BibTex format
@article{O'Dea:2011,
author = {O'Dea, DT and Ade, PAR and Amiri, M and Benton, SJ and Bock, JJ and Bond, JR and Bonetti, JA and Bryan, S and Burger, B and Chiang, HC and Clark, CN and Contaldi, CR and Crill, BP and Davis, G and Dore, O and Farhang, M and Filippini, JP and Fissel, LM and Fraisse, AA and Gandilo, NN and Golwala, S and Gudmundsson, JE and Hasselfield, M and Hilton, G and Holmes, W and Hristov, VV and Irwin, K and Jones, WC and Kuo, CL and MacTavish, CJ and Mason, PV and Montroy, TE and Morford, TA and Netterfield, CB and Rahlin, AS and Reintsema, C and Ruhl, JE and Runyan, MC and Schenker, MA and Shariff, JA and Soler, JD and Trangsrud, A and Tucker, C and Tucker, RS and Turner, AD and Wiebe, D},
journal = {The Astrophysical Journal: an international review of astronomy and astronomical physics},
title = {Spider Optimization II: Optical, Magnetic and Foreground Effects},
url = {http://arxiv.org/abs/1102.0559v1},
volume = {738},
year = {2011}
}
RIS format (EndNote, RefMan)
TY - JOUR
AB - Spider is a balloon-borne instrument designed to map the polarization of thecosmic microwave background (CMB) with degree-scale resolution over a largefraction of the sky. Spider's main goal is to measure the amplitude ofprimordial gravitational waves through their imprint on the polarization of theCMB if the tensor-to-scalar ratio, r, is greater than 0.03. To achieve thisgoal, instrumental systematic errors must be controlled with unprecedentedaccuracy. Here, we build on previous work to use simulations of Spiderobservations to examine the impact of several systematic effects that have beencharacterized through testing and modeling of various instrument components. Inparticular, we investigate the impact of the non-ideal spectral response of thehalf-wave plates, coupling between focal plane components and the Earth'smagnetic field, and beam mismatches and asymmetries. We also present a model ofdiffuse polarized foreground emission based on a three-dimensional model of theGalactic magnetic field and dust, and study the interaction of this foregroundemission with our observation strategy and instrumental effects. We find thatthe expected level of foreground and systematic contamination is sufficientlylow for Spider to achieve its science goals.
AU - O'Dea,DT
AU - Ade,PAR
AU - Amiri,M
AU - Benton,SJ
AU - Bock,JJ
AU - Bond,JR
AU - Bonetti,JA
AU - Bryan,S
AU - Burger,B
AU - Chiang,HC
AU - Clark,CN
AU - Contaldi,CR
AU - Crill,BP
AU - Davis,G
AU - Dore,O
AU - Farhang,M
AU - Filippini,JP
AU - Fissel,LM
AU - Fraisse,AA
AU - Gandilo,NN
AU - Golwala,S
AU - Gudmundsson,JE
AU - Hasselfield,M
AU - Hilton,G
AU - Holmes,W
AU - Hristov,VV
AU - Irwin,K
AU - Jones,WC
AU - Kuo,CL
AU - MacTavish,CJ
AU - Mason,PV
AU - Montroy,TE
AU - Morford,TA
AU - Netterfield,CB
AU - Rahlin,AS
AU - Reintsema,C
AU - Ruhl,JE
AU - Runyan,MC
AU - Schenker,MA
AU - Shariff,JA
AU - Soler,JD
AU - Trangsrud,A
AU - Tucker,C
AU - Tucker,RS
AU - Turner,AD
AU - Wiebe,D
PY - 2011///
TI - Spider Optimization II: Optical, Magnetic and Foreground Effects
T2 - The Astrophysical Journal: an international review of astronomy and astronomical physics
UR - http://arxiv.org/abs/1102.0559v1
VL - 738
ER -