adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Left: one of the TRIPOL g-band images of Wolf 359 taken on 2023 February 22, with the target and two selected differential standard stars (S1 and S2) labeled. Right, top panel: raw light curves of Wolf 359 (green), the sum of the two reference stars (blue), and the individual reference stars (orange), in units of instrumental counts. Right, bottom panel: calibrated relative flux light curves from differential photometry. A flare event is clearly visible in Wolf 359 around 60 minutes after the start of the observation run. The two reference stars exhibit minimal variability, validating their use as stable differential standards. The same processing was applied to the data obtained in all other bands and on all other observation nights.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Temporal evolution of flare temperature and filling factor (XBB) for all flares analyzed in this study. Each row corresponds to an individual flare event. The left panels display the flare light curves in the g (green) and r (red) bands, with the flare identification labeled accordingly. The middle panels illustrate the flare temperature as a function of time, derived from the g/r flux density ratio. The brown horizontal dashed line represents the effective temperature of Wolf 359, which is 2800 K. The right panels show the corresponding evolution of the filling factor (XBB) throughout the flare duration. For flares F5-0220, F10-0221, and F12-0222, which exhibited detectable amplitudes in the i band, the i-band light curves are also shown.
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: Inferred Bond albedo (AB) and heat recirculation efficiency (ϵ) of WASP-121 b derived from dayside and nightside emission measurements using irradiation temperature T0 = 3398 K. The blue contours represent 1σ, 2σ, and 3σ confidence intervals from the fit to the exoTEDRF reduction, while the red contours correspond to the NAMELESS reduction. The gold contours show the results from the Hubble WFC3 phase curve presented by T. Mikal-Evans et al. (2022), using the brightness temperatures reported in G. Morello et al. (2023). The purple and teal contours correspond to brightness temperatures from NIRSpec NRS1 and NRS2, respectively (T. Mikal-Evans et al. 2023). For the Spitzer 3.6 μm phase curve (brown contours), we use brightness temperatures from G. Morello et al. (2023); while the magenta contours represent results from the comprehensive analysis of the 4.5 μm phase curve by L. Dang et al. (2025). Top: inferred contours when using standard uncertainties of day- and nightside. Only NIRISS SOSS measurements fully propogate astrophysical uncertainties. Bottom: inferred contours when uncertainties are inflated by 1/γ, i.e., the captured flux fraction for a given instrument at the reported temperature. When accounting for captured flux, only NIRISS provides constraints on both the Bond albedo and heat recirculation efficiency. Our phase measurements show a Bond albedo of 20%–35% and relatively poor day-to-night heat transport.
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: Estimated captured flux of the planet assuming the planet radiates as a blackbody. The captured flux is calculated as the ratio of the integrated blackbody emission within the instrument’s bandpass to the total emission over all wavelengths, i.e., ﹩\gamma ={\int }_{{\lambda }_{{\rm{\min }}}}^{{\lambda }_{{\rm{\max }}}}B(\lambda ,T)\,d\lambda /{\int }_{0}^{\infty }B(\lambda ,T)\,d\lambda ﹩. The captured flux fraction is shown for NIRISS SOSS [0.6–2.85 μm] (red line); Hubble WFC3 [1.12–1.64 μm] (dashed green line); NIRSpec G395H [2.7–5.15 μm] (dashed–dotted blue line). The red-shaded region shows the temperature range on WASP-121 b based on our Teff estimates. Red dashed lines indicate the boundaries of the planet’s temperature range within the NIRISS SOSS captured flux fraction. From this we estimate that these observations capture between 55% and 82% of the planet’s bolometric flux, depending on orbital phase. Using the minimum temperature from the NAMELESS fit, this estimate decreases to 50%. In either case, the wavelength coverage of NIRISS exceeds that of any other instrument.
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: Phase offset vs. normalized phase amplitude from the spectroscopic fits of WASP-121 b. The normalized phase amplitude is given by ﹩({F}_{{\rm{\max }}}-{F}_{{\rm{\min }}})/{F}_{{\rm{\max }}}﹩. The phase offset is defined such that 0° corresponds to mid-eclipse with positive offset values indicating an eastward shift and negative a westward. Symbols are colored by wavelength with blue indicating the shortest wavelengths and red the longest. Order 2 values are binned with three points per bin for visual clarity. Relative amplitudes above 1 correspond to Order 2 wavelengths with a negative minimum flux. The values from the white light-curve fits are also shown as stars with colored cyan edges for Order 2 and red for Order 1. We robustly detect an eastward offset of 5.1° ± 1.4° in Order 1 and an insignificant offset of 10.5° ± 9.9° in 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: Left: (a) Order 1 white light-curve fit to the flux that is normalized to the first eclipse. The red line is the best-fit full model. (b) Components of the systematics model in ppm, including the linear trend in green; the PCA model in pink; the tilt jump model in blue; the GP model in purple; the ellipsoidal variation contribution in black; and the stellar sinusoid model in red (Order 2 only). (c) Detrended light curve created after removing all contributions from (b). The remaining planetary signal is shown in green. (d) Residuals of the best-fit model to the data. Darker blue points are residuals binned for visual purposes. The rms in ppm is printed in the bottom left. Right: same as the left plot except for 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: Top: reflected light and thermal emission components from the Order 2 detrended white light curve. Model is described in Section 2.4 and was fit four longitudinal slices across the planet; slices are centered at ϕ = 45°, 135°, 225°, 315°. Red shows thermal emission, blue shows reflected light, and black shows the full model. Solid lines show the median retrieved value while shaded regions show the 1σ uncertainties on each model component. The detrended data are shown in black, binned with 20 points per bin for visual clarity. Bottom: residuals of median model to the data. Larger points are residuals binned to 20 points per bin.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: (a) Flyby outcome distribution as a function of flyby orbit’s perigee distance and orbit eccentricity. The magenta star marks an example nominal flyby orbit, and the magenta ellipse indicates its 3σ uncertainty ellipsoid. Green indicates BA dissociation, blue mutual collision, and dark red staying in orbit. The same color scheme applies to subsequent figures. (b) Same as (a) but for a different set of BA parameters.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: (a) The 3σ uncertainty ellipsoid at perigee for the nominal Apophis 2029 flyby orbit. (b) Postflyby 3σ uncertainty ellipsoid at 1.1 Earth’s Hill radii for a staying-in-orbit example. (c) Postflyby 3σ uncertainty ellipsoid at 1.1 Earth’s Hill radii for a dissociation event. (d) Projections of the 3σ uncertainty ellipsoids onto the B-plane corresponding to Apophis 2051 flyby event. All the 3σ uncertainty ellipsoids are represented by 10,000 Monte Carlo samples.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: Time history of the mutual orbit semimajor axis (first row), orbit eccentricity (second row), A’s rotation rate (third row), and B’s rotation rate (fourth row). For the hyperbolic flyby orbit, the negative value of the semimajor axis a is plotted, ensuring a > 0.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: Time history of the ratio between Earth’s torque on A and B’s torque on A (upper), and the ratio between Earth’s torque on B and A’s torque on B (lower).
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: Flyby outcome distributions similar to Figure 2, but for the parameters listed in Table 3. (a) Two spherical asteroids; (b) two ellipsoidal asteroids.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: Flyby outcome contours with respect to: (a) the primary’s and the secondary’s rotation rates, and (b) the primary’s and the secondary’s initial phase angles ψA and ψB.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: Comparison of the critical flyby condition derived in this work (black and magenta lines) with the empirical relation from R. A. N. Araujo & O. C. Winter (2014; green region). The green region encompasses results for V∞ between 5 and 35 km s−1. The two blue boundary lines indicate the linear relations for the velocity V∞ = 5 km s−1 and V∞ = 35 km s−1.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: (a) The separation between components A and B (black) and the radius of the 3σ uncertainty ellipsoid (red) at 1.1 Earth Hill radii, plotted against the velocity scaling factor k. (b) The absolute separation between A and B (black, left axis) and the corresponding magnification ratio relative to the initial orbit size (blue, right axis) at 1.1 Earth Hill radii, as a function of the initial mutual orbit semimajor axis.
Paper: Influence of Planetary Flyby Events on Binary Asteroid’s Impact Risk
Authors: Xiyun Hou, Pan Tan, Xin Liu, Bosheng Li
Figure caption: (a) Diagram of a binary asteroid flyby event. (b) Hyperbolic flyby orbit and the synodic frame.
Paper: An Efficient Shift-and-stack Algorithm Applied to Detection Catalogs
Authors: Steven Stetzler, Mario Jurić, Pedro H. Bernardinelli, Dino Bektešević, Colin Orion Chandler, Andrew J. Connolly, Fred C. Adams, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Luis E. Salazar-Manzano, Hilke Schlichting, Scott S. Sheppard, Dallin Spencer, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: The expected number of detection counts in a bin of size Δx for objects of different SNR ν found in catalogs of different SNR thresholds νth. Thick (thin) colored lines approximately indicate when the expected number of signal detections will be larger (less) than the expected number of noise detections, i.e., when ﹩{\mathbb{E}}[{N}_{{\rm{signal}}}]/{\mathbb{E}}[{N}_{{\rm{noise}}}]\gt 1﹩ (or <1), indicating when a single object of the given SNR ν is distinguishable from noise in a stack of the detection catalog that corresponds to the given object’s trajectory. Black solid (dashed) lines indicate values of ﹩{N}_{{\rm{\min }}}﹩ that produce a false-positive rate of ϵ = 100/Nstacks in an example MBA (TNO) search covering Ω = 162 arcmin2 with a = 1″ seeing and a Δt = 4 hr time baseline. Colored lines lying in regions of the parameter space ﹩{N}_{\min }={\mathbb{E}}[{N}_{\mathrm{signal}}]+{\mathbb{E}}[{N}_{\mathrm{noise}}]﹩ and Δx above (below) the black lines represent when objects of the given SNR ν are (un)likely to appear in the results of a search before producing 100 results corresponding to stacks of noise detections.
Paper: An Efficient Shift-and-stack Algorithm Applied to Detection Catalogs
Authors: Steven Stetzler, Mario Jurić, Pedro H. Bernardinelli, Dino Bektešević, Colin Orion Chandler, Andrew J. Connolly, Fred C. Adams, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Luis E. Salazar-Manzano, Hilke Schlichting, Scott S. Sheppard, Dallin Spencer, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: The on-sky coordinates of a moving object with respect to time. The dashed black line represents a trajectory estimated using least-squares multivariate regression, which does not predict the trajectory accurately, due to the presence of outliers in the data set. The solid black line represents a trajectory estimated using robust multivariate regression utilizing the MCD, which accurately predicts the moving-object trajectory in the presence of outliers.
Paper: An Efficient Shift-and-stack Algorithm Applied to Detection Catalogs
Authors: Steven Stetzler, Mario Jurić, Pedro H. Bernardinelli, Dino Bektešević, Colin Orion Chandler, Andrew J. Connolly, Fred C. Adams, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Luis E. Salazar-Manzano, Hilke Schlichting, Scott S. Sheppard, Dallin Spencer, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: The number of peaks and pixels in a likelihood image derived from a 2048 × 4096 CCD difference image as a function of the SNR threshold. At all values of SNR, the number of detection peaks is smaller by factors of 102–106×.
Paper: An Efficient Shift-and-stack Algorithm Applied to Detection Catalogs
Authors: Steven Stetzler, Mario Jurić, Pedro H. Bernardinelli, Dino Bektešević, Colin Orion Chandler, Andrew J. Connolly, Fred C. Adams, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Luis E. Salazar-Manzano, Hilke Schlichting, Scott S. Sheppard, Dallin Spencer, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: The distributions of the velocities and magnitudes of the injected synthetic MBAs and TNOs.
Paper: Survey of S-type AGB Stars Using the KVN Four-band Receiving System: SMASTES II
Authors: Seong-Min Son, Se-Hyung Cho, Jaeheon Kim, Hyeon Baek, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Observational results of S-type stars in the IRAS Two-color diagram for 146 stars with available IRAS data. The curved black solid line is the evolutionary track defined by W. E. C. J. Van der Veen & H. J. Habing (1988). The blue dashed line indicates the two groups of post-AGB stars, LI (left of IRAS; blue group) and RI (right of IRAS; red group; M. N. Sevenster 2002b). Gray circles indicate S-type stars in which no maser or thermal lines were detected. Red circles indicate (9: RW And, 15: V418 Cas, 91: S Her, 100: ST Sgr, 126: V865 Aql, 150: WY Cas), red rectangles SiO and HCN detected sources (16: S Cas, 102: W Aql, 110: R Cyg, 114: χ Cyg). Yellow circle (83: RS Cnc) and blue circles (6: R And, 21: W And). Green stars mark M-type stars in which the SiO v = 2, J = 2−1 maser was detected (a: NV Aur, b: TX Cam, c: IU Tau, d: V1111 Oph).
Paper: Survey of S-type AGB Stars Using the KVN Four-band Receiving System: SMASTES II
Authors: Seong-Min Son, Se-Hyung Cho, Jaeheon Kim, Hyeon Baek, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: Wind velocity profile according to radial distances for 4 HCN detected S-type stars: S Cas (16), W Aql (102), R Cyg (110), and χ Cyg (114). The distances of the dominant line formation region in units of stellar radius from the central star are as follows. SiO maser adopted 3 R* as the median value between 2 and 4 R* (P. J. Diamond et al. 1994; D. A. Boboltz & M. Wittkowski 2005), and 120 R* for HCN, 440 R* for the SiO thermal lines, and 1300 R* for CO lines based on the median values measured by S. H. J. Wallström et al. (2024). The vertical dashed line indicates dust condensation radius, Rdust at ∼6 R* derived by C. A. Gottlieb et al. (2022b).
Paper: Survey of S-type AGB Stars Using the KVN Four-band Receiving System: SMASTES II
Authors: Seong-Min Son, Se-Hyung Cho, Jaeheon Kim, Hyeon Baek, Dong-Hwan Yoon, Kyung-Won Suh
Figure caption: The spectra of 14 detected S-type stars observed from simultaneous observations of 19 molecular lines. The X-axis indicates the velocity of the local standard of rest (VLSR), and the Y-axis indicates the flux density. The vertical gray solid line marks the stellar velocity. Additionally, spectra of W Aql observed with KVN from 2010 to 2022 are included, displaying five detected epochs. Observational dates are presented in yymmdd format, and the corresponding pulsation phase at each epoch is labeled as ϕ. The pulsation phases were calculated using available optical data from the American Association of Variable Star Observers (AAVSO; https://www.aavso.org).
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: Photograph of the L1/L2 assembly being hoisted into the SDSS telescope primary mirror cell.
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 best image recorded during commissioning, 2021 November 4.
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: A focus sweep mosaic of images in i’ and associated through-focus curve (field angle = 0).
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: Focal surface sag measured deviation at the edge of the field for the g’, r’, and i’ filters.
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: Rendering of the FSC with the fiber cartridge made semitransparent for viewing.
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: Spot diagrams 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.
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 optical bandpass. (a) Spatial distribution, relative to the centroid location. (b) Angular distribution, relative to the focal surface normal.