Measurements of Degree-Scale B-mode Polarization with the BICEP/Keck Experiments at South Pole

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1 Measurements of Degree-Scale B-mode Polarization with the BICEP/Keck Experiments at South Pole Benjamin Racine for the BICEP/Keck Collaboration March 18th, èmes Rencontres de Moriond La Thuile

2 Figure from Wikipedia Earliest Time Visible with Light??? 2

3 CMB Polarization Density Wave Gravitational Wave Temperature Pattern Seen by Electrons r = Tensor Scalar Credit: Bicep2 collaboration 3

4 CMB Polarization Density Wave E Gravitational Wave Temperature Pattern Seen by Electrons r = Tensor Scalar B Credit: Bicep2 collaboration 4

5 CMB T Planck s all sky CMB temperature map scale ±500 µk Intensity Polarization 5

6 T CMB Polarization Bicep2 s CMB polarization map...familiar choice: Stokes Parameters Q&U Stokes Q Stokes U 6

7 T CMB Polarization Bicep2 s CMB polarization map E B...clever choice for cosmology: E&B-modes E modes B modes 6

8 T CMB Polarization Bicep2 s CMB polarization map E B...clever choice for cosmology: E&B-modes E modes B modes 0.3 6

9 CMB Polarization T Intensity In standard ΛCDM only E-modes are present at last scattering E B Primordial GW lensing B-mode During propagation some of the E-modes are confused into B-modes by lensing Primordial gravitational waves are the unique source of B-modes peaking at l 100 : degree scales 7

10 Galactic Foregrounds For now, two known foregrounds can produce E and B modes Flavien Vansyngel s and Angela Taylor s talk Synchrotron emission Dominates at low frequencies (radio) electrons spiraling in magnetic fields. Dust emission Dominates at High frequencies (IR) small interstellar dust grains aligned by magnetic fields. Planck Collaboration X:

11 Galactic Foregrounds For now, two known foregrounds can produce E and B modes Cartoon model of the polarized emissions Flavien Vansyngel s and Angela Taylor s talk Rms Brightness temperature (µk) Dust emission Dominates at High frequencies (IR) small interstellar dust grains aligned by magnetic fields. Synchrotron Frequency (GHz) Synchrotron emission Dominates at low frequencies (radio) electrons spiraling in magnetic fields. Dust Planck Collaboration X:

12 Victor Buza S4 talk on Thursday Kimmy Wu BK-SPT talk just after

13 Photo Credit: USAP, NSF Bicep 2 x5 = Keck Array Bicep 3 x4 = Bicep Array Keck Array Bicep Array 2019 Bicep 1 Bicep 2 Bicep 3 Since 2015 Small aperture telescopes (cheap, fast, low systematics) Target the 2 degree peak of the B-mode Integrate continuously from South Pole Observe 1% patch of sky SPT (3G) Bender + Manzotti + Wu talk 10

14 The BICEP2/Keck Telescopes 26cm Lens Telescope as compact as possible while still having the angular resolution to observe degree-scale features. Optical elements cooled to 4 K. On-axis, refractive optics allow the entire telescope to rotate around boresight for polarization modulation. A 3-stage helium sorption refrigerator further cools the detectors to 250 mk. 1.2 m Camera tube Optics tube Nylon filter Lens Nb magnetic shield Focal plane assembly Passive thermal filter Flexible heat straps Fridge mounting bracket Refrigerator Camera plate 11

15 Mass-produced Superconducting Detectors Focal plane Planar antenna array 0.3mm Slot antennas A B Transition Edge Sensor Microstrip filters 12

16 BICEP2/Keck Band Response Rms Brightness temperature (µk) Cartoon model of the polarized Dust Synchrotron Frequency (GHz) Typical South Pole atmospheric transmission 95 GHz 150 GHz 220 GHz Detectors Designed to Scale in Frequency (JPL) 13

17 Keck Array Frequency Coverage Simple raw observing effort, doesn t take into account how years performed Bicep2 receiver at 150 GHz in Keck Array receivers all at 150 GHz in

18 Keck Array Frequency Coverage Simple raw observing effort, doesn t take into account how years performed Bicep2 receiver at 150 GHz in Keck Array receivers all at 150 GHz in replaced two 150 GHz receivers with 95 GHz receivers in BK14 The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 116, ,

19 Keck Array Frequency Coverage Simple raw observing effort, doesn t take into account how years performed Bicep2 receiver at 150 GHz in Keck Array receivers all at 150 GHz in replaced two 150 GHz receivers with 95 GHz receivers in replaced two additional 150s with 220s for BK15 Soon out! 14

20 Scanning A B Each focal plane pixel is really two detectors a horizontally polarized one and a vertically polarized one. A+B -> Full signal A-B -> Polarization only Video from Robert Schwarz

21 A B Raw Data - Typical Weather Time 50 mins Telescope Movement Sum of detector pairs Difference of detector pairs Scanning over lumpy atmosphere clouds Pair difference still clean atmosphere is unpolarized 16

22 A B Timestream PSDs Pair Diff Pair Sum Multipole 100 at 0.4Hz 17

23 Upcoming BK15 95 GHz Maps BK15 95GHz 5 μk arcmin 18

24 Upcoming BK GHz Maps BK15 150GHz 2.8 μk arcmin 18

25 Upcoming BK GHz Maps BK15 220GHz 25 μk arcmin 18

26 Upcoming Keck 2015 only E-Mode Maps Keck GHz µk Keck GHz µk Already 3 times deeper than Planck 217GHz Keck GHz µk 19

27 Upcoming BK15 Spectra cross-spectra only trace spatially correlated component of maps Cyan lines: BK14 CMB + polarized dust model with r = 0 Spectra using all data up to and including for the first time adding Keck 220GHz 220 GHz data in excellent agreement with Planck 353 GHz at similar dust sensitivity 20

28 Planck polarized maps at 7 frequencies + WMAP at 2 frequencies 30 GHz 44 GHz Q U Polarized galactic synchrotron dominates at low frequencies 70 GHz 23 GHz Q U 100 GHz 33 GHz 143 GHz From arxiv GHz 353 GHz From arxiv Polarized thermal emission (~20K) from galactic dust aligned in magnetic fields dominates at high frequencies 21

29 BK15 Band Sensitivity (at l = 80) BK17 errors BK15 on errors r will on be r dominated by dust synchrotron sensitivity sensitivity BK17 sensitivity 22

30 Auto and cross-spectra between BICEP2 + Keck Array and all WMAP/ Planck maps BK14 (no 220GHz): 66 spectra BK15: 78 spectra Statistics for all spectra and covariance matrix derived from simulations of signal and noise. PRL 116,

31 A selected sample of cross spectra between BK and WMAP/Planck: 23x150 shows hint of synchrotron but 30x150 doesn t want it BK14 (no 220GHz) Strong detection of dust in 150x353 No evidence for dust/sync correlation in 23x353 etc.

32 Multicomponent Likelihood Analysis Hamimeche Lewis: Take the joint likelihood of all the spectra simultaneously vs. model for BB : ΛCDM lensing expectation + r + 7 foreground parameters Victor Buza s talk Rms Brightness temperature (µk) Synchrotron foreground model = dust + synchrotron Cartoon model Dust A dust β dust A synch β synch l=80 frequency spectral indices Frequency (GHz) 24

33 Multicomponent Likelihood Analysis Hamimeche Lewis: Take the joint likelihood of all the spectra simultaneously vs. model for BB : ΛCDM lensing expectation + r + 7 foreground parameters Victor Buza s talk foreground model = dust + synchrotron (µk 2 ) Power `(` + 1)/2 C` r=0.1 r=0.01 r=0.001 Cartoon model Dust Synchrotron Multipole ` lensing A dust A synch l=80 β dust α dust ε β synch α synch frequency spectral indices spatial spectral indices dust/synch spatial correlation 24

34 BK14 Results Allow dust/sync correlation A synch A dust L/L peak dust vs. r degeneracy lifted Put priors on the frequency spectral indices of dust & sync Marginalize over generous ranges in spatial spectral indices r A dust A synch 25

35 BK14 Results Allow dust/sync correlation A synch A dust L/L peak dust vs. r degeneracy lifted r < 0.09 (95% CL) Put priors Put on the priors frequency on the spectral indices of frequency dust & sync spectral indices of dust & sync Now beats temperature constraints Marginalize over generous ranges in spatial spectral indices r A dust A synch 25

36 BK15 Simulated Results Allow dust/sync correlation ( now [-1,1] ) A synch A dust L/L peak Put priors on the frequency spectral indices of dust & sync Simulation Marginalize over generous ranges in spatial spectral indices Plus: many alternate analyses presented Foreground priors Including EE WMAP/Planck data Dust decorrelation r A dust A synch 25

37 BK15 Simulated Results: Variations with Data Selection BK15 sim119 BK+WMAP+HFI BK+WMAP BK15 sim494 Simulation BK+LFI BK+WMAP BK+WMAP BK+LFI r A dust A synch 26

38 Dust Decorrelation? Planck 2016 Planck 2018 R` = C`( ) p C`( )C`( ) Spatial variations of the dust SED or polarization angle? A departure of the correlation ratio from unity that cannot be attributed to a spurious decorrelation due to the cosmic microwave background, instrumental noise, or instrumental systematics detected at more than 99% confidence We find no evidence for a loss of correlation. might not be a problem for CMB experiments aiming at a primordial B-mode detection limit on the tensor-to-scalar ratio r ~

39 BK15 Simulated Results: Variations with Dust Modeling BK15 sim119 BK15 sim266 Soon out! Simulation r A dust A synch degree of dust decorrelation from spatial SED variation 28

40 BICEP3: Super Receiver 52cm All 95 GHz 2560 detectors in modular focal plane 26 cm Large-aperture optics and infrared filtering > 10x optical throughput of single BICEP2/Keck receiver Bicep2 Bicep3 Keck receiver BICEP3 29

41 30

42 Keck Array Frequency Coverage Simple raw observing effort, doesn t take into account how years performed Bicep2 receiver at 150 GHz in Keck Array receivers all at 150 GHz in replaced two 150 GHz receivers with 95 GHz receivers in replaced two additional 150s with 220s for Soon out! 31

43 +B3 Keck Array Frequency Coverage Simple raw observing effort, doesn t take into account how years performed Bicep2 receiver at 150 GHz in Keck Array receivers all at 150 GHz in replaced two 150 GHz receivers with 95 GHz receivers in replaced two additional 150s with 220s for 2015 switched 95 GHz receivers to 220 GHz for 2016 (BICEP3 at 95 GHz) 2016 Analysis ongoing 31

44 +B3 Keck Array Frequency Coverage Simple raw observing effort, doesn t take into account how years performed Bicep2 receiver at 150 GHz in Keck Array receivers all at 150 GHz in replaced two 150 GHz receivers with 95 GHz receivers in replaced two additional 150s with 220s for 2015 switched 95 GHz receivers to 220 GHz for 2016 (BICEP3 at 95 GHz) 2017 Analysis ongoing replaced a 220GHz receivers with 270 GHz in 2017 (BICEP3 at 95 GHz) 31

45 BICEP2 ( ) Stage 2 Stage 3 Keck Array ( ) BICEP3 (2015-) BICEP Array (2018-) Beam on sky Focal Plane Telescope and Mount detectors:

46 BICEP Array Under Construction 4 wide-field receivers 30/40 GHz 95 GHz 150 GHz 220/270 GHz 60 cm Wide-field cryogenic receiver 30GHz Focal plane layout 40GHz 33

47 BKP BK14 BK15 delensing with SPT See Kimmy Wu s talk 34

48 BICEP/Keck data: B-modes and Progress on r Kimmy Wu s talk Keck GHz 95 GHz no B-modes with B-modes Keck GHz + SPTpol 150 GHz Keck GHz Deep degree-scale maps: multiband for foreground separation Deep high-resolution maps: precision delensing BICEP-Keck / Planck joint analysis (published Feb 2015) raw sensitivity with no foregrounds or lensing: σ(r) = it is now all about component separation! σ(r) = arxiv: BICEP/Keck adds deep 95 GHz σ(r) = arxiv: BICEP/Keck adds deep 220 GHz expect σ(r) = next month 2017 BICEP/Keck plus SPTpol delensing (data all in the can) expect σ(r) = coming next year BICEP Array + SPT3G forecast σ(r) ~

49 Conclusions BICEP/Keck lead the field in the quest to detect or set limits on inflationary gravitational waves: Best published sensitivity to date Best proven systematic control at degree angular scales Adding 2014 data including, for the first time 95GHz data: Results in modest improvement: r 0.05 <0.12 goes to r 0.05 <0.09 However this is an important milestone: for the first time B-mode only constraint exceeds the sensitivity of (Planck) TT derived constraint (r 0.05 <0.12) 2015 data also includes 220GHz: Expected σ(r)=0.019 We can explore more data/model variations And we can go much further: BICEP3 is now online at 95GHz Delensing using SPT/SPT3G (see Kimmy s talk) and we have BIG plans for the BICEP Array σ(r)=

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