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Measuring the flatness of focal plane for very large mosaic CCD camera

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Jiangang Hao, Juan Estrada, Herman Cease, H. Thomas Diehl, Brenna L. Flaugher, Donna Kubik, Keivin Kuk, Nickolai Kuropatkine
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Huan Lin, Jorge Montes, Vic Scarpine, Ken Schultz, William Wester (for the DES collaboration)

Instrumentation and Methods for Astrophysics · Submitted 28 Oct 2010

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Simulation and real measurements show that the two methods work very well for our purpose, and are in good agreement with the direct optical measurements.

how it is stated · asserted 1.00 read the record →

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arXiv ID1010.6072 (version 1)
Pith IDL7XEOWCN, Pith's permanent record of this paper and its review
CitationBrenna L. Flaugher, Donna Kubik, Herman Cease, H. Thomas Diehl, Huan Lin, Jiangang Hao, Jorge Montes, Juan Estrada, Keivin Kuk, Ken Schultz, Nickolai Kuropatkine, Vic Scarpine, William Wester (for the DES collaboration). "Measuring the flatness of focal plane for very large mosaic CCD camera." arXiv:1010.6072 (2010). https://pith.science/paper/L7XEOWCN
Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Open the compiled record

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 10,868 input tokens, $0.0005 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.42 · human participants 0.02 · controlled comparison 0.18 · randomized assignment 0.01 · states quantitative result 0.89 · compares with prior results 0.87 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

Large mosaic multiCCD camera is the key instrument for modern digital sky survey. DECam is an extremely red sensitive 520 Megapixel camera designed for the incoming Dark Energy Survey (DES). It is consist of sixty two 4k$\times$2k and twelve 2k x 2k 250-micron thick fully-depleted CCDs, with a focal plane of 44 cm in diameter and a field of view of 2.2 square degree. It will be attached to the Blanco 4-meter telescope at CTIO. The DES will cover 5000 square-degrees of the southern galactic cap in 5 color bands (g, r, i, z, Y) in 5 years starting from 2011. To achieve the science goal of constraining the Dark Energy evolution, stringent requirements are laid down for the design of DECam. Among them, the flatness of the focal plane needs to be controlled within a 60-micron envelope in order to achieve the specified PSF variation limit. It is very challenging to measure the flatness of the focal plane to such precision when it is placed in a high vacuum dewar at 173 K. We developed two image based techniques to measure the flatness of the focal plane. By imaging a regular grid of dots on the focal plane, the CCD offset along the optical axis is converted to the variation the grid spacings at different positions on the focal plane. After extracting the patterns and comparing the change in spacings, we can measure the flatness to high precision. In method 1, the regular dots are kept in high sub micron precision and cover the whole focal plane. In method 2, no high precision for the grid is required. Instead, we use a precise XY stage moves the pattern across the whole focal plane and comparing the variations of the spacing when it is imaged by different CCDs. Simulation and real measurements show that the two methods work very well for our purpose, and are in good agreement with the direct optical measurements.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Large mosaic multiCCD camera is the key instrument for modern digital sky survey. background 1.00 0.04 0.02 asserted 1.00
s1 DECam is an extremely red sensitive 520 Megapixel camera designed for the incoming Dark Energy Survey (DES). background 0.91 0.09 0.02 asserted 1.00
s2 It is consist of sixty two 4k$\times$2k and twelve 2k x 2k 250-micron thick fully-depleted CCDs, with a focal plane of 44 cm in diameter and a field of view of 2.2 square degree. background 0.77 0.21 0.02 asserted 1.00
s3 It will be attached to the Blanco 4-meter telescope at CTIO. background 0.98 0.08 0.02 asserted 0.94
s4 The DES will cover 5000 square-degrees of the southern galactic cap in 5 color bands (g, r, i, z, Y) in 5 years starting from 2011. background 1.00 0.07 0.02 asserted 0.99
s5 To achieve the science goal of constraining the Dark Energy evolution, stringent requirements are laid down for the design of DECam. background 0.99 0.07 0.02 asserted 1.00
s6 Among them, the flatness of the focal plane needs to be controlled within a 60-micron envelope in order to achieve the specified PSF variation limit. background 0.99 0.10 0.07 asserted 1.00
s7 It is very challenging to measure the flatness of the focal plane to such precision when it is placed in a high vacuum dewar at 173 K. background 0.72 0.14 0.03 asserted 1.00
s8 We developed two image based techniques to measure the flatness of the focal plane. contribution 0.92 0.96 0.11 asserted 1.00
s9 By imaging a regular grid of dots on the focal plane, the CCD offset along the optical axis is converted to the variation the grid spacings at different positions on the focal plane. method 1.00 0.76 0.05 asserted 1.00
s10 After extracting the patterns and comparing the change in spacings, we can measure the flatness to high precision. method 0.94 0.84 0.17 asserted 0.86
s11 In method 1, the regular dots are kept in high sub micron precision and cover the whole focal plane. method 0.99 0.77 0.04 asserted 1.00
s12 In method 2, no high precision for the grid is required. method 0.97 0.54 0.03 asserted 1.00
s13 Instead, we use a precise XY stage moves the pattern across the whole focal plane and comparing the variations of the spacing when it is imaged by different CCDs. method 0.99 0.92 0.05 asserted 0.99
s14 Simulation and real measurements show that the two methods work very well for our purpose, and are in good agreement with the direct optical measurements. result 0.97 0.95 0.73 asserted 1.00

What kind of paper the classifier reports this is: method or tool 1.00 · evidence from observation or experiment 0.98.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

Large mosaic multiCCD camera is the key instrument for modern digital sky survey. DECam is an extremely red sensitive 520 Megapixel camera designed for the incoming Dark Energy Survey (DES). It is consist of sixty two 4k$\times$2k and twelve 2k x 2k 250-micron thick fully-depleted CCDs, with a focal plane of 44 cm in diameter and a field of view of 2.2 square degree. It will be attached to the Blanco 4-meter telescope at CTIO. The DES will cover 5000 square-degrees of the southern galactic cap in 5 color bands (g, r, i, z, Y) in 5 years starting from 2011. To achieve the science goal of constraining the Dark Energy evolution, stringent requirements are laid down for the design of DECam. Among them, the flatness of the focal plane needs to be controlled within a 60-micron envelope in order to achieve the specified PSF variation limit. It is very challenging to measure the flatness of the focal plane to such precision when it is placed in a high vacuum dewar at 173 K. We developed two image based techniques to measure the flatness of the focal plane. By imaging a regular grid of dots on the focal plane, the CCD offset along the optical axis is converted to the variation the grid spacings at different positions on the focal plane. After extracting the patterns and comparing the change in spacings, we can measure the flatness to high precision. In method 1, the regular dots are kept in high sub micron precision and cover the whole focal plane. In method 2, no high precision for the grid is required. Instead, we use a precise XY stage moves the pattern across the whole focal plane and comparing the variations of the spacing when it is imaged by different CCDs. Simulation and real measurements show that the two methods work very well for our purpose, and are in good agreement with the direct optical measurements.

Human review

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How the literature uses it

1 arXiv paper cite this in 1 sentence

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it

Uses its method or tool 1 paper

What it cites

Cites as background 1 paper
  • Dark Energy Survey (DES) [ref] is a project dedicated to understanding the nature of Dark Energy by imaging 5000 square degree southern galactic cap in 5 color bands (g, r, i, z, Y) and up to redshift 1.3.

    The Dark Energy Survey · INTRODUCTION · 0.93

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