PoS(CMB2006)071 http://pos.sissa.it/ ce. ov, Bill Jones, Chao-Lin A Columbia, Canada ute of Technology, USA ive Commons Attribution-NonCommercial-ShareAlike Licen , Dick Bond, Olivier Doré ∗ [email protected] Copyright owned by the author(s) under the terms of the Creat c Carlo Contaldi Theoretical Physics Group, Imperial College, UK Brendan Crill IPAC, California Institute of Technology, USA Lionel Duband Commissariat A L'energie Atomique, France Mark Halpern Deptarment of Physics and Astronomy, University of British Kuo, Andrew Lange, Peter Mason, Amy Trangsrud Division of Physics, Math and Astronomy, California Instit CITA, University of Toronto, Canada E-mail: Rick Bihary, Tom Montroy, John Ruhl Department of Physics, Case Western Reserve University, US Peter Ade, Carole Tucker Cardiff University, U.K. James Bock, Warren Holmes, Jerry Mulder, Anthony Turner NASA, Jet Propulsion Laboratory, USA Justus Brevik, Abigail Crites, Sunil Golwala, Viktor Hrist Carrie MacTavish SPIDER: A Balloon-Borne Polarimeter for Measuring Large Angular Scale CMB B-modes PoS(CMB2006)071 ce. MB B-mode polarization. will map out roughly 50% of the stralia in December of 2009 and m primordial gravity waves domi- rom 80 GHz up to 275 GHz enabling SPIDER sity of Toronto, Canada ound. ive Commons Attribution-NonCommercial-ShareAlike Licen is a balloon-borne polarimeter that is designed to measure C will target large angular scales where the B-mode signal fro The experiment is scheduled to launch from Alice Springs, Au nates. In a mid-latitude, around the world,sky. 25 The day instrument flight will observe in fiveaccurate freqencies characterization ranging of f the interstellar dust foregr Speaker. SPIDER ∗ Copyright owned by the author(s) under the terms of the Creat c CMB and Physics of the Early20-22 Universe April 2006 Ischia, Italy

Gene Hilton, Kent Irwin National Institute of Standards and Technology, USA Barth Netterfield, Enzo Pascale, Marco Viero Department of Physics/Astronomy and Astrophysics, Univer PoS(CMB2006)071 SPIDER opticsare based on the BI- Reionization peak of the ts the large angular scale ℓ will also measure the curl-free vely probes the energy scale of matic telescope inserts enclosed SPIDER i-frequency experiment he low- ermination of the Compton depth, The bital experiments. For example the gns incorporated in the BLAST and will use a new generation of antenna- with unprecedented precision. This aced at each telescope aperture, will gnal. round the world in roughly 25 days. gular Scale CMB B-Modes SPIDER tion of CMB foregrounds essential to any SPIDER Figure 2: CEP design. SPIDER willhalf-wave incorporate plate to a modulate incoming rotating polarization signal. 2 optical train, show in Figure 2 is based on the well- flight plan is to launch from Alice Springs, Australia in will spin in azimuth with telescopes fixed in elevation. The SPIDER SPIDER SPIDER payload is designed to SPIDER is a balloon-borne millimeter-wave polarimeter that targe The SPIDER The instrument, depicted in Figure 1, consists of 6 monochro , and possibly th details of the Reionization epoch. As a mult EE angular power spectrum will significantly improve the det E-mode component of the CMB. Constraining the amplitude of t B-mode polarization of the CMB.Inflation, Probing addressing CMB the B-modes most effecti fundamental of questions. Figure 1: τ Carrie MacTavish SPIDER: A Balloon-Borne Polarimeter for Measuring Large An 1. Introduction 2. The Spider Instrument and Flight space mission that would target the tiny CMB polarization si will measure the polarizedrepresents emission a crucial from step toward interstellar the dust accurate characteriza in a single LN/LHe cryostat. characterized BICEP design. Aprovide ideal rotating polarization half-wave modulation. plate, For detectors pl obtain maximum sky coveragethirty from day a mid-latitude twenty balloon to world. flight The experiment around will the map outof roughly the 50% sky observing only at night. experiment builds on thepayload legacy attitude of control several system successful willBOOMERANG subor use experiments. the The same basic desi coupled bolometer arrays. The December 2009, maintaining constant latitude, traveling a PoS(CMB2006)071 SPIDER SPIDER s) √ ividing the single 7.8 4.2 4.4 9.0 CMB 15.5 35. Curves are esti- K µ Sensitivity Instrument = ( e simulated ℓ meets this challenge by sensitivities in each of the he CMB polarization on s) σ √ 1 CMB 110 100 204 351 100 will have a total of 2312 detectors K µ Sensitivity ( SPIDER obtaining high precision measure- Single-Detector SPIDER of pixels/detectors in each band and d emission from dust dominates and und emission. The vertical bars show es. y’s range in elevation. SPIDER gular Scale CMB B-Modes uency from 80 GHz up to 275 GHz. Fig- )288 200 512 512 512 × ctors. (2 Detectors Number of Figure 4: mates for foreground dust (risingand with frequency) synchrotron (fallingdata with points are frequency). from the WMAP 3 The year data [1]. 5 observing frequencies at 3 )144 100 256 256 256 × Pixels Spatial (2 Number of 72 58 40 26 21 Beam FWHM (arcmin) 35 at each of the observing frequencies. A summary of = observing bands. Instrument sensitivities are derived by d sky coverage for a ℓ 19 24 35 54 66 (GHz) Bandwidth SPIDER SPIDER 80 100 145 225 275 Band Science (GHz) ’s primary scientific goal is to measure, with high fidelity, t sensitivities at Observing σ Simulated aims to map out approximately 50% of the sky. Figure 3 shows th 1 Summary of Astrophysical foregrounds will be the biggest challenge to SPIDER SPIDER observing, with high sensitivity, in 5 bandsure ranging 3 in summarizes freq the current knowledgeSPIDER of polarized foregro sky coverage for 16 detectors spread over the bolometer arra 3. Astrophysical Foregrounds ments of CMB polarization. Atat high low frequencies frequencies the polarize polarized synchrotron emission dominat observing at 5 different frequencies. mid-latitude, 25 day flght, observing only at night. detector sensitivity by the square root of the number of dete observing bands, including beam sizes,detector/instrument bandwidths, sensitivities number is given in Table 1. 4. SPIDER Table 1: Figure 3: Carrie MacTavish SPIDER: A Balloon-Borne Polarimeter for Measuring Large An PoS(CMB2006)071 SPIDER SPIDER plane. parameter space r r (it may well be that − − s r τ n − by more than a factor of s n τ minimizes the contamination tational lensing. Figure 5 (left ata in the ision determination from nduced contribution). From the EE in a minimal inflation model, with a SPIDER gular Scale CMB B-Modes opy Probe (WMAP) Observations: h/0603450 will measure the TT, TE, EE and BB angular 4 constraints on r will break one of the more sever . τ SPIDER ) and a single tensor-to-scalar ratio, s SPIDER n sensitivity. balloon flight. SPIDER will improve the WMAP 8 year constraint on SPIDER represent a reduction in the allowed volume in the r and SPIDER τ plane. Top left panel: r − s n Polarization Analysis”, submitted to Astroph. J., astro-p [1] Page, L. et al., “Three Year Wilkinson Microwave Anisotr to the BB angular powerpanel) spectrum illustrates from the B-mode accuracy induced with by which gravi Minimal modifications towill the result existing inmultipole an pipeline BB: improved the accuracy errors oflytical will errors the (blue approach boxes) low which the arewith ana- fully respect optimal to theright leakage panel: of EE One-dimensional into constraints BB. on Top Bottom right panel: Two dimensionalin constraints the three (figure 5 top right panel). The by a factor greater then 50. References the inflation model is more complex in which case the high prec will be even more essentialspectrum for alone unraveling the gravity wave i power spectra. We consider the effects on cosmic parameters uniform power law primordial index ( large angular scales. By aiming for large scale B-modes Figure 5: Carrie MacTavish Data points and errors are derived from end-to-endrealizations of a simulated SPIDER: A Balloon-Borne Polarimeter for Measuring Large An degeneracies (figure 5 bottom right panel) remaining in CMB d constraints on