adsabs/AstroCLIMB huggingface dataset:
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Comparison of our color–absolute magnitude distribution to various literature sources, as presented in rows (1)–(5) (panel (a)) and (6)–(10) (panel (b)) of Table 2. The dots and triangles represent the distributions of all identified M giants. The ages of host OCs are color coded, with triangles indicating those over 1 Gyr.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Distance modulus comparison between the relations presented in rows (2) (brown) and (6) (yellow) of Table 2 vs. the parallax distances from Gaia DR3, segmented based on the latter distance modulus. The dots represent the median of each bin.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Distance modulus comparison between the linear relation fitted using the subsample vs. the parallax distances from Gaia DR3, with the reddening errors added ranging from –30% to 30% in steps of 5%. The blue line depicts the comparison between the two types of distance moduli without any reddening correction. The dots represent the median of each bin.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Distributions of M giants (shown as gray dots) from LAMOST DR9 and OCs (shown as blue dots) from Gaia DR3 in Galactic coordinates.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Top-left panel: the histogram distribution of the projected Galactocentric distances (R) of M giants with the bin width of 0.5 kpc, and different colors representing different disk heights. Top-right and bottom panels: The variations of the radial velocity (VR), azimuthal velocity (Vϕ), and vertical velocity (Vz) with R at different disk heights, respectively. The bin width is also 0.5 kpc and the number of M giants in each bin is greater than 50.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Left and top-right panels: distance modulus comparison between the photometric and spectroscopic distances, segmented based on the latter's distance modulus. The blue dots and error bars in the top-right panel represent the median and standard deviation of each bin. Bottom-right panel: the histogram distribution of the relative difference Δ = (dphoto − dspec)/dspec. The histogram is divided into 150 bins, with each bin having a bin size of approximately 0.02.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: The columns of each panel represent the distributions of the member stars of OCs (blue dots) and M giants (red stars) for positions in R.A.(α) and decl.(δ), proper motions in ﹩{\mu }_{{\alpha }^{\ast }}﹩ and ﹩{\mu }_{\delta }﹩, the CMD in G vs. GBP − GRP, as well as the mean parallax and total proper-motion dispersion of OCs. Here, the listed OCs are CWNU 1295, OC 0094, Teutsch 57, PHOC 9, NGC 6791, NGC 6819, UBC 203, UBC 1246, and UBC 1313. The identification numbers of M giants and the ages of OCs are displayed in the upper right of the CMD.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Left and top-right panels: distance modulus comparison between the photometric and parallax distances, segmented based on the latter's distance modulus. The blue dots and error bars in the top-right panel represent the median and standard deviation of each bin. Bottom-right panel: the histogram distribution of the relative difference Δ = (dphoto − dGaia DR3)/dGaia DR3. The histogram is divided into 600 bins, with each bin having a bin size of approximately 0.02.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: The space distributions of M giants in different spaces, where the Sun is located at (X, Y, Z) = (0, 8.34, 0) kpc.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Here, the listed OC is Theia 3318.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Here, the listed OCs are LP 1375, Waterloo 1, HSC 1450, UBC 1256, FSR 0702, Berkeley 70, Berkeley 24, Berkeley 34, and Berkeley 29.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Here, the listed OCs are UBC 1344, UBC 52, Juchert 20, HSC 1552, Kronberger 84, Koposov 53, UBC 1255, LP 1973, and HSC 1322.
Paper: Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: X. Y. Tang, C. J. Hao, J. Li, Z. Z. Yan, Y. Xu, J. Zhong, Z. H. Lin, Y. J. Li, D. J. Liu, L. F. Ding, X. F. Long
Figure caption: Here, the listed OCs are CWNU 1697, NGC 7789, HSC 1593, OC 0285, UBC 1314, SAI 25, UBC 1108, Berkeley 72, and HSC 1181.
Paper: Mass, Luminosity, and Stellar Age of Early-type Stars from the LAMOST Survey
Authors: Qida Li, Jianping Xiong, Jiao Li, Yanjun Guo, Zhanwen Han, Xuefei Chen, Chao Liu
Figure caption: Comparison of t (left) and [Fe/H] (right) between the two components in wide binaries. The t is predicted by our method, and the sample of wide binaries is obtained from H.-C. Hwang et al. (2022). The points are categorized into two types based on the Δ[Fe/H]. The values of [Fe/H] are from the catalog of M. Xiang et al. (2022).
Paper: Mass, Luminosity, and Stellar Age of Early-type Stars from the LAMOST Survey
Authors: Qida Li, Jianping Xiong, Jiao Li, Yanjun Guo, Zhanwen Han, Xuefei Chen, Chao Liu
Figure caption: The impact of metallicity on predictions in the testing set. Different columns represent the relative error distribution of the L, M, t, and M i. The first row shows the prediction with an incorrect [M/H] value input, and the second row shows the prediction without using [M/H]. The x-axis represents the predictions made using the correct metallicity values.
Paper: Mass, Luminosity, and Stellar Age of Early-type Stars from the LAMOST Survey
Authors: Qida Li, Jianping Xiong, Jiao Li, Yanjun Guo, Zhanwen Han, Xuefei Chen, Chao Liu
Figure caption: The difference in atmospheric parameters between M. Xiang et al. (2022) and W. Sun et al. (2021). The x-axis represents the values from W. Sun et al. (2021), and the y-axis represents the values from M. Xiang et al. (2022).
Paper: Mass, Luminosity, and Stellar Age of Early-type Stars from the LAMOST Survey
Authors: Qida Li, Jianping Xiong, Jiao Li, Yanjun Guo, Zhanwen Han, Xuefei Chen, Chao Liu
Figure caption: Comparison between our predicted L and Gaia’s observations. The values on the y-axis represent our predicted L, while the values on the x-axis are obtained through the conversion of Gaia DR3.
Paper: Mass, Luminosity, and Stellar Age of Early-type Stars from the LAMOST Survey
Authors: Qida Li, Jianping Xiong, Jiao Li, Yanjun Guo, Zhanwen Han, Xuefei Chen, Chao Liu
Figure caption: The impact of metallicity on predictions in our sample. Different panels show the predictions of L, M, t, and M i. The x-axis represents the prediction with [M/H], while the y-axis represents the prediction without [M/H].
Paper: Introducing the Condor Array Telescope. V. Deep Broad- and Narrowband Imaging Observations of the M81 Group
Authors: Kenneth M. Lanzetta, Stefan Gromoll, Michael M. Shara, David Valls-Gabaud, Frederick M. Walter, John K. Webb
Figure caption: Mosaic image of the M81 Group obtained through the luminance filter. The image is displayed block averaged by 32 × 32 pixels.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: DEM for the QS off-limb on 2007 March 11. The points are plotted at the temperature ﹩{T}_{\max }﹩, and at the theoretical vs. the observed intensity ratio multiplied by the DEM value.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Top: Hinode EIS quiet Sun count rates (DN s–1) in two cooler SW lines. Bottom: radiances with the present calibration.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Example fit effective area curves for an active region observed on 2011 July 26.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Top: Hinode EIS quiet Sun count rates in two cooler LW lines. Bottom: radiances with the present calibration.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Normalized effective areas at selected wavelengths in both the shortwave and longwave channels. For each line, the trend has been normalized by the initial value in order to show the relative change over time.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Two-dimensional histograms of the fit effective areas before smoothing (top two panels) and after smoothing (middle two panels). The bottom two panels show the “recalibration factor” computed as the ratio of pre-flight/fit (smooth) effective area. The white tick marks along the edge of the plots indicate the center of each 6 month fitting window.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Hinode EIS spectra (DN s–1/1″ slit) for the quiet Sun on-disk, for three sample dates. The dashed line is the scaled ground-calibration effective area.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: The ratio of EIS 193 to AIA 193 Å as a function of time using the pre-flight calibration (top panel) and the new, time-dependent effective areas (bottom panel). The EIS intensities have been convolved with the AIA 193 effective area to compute the expected AIA 193 count rates.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Emissivity ratio curves obtained with the present calibration for the main Fe XVII EUV transitions observed by Hinode EIS during two M-class flares, on 2012 March 9 and 2015 June 21. Iob is the calibrated measured intensity in erg cm−2 s−1 sr−1.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: The Fe XXIV 192/255 Å ratio relative to theory as a function of time using the pre-flight calibration and the present time-dependent effective areas.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Relative line ratios observed in AR over time. Ratios computed using the pre-flight (black diamonds), G. Del Zanna (2013a; GDZ; red X’s), H. P. Warren et al. (2014; WUL; green crosses), and new fit (blue circles) calibrations are shown for comparison.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Relative line ratios observed in QS over time. Ratios computed using the pre-flight (black diamonds), G. Del Zanna (2013a; GDZ; red X’s), H. P. Warren et al. (2014; WUL; green crosses), and new fit (blue circles) calibrations are shown for comparison.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Example fit effective area curves for an active region observed later in the mission on 2019 June 28.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Normalized emissivity curves for Fe XII, Fe XIII, Fe XIV, and Si X. The left two columns show the curves computed using the pre-flight and fit effective areas for a QS off-limb subregion observed on 2017 July 28. The right two columns show the results for a subregion containing an AR observed on 2019 June 28.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Ratio of two relatively strong Si and S lines in the LW channel, from the on-disk quiet Sun observations, and applying the various calibrations. Note the constancy of the ratio until early 2021 when the count rates in the S X 264.23 Å start to decrease considerably.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Relative density ratios computed using two density-sensitive line ratios for each of Fe XII, Fe XIII, Fe XIV, and Si X. Values computed using the pre-flight calibration are shown as black diamonds, and ratios computed from the new fits are shown as blue crosses.
Paper: Hinode EIS: Updated In-flight Radiometric Calibration
Authors: G. Del Zanna, M. J. Weberg, H. P. Warren
Figure caption: Effective areas for a sample of dates. The present one is displayed as a gray band, which shows ±20% from the recommended values.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Top left: raw averages of all 90 GHz (blue) and 150 GHz (orange) detectors with 1σ statistical error bars. Simulated bands are shown in black. Bottom left: final passband averages of all detectors measured with the FTS. The effects of the NDF are corrected for by dividing out its calibration function. This correction has the side effect of exponentially magnifying the noise floor, which introduces a large bias at high frequencies. To remove this bias, we subtract an exponential fit term based on estimates of the noise floor. The error bars are a quadrature combination of 1σ statistical and NDF calibration function errors. The main band shapes are in excellent agreement with the passbands expected from simulations of the designed optical system, while any spurious above-band features and noise are exponentially magnified by the NDF correction. Right: all 265 90 GHz and 195 150 GHz FTS detector measurements are plotted together. The simulated bands and final averages are overplotted. These measurements have been corrected for the NDF transmission.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Lower edge, upper edge, and center frequencies of individual detector passbands plotted vs focal plane position. The focal plane positions are found by mapping through the coupling optics of the FTS to obtain finely focused beams. The lower and upper edges are fitted as 5% transmission frequencies. To reduce noise in the fitted edges, these passbands are not corrected for the NDF transmission. There is a clear radial trend in the band edge frequencies, with pixels at the wafer edge measuring about 3% lower frequency than pixels at the wafer center. This is more prominent in the upper edge of 90 GHz, lower edge of 150 GHz, and upper edge of 150 GHz, all of which are defined by on-chip filters. The lower edge cutoff of the 90 GHz detectors is defined by the waveguide response that is independent of wafer properties. “A” group detectors are plotted with a left half-circle, and “B” or missing group detectors are plotted with a right half-circle. The large sections of missing detectors are due to a loose-fitting coaxial connection on the prototype detector array, which has since been reworked for the production arrays. The color bar percent spread shown is bounded by 99% intervals for the data set to avoid outlier effects.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Top: polarized beam power (band averaged from 85 to 120 GHz) as a function of grid rotation, measured with the holography setup described in Section 5.1. Copolarization (WO, blue) holds the source waveguide aligned with the receiver orientation. Cross polarization (WT, red) uses a 90° waveguide to make the source aligned perpendicular to the receiver orientation. The polarization model (K. Harrington 2022) is fit using a Markov Chain Monte Carlo with no instrument polarization. Bottom: constrained parameters from the polarization model include cross-polarization (CP), receiver angle ﹩{\theta }_{\det }﹩, and grid efficiency η grid. The cross polarization of the optical system is constrained to the percent level.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: Top: band-averaged near-field holography beam maps with and without the 1 K low-pass edge (LPE) filter in the optics tube. With the filter, beam maps show extra scattering in the top parts of the map through the upper portion of the LATR-Tester hexagonal window (hexagonal power around the main beam at roughly −20 dB due to reflection). Bottom: in orange is the measured reflectivity (1-transmission) of the 6.8 cm−1 low-pass edge filter, which is placed at the 1 K stage in the optics tube. The red (blue) line shows the measured integrated fractional power outside the main beam at each frequency with (without) the filter in the optics tube.
Paper: Simons Observatory: Predeployment Performance of a Large Aperture Telescope Optics Tube in the 90 and 150 GHz Spectral Bands
Authors: Carlos E. Sierra, Kathleen Harrington, Shreya Sutariya, Thomas Alford, Anna M. Kofman, Grace E. Chesmore, Jason E. Austermann, Andrew Bazarko, James A. Beall, Tanay Bhandarkar, Mark J. Devlin, Simon R. Dicker, Peter N. Dow, Shannon M. Duff, Daniel Dutcher, Nicholas Galitzki, Joseph E. Golec, John C. Groh, Jon E. Gudmundsson, Saianeesh K. Haridas, Erin Healy, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Claire S. Lessler, Richard A. Lew, Michael J. Link, Tammy J. Lucas, Jeffrey J. McMahon, Jenna E. Moore, Federico Nati, Michael D. Niemack, Benjamin L. Schmitt, Max Silva-Feaver, Robinjeet Singh, Rita F. Sonka, Alex Thomas, Robert J. Thornton, Tran Tsan, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R. Vissers, Yuhan Wang, Kaiwen Zheng
Figure caption: A single detector beam across three separate cooldown configurations measured using the thermal source described in Section 5.2. The first beam map (Cooldown 2) shows significant reflections and spills off the copper NDF mounting plate after it was initially installed at the end of the 4 K optics tube. The second beam map (Cooldown 3) shows a much-improved beam quality and signal-to-noise after repositioning the NDF to 20 mm from the focal plane. In the third beam map (Cooldown 4), the 1 K low-pass filter is removed with no adverse impact on the beam shape or noise level. The diffuse background hexagon observed in these beam maps is due to reflections between the copper focal plane and the NDF and will not be present in the on-sky optical configuration.