adsabs/AstroCLIMB huggingface dataset:
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Associated corner plot for the atmospheric retrieval discussed in Section 5.
Paper: Simulating Self-lensing and Eclipsing Signals due to Detached Compact Objects in the TESS Light Curves
Authors: Sedighe Sajadian, Niayesh Afshordi
Figure caption: Top panel: the scatter plot of all simulated WDMS binaries (black points) and the ones with detectable WD-induced impacts (colored points) in 2D space ﹩{\mathrm{log}}_{10}[{ \mathcal F }]-{\mathrm{log}}_{10}[b/{R}_{\star }]﹩. Their 1D and normalized distributions are shown at two sides of the plot. The red, blue, and green circles represent detectable events owing to their eclipsing, self-lensing, and occultation signals, respectively. Middle panel: same as the previous one but resulting from the Monte Carlo simulation of NSMS binaries. Last panel: same as the two previous ones but resulting from simulating BHMS binaries and in 2D space ﹩{\mathrm{log}}_{10}[T(\mathrm{days})]-{\mathrm{log}}_{10}[b/{R}_{\star }]﹩.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Left image: an example of the sources detected in CLOWN is displayed by green circles in an all-sky image from PASO. Right image: the mask created for the PASO all-sky camera (area of interest in white) to eliminate false detections on the horizon. A small area with several detections can be seen on the left image, which is caused by a glint caused by an illumination lamp in the area. It can be ignored because it is a small area in the sky. If the glint becomes persistent, it can be resolved by including this zone in the mask or even better by physically removing that light source.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Basic flow diagram of the CLOWN pipeline.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Illustration of the polar coordinate transformation. Left image: the image pixel coordinate system (x, y) is drawn on the top left in white, and the polar coordinates system for a perfect camera installation is overlaid in red. On the right image, we have the polar coordinate system for the real system, obtained after correction for the fixed angle offset.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Relation between the number of missing stars and their magnitude.
Paper: A Photometric Redshift Catalogue of Galaxies from the DESI Legacy Imaging Surveys DR10
Authors: Changhua Li, Yanxia Zhang, Chenzhou Cui, Shirui Wei, Jingyi Zhang, Yongheng Zhao, Xue-Bing Wu, Yihan Tao, Shanshan Li, Youfen Wang, Zihan Kang
Figure caption: Left-hand panel: spectroscopic redshift distribution for the KST sample; right-hand panel: spectroscopic redshift vs. r magnitude for the KST sample.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: Snapshots showing the different stages of the encounter for the three major types of outcomes. In each panel, the reference frame is centered at the position of the most massive SPH particle, initially situated at the center of the more massive planet, and the colors represent the column density. The white arrows on the less massive planet represent its velocity relative to the more massive planet, with arrow length proportional to the velocity. The Hill spheres of the planets are shown by the white dashed circles on the rightmost panels. The top (middle) row shows an example of Hit & Run (Merger) encounter with ﹩{v}_{\mathrm{im}}\sim {v}_{\mathrm{esc}}﹩ and ﹩b^{\prime} =0.8﹩ (﹩b^{\prime} =0.08﹩). The bottom row shows the snapshots of a highly energetic (﹩{v}_{\mathrm{im}}/{v}_{\mathrm{esc}}\approx 4﹩) encounter with low impact parameter (﹩b^{\prime} =0.05﹩) that results in the destruction of both the planets, categorized as a Catastrophic collision.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: Fractional change in planet masses, against impact parameter for different impact velocities. The vertical dashed lines indicate the lowest impact parameters at which both planets survive for each ﹩{v}_{\mathrm{im}}﹩/v esc (see legend). Collisions resulting in the destruction of both planets are marked by crosses.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: The fractional change in the overall planet mass (top), and the atmospheric mass (bottom) as a function of the impact parameter. The circles represent collisions leading to Merger. Square and diamond markers represent the higher-mass and lower-mass planets for Hit & Run collisions, respectively. The additional simulations conducted with a resolution of ∼105 SPH particles per planet using minor variations in the initial conditions are shown in blue markers. Red (yellow) markers represent simulations conducted with resolutions of ∼5 × 104 (∼2 × 105) SPH particles per planet. The corresponding simulations used in our primary analysis of the study are shown in black. The marker sizes are scaled to the simulation resolutions. Some of the blue markers overlap due to identical simulation results (see Table A1). The proximity between the black and the colored markers indicates that our results are expected to be robust against minor variations of initial conditions as well as reasonable variations in the resolution of the simulations.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: The 2D grid of simulations considered in our study in impact parameter (﹩b^{\prime} ﹩) and impact velocity (﹩{v}_{\mathrm{im}}﹩) at the moment of contact. The colored dots represent the simulations conducted in this study. The colors of the individual crosses reflect the overall mass loss during the encounter. The blue circles (green hexagons) enclosing the crosses highlight the simulations where one (or both) planet(s) survive. Collisions resulting in the destruction of both planets are shown without any enclosure. The gray dots represent the collisions produced in typical planet–planet scattering experiments (adapted from ensemble n8-e040-i024 of T. Ghosh & S. Chatterjee 2024). The dot sizes are proportional to the impact energy.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: Similar to Figure 5 but shows fractional change in the atmospheric mass of the planets with varying ﹩b^{\prime} ﹩ for different values of ﹩{v}_{\mathrm{im}}﹩/v esc.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: Summary of overall outcomes in ﹩b^{\prime} ﹩ − ﹩{v}_{\mathrm{im}}﹩ space. The black dots mark the ﹩{b}_{{\rm{c}}}^{{\prime} }﹩ values from our simulation grid. The boundary separating Hit & Run collisions with other outcomes, follows ﹩{b}_{{\rm{c}}}^{{\prime} }/{b}_{{\rm{c}},1}^{{\prime} }\approx {({v}_{\mathrm{im}}/{v}_{\mathrm{esc}})}^{-2}﹩, for ﹩{v}_{\mathrm{im}}/{v}_{\mathrm{esc}}\lesssim 2.5﹩ and ﹩{b}_{{\rm{c}}}^{{\prime} }﹩ increases linearly (﹩{b}_{{\rm{c}}}^{{\prime} }/{b}_{{\rm{c}},2.5}^{{\prime} }\approx ({v}_{\mathrm{im}}/{v}_{\mathrm{esc}})-1.5﹩) at higher impact velocities. Similar to Figure 1, the gray dots represent the collisions produced in typical planet–planet scattering experiments (ensemble n8-e040-i024 of T. Ghosh & S. Chatterjee 2024).
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: Density (upper panel) and pressure (lower panel) profiles of Planet 1 (Table 1). The black dashed line shows the analytic profile of the planet in hydrostatic equilibrium. The initial profiles of the SPH planet are shown in blue, and the same after relaxing the SPH planet in isolation for 177 hr, is shown in orange.
Paper: Outcomes of Sub-Neptune Collisions
Authors: Tuhin Ghosh, Sourav Chatterjee, James C. Lombardi
Figure caption: Relative energy error (∣ΔE/E∣) throughout the runtime for three example collisions: ﹩b^{\prime} =0.9﹩ at ﹩{v}_{\mathrm{im}}/{v}_{\mathrm{esc}}\sim 0.78﹩ for Hit & Run (green), ﹩b^{\prime} =0.14﹩ at ﹩{v}_{\mathrm{im}}/{v}_{\mathrm{esc}}\sim 1﹩ representing a Merger (blue), and ﹩b^{\prime} =0.19﹩ at ﹩{v}_{\mathrm{im}}/{v}_{\mathrm{esc}}\sim 5﹩ depicting a Catastrophic collision. The marginalized histograms represent the distribution of ∣ΔE/E∣ at simulation stopping time.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Two-band light curve of galaxy LEDA 174461. Period was determined to be 30.368 days. Quality of phase-folded curve is impacted, as the period is close to a clean factor of the observation cadence.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Light curve of 2MASS J01542169–5944445. Bottom curve is phase folded at 5.8061 days.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Light curve of LEDA 358365. The transient event is visible through WISE in the second-to-last observation epoch, mid-2023.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: CRTS J054306.5−024247 as seen by WISE in the W1 band. Bottom curve is folded at period ∼3.89 days.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: V1403 Ori as seen by WISE in the W1 band. The bottom curve is folded at period ∼4.63 days.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Left: Legacy Survey Data Release 9 imaging of LEDA 174461. Right: unWISE W1/W2 NEOWISE Data Release 7 imaging.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Light curve of LEDA 340305. Transient activity in the first half of the WISE observation window.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Light curve of binary system at J2000 R.A./decl. 1.53483, −59.08751. Bottom curve is phase folded at 5.877 days.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: LEDA 340305 imaging from Legacy Survey Data Release 9. Note the extended spiral arms and irregular shape.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Schematic of the DESI fiber system. The 5000 fibers connecting to the spectrographs are divided into 10 identical bundles of 500 fibers, each of which is integrated with one focal plane unit, defined as a “petal.” The prime focus corrector injects light into the focal plane fibers at an average focal ratio of f/3.9. A spool box at each end of the fiber cable allows for excess in the fiber system. Each 500 fiber cable is subfurcated into 10 smaller bundles and wrapped in a helical fashion about a central Kevlar strength member. The focal plane fibers are fused to the main fiber cables in the focal plane spool boxes. The output of each unit of the fiber system is terminated in a fiber slit. Each fiber slit feeds one of 10 spectrographs which accepts light within f/3.57. Values at the top of this figure give the outer diameter for each of the elements.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Panel (a) shows the lab setup for full-cone FRD measurements. A 500 μm input spot is reimaged onto a test fiber, which is held on an x, y, z, tip, and tilt translation stage. An iris with obscuration is placed in the collimated beam to set the input focal ratio. A fiber view camera (FVC) images the front face of the fiber and ensures that the input spot is properly aligned with the fiber. Panel (b) shows the result of this test when measuring the energy enclosed in the far field at different input focal speeds of f/3.7, f/3.9, f/4.1 (colored lines) and with chief-ray injection angle tilts of ±240′. The plot shows that 90% of the input flux will be captured for the average DESI injection cone of f/3.9 (green line) and the DESI collimator acceptance speed of f/3.57 (horizontal line) if the injection angles are kept below about ±60′ (vertical dashed lines).
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Bulk fiber transmission for 43.5 m of DESI fiber. The attenuation of each batch of fiber was measured prior to shipment by the manufacturer. Although there is variation at blue wavelengths, it is assumed that this is a result of the measurement method, and we see no dependence on throughput with fiber batch in the on-sky data.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Schematic of the DESI fiber system installed on the 4 m Mayall telescope. The fiber system is installed on the outside of the telescope with no feedthroughs in order to facilitate maintenance.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: (a) Encircled energy for three Moffat PSFs whose full width at half-maximum sizes, in arcseconds, are shown. The Moffat parameters FWHM = 1.″1 and β = 3.5 are good fits to the historical Mayall delivered image quality (A. Dey & F. Valdes 2014). (b) Relative signal-to-noise ratios for these same three cases.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Left: a close-up image of a curved slit plate to which 20 V-blocks (fibers inside 20 PTFE tubes and 10 Miniflex tubes) are bonded. Fibers, cover lids, V-blocks, and AR windows are visible, with the 20 V-blocks approximating the curvature of the slit plate below. Right: an image of the entire slit assembly featuring the “race track” of fiber bundles retained in “T-cut” slots.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Left: to the rear of the bench, black tubes connect to the Venturi pumps. The “X-shaped” polishing jig rests upon the glass plate used for polishing single blocks by hand. The Adaptaflex cable is held in black clamps held to the worktop with G-clamps. 3D-printed parts retain and separate the 19 PTFE bundles not in use, and the single bundle to be polished hangs vertically. An array of different colored polishing films sit in front of the plate. A spreadsheet keeps track of production and QA. To the rear, the ultrasonic bath is used for cleaning parts. Right: a closer view of the 20 3D-printed guides used to keep PTFE bundles tidy, with clamps held in place with magnets.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Panel (a) shows a “top-down” polished slit block with perpendicular polish (with respect to fibers) and no bubbles in the epoxy channels. Fiber output face is at the bottom of the image. Panel (b) shows a “fiber face on” polished slit block with no bubbles or edge chips, optically flat, scratch-free polish, well-positioned cover lid in x and evenly spaced fibers.