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Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Ray-trace schematic of the 90 GHz telescope showing the major optical components. Color-coded rays tracing the light’s path originate from five fields on the sky and converge at five feedhorns in the focal plane. The VPM is the first optical element in the path of the incoming light through a comoving baffle. The comoving baffle comprises a “cage” structure (shown in Figure 2, which houses the fore-optics and the receiver), and an “extension.” The solid black line shows the boresight pointing; the dashed red line connects the top of the VPM mirror to the rolled top of the extension. At 45° elevation and 0° rotation about boresight, the red line (when extended) clears the highest ground feature by 6° in elevation. Stray light from the ground entering through other sides of the baffle is terminated on absorber covered interiors of the baffle (see Section 4.4 for further discussion). The primary and secondary mirrors produce an image of the VPM near the cold stop. High-density polyethylene (HDPE) lenses then focus the light onto feedhorn-coupled dual-polarization detectors with speed f/1.8. Seven detector modules, each comprising 37 pixels, constitute the focal plane array. A picture of the installed detector modules is shown, surrounded by an absorber-coated copper structure serving as a field stop. See the Appendix for further details of the optical design.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Photos of a telescope mount showing the seven boresight rotation angles. Each of two mounts can support two telescopes. This rotation keeps the telescope boresight pointing unchanged while rotating the detector antenna orientation on the sky in steps of 15° within a 90° range, thus enabling measurement of the polarization signal projected onto different orientations.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Extended intensity beam map. Left: Peak-normalized instrument beam, obtained from a combination of the average beam map from dedicated Jupiter scans and the detector-centered Moon map generated from survey data. The color bar scale is logarithmic from 1 to 10−4, and linear from 10−4 to −10−4 in order to display negative values. The negative values in this intensity beam map are a result of mapping artifacts and measurement noise. The 8° radius dashed circle indicates the extent of the measured 1D beam profile plotted in the right panel. Right: Azimuthally averaged beam profile to 8°. The shaded error region represents 1σ uncertainties, also indicated by the blue line. The red line is the best-fit model (Equation (4)). The green line shows the solid angle enclosed as a function of angular distance. The larger scatter in the measured beam profile between 1.°5 and 4° is a result of different bin sizes used between the planet beam map and the survey Moon map.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Examples of ghosting beam. Selected detector-centered peak-normalized Moon maps in intensity (top) and linear polarization (bottom) with their locations on the focal plane indicated by the array plot in the background. These maps span 30° × 30° about the center of the focal plane indicated by the black “+” symbol. Subpercent level reflections (relative to the peak) off the opposite side of the focal plane are seen in these maps. For instance, in the top right panel, the bright circular spot with unit amplitude is the main beam. On the other side of the focal plane, ghosts trace the field stop between detector modules. The negative blue dots near the main beam come from electrical crosstalk.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Moon scan illustration and coordinate-system conversion. Left: Schematic of the focal plane detector array, centered at a scan elevation of 45° with a −45° boresight rotation. Each blue (orange) bar represents a detector sensitive to −45° (+45°) polarization orientation. The Moon slowly rises or sets (the red dot indicates the position of the Moon for an example scan, and the red arrow indicates that it is setting in this example) as the telescope scans ±14° along the azimuthal direction. In the azimuth–elevation coordinate system, the focal plane array spans 23.°6 in azimuth and 24° in elevation. The dashed line represents the plane of optical symmetry for the telescope. Right: Moon positions are transformed to the “Receiver Coordinate System,” where the telescope boresight pointing is the origin. Every detector has fixed Δx and Δy angular offsets while the Moon appears to zigzag across the array. In the azimuth–elevation coordinate system, both the telescope and the Moon are moving, while in the receiver coordinate system only the Moon is moving. The apparent movement of the Moon across the array due to Earth’s rotation during one such scan is indicated, where the spacing of the zigzag path is exaggerated for illustration.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Left: Ratio of measured FWHM along the major and minor axes plotted against FWHM along the minor axis for each detector. The error bars represent 1σ measurement uncertainties. Data points closer to the horizontal dashed line correspond to more circular beams. Middle: histogram showing the distribution of the measured beam effective FWHM (Equation (2)) for all detectors. Right: Histogram showing the distribution of the beam orientations, defined as the angle on the sky from the local meridian to the beam major axis with positive (negative) corresponding to a counterclockwise (clockwise) direction. In the middle and right panels, each row represents a focal plane module. The large spread in the distribution for the central module 4 is indicative of nearly circular beams. Boresight rotations help with mitigating the impact of deviations from perfectly symmetric circular beams. The correspondence between colors and modules is the same in all plots.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Gain calibration factors for −45° oriented detectors (ϵ −) plotted against corresponding +45° oriented detectors (ϵ +) in the pair. Each subplot represents a focal plane module, where the module numbers are annotated in the top right corners. The large scatter in the data and deviations from the diagonal dashed line are due to variations in detector optical efficiencies within each module and within each pair, respectively. Taking into account various detector performance parameters, the wafers from modules 2, 4, 5, and 6 were swapped with new wafers having more uniform optical efficiencies during the 90 GHz instrument upgrade (Núñez et al. 2023) in 2022.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Deviations from the pointing model in arcminutes for telescope azimuth, elevation, and boresight rotation angle inferred from Moon scans over the period of 2018 July through 2021 April. The seven telescope boresight angles ranging from −45° to +45° are indicated by different colors. Diamonds represent deviations inferred from dedicated Moon scans, and tri-left markers from survey Moon scans. Deviations are inferred separately from scans conducted during the Moon rising and setting, when available. Gray vertical lines (eight in total) highlight the start date of each new pointing correction model based on a series of dedicated Moon scans. The standard deviations of the pointing error are 1.′3, 2.′1 , and 2.′0 in azimuth, elevation, and boresight rotation angle, respectively, which amount to a combined pointing uncertainty that is ∼7% of the beam FWHM.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Left: Measured detector pointing offsets within a colocated pair are represented by vectors originating at the pointing of the −45° oriented detector and directed toward the pointing of the +45° oriented detector on the sky. The length of the vectors are exaggerated by a factor of 20 for visibility (see annotation in the top right corner). The different colors represent the seven modules (module numbers are annotated) that constitute the focal plane. The modules are numbered left to right rowwise starting from the bottom row. Right: Histogram showing the distribution of the differential pointing offsets grouped by focal plane module. Most of the differential pointings are within ﹩3{\rm{^{\prime} }}﹩.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Left: Per-detector beam shapes and orientations as projected onto the sky represented by ellipses whose major and minor axes correspond to the FWHM beamwidths. The +45° and −45° oriented detectors are shown in orange and blue, respectively. Right: The blue filled circles are centered at the location of feedhorns that have fully operational pairs of detectors and represent the differential beam shapes within a colocated ±45° detector pair, the area of the circle being proportional to the extent of beam mismatch as defined in Equation (3). The two pairs with the largest mismatch in beam shapes are indicated by the red and green arrows.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Instrument beam. Peak-normalized beam map to 4° in radius obtained by stacking beam measurements of 206 detectors from multiple dedicated scans of Jupiter. The color bar scale is logarithmic from 1 to 10−3, and linear from 10−3 to −10−3 in order to display negative values. The map has a resolution of 0.05°.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Electrical crosstalk per readout column inferred from dark detector and dark SQUID channels and their 1σ uncertainties. Each color represents a module as indicated in the legend, and each module is read out by four columns. The gray region represents electrical crosstalk <1%.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption:  T → P leakage probed using dedicated Jupiter scan data. Top row: Peak-normalized average intensity maps spanning 3° × 3° generated from single-detector (−45° and +45° oriented detectors averaged separately) and pair-differenced raw (i.e., not demodulated) Jupiter scan data. The black contours are plotted at 3, 6, and 10 dB below the peak. Bottom row: Corresponding average linear polarization maps (Stokes U in the instrument frame) generated from single-detector and pair-differenced demodulated Jupiter scan data. These maps are normalized by the peak value of the intensity map. The contours from the corresponding intensity maps are overplotted. Jupiter is not expected to have a polarized signal at 90 GHz. However, a dipolar T → P leakage component is seen in the Stokes U maps made from averaging over only −45° or +45° oriented single detectors. In addition, there is also a monopole leakage component in the average single-detector Stokes U maps. No leakage signal is seen in the Stokes U map made from pair-differenced detector data in the bottom right panel.
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Simulations of beam systematics induced by internal reflections and dipolar T → P leakage. Modeled systematic (only) beams for dipolar T → P leakage and internal reflections (i.e., ghosting) are convolved with simulated sky temperature and linear polarization maps using pisco (Fluxá et al. 2020). The simulated maps are based on Planck CMB realizations with B-mode amplitude set to zero. The resulting power spectra are plotted and represent the expected systematic bias to the EE (top) and BB (bottom) power spectra. The curves with downward-pointing arrows represent the 95% confidence level upper limit for systematics that are not detected given the sample variance in the simulations. The red squares indicate negative values in the orange curves. These spectra are equivalent to the difference between the auto spectra from maps with and without systematics. The expected impact of these systematics that are not accounted for in our cosmological beam model are at the subpercent level compared to the cosmological signals (dashed lines, BB corresponds to the primordial B-mode power spectrum for r = 0.01; Planck Collaboration et al. 2020c).
Paper: Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance
Authors: Rahul Datta, Michael K. Brewer, Jullianna Denes Couto, Joseph Eimer, Yunyang Li, 云炀 李, Zhilei Xu, 智磊 徐, Aamir Ali, John W. Appel, Charles L. Bennett, Ricardo Bustos, David T. Chuss, Joseph Cleary, Sumit Dahal, Francisco Raul Javier Espinoza Inostroza, Thomas Essinger-Hileman, Pedro Fluxá, Kathleen Harrington, Kyle Helson, Jeffrey Iuliano, John Karakla, Tobias A. Marriage, Sasha Novack, Carolina Núñez, Ivan L. Padilla, Lucas Parker, Matthew A. Petroff, Rodrigo Reeves, Karwan Rostem, Rui Shi, 瑞 时, Deniz A. N. Valle, Duncan J. Watts, Janet L. Weiland, Edward J. Wollack, Lingzhen Zeng
Figure caption: Beam window function. Top: the nominal window function ﹩{b}_{{\ell }}^{2}﹩ unit normalized at ℓ = 0 plotted as a function of multipole ℓ. Bottom: The gray band shows the relative uncertainties ﹩{\rm{\Delta }}{b}_{{\ell }}^{2}/{b}_{{\ell }}^{2}﹩, estimated from simulated window functions computed from bootstrapped beam profiles. Uncertainties from the 1D beam debiasing are also plotted. Residuals (in percentages) between test window functions computed to understand impact of pointing uncertainties and far-sidelobes and the nominal window function are also plotted.