adsabs/AstroCLIMB huggingface dataset:
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Histograms for the original SDSS corrector design in the H-band. (a) Spatial distribution, relative to the centroid location. (b) Angular distribution, relative to the focal surface normal.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: The original SDSS corrector optical layout. The Gascoigne (“common”) corrector is located near the vertex of M1 and was used in both imaging and spectroscopic modes.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Layouts of the SDSS 2.5 m telescope. (a) Figure 3 from the Gunn telescope paper, showing details of the windscreen and baffle design. (b) Optical layout from the Zemax model.
Paper: Ten Aligned Orbits: Planet Migration in the Era of JWST and Ariel
Authors: J. Zak, H. M. J. Boffin, A. Bocchieri, E. Sedaghati, Z. Balkoova, P. Kabath
Figure caption: Statistics of the planets with spin–orbit angle and atmospheric measurements; see the text for more details. (Top) We show how many planets with JWST and HST measurements have their spin–orbit angle measured. We show the same for Ariel Mission Candidate Sample (MCS) and Ariel Tier 3 candidates. While only 41% of HST/JWST atmospheric targets and 29% of the full Ariel sample have measured spin–orbit angles, the Ariel Tier 3 sample achieves 70% completeness. (Bottom) The total sample of planets with their spin–orbit angle measured shows 62% aligned, 30% misaligned, and 8% intermediate cases. This is consistent with their distributions in the JWST/HST atmospheric sample and also Ariel Tier 3 candidate list revealing no biases toward either population.
Paper: Ten Aligned Orbits: Planet Migration in the Era of JWST and Ariel
Authors: J. Zak, H. M. J. Boffin, A. Bocchieri, E. Sedaghati, Z. Balkoova, P. Kabath
Figure caption: The Rossiter–McLaughlin effect of WASP-35b, WASP-44b, WASP-45 Ab, WASP-54 Ab, WASP-91b, and WASP-99b. The observed data points (black) are shown with their error bars. The systemic and Keplerian orbit velocities were removed. The blue line shows the best fitting model to the data, together with 1σ (dark gray) and 3σ (light gray) confidence intervals.
Paper: Ten Aligned Orbits: Planet Migration in the Era of JWST and Ariel
Authors: J. Zak, H. M. J. Boffin, A. Bocchieri, E. Sedaghati, Z. Balkoova, P. Kabath
Figure caption: Same as Figure 1 for WASP-129 Ab, WASP-162b, Qatar-7b, and EPIC 219388192b.
Paper: Ten Aligned Orbits: Planet Migration in the Era of JWST and Ariel
Authors: J. Zak, H. M. J. Boffin, A. Bocchieri, E. Sedaghati, Z. Balkoova, P. Kabath
Figure caption: Phase curve of WASP-44b (top) and Qatar-7b (bottom) using TESS data centered around the primary transit. Observed data are shown in black, binned data in blue and the obtained transit model in orange color.
Paper: Precise Constraints on the Energy Budget of WASP-121 b from Its JWST NIRISS/SOSS Phase Curve
Authors: Jared Splinter, Louis-Philippe Coulombe, Robert C. Frazier, Nicolas B. Cowan, Emily Rauscher, Lisa Dang, Michael Radica, Sean Collins, Stefan Pelletier, Romain Allart, Ryan J. MacDonald, David Lafrenière, Loïc Albert, Björn Benneke, René Doyon, Ray Jayawardhana, Doug Johnstone, Vigneshwaran Krishnamurthy, Caroline Piaulet-Ghorayeb, Lisa Kaltenegger, Michael R. Meyer, Jake Taylor, Jake D. Turner
Figure caption: The level of contribution of reflected light and thermal emission coming from the planet if we assume the planet and star as a blackbody and a gray albedo. The red line shows the thermal emission from the planet given it’s dayside Teff value. The blue, orange, and green dashed lines show the reflected light contribution for albedo values of 1, 0.5, and 0.2, respectively. Blue region shows the wavelength range covered by Order 2 while the red region shows for Order 1. With a bond albedo of 20%–30% we would expect reflected light to dominate over thermal emission at the shortest wavelengths of Order 2.
Paper: Precise Constraints on the Energy Budget of WASP-121 b from Its JWST NIRISS/SOSS Phase Curve
Authors: Jared Splinter, Louis-Philippe Coulombe, Robert C. Frazier, Nicolas B. Cowan, Emily Rauscher, Lisa Dang, Michael Radica, Sean Collins, Stefan Pelletier, Romain Allart, Ryan J. MacDonald, David Lafrenière, Loïc Albert, Björn Benneke, René Doyon, Ray Jayawardhana, Doug Johnstone, Vigneshwaran Krishnamurthy, Caroline Piaulet-Ghorayeb, Lisa Kaltenegger, Michael R. Meyer, Jake Taylor, Jake D. Turner
Figure caption: Spectroscopic precision from exoTEDRF fits of WASP-121 b using 5 pixels bin−1. Dashed black lines show the photon noise limit and 2x the photon noise limit, respectively. Precision is generally 50% above the photon limit with the exception of the shortest wavelengths in Order 2 and the longest wavelengths in Order 1.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: A comparison between our results for the 14 CBs in this paper with published ﹩{q}_{{\rm{\min }}}﹩ boundaries in the q–P plane.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sector 47) for J082700 with the LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sector 50) for J134010 with the LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sector 48) for J141530 with the LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sectors 44–46) for NSVS 7399728 with the LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system J134010, as in Figure 14.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system J082700, as in Figure 14. The gray line shows the original unsmoothed BF that contains the l3 spike.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system J141530, as in Figure 14. The gray line shows the original unsmoothed BF that contains the l3 spike.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system NSVS 7399728, as in Figure 14.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Full corner plot comparing the four-component joint retrieval with the results from each band separately. While the L band is consistent with the results from the six-component joint retrieval, the K band prefers a carbon-rich composition, and dominates the joint fit. Comparison with the L band and six- and eight-component cases indicates that this mode is a result of residuals in the K-band time series when omitting four PCs.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Full corner plot comparing the six-component joint retrieval with the results from each band separately. The posteriors are generally consistent, except for a slight offset in the Kp and Δvsys parameters. This could be explained by errors in the L-band wavelength calibration, and may be responsible for the relatively large value of vrot.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Full corner plot for the eight-component joint retrieval.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Full corner plot for the four-component joint retrieval.
Paper: The Watery Atmosphere of HD 209458 b Revealed by Joint K- and L-band High-resolution Spectroscopy
Authors: Luke Finnerty, Julie Inglis, Michael P. Fitzgerald, Daniel Echeverri, Nemanja Jovanovic, Dimitri Mawet, Geoffrey A. Blake, Ashley Baker, Randall Bartos, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Katelyn Horstman, Chih-Chun Hsu, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato-Rovner, Jean-Baptiste Ruffio, Ben Sappey, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Nicole L. Wallack, Jason J Wang, 劲飞 王, Ji Wang, 吉 王, Yinzi Xin, Jerry W. Xuan
Figure caption: Full corner plot for the six-component joint retrieval.
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Comparison of COH molecule abundances relative to CH3OH in comets and IRAS 16293–2422B. Included in the plots are the Pearson correlation (r), Spearman’s rank correlation (ρ) and Kendall correlation (τ) coefficients for the log–log comparison. The solid line shows the 1:1 agreement, with the shaded area indicating a variation of a factor of 10 on either side of this. The dashed line is the regression line calculated using the least-squares method (with the upper limits replaced by 50% of their reported value), and the dotted line is the regression line calculated using the ATS method.
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Division of carbon and oxygen among the molecules CO, H2CO, CH3OH, HCOOH, CH3CHO, (CH2OH)2, HNCO, and NH2CHO.
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Top: major carriers of sulfur in IRAS 16293–2422B. Middle: division of sulfur among the molecules H2S, SO, H2CS, and OCS. Bottom: division of sulfur among the molecules H2S, SO, SO2, H2CS, and OCS.
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Comparison of N molecule abundances in comets and IRAS 16293–2422B relative to CH3CN. The best-fit regression lines are shown calculated using the least-squares method (dashed line) and the ATS method (dotted line).
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Comparison of S molecule abundances in comets and IRAS 16293–2422B relative to H2S. The best-fit regression lines are shown calculated using the least-squares method (dashed line) and the ATS method (dotted line).
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Comparison of S molecule abundances relative to CH3SH in 67P with those in IRAS 16293–2422B. The best-fit regression lines are shown calculated using the least-squares method (dashed line) and the ATS method (dotted line).
Paper: The Interstellar Heritage of Comets
Authors: Karen Willacy, Liton Majumdar, Boncho Bonev, Erika Gibb, Neil Dello Russo, Michael DiSanti, Ronald J. Vervack, Nathan X. Roth
Figure caption: Division of nitrogen among the molecules HCN, NH2CHO, HNCO, CH3CN, and HC3N.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Three-example J-band spectra of spectral type L3 objects from the BDSS. Each spectrum represents a different gravity type: low gravity (2MASS 2208+2921), intermediate gravity (2MASS 1726+1538), and high gravity (2MASS 1300+1912). Major absorption features in the J band are also labeled. Light gray shaded regions denote the locations used to calculate K I equivalent widths and the FeHJ index. Dark gray regions denote the locations of the pseudocontinua used in our calculations. The K I line at 1.2437 μm is marked but not shaded. This line was not used to determine gravity types because of contamination from FeH absorption at ∼1.24 μm (E. C. Martin et al. 2017).
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Layout and fiber capacity of the 2 × 2 NIR detector mosaic. The focal plane consists of a 2 × 2 mosaic of four detectors (each 640 × 512 pixels with a 20 μm pixel pitch) within a mechanical envelope of 61.22  ×  61.22 mm2. The total effective light-sensitive area measures 25.6 mm (dispersion) × 20.48 mm (spatial). Along the spatial direction, a single detector accommodates 53 fibers, yielding a total capacity of 106 fibers for the entire mosaic, which satisfies the multiplexing requirements for multiobject NIR spectroscopic observations with the spectrograph prototype.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Three-dimensional structure (left) and working principle (right) of the LAMOST NIR spectrograph prototype. The right panel illustrates the light path: light from the slit is collimated and then split by the blue and NIR dichroic mirrors, with NIR light being reflected into the NIR channel. The core of the NIR channel is an integrated rotary stage housing the VPH grating, camera, and dewar. A coordinated rotation of the grating (independent) and the entire stage enables the system to maintain the grating blaze angle at optimal efficiency for different wavelengths. Brakes at the rear of the stage lock the position after adjustment to ensure operational stability.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Schematic of the three-channel dichroic design in the LAMOST spectrograph prototype. To extend the spectral coverage to the NIR, a new NIR dichroic mirror was added after the original blue dichroic. As illustrated, the collimated beam from the telescope is first split by the blue dichroic, which separates the short-wavelength component (λ < 570 nm). The remaining beam is then directed to the NIR dichroic, which transmits light at 570–900 nm to the red channel and reflects light at λ > 900 nm into the new NIR channel, enabling simultaneous three-channel spectroscopic observation.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Optical design of the refractive camera for the LAMOST NIR spectrograph prototype. The layout shows a six-lens design incorporating two aspheric elements for effective correction of spherical and comatic aberrations. The last lens also functions as the detector window. The camera has a focal length of 260 mm and operates at F/1.3. Its design covers the mechanical detector envelope (61.22 ×  61.22 mm2), providing ample alignment tolerance to ensure excellent image quality across the scientific field of view.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Schematic layout of the entire optical system for the LAMOST NIR spectrograph prototype. The system consists of the slit, collimator, blue dichroic mirror, NIR dichroic mirror, NIR channel collimator corrector, VPH grating, NIR camera lens group, and detector. The VPH grating, refractive camera, and detector are integrated into a modular unit (NIR rotary stage) that rotates about the grating center.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: 2MASS Point Source Catalog source counts (per 0.2 mag bin) for several hundred square degrees near the north Galactic pole. Blue, green, and red histograms represent J (1.25 μm), H (1.65 μm), and Ks (2.16 μm) counts, respectively (M. F. Skrutskie et al. 2006).
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Near-Infrared J-band spectrum (R ≈ 2000) of RSGs, with major spectral features marked at their rest-frame wavelengths (B. Davies et al. 2010).
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: RGB image of the foreground-corrected target field, formatted as in Figure 1. The ζ Oph Group and Far Group have been corrected by the average values of the ζ Oph Group (﹩\bar{q}=-0.76 \% ﹩ and ﹩\bar{u}=-1.22 \% ﹩). Because they are nearer than the foreground, polarizing dust, the Near Group targets have not been corrected.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: Target stars’ polarization efficiencies. Colored points (green, blue, and purple for Near Group, ζ Oph Group, and Far Group, respectively) represent individual targets, while black points represent the weighted averages of each distance group. The dashed line is the polarization efficiency limit determined by K. Serkowski et al. (1975), and the dotted line is the limit from G. V. Panopoulou et al. (2019). The dashed–dotted line represents 25% mag−1 as a reference.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: The target stars’ RV vs. d. The red ×’s indicate the location of the weighted averages of each distance group.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: The SDSS-V wide-field corrector preliminary three-element design (thin design).
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Estimated throughput of the SDSS-V corrector. Green and red highlighted areas represent the optical and near-infrared regions of the SDSS-V survey, respectively. Plots are given for both candidate coating designs from SESO (1 and 1b), both on axis (0°) and at the edge of the field (1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5).
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Histograms for the SDSS-V corrector design in the optical bandpass. (a) Spatial distribution, relative to the centroid location. (b) Angular distribution, relative to the focal surface normal.
Paper: The New SDSS 2.5 m Telescope Wide-field Corrector for SDSS-V
Authors: Stephen A. Smee, Robert H. Barkhouser, Randolph P. Hammond, Albert C. Harding, Aidan C. Gray, Solange Ramirez, Stefanie Wachter, Juna Kollmeier, John Downey, Jamey E. Eriksen, Dmitry Bizyaev, Dylan Gatlin, Katie Grabowski, Karen Kinemuchi, Daniel Oravetz, Audrey Oravetz, Dan Long, Viktor Malanushenko, Fred Mrozek, Tracy Naugle, Kaike Pan, Ryan Wagner, John C. Wilson
Figure caption: Encircled energy curves for the original SDSS corrector design. The back focal distance was optimized here for average rms spot size in each bandpass. (a) Optical. (b) H band.