer (U. Chicago) Amber Miller (Columbia) Harvey Moseley (GSFC) Barth Netterfield (U. Toronto) Angelica Oliviera-Costa (U. Penn) Lyman Page (Princeton) John Ruhl (Case Western) Uros Seljak (Princeton) David Spergel (Princeton) Suzanne Staggs (Princeton) Max Tegmark (U. Penn) Bruce Winstein (U. Chicago) Ed Wollack (GSFC) Ned Wright (UCLA) Matias Zaldarriaga (Harvard) Cliff Jackson (GSFC)

6. Why the Inflation Probe? The B mode signal in CMB polarization (at l<100) is produced by gravity waves left over from inflation. This signal is the only current observational handle we have on physics at the 10 16 GeV scale -- 12 orders of magnitude beyond the LHC. A measurement of the l<100 B mode signal would directly measure the energy scale of inflation and probe the fluctuation spectrum. It is also a test for alternate models of inflation (e.g., the cyclic universe). CMB polarization acts as a filter on cosmological processes. It allows one to probe directly the decoupling epoch, the matter power spectrum (through gravitational lensing), the ionization history, and cosmological parameters.

7. (lensing) TT EE BB r=0.1 r=0.01 (gravity waves) BB 101001000 0.01 0.1 1 10 100 Multipole l  T = [ l ( l +1)C l /2π] 1/2 [µK] TE CMB Polarization DASI TT - temperature from scalar and tensor modes TE - temperature × polarization covariance EE – “gradient” polarization from scalar & tensor modes BB – “curl” polarization from tensor modes (only) DASI EE, 2002 (r limit→BB)

8. E mode & B mode Polarization Polarization decomposable into E mode (gradient) and B mode (curl) components. Tensor fluctuations produce both E and B mode components. Scalar fluctuations produce only E mode component (except for transformation by gravitatiuonal lensing). B modes directly probe gravity waves. Q > 0 U = 0 Q < 0 U = 0 Q = 0 U < 0 Q = 0 U > 0

9. Inflation Probe Sensitivity One goal of the mission concept study is to define the mission requirements for sensitivity. Roughly: –The amplitude of B mode polarization follows: ∆T BB ~ r 1/2 ~ E 2 infl –The power in B mode polarization follows: (∆T BB ) 2 ~ P tensor (k)/P scalar (k) ~ r ~ E 4 infl “Inflationists” anticipate r ~ 0.01 The current limits are r<0.9 (95% cl) at k=0.002/Mpc (l~10) from WMAP (Spergel et al.), and r<0.5 (95% cl) at k=0.05/Mpc from WMAP+SDSSS (Tegmark et al.) To reach r~0.01, require >~100 sensitivity of WMAP (see later). If the energy scale of inflation is low (r<<0.01), the Inflation Probe could rule out inflation occurring at the GUT-scale!

10. Sensitivity Advances WMAP 2001 ×60 >×20 Planck ~2007 Inflation Probe COBE 1989 ×??

11. Detector Development: History COBE FIRAS 1 pixel, handmade KAO spectrometer 24 pixels, handmade KAO, SHARC I 24 pixels, micromachined SHARC II on CSO: 12x32= 384 pixels Largest array in operation SCUBA-2: 4000 pixels in quadrants Multiplexer behind detectors

12. WMAP (Handmade) Microwave Receivers 10 “Differencing Assemblies” 4 @ 94 GHz W-band 2 @ 61 GHz V-band 2 @ 41 GHz Q-band 1 @ 33 GHz Ka-band 1 @ 23 GHz K-band Jarosik et al. (2003) ApJS, 145, 413 Jarosik et al. (2003) ApJS, 148, 29

13. Foreground Emission Polarized foreground emission arises from our galaxy. The signal from our galaxy is currently poorly known, but it is likely comparable to or larger than the gravity wave signal over most of the sky. Foreground emission has both E and B mode symmetry. Multiple frequencies are necessary to discriminate CMB emission from galactic foreground emission. Unlike the temperature case, modeling and subtracting polarized foreground emission will be necessary. Foreground contamination also results from the conversion of primordial E mode signal to B mode signal by gravitational lensing. If the lensing contamination not cleaned, it sets a lower detection limit on r of 10 -4 at l~100 (the recombination peak) and 10 -5 at l~10 (the reionization peak).

14. Temperature Foreground Spectra Bennett et al. (2003) ApJS, 148, 97 WMAP foreground estimates from 1 st year temperature data (WMAP observing bands shown in grey) CMB dominates foregrounds over most of the sky Free-free emission is unpolarized Key question: what is polarization fraction of foregrounds relative to B- mode CMB? WMAP and other polarization data will be very helpful in guiding our study of foregrounds.

15. Projected Lensing Foreground (Green) 101001000 0.01 0.1 1 10 100 Multipole l  T = [ l ( l +1)C l /2π] 1/2 [µK]

16. Projected Galactic Foreground (Dust/Synch) 101001000 0.01 0.1 1 10 100 Multipole l  T = [ l ( l +1)C l /2π] 1/2 [µK]

17. Angular resolution The angular resolution required of the Inflation Probe is a major topic of the mission concept study. –High resolution permits more thorough cleaning of the B-mode signal due to gravitational lensing → better signal to noise at low l –High resolution is a major cost driver for a space mission! –Concept Study must perform a careful trade study of the cost- benefit of high angular resolution: High resolution optical coupling vs. high throughput Thermal loading with large optics Spacecraft attitude control requirements/costs Data rate requirements/costs

18. Noise Floor for “Strawman I” 101001000 0.01 0.1 1 10 100 Multipole l  T = [ l ( l +1)C l /2π] 1/2 [µK] 675 background limited detectors @ 3 frequencies

19. Noise Floor for “Strawman II” 101001000 0.01 0.1 1 10 100 Multipole l  T = [ l ( l +1)C l /2π] 1/2 [µK] 2100 background limited detectors @ 3 frequencies

20. Control of Systematic Errors Control of systematic errors is critical to the success of any CMB polarization measurement. A key element in rejecting systematic errors is to modulate the signal on many different time scales. The efficiency of different modulation schemes must be assessed. It is crucial to verify in flight that systematic effects have been reduced to acceptable levels. The most sensitive detectors (e.g. bolometers) are power detectors. Any effect that leads to a difference in power can be confused with a polarization signal, e.g. bandpass mismatch, far side-lobe pick-up, higher order beam effects, etc. The gain of the system has to be stable on the time scale that one can measure it in flight.

21. Sky Coverage and Scan Strategy The maximum S/N for B modes is at l~5. To reliably measure l<10 (to really be sure we are seeing B modes) nearly full sky coverage is required. Depending on the degree to which the lensing and galactic foreground may be cleaned, smaller patches might yield a detection of gravity waves. The scan pattern used to modulate the signal and achieve sky coverage will be critical. Detailed mission simulations of different scan modes, coupled with realistic instrument models will be used to assess scan patterns and other experimental approaches. The decomposition of the polarization signal into E and B modes is sensitive to sky coverage and correlations between data points.

22. WMAP Scan Pattern as Example Bennett et al. (2003) ApJ, 583, 1

23. Do We Need a Satellite? Only in space can one achieve the stability and vantage needed to probe large angular scales (>1˚)… This is the range where the telltale remnants of inflation are most likely to be found… Therefore… yes!

24. Inflation Probe Concept Study - Summary Study period is two years. Starting in June 2004, study teams will participate a joint NASA/NSF/DOE task force to chart the next steps CMB polarization studies. The obstacles to detecting gravity waves are sensitivity, systematic errors, and astrophysical foregrounds. With a well designed mission, these obstacles can be surmounted. The goal of directly measuring the energy scale of inflation is within sight!

25. The 6 Phases of a Project 1.Enthusiasm!(Now) 2.Disillusionment… 3.Panic!! 4.Search for the Guilty…… 5.Punishment of the Innocent!!! 6.Praise and Honors for the Non-Participants

26. The End

27. Experimental Approach: Minimize Systematic Measurement Errors Differential design to minimize systematic errors 5 microwave frequencies to understand foregrounds 20 radiometers to allow multiple cross checks Sensitivity to polarization Accurate calibration (<0.5%)  calibration using modulation of the dipole from Earth’s velocity In-flight beam measurements on Jupiter Minimize sidelobes & diffracted signals from Earth, Sun, Moon  L2 orbit Multiple modulation periods to identify systematic effects Minimize all observatory changes  L2 orbit; constant survey mode operations Rapid and complex sky scan  observe 30% of the sky in an hour SPIN-SYNCHRONOUS NON-SKY SIGNALS WERE THE LEADING CONCERN SWITCH (0.4 msec) SPIN (2 min) PRECESS (1 hr) ORBITAL (1 year) Bennett et al. (2003) ApJ, 583, 1

28. Systematic Error Cross-Checks (Q1+Q2)/2 (W12-W34)/2(W12+W34)/2 (V1-V2)/2(V1+V2)/2 (Q1-Q2)/2 Hinshaw et al. (2003) ApJS, 148, 63

29. Temp x E-Polarization Power Spectrum million years uniformly suppress l>40 anisotropy by 30% (!) Reionization from z=1089 scattering of CMB from electrons with non-random velocities Kogut et al. (2003) ApJS, 148, 161 Bennett et al. (2003) ApJS, 148, 1

30. http://lambda.gsfc.nasa.gov

31. Radial pattern around cold spots Tangential pattern around hot spots Temperature quadrupole at z~1089 generates polarization Temperature-Polarization Correlation

32. Jupiter Beam Maps A-side B-side Measured in flight Modeled

33. 1.z=20 reionization: scattering of CMB from free electrons uniformly suppress l>40 anisotropy by 30% (!) Now detected: 2.z=1089 decoupling: scattering of CMB from electrons with non-random velocities polarization correlates with temperature map 1 st detected by DASI, now have power spectrum 3.Gravity waves: Inflation-generated gravity waves polarize CMB need new mission (e.g., NASA’s “Einstein Inflation Probe” CMB Polarization million years

38. Sky Coverage Not to scale: Earth — L2 distance is 1% of Sun — Earth Distance Earth Sun MAP at L 2 1 Day 3 Months 6 Months - full sky coverage 129 sec. (0.464rpm) Spin 22.5° half-angle 1 hour precession cone A-side line of site B-side line of site MAP990159

39. Designed by M. Pospieszalski at NRAO

40. Lay of the Land B modes from lensing of E modes. Reionization peak (z=20) Recombination peak (z=1089) E polarization from scalars and tensors B polarization from tensors (gravity waves) only Temperature (T) from scalar and tensor fluctuations Gravity waves decay inside the horizon. Current limit on tensors

41. Universe began unimaginably hot and dense - billions of years ago Expanded and cooled Predictions: A microwave afterglow light from the Big Bang Specific spectrum (intensity with wavelength) Many other predictions - all predictions since verified 1948: Big Bang Theory

42. 1965: Discovery of Afterglow Light from Big Bang Measurement Receiver Bell Telephone Labs New Jersey 1978 Nobel Prize in Physics Robert Wilson Arno Penzias Full sky image, green represents the afterglow

43. Beyond Einstein – Inflationary Universe One slide summary of inflation.