PICO - Probe of Inflation and Cosmic Origins

Transcription

1 PICO - Probe of Inflation and Cosmic Origins Shaul Hanany University of Minnesota Executive Committee Bock, Borrill, Crill, Devlin, Flauger, Hanany, Jones, Knox, Kogut, Lawrence, McMahon, Pryke, Trangsrud Steering Committee Bennett, Dodelson, Page

2 PICO in Brief Millimeter/submillimeter-wave, polarimetric survey of the entire sky 21 bands (25% bandwidth) between 20 GHz (15 mm) and 800 GHz (0.375 mm) 1.4 m aperture telescope I GHz Diffraction limited resolution: 38 to 1 12,400 transition edge sensor bolometers + multiplexed readouts 4 year survey from L2 70 times the sensitivity of Planck Q U 30 * /K_CMB * * * * * e* Open collaboration, led by Executive and Steering Committees 353 Planck 2015 δt [μkcmb]

3 Explore How the Universe Began Detect or set upper bound on the energy scale of inflation Figure: Flauger E = r 1/4 GeV Currently r<0.07 (95%) PICO: r<10 4 (95%) 700 times lower than current constraint Figure: Flauger (r) = r, (r) quoted constraints already include x2.5 margin Includes internal delensing, removal of a simple foregrounds model; excludes systematic uncertainties

4 Explore How The Universe Began Detection would point to specific large field inflation models as the drivers for inflation, and would motivate their connection to string theory An upper limit will exclude classes of inflation potentials r M=10 M P M=12 M P M=2 M P M=20 M P BK14/Planck 4 V (1- (φ/m) ) m φ 47< N μ 3 * < 57 φ 47< N * < 57 10/3 2/3 μ φ 47< N < n s Figure: Flauger Higgs R 2 PICO 2 V tanh (φ/m) * N = 57 * N = 50 *

5 Explore how the Universe Evolved Determine the reionization history of the Universe Through measurement of the EE power spectrum on the largest angular scales Figure: Battaglia, Alvarez

6 Discover How The Universe Works Determine the sum of neutrino masses ( m ) = 14 mev Determine mass hierarchy, or mass of the lightest neutrino (if mass hierarchy known) Figure: Green ( P m ) Planck ( ) mev PICO 20 mev P m (ev) 10 1 Planck+BOSS 2 Inverted Normal PICO PICO (CVL) 15 mev Polarization Noise (µk arcmin) 10 2 Figure: Green m lightest (ev)

7 Discover How The Universe Works Determine the number of relativistic species of particles Standard model: N eff =3.046 Figure: Green Planck: PICO: N eff =3.04 ± 0.18 (N eff )= (N eff ) 10 0 QCD Real Scalar Weyl Fermion Vector fsky PICO Polarization Noise (µk arcmin) Neff Figure: 10 1 Planck 2 now PICO 2 with PICO x T F (GeV)

8 Explore how the Universe Evolved Determine the relative roles of turbulence and magnetic field in Milky Way dynamics and star formation efficiency Planck, 5 PICO, 1 PICO, smoothed to 5 Map sub-mm emission from the ISM in nearly 100 nearby galaxies: is the Milky Way typical? Constrain the shape and composition of interstellar dust grains p apple 0.33% Figure: Fissel, Chuss

9 Legacy Science Discover 3000 highly magnified dusty galaxies at z up to ~4.5; Discover 3000 proto-clusters over the sky and extending to high redshift; Detect polarization of 4000 radio and FIR-emitting galaxies; NSF News Release Dec. 6, 2017 Marrone et al. 2017; two strongly lensed massive galaxies, z=6.9 (SPT initial detection) x more than known today Probe star formation history; determine galaxy and cluster formation and evolution; learn about dark matter substructure; and measure properties of jets in radio-loud sources. Ivison et al. 2013; proto-cluster core, z=2.4 (Herschel initial detection)

10 PICO Summary Inflation, quantum gravity, particle physics, extragalactic and galactic structure and evolution: All unique goals for the measurements proposed, PICO is the only instrument with the combination of sky coverage, resolution, frequency bands, and sensitivity to achieve all of this science with one platform. Initial engineering + costing study complete: Technology implementation is a simple extension of today s technologies; no technological breakthroughs required Mission is a good fit to the cost window

11 Additional Slides

12 PICO and Sub-Orbital CMB Efforts PICO s capabilities are not matched by any other foreseeable experiment Full sky coverage with ~4 resolution (and the same depth S4 has on 5% of the sky) Access to the entire range of angular scales of the B- mode signal, including the largest, while maintaining the capability to delens

13 PICO and Sub-Orbital CMB Efforts Unmatched/unmatcheable frequency coverage Galactic foregrounds are known to overwhelm the cosmological B-mode signal Signals are at the nano-k level: even low level of residual foregrounds can bias the measurement Space gives the most systematic-error-robust platform Signals are at the nano-k level Rms brightness temperature [μk] 1/2 ( ( + 1) C / 2π ) µk Synchrotron EE Frequency [GHz] 220 GHz 70 GHz r=10-2 r=10-4 Sum fg BB, r = 10-2 BB, r = 10-4 Thermal dust E-modes f sky = 0.93 f sky = 0.73 f sky = % sky Multipole moment

14 PICO Summary Extraordinarily compelling science goals, extraordinarily broad range of science deliverables: Inflation, quantum gravity, particle physics, extragalactic, and galactic astrophysics PICO had initial engineering study at JPL in mid- December: Technology implementation is simple extension of today s technologies; no technological breakthroughs required Mission is an excellent fit to the cost window