EPIC Medium-Scale Optical Design EPIC-IM optical layout EPIC-IM optical properties EPIC-IM optical properties EPIC-IM aberration per as long as mance

EPIC Medium-Scale Optical Design EPIC-IM optical layout EPIC-IM optical properties EPIC-IM optical properties EPIC-IM aberration per as long as mance www.phwiki.com

EPIC Medium-Scale Optical Design EPIC-IM optical layout EPIC-IM optical properties EPIC-IM optical properties EPIC-IM aberration per as long as mance

Clawson, Laura, Contributing Editor has reference to this Academic Journal, PHwiki organized this Journal EPIC Medium-Scale Optical Design Huan Tran Brad Johnson Mark Dragovan April 2009 EPIC-IM optical layout EPIC-IM optical properties Crossed Dragone ABS, Clover, QUIXOTE, QUIET . Unprecedented Large FOV 30×20 degrees Extreme Compact design Maximize resolution/throughput in shroud Telecentric NO refractive elements

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EPIC-IM optical properties “ as long as ce” telecentric focal plane => cold aperture Oversize mirrors EPIC-IM aberration per as long as mance Elliptical focal plane Limited by vignetting in Y Limited by aberration in X Multib in addition to High Frequencies in center 30—800 GHz 11,000 bolometers 30 deg/ 160 cm 150 GHz 30 GHz 30 GHz 850 GHz EPIC-IM cold vs warm

Main Beam Simulations Beam shapes No Refracting elements Calculated with Perfect Gaussian Feed horns Calculated as long as each “Hex” Polarized beam-scale distortions Fit Gaussians to beams Compare to benchmarks PO co in addition to cross–pol beams as long as single feed PO vs GO sanity check 30 GHz beam, from Grasp 9 Spot diagram, from Zemax

Main beam effects vs benchmark Fig. 6.4 Histograms of main beam effects. Refer to Section 5.4.1 as long as definitions of each effect. Histograms are color coded by frequency. Colored Arrows denote the frequency dependant goals from table 5.4. Goals as long as some EPIC-IM mirrors alone are below benchmarks w/o modulation Sidelobes Analyzed with Physical Optics(PO) an Geometric Theory of Diffraction (GTD) Aperture Integration Method Optics box Galaxy Convolution EPIC-IM straylight

EPIC-IM farsidelobes Co-pol beam, no baffling ~15d simulation time Calculate Equiv J Aperture Integration method Set J =0 outside 28d sim time Polarized Far Sidelobes (QT2 + UT2 + VT2)1/2 2 x15d sim time

Galactic Contamination In order to evaluate the effect of the signal from the far sidelobes, we convolve the qt beam maps with a 150 GHz sky model. The beam patterns have the primary beam masked, so only the response to the sidelobes are evident in the output. The sky data is an all sky map at long wavelengths (150 GHz). Since the beam is asymmetric, it is necessary to rotate the beam with respect to the sky at each point to get the complete convolution. The convolutions were done using the totalconvolver code developed by the Planck community. (Gorski et. al.) M.Dragovan (above) The 150 GHz sky map with which the beams are convolved. Units are log(uK). (below) The results of the convolution, qt beam with the above sky . Units are (uK). M.Dragovan In order to further quantify this result, we make two histograms: the number of pixels with a given intensity (left plot), in addition to the integrated histogram giving the total number of pixels less than a given intensity (right plot). This is similar to the plots that are shown as long as site surveys. By inspection one can see that fully 90% of the pixels are <0.2nK. M.Dragovan Goal 1nK GTD in addition to Polarization of sidelobes Our Far sidelobe simulations were as long as 3.25 –f –l, but Conclusions EPIC-IM has enormous throughput Systematic beam effects are below benchmark Sidelobes are manageable More analysis time required to be sure Clawson, Laura DAILY KOS Contributing Editor www.phwiki.com

Clawson, Laura Contributing Editor

Clawson, Laura is from United States and they belong to DAILY KOS and they are from  Emeryville, United States got related to this Particular Journal. and Clawson, Laura deal with the subjects like Opinion/Commentary

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