adsabs/AstroCLIMB huggingface dataset:
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Overlaid histograms of the planetary radius distributions for planets in single-transiting systems with radius values less than 6 R ⊕ (blue) and compact multiple planets (pink) after performing a 95th percentile quality cut on both samples. The median of each sample is plotted as a vertical line of the same color. The median lines are off-shifted by 0.301 R ⊕. Our quality cut threw out 15 planets from our study that had σ  Rp /R  p  > 0.2299. The two-sample K-S test, Mann–Whitney U test, and Anderson–Darling k-sampling test were reapplied to the planets surviving the quality cut. Tables 12 and 13 display the significance of our statistical tests that endured our jackknife resampling.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: (A) Overlaid histograms of planetary radius distributions for planets in single-transiting systems (blue) and compact multiple planets (pink). (B) Overlaid histograms of planetary radius distributions for planets in single-transiting systems (blue) and compact multiple systems (pink) with radius values less than 6 R ⊕. We performed a two-sample K-S test, a Mann–Whitney U test, or Anderson–Darling k-sampling test for both the full planetary and consideration of only planets ≤6 R ⊕. In Tables 7 and 8 we present the results of the statistical tests, finding the radius distributions of single-transiting planets and planets in compact multiples to be significantly different in all statistical tests. Importantly, the test results become more significant (p < 0.0009) when only accounting for planets ≤6 R ⊕. The inclusion or exclusion of gas giant planets is not significant when assessing the radius distributions of these two samples.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Histogram of the relative percent errors (﹩{\sigma }_{{R}_{p}}/{R}_{p}﹩) on derived planetary radii. Relative percent errors on planetary radius values for 263 planets were propagated from errors on the transit depth such that ﹩{\sigma }_{{R}_{p}}=\tfrac{{\sigma }_{\delta }}{\delta }﹩. For the 27 remaining planets in our sample, relative percent errors were calculated from ﹩{\sigma }_{{R}_{p}}=\tfrac{{\delta }_{{R}_{p}/{R}_{\star }}}{{R}_{p}/{R}_{\star }}﹩. Our relative errors on planetary radii do not factor in stellar uncertainties since our planetary sample is built from a uniform stellar sample.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Color–magnitude diagram of host stars in Gaia G G vs. G BP − G RP. Anderson et al. (2021) found that the linear fit to these stars represents a boundary of average metallicity for main-sequence stars, with most compact multiple host stars occupying the left of the linear trend line in the metal-poor regime.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Left: overlaid histograms of the orbital period distributions for planets in single-transiting systems (blue) and compact multiple planets (pink). We plot the median period of each sample as a solid vertical line of the respective color. The single-transiting planets have a median period of 6.29 days. The compact multiples have a median period of 8.04 days. Right: overlaid histograms of the orbital period distributions for planets with orbital periods less than 50 days. This panel contains 104 single-transiting planets and 133 planets from a compact multiple system. The median of the single-transiting systems is 4.81 days, while the median of the compact multiples is 7.88 days. In both panels, the compact multiples have a longer average orbital period. In Tables 16 and 17, we display the results of statistically testing the difference in the orbital period distributions. With a p-value of 4.41 × 10−5, we find that the orbital period distributions are significantly offset from each other.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Left: histogram of our single-transiting-planet systems (blue) and a histogram of those same planets with a steam atmosphere consisting of 0.27 wt.% of the planet’s mass (aquamarine). We estimate the planets’ mass with the mass–radius relation calculated by Zeng et al. (2019) and the extent of the steam atmosphere with the atmospheric model of Turbet et al. (2020). The blue and aquamarine vertical lines represent the median of the sample. We find with 1 bulk Earth-content of water, including the surface water (the physical oceans) and the amount of water in the mantle,degassed from the interior to form a secondary atmosphere that the radii of these planets are inflated by 0.1 Earth radii, insufficient to explain our observed difference between the single and compact multiple planetary systems. Right: identical to left but for a bulk water content inflated by a factor of 11 relative to the Earth. We find that to reproduce the observed differences between compact multiple planetary radii and single planetary radii through excess degassing from tidal forces, these planets would have to have a bulk water content 11× that of the Earth and for this water to be 100% degassed to form a secondary steam atmosphere.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Overlaid histograms of the planetary radius distributions for planets surviving the quality cut in single-transiting systems (blue) and compact multiple systems (pink) with radius values less than 6 R ⊕ and orbital periods greater than 1.5 days. We plot 110 single-transiting planets and 136 planets from compact multiple systems. The solid lines representing the median of the respective populations are located at 2.013 R ⊕ and 1.884 R ⊕ for compact multiple and single-transiting planets respectively. Table 18 contains the results from running a two-sample K-S test, Mann–Whitney U test, and Anderson–Darling k-sampling test on our reduced sample. We still obtain a significant Mann–Whitney U test p-value when making a period cutoff greater than 1.5 days in our sample.
Paper: Variations in the Radius Distribution of Single- and Compact Multiple-transiting Planets
Authors: Benjamin T. Liberles, Jason A. Dittmann, Stephen M. Elardo, Sarah Ballard
Figure caption: Overlaid histograms of compact multiple planets found in 3:2 and 2:1 orbital resonances with at least one other planet in their planetary system (purple) and all remaining other remaining compact multiple planets post–quality cut (pink). The median of each sample is plotted as a vertical line of the same color. There are not enough planets that are in resonance orbits in our sample to make a robust statistical conclusion on whether orbital resonant systems inhabit larger planets, and we do not find a significant difference between the population of compact multiple planets in a 3:2 or 2:1 resonance vs. those not exhibiting those desired resonances.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Demonstration of the ADC concept. Left: the prisms produce leftward and rightward dispersions that cancel each other when oppositely oriented, leaving the input light unchanged. Right: the prisms can be rotated to other orientations to produce a net dispersion that negates atmospheric dispersion.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Layout of the Mayall telescope and the DESI instrument. (Image previously published in Miller et al. 2018.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Optical layout of DESI corrector lens assembly. (Image previously published in Miller et al. 2018.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Description of the corrector aspheric surfaces. Top: aspheric departure of the surfaces. Bottom: slope of the aspheric departures.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Image quality of the corrector optical design. Blur is due to design aberrations and is shown as FWHM blur in arcseconds. Each plot corresponds to the DESI 3.°2 circular field of view. Left panels are calculated for a 360–450 nm bandpass, and right panels are calculated for a 450–980 nm bandpass. Top, middle, bottom panels are for zenith angles of 0°, 30°, and 60°, respectively.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Layout of the C1 transmission test. Configuration includes a 1.5 m diameter spherical reference mirror and small null lens to remove test aberrations. (Credit: L3 Brashear.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Chief ray angle compared to the normal angle of the focal surface, as a function of radial position in the focal plane. Top: the absolute angles of the chief ray at 500 nm and of the local surface normal. Angles are with respect to global z-axis. Bottom: the chief ray deviation (i.e., the difference between the chief rays and surface normal angles) meets the requirements, shown as coarse and fine dashed lines for the maximum and average chief ray deviation allowed, respectively.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Homogeneity map of the C1 lens blank. The measured range of index variation across the full diameter is 1.0 ppm, which meets the 3 ppm requirement. The requirement allows an overall defocus term to be removed from the data.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Measurement of high-frequency figure error. Left: locations of measurements on C1 convex surface. The large circle represents the surface clear aperture, and small circles represent the 11 sample locations. Locations are noted with the labels used by the vendor. Right: data for the “TR” sample; one edge of the sample is truncated since the sample is located near the lens edge. (Credit: L3 Brashear.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Corrector lenses in various phases of fabrication. From top left to bottom right: C1 in transmission test configuration, mechanical measurements of C2 lens, polishing of the C3 convex surface, dimensional probe of C4 after its generation, inspection of the ADC1 blank, and machining of ADC2. (Images of C1, C2, C3, ADC1 previously published in Miller et al. 2016a.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Telescope parameters calculated from the optical design. Parameters vary owing to anamorphic pupil distortion as a function of field position and whether the meridional or sagittal directions are considered. Top: F/#. Middle: focal length. Bottom: plate scale.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Measured wave-front error of the C1 lens. Plot shows the calculated single-pass transmission error in nm. The central rings are due to the known inhomogeneity in the C1 glass. The step feature in the upper left is due to an MRF process error during final polishing. (Credit: L3 Brashear.)
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Focal ghosts present at the focal surface. Plots left to right show ghosts at several field locations across the focal surface. The arrow in the middle panel identifies the brightest focal ghost feature, a reflection between the two ADC lenses.
Paper: The Optical Corrector for the Dark Energy Spectroscopic Instrument
Authors: Timothy N. Miller, Peter Doel, Gaston Gutierrez, Robert Besuner, David Brooks, Giuseppe Gallo, Henry Heetderks, Patrick Jelinsky, Stephen M. Kent, Michael Lampton, Michael E. Levi, Ming Liang, Aaron Meisner, Michael J. Sholl, Joseph Harry Silber, David Sprayberry, Jessica Nicole Aguilar, Axel de la Macorra, Daniel Eisenstein, Kevin Fanning, Andreu Font-Ribera, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Jorge Jimenez, Dick Joyce, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Christophe Magneville, Paul Martini, Ramon Miquel, John Moustakas, Jundan Nie, Will Percival, Claire Poppett, Francisco Prada, Graziano Rossi, David Schlegel, Michael Schubnell, Hee-Jong Seo, Ray Sharples, Gregory Tarlé, Mariana Vargas-Magaña, Zhimin Zhou
Figure caption: Measured wave-front error of the C2 lens. The plot shows the calculated single-pass transmission error in microns. The map was created by stitching together 12 off-axis subaperture measurements and calibrating out test errors. A radial pattern of middle-frequency polishing errors is visible, caused by the small tools used during polishing. A series of small fiducial marks were placed on the lens to enable subapertures to be stitched together; these are blocked out in the data (white spots). One particular low spot (at the bottom of the plot) is also blocked, being too steep for the interferometer to measure accurately; this was assessed separately. This surface was analyzed and accepted by DESI. (Credit: Arizona Optical Systems.)