The Atacama Cosmology Telescope: ACTPol Suzanne Staggs CMB2013 - PowerPoint PPT Presentation

The Atacama Cosmology Telescope: ACTPol Suzanne Staggs CMB2013 Okinawa, 11 June

The Atacama Cosmology Telescope • 6m off-axis Gregorian telescope • 2m primary • Located at 5200 m (0.5 mm PWV) • Latitude -23 o

The Atacama Cosmology Telescope • 6m off-axis Gregorian telescope • 2m primary • Located at 5200 m (0.5 mm PWV) • Latitude -23 o ACT ground screens: large co- moving screen and 13 m • 72 panels outer screen. Reflector • 25-30 µ m rms Secondary Reflector • All aluminum

ACTPol – Next Generation Receiver • 16x mapping speed of MBAC • 150 GHz and 100 GHz • Polarization-sensitive detectors Funded 2011-2016; first array in the field now, first light imminent. Staggs; Okinawa 2013

ACTPol Science Goals in Brief Statistical Noise Curves Cluster Catalog - Planck Overlap with existing surveys • 10 Complementary to SPT/Planck ACT Wide • Improved power spectra – (TT) • EE 1 TE • E-modes • B-modes BB • ACT Deep 0.1 Deflection field • Maps – CMB • 0.01 Deflection field • 0 2000 4000 Wide survey (~4000 deg 2 ); Deep survey (5 fields, each 25 deg 2 ) Details in Niemack et al, arXiv:1006.5049 Staggs; Okinawa 2013

ACTPol Science Goals in Brief EE Power Spectrum Smaller than TT but cleaner! • At l ~ 3000, CMB is 20% • polarized; dust is 1-2% polarized. Forecast factor of ~2 • improvements over forecasts for Planck (TT and EE) on: Σ m ν (.06 eV) • Y He (0.005) • Ω b h 2 (1.3 x 10 -4 ) • Forecasts N eff (CMB alone, 0.5) • relatively Recall Y He impacts the high-l spectrum simple so because those modes enter the horizon far. while He is not yet fully ionized. Staggs; Okinawa 2013

Polarization & Lensing (Reminder) EE and BB and Deflection Field Maps Lensing peak smearing more • evident for polarization Note also SHO – x & v out-of-phase • enhancement TT is a ~3:1 combo of x & v • at high l Polzn peaks are sharper! • BB modes directly generated by • lensing ACTPol BB errors Planck BB errors From Zaldarriaga & Seljak, 1998 Staggs; Okinawa 2013

CMB Lensing Deflection Field Power Spectrum and Maps CMB Lensing is going to explode as a field in the next few years Planck S 100 100 i g n 75 70 a 4 50 l 6 - ACT -I t 50 7 20 o ACT Full - SPT -1 N 25 SPT Full o i Planck s 0 +ACTpol/SPTPol e ACTpol Large Sky Pre-Planck figure from S. Das Staggs; Okinawa 2013

ACTPol Lensing Goals in Brief Dark Energy from Deflection Field Power Spectrum and Maps Lensing kernel at intermediate z (<5) the CMB Alone! • Breaks degeneracies • Makes cross-correlation studies rich • Sherwin et al, 2011 Plot from Smith, Cooray, Das, Dore et al, 2009 White Paper. Staggs; Okinawa 2013

ACTPol Lensing Goals in Brief Dark Energy from Deflection Field Power Spectrum and Maps Lensing kernel at intermediate z (<5) the CMB Alone – • Breaks degeneracies • Updated! Makes cross-correlation studies rich • Planck Collaboration, XVII, 2013 Plot from Smith, Cooray, Das, Dore et al, 2009 White Paper. Staggs; Okinawa 2013

ACTPOL Lensing Forecasts Assuming no systematics other than instrumental noise, these plots show the signal and noise power spectra for the Deep and Wide configurations. Signal Signal Optimal Noise Optimal Noise ACTPOL-WIDE: ACTPOL-DEEP: 4000 sq-deg @ 20 µ K-arcmin (temp) 150 sq-deg @ 3 µ K-arcmin (temp) and 28 µ K-arcmin (pol) and 5 µ K-arcmin (pol)

Primordial B-modes 10 4 Primordial B- Temperature modes peak at measurements 10 2 even larger ACBAR ACT BICEP BOOMERANG angles than TT! CAPMAP CBI DASI MAXIPOL QUAD (c > c/3 1/2 ) QUIET SPT 10 0 WMAP lensing E-mode -2 B-mode 10 dashed horizontal lines- limits on B-modes primordial solid vertical lines - measurements of T and E 100 10 1000 Staggs; Okinawa 2013

Primordial B-modes Primordial B- modes peak at even larger angles than TT! (c > c/3 1/2 ) ACT has great dynamic range (cross-linking, ML maps  little filtering) ... but ACTPol’s guaranteed capability in the GW quest is delensing because large angles are hard with large telescopes. Staggs; Okinawa 2013

ACTPol Cross-correlations 25,000 deg 2 available; wide survey will overlap with SDSS-III BOSS; deep surveys may overlap with XMM-LSS, CFHTLS, HerMES,UKIDSS, DES, GAMA, etc

ACTPol Cross-correlations HyperSuprime Camera on Subaru • Prime Focus Spectrograph • IPMU/NAOJ/Princeton*/ Caltech/JHU/Sao Paolo/ Marseilles/Edinburgh • First light this summer • Galaxy cosmic shear in wide and deep surveys; overlap to ACTPol with some of each *but not me

ACTPol Instrument (Deltas) Old optical path • Increased throughput optical design (M.Niemack) • Wideband silicon lenses (J. McMahon) • Feedhorn-coupled 30 cm polarization arrays of TES bolometers from NIST New optical path (TRUCE) New optical path • 2 arrays at 150 GHz; • 1 at 100/150 GHz • 100 mK cryogenics with 24 hour operations 30 cm

Wide Bandwidth Silicon Lenses • Low loss material • High n = 3.4 => excellent image quality – Need good AR coating • Developed 2-layer simulated-dielectric AR coating Smallest ACTPol lens ACT production developed at UMich in McMahon group ( Datta, Niemack, McMahon et al. in prep. )

Polarization Sensitive Detectors Truce Collaboration: ABS, SPTPol, and ACTPol ( ABS: Essinger-Hileman et al. LTD 2009, SPTPol: Bleem et al. JLTP 2012, ACTPol: Niemack et al. SPIE 2010 ) • Feedhorn Coupled TES Polarimeters TES bolometer • Bulk absorption vs. Superconducting circuits • 2D wafers (cf 1x32) 5mm Old ACT detector 1 mm 150 GHz ABS single detector OMT couples to feedhorn

Silicon Polarimeter Arrays Silicon feedhorn array Sub-array with 255 TES Polarimeter 5mm 90/150 GHz path • Three arrays (~1000 TES each) • 0.1K bath temperature (0.3K previously) Better detectors + optics + cryogenics => ~ 4x increase in sensitivity (16x mapping speed) 150 GHz paths

Detectors + TDM muxing SQUID Readout Superconducting flexible cabling; double layer Multiplexing SQUIDs, shunt resistors, Nyquist 0.3 m eters Staggs : Okinawa 2013

Detectors + TDM muxing SQUID Readout Monolithic feedhorn array Staggs : Okinawa 2013

First ACTPol Array! Emily Grace, Laura Newburgh and Christine Pappas with the first completed ACTPol array. See Emily Grace’s poster! Characterization and Performance of a Kilo-TES Sub-Array for ACTPol Emily Grace 1 for the ACTPol Collaboration 1 Department of Physics, Princeton University, Jadwin Hall, Princeton, NJ 08544 (Email:egrace@princeton.edu) ABSTRACT: ACTPol is a polarization-sensitive receiver upgrade to the Atacama Cosmology Telescope, located at an elevation of 5200 meters in the Atacama Desert in Chile. With the new receiver, we will make millimeter wavelength measurements of the small-scale polarization anisotropies of the Cosmic Microwave Background (CMB) to explore structure formation, constrain the sum of the neutrino masses, probe early dark energy, and perform other cosmological tests. ACTPol will employ three arrays of transition edge sensor (TES) bolometer detectors. The detectors, with a target transition temperature of 150 mK, will be operated at a bath temperature of ~100 mK provided by a dilution refrigerator. One array operating at a central frequency of 150 GHz and consisting of 1020 TESes has recently been installed in the telescope at the ACT site.. We anticipate fielding a second identical array and a multi-chroic array that simultaneously measures 90 GHz and 150 GHz near the end of this observing season.

ACTPol Receiver Deployment Observing the sky with the receiver at 17kft Putting the receiver into the telescope cabin ~ last week! Staggs; Okinawa 2013

ACTPol Receiver Deployment Special thanks to graduate students Ben Schmitt and Marius Lungu in the field with Pato Gallardo and Masao Uehara. Staggs; Okinawa 2013

THE END Many thanks to many collaborators for slides, figures & slide concepts.