adsabs/AstroCLIMB huggingface dataset:
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: The reprocessed temperature profiles from Figure 2(a), with the color mapped to the latitude of the suboccultation point, as indicated in the color bar and legend. The 1σ uncertainty regions for the U0 ingress and egress are provided as a representative uncertainty. While there may appear to be a trend of northern latitudes having slightly warming temperatures, this is likely a reflection of the correlation of latitude and year and the temperature–year trends from Figures 4–6. There is no clear and compelling trend from this figure alone.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: The reprocessed temperature profiles from Figure 2(a) with the color mapped to the LST of the suboccultation point, as indicated in the color bar and legend. See the text for the definition of LST on Uranus. The 1σ uncertainty regions for the U0 ingress and egress are provided as a representative uncertainty. While there might appear to be a weak trend of midday times having warmer temperatures, that trend is disrupted by at least three instances. Additionally, LST is not as physically insightful for a planet with high obliquity near solstice, as was the case for many of these observations. As such, we find there to be no clear and compelling trend from this figure.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Comparison of reprocessed and original profiles. (a) Reprocessed profiles as in Figure 2, showing only the profiles that were previously published. (b) Originally published profiles. For references to the publications for the data in panel (b), see Table 1. We note that the original profiles have a closer agreement at the top of the profiles, which is consistent with their similar boundary conditions. Use of more realistic boundary conditions (thermal gradient instead of isothermal) results in a greater spread, as seen in panel (a).
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: The reprocessed temperature profiles from Figure 2(a), with the color mapped to the SZA of the suboccultation point, as indicated in the color bar and legend. See the text for the definition of SZA. The 1σ uncertainty regions for the U0 ingress and egress are provided as a representative uncertainty. There is no clear and compelling trend from this figure.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. II. Revised Temperatures in the Upper Stratosphere and Lower Thermosphere
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Same as Figure B1.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Principal component values for all 11 meteorites studied across different grain sizes are shown with the “α-line” boundary from F. E. DeMeo et al. (2009) that separates S- and C/X-complexes. Marker size increases with grain size; this includes 45–90 μm, 90–150 μm, 150–300 μm, 300–500 μm, and 500–1000 μm. The dotted line connecting PC values of the same meteorite allows grain size variation to be seen. Slabs have been excluded owing to their drastically different values compared to powdered grain size samples.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: (a) Plot of 0.55 μm (photometric V filter) absolute reflectance of 5 of the 11 meteorites studied across grain size bins. Due to the number of samples, this plot has been separated into two. The samples in this figure have a relatively higher reflectance than those in panel (b). There is a trend of decreasing reflectance with increasing grain size. (b) Plot of 0.55 μm (photometric V filter) absolute reflectance of 6 of the 11 meteorites studied across grain size bins. There is a general trend of decreasing reflectance with increasing grain size. However, these samples show an increase in 0.55 μm reflectance at slab size. NWA 4024 shares an increase of reflectance at 90–150 μm with Fukang, which can be seen in panel (a).
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Plot of ∼2 μm band depth for 3 of the 11 studied meteorites across all grain sizes, including slab. Only those samples that show the 2 μm band are included here. It should be noted that NWA 4024 and Norton County are not included, as their 2 μm features are from terrestrial weathering.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Plot of ∼1 μm depth for 8 of the 11 studied meteorites across all grain sizes, including slab. The 1 μm band depth for most samples decreases with increasing grain size except for the slabs.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Plot of 0.8–1.8 μm spectral slope for 4 of the 11 studied meteorites across the five grain sizes, including slab. Note that the range used for NWA 6685 to find the slope was 1–2 μm.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Plot of Band I center for 8 of the 11 studied meteorites across all grain size bins, including slab.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Plot of the BAR vs. grain size for three of the samples covered in this study: acapulcoite Dhofar 125, mesosiderite NWA 6370, and ureilite Almahata Sitta. The BAR is the ratio of the Band II area to the Band I area.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Rare Meteorite Classes
Authors: K. I. Ridenhour, V. Reddy, A. Battle, D. Cantillo, N. C. Pearson, J. A. Sanchez
Figure caption: Plot of Band II center for 3 of the 11 studied meteorites across all grain size bins, including slab.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Schematics of the instrument-level TVAC chamber setup in the OCF. (a) The large TVAC chamber is shown with the door open and its rolling table positioned partly outside of the chamber. During TVAC testing, DRACO was covered in a temperature-controlled shroud (not shown). The path of the light through the collimator is shown in red. (b) A detailed schematic of the collimator. Here the gray lines show the path of the light through the system. M1–M5 represent other mirrors in the system. The steering mirror can be used to position the target with high accuracy throughout the FOV. The target, positioned at the focus of the collimator, can be a pinhole (used for geometric and focus tests) or a Ronchi ruling (used for MTF tests).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: (a) An example of a scene an observer looking out the DRACO boresight would see. The spacecraft and DRACO frames shown here are each oriented with respect to the scene, and not with respect to one another (see Figure 4 for their mutual orientation). Detector A and B labels are purposefully backward to illustrate that the view is looking out the DRACO boresight (i.e., looking through the back of the detector). The square image here corresponds to the central 2048 × 2048 pixels of the detector (Window 1; see Figure 5). (b) The scene as it appears on the DRACO detector, or in the image when viewed with software that places the image origin at the upper left corner. The image is mirror flipped across the x-axis from reality. (c) The scene as it appears when viewed with software that places the image origin at the lower left corner. This view matches reality and is simply rotated with respect to panel (a).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Examples of raw global and rolling shutter images of star cluster NGC 3766 taken during Star Cal B (see Section 4.3.2). Images here are shown with the origin at the lower left to match the scene an observer looking out the DRACO boresight would see. Top: a raw, global shutter image taken with 90 ms exposure time and 2× gain. A reset frame was subtracted on board the spacecraft. In addition to a number of stars, single-pixel popcorn noise can be observed. DRACO image dart_0391875686_12372. Bottom: a raw, rolling shutter image taken with 90 ms exposure time and 30× gain of a star cluster. The fixed-pattern noise is obvious because a bias frame has not yet been subtracted. Rolling shutter images do not exhibit popcorn noise. DRACO image dart_0391877527_07839.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: ConOps schematic for Star Cals A, B, and C. The star represents a reference point near the center of the cluster. The blue circles show the locations of the 13 spots DRACO was pointed to relative to that reference point. Black arrows show the paths taken while slewing between these positions. The black square is the DRACO FOV, shown centered on position 7. The black circle shows the approximate size of the pointing deadband for these observations relative to the DRACO FOV. The dotted line indicates the division between detectors A and B.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: The DART spacecraft frame (referred to as DART_SPACECRAFT in SPICE kernels) and DRACO (DART_DRACO) frame oriented correctly to one another. The origin of the DRACO frame is at the camera focal point. See the DART frames kernel and DART DRACO instrument kernel for more information. Detector A and B labels are purposefully backward to illustrate that the view is looking out the DRACO boresight (i.e., looking through the back of the detector). The dashed box shows the central 2048 × 2048 pixels (Window 1).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: The path of an image through the DRACO onboard image processing pipeline for (a) 512 × 512 images (e.g., Terminal and Final Phase images) and (b) 1024 × 1024 images (e.g., optical navigation, calibration, light-curve images). The Window 2 step was optional but enforced for Terminal and Final Phase images. The 512 × 512 image path fit within the link budget of the radio and supported real-time streaming. The 1024 × 1024 image path was often routed to onboard storage and replayed to the radio at a later time. Additional processing (not shown) was performed to support Small-body Maneuvering Autonomous Real-Time Navigation (SMART Nav) targeting and operated on image data immediately after onboard calibration (D. Bekker et al. 2021).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Diagram of the DRACO detector, indicating pixel numbering, readout direction, and the position of Window 1 (the central 2048 × 2048 pixels). Row numbers start from 1 to account for the header row (see Section 2.7). Corresponding pixels from both halves were read out simultaneously. Note that in order to show an image as an observer looking out the DRACO boresight would have seen, it has to be flipped vertically to place the origin at the lower left (see Section 2.4).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Location of DRACO on the DART spacecraft. The image shows the cover in its open position.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Overall DRACO instrument ground characterization flow. Section 5 provides details about the tests shown in bold.
Paper: A Novel Orbit Parameterization in Spherical Coordinates
Authors: Kevin J. Napier, Matthew J. Holman
Figure caption: Schematic of the coordinate system described in this paper. The tangential coordinate plane is defined by the ﹩\hat{{\boldsymbol{A}}}﹩ and ﹩\hat{{\boldsymbol{D}}}﹩ vectors. The ﹩\hat{{\boldsymbol{r}}}﹩ vector is going into the page at the coordinate origin. The angle ψ is measured with respect to the ﹩\hat{{\boldsymbol{A}}}﹩ vector, and v Ω gives the body’s speed in the plane. Note that for values of ψ ∈ (−π/2, π/2), all orbits are prograde with respect to the sphere’s equator. All other values of ψ represent retrograde orbits. Intuitively this makes sense because the prograde orbits go in the counterclockwise direction when viewed from above the solar system.
Paper: A Novel Orbit Parameterization in Spherical Coordinates
Authors: Kevin J. Napier, Matthew J. Holman
Figure caption: Relative sky density of synthetic objects encounterable by Lucy between 2032 July 16 and 2033 January 15, as viewed from Cerro Tololo on 2024 July 16.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: (a) Composite image of Vega made from combining images with a range of exposure times, allowing for an assessment of PSF over a large dynamic range. The image is logarithmically stretched to reveal the very low level, extended brightness halo surrounding Vega that is likely caused by in-field stray light. The six spikes around the star are caused by light diffracted by the spider structure that holds DRACO’s second mirror in place. Vertical and horizontal dotted lines show the positions of the profiles taken across the center of Vega shown in panels (c)–(e). A few background stars are visible. (b) The central region of pixels centered on Vega, stretched linearly such that the PSF can be visualized. No pixels are saturated in the composite. (c) Horizontal (DRACO pixel X-direction) and vertical (DRACO pixel Y-direction) profiles taken across Vega. The halo is 5–7 orders of magnitude lower than the peak brightness. The rectangles indicate the data shown in panels (d)–(e). (d, e) Zoomed-in views of the central PSF, with XFWHM and YFHM shown, respectively, as measured by fitting the core of the light distribution (not the wings).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Measurements of the PSF FWHM made on 236 rolling shutter, 30× gain images of NGC 3766. The stars wandered across the 1024 × 1024 binned pixels of the detector, enabling an evaluation of the spatial variability of the FWHM. There appears to be a small dependence between FWHM measurements and the location within the FOV. The plots displayed here have the image origin at the lower left (detector A is on the bottom).
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: Measurements of the PSF FWHM made on two low-smear DRACO images (dart_0376847253_36504 and dart_0376848147_03798). The left panel shows the results in the DRACO x–y axes. The right panel shows the results as the major and minor axes of the best-fit Gaussian ellipse. The radius of the dark circle plotted at the mean position is the error in the mean FWHM value. The lengths of the error bars are the standard deviations of the measurements, as are the uncertainties quoted in the lower right corner of the plot. The error reported for the mean value is the standard error (i.e., error in the mean). The pink dashed line indicates a 1:1 ratio.
Paper: Calibration and In-flight Performance of DART’s Didymos Reconnaissance and Asteroid Camera for OpNav (DRACO)
Authors: Carolyn M. Ernst, R. Terik Daly, Zachary J. Fletcher, Kyle J. Ryan, Andrew F. Cheng, Syau-Yun W. Hsieh, Tony L. Farnham, Carolyn A. Sawyer, Allison K. Glantzberg, Olivier S. Barnouin, Harold A. Weaver, Dmitriy L. Bekker, Nancy L. Chabot, Raymond C. Espiritu, Joseph Dickman, Jacob M. Greenberg, Derek A. Lewis, Bryan J. Maas, Declan M. Mages, Hari Nair, Tyler W. Nelson, Luis M. Rodriguez, Brian P. Rush, Ronald D. Smith, C. Dany Waller
Figure caption: QE of an engineering prototype FPE. The measured data match well with the manufacturer data. The VIS and UV measurements were taken with different reference photodiodes to determine the lamp irradiance. Note that the small upturn at the left-hand side of the manufacturer data is likely a measurement error.