adsabs/AstroCLIMB huggingface dataset:
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: Multiwavelength maps of SNR G40.5−0.5. Red: the MeerKAT radio continuum flux density at an effective frequency of 1.36 GHz. Green: Nobeyama 12CO J = 1–0 intensity map integrated in the velocity interval of +33–+36 km s−1 plus +39–+40 km s−1 (left; the emission between +37 km s−1 and +38 km s−1 is excluded to highlight the comparatively weak western part of the cap-like structure) and +45–+65 km s−1 (right). The white contours are the same as those in Figure 2.
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: Averaged spectra of regions “1” (top), “2” (middle), and “3” (bottom) in the velocity range +35–+47 and +30–+40 km s−1, respectively. The three regions are defined in Figures 4 and 5.
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: H I 21 cm intensity map integrated in the velocity interval of +33–+40 km s−1. The black boxes labeled “a” and “b” mark the regions where the spectra of H I and 12CO are extracted (see Figure 9).
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: Top: 12CO J = 3–2/J = 1–0 ratio map in the velocity interval of +45–+50 km s−1. The JCMT 12CO J = 3–2 data and Nobeyama 12CO J = 1–0 data are convolved to the same beam size (60″) and velocity resolution (0.65 km s−1). Values <3σ are masked. Bottom: the line profiles extracted from the black box on the northeastern radio boundary in the top panel. The vertical dashed line denotes the line wing at +46 km s−1.
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: PMOD CO spectra from a circular region covering SNR G40.5−0.5 (see the first panel of Figure 2). The blue and orange curves represent 12CO and 13CO J = 1–0 spectra, respectively. The dashed line denotes the 0 K main-beam temperature.
Paper: A New Investigation of the Molecular Environment of Supernova Remnant G40.5–0.5
Authors: Qian-Qian Zhang, Yang Chen, Qian-Cheng Liu, Xin Zhou, Tian-Yu Tu
Figure caption: VGPS H I (thick lines) and PMOD 12CO J = 1–0 (thin lines) spectra for positions “a” and “b” labeled in Figure 8. The vertical dashed lines denote the 12CO peak velocities of the MCs of +40.5 (a) and +34 km s−1 (b).
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 offsets from the exoTEDRF fit (purple) and NAMELESS fit (gold). Colors at the bottom of the plot show normalized and scaled cross-sections for TiO (cyan), VO (pink), H− (yellow), H2O (blue), and CO (orange) in order to visualize possible contributions to the phase offsets. Only H− could appear to trace the increase at shorter wavelengths. The larger offsets in the NAMELESS fit likely result from the inclusion of ellipsoidal variation in exoTEDRF, except in Order 2, where the addition of a stellar variability model causes a sharp drop in phase offsets. For clarity, Order 2 phase offsets from exoTEDRF are binned with three points per bin. Both reductions consistently show increasing eastward offsets at shorter wavelengths.
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: Nightside and dayside emission spectra from exoTEDRF (purple) and NAMELESS (gold) fits. As discussed in Section 2.3.5, the exoTEDRF fit penalizes negative planetary flux while NAMELESS does not, accounting for the differences in the nightside emission. Both model assumptions have implications on the inferred nightside temperatures as seen in Figure C6.
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: Nightside brightness temperature from exoTEDRF (purple) and NAMELESS (gold) nightside emission seen in the bottom panel of Figure C5. Negative flux values cannot be converted into a brightness temperature thereby the exoTEDRF fit has more points in brightness temperature at shorter wavelengths. Dashed vertical lines show the nightside effective temperature for exoTEDRF (purple) and NAMELESS (gold) showing that the inclusion of more brightness temperatures moves the effective temperature slightly higher.
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: Visualization of exoTEDRF reduction steps. (A) A raw, uncalibrated frame in counts of data numbers (DN). (B) Frame after superbias subtraction and 1/f correction on group level. (C) Frame after ramp fitting, at the end of Stage 1—detector level processing operations. (D) Final data product at the end of Stage 2—spectroscopic processing operations including second background subtraction, flat-field correcting, and bad pixel correction. The centroids for the spectral orders including the extraction width of 30 pixels are included in red (Order 1), blue (Order 2), and green (Order 3). Only Order 1 and 2 are used in this analysis. There are two bright order 0 contaminants located around x = [1000, 1150] and y = [125, 250]. With the absence of a GR700XD/F277W exposure for this observation, we are unable to measure the dilution effects of the contaminants within the spectral trace.
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: Contour plots from the BELL_EBM grid showing parameter slices from the best matched model to the planetary effective temperature. A red star is plotted in each contour to guide the eye to the location of the best matched model. Bond albedo is in line with simpler estimates based solely on dayside and nightside spectra, P0 is roughly in line with expected deposition depth of incoming stellar radiation, and estimated wind speed is much slower than expected.
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: Comparison of reduction pipelines between exoTEDRF (purple) and NAMELESS (gold) white light curves for Order 1 (left) and Order 2 (right). A difference between the two reductions (exoTEDRF—NAMELESS) is shown in the bottom row with the rms of the differences in the lower left corner. The two reductions agree well and show no noticeable differences.
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 panel: median reflected light contribution (blue) compared to Lambertian reflectors (dashed lines) with geometric albedos of 0.05 (green), 0.075 (gray), and 0.1 (red). Plotted in terms of the subobserver longitude, which is inversely related to the orbital phase (top ticks). Bottom panel: the measured apparent albedo for longitudinal slices centered at ϕ = 45°, 135°, 225°, 315°. The subobserver longitudes are then shifted to be from −180° to +180° for better visible clarity. Observations show a small geometric albedo compared to the Bond albedo and perhaps an eastward reflected offset.
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: Fits of systematics corrected spectroscopic light curves at various wavelengths at the 5 pixel per bin level. First two light curves are from Order 2 and the rest from Order 1 to show full wavelength coverage. Left: spectroscopic light curves (colored points) with the best-fit astrophysical model (black line). The data are fitted considering all integrations but are shown with 40 integrations per bin for visual clarity. Right: residuals of the best-fit astrophysical model to the detrended data shown at all integrations. A black dashed line is shown at zero to guide the eye. The rms of the residuals is shown in the top right.
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: Diagnostic plot showing results on five component PCA of time series to explain variance in the data. Left column corresponds to the eigenvalues while right column shows the corresponding eigenimages. First component shows the white light curve while other components correspond to detector-based signals (thermal beating pattern, position drifts, etc.) and noise. Components 4 and 5 revealed the presence of a minor tilt event. We use PCA components 2–4 in our light-curve fitting (see Methods).
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 m50 depth from fitting of the completeness (left), the number of candidate detections produced per detector (middle), and the number of synthetic objects (fakes) recovered (right) for the TNO and MBA searches as a function of the ﹩{N}_{{\rm{\min }}}﹩ parameter. The solid black line visualizes the estimated single-epoch m50 = 23.7. The dashed black line represents the theoretical achievable depth by coadding all of the images and is equal to ﹩{m}_{50}^{{\rm{coadd}}}=26.2﹩. Decreasing the value of ﹩{N}_{{\rm{\min }}}﹩ increases m50 depth and the number of synthetic objects recovered, at the cost of vastly increasing the number of results produced. Most of the results produced at low values of ﹩{N}_{{\rm{\min }}}﹩ are false-positive candidates.
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: Distributions of average separation between the ground truth and recovered trajectories of synthetic objects found via the image-based shift-and-stack (KBMOD) and catalog-based shift-and-stack (this work) over SNR = 1–5. Separation is computed as the great-circle distance between the two trajectories at a given point in time, and an average separation is computed over the 4 hr observing period. Distributions are represented as box-and-whisker plots that visualize (excluding outliers) the minimum, maximum, and 25th, 50th (median), and 75th percentiles of the distribution. A black dashed line visualizes an angular separation that corresponds to a fiducial pixel scale for DECam ps = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩263 pixel−1.
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: A visualization of the sky locations of a stacked detection catalog derived from a 4 hr sequence of DECam images with a grid of constant ecliptic latitude/longitude overlaid. Detections at a single epoch represent the on-sky location of a putative source on a difference image. Detections are accumulated across all 104 epochs and plotted jointly in this visualization. Moving objects appear as lines in this stacked visualization. Stationary variable sources as well as difference imaging artifacts appear as clusters and isolated points. Holes or voids in this visualization represent regions of the CCDs that were masked out due to the presence of bright stars and the resulting saturation of portions of the detector.
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 m50 depth achieved for the TNO (blue) and MBA (orange) searches as a function of the SNR of the input catalog choosing ﹩{N}_{{\rm{\min }}}﹩ such that the number of results per detector is fixed at 200. The solid black line represents a single-epoch SNR ∼ 5 limiting magnitude of m50 = 23.7, while the dashed black line represents the theoretical optimal achievable coadded depth of ﹩{m}_{50}^{{\rm{coadd}}}=26.2﹩. The dotted black line visualizes the expected scaling of achieved depth with SNR, extrapolated from the single-epoch limiting magnitude.
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 fraction of synthetic objects recovered as a function of their magnitude for the TNO and MBA searches. Dots represent the detection fraction in bins of size 0.5 mag, and error bars represent the asymmetric uncertainty in the estimated fraction using the Wilson score interval. Two reference magnitudes are visualized as black solid and dashed vertical lines. The solid black line visualizes the estimated single-epoch m50 = 23.7. The dashed black line represents the theoretical achievable depth by coadding all of the images, and it is equal to ﹩{m}_{50}^{{\rm{coadd}}}=26.2﹩.
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 CPU time and memory usage of our algorithm as a function of the m50 depth achieved. The black solid line visualizes the single-epoch m50 = 23.7, while the dashed black line visualizes the theoretical maximum ﹩{m}_{50}^{{\rm{coadd}}}=26.2﹩ that could be achieved through optimal coaddition.
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 median wall-clock runtime and memory usage of our catalog shift-and-stack algorithm for the TNO (blue) and MBA (orange) searches across the 60 DECam detectors searched. Error bars represent the standard deviation of the runtime and memory usage values measured.
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 CPU time and memory usage of the core-search component of our algorithm as a function of the Δx value and the SNR of the catalog searched. The black lines represent the predicted scaling of CPU time and memory with Δx−2.
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 fraction of synthetic TNOs recovered as a function of their magnitude using KBMOD and our algorithm at SNR ≥ 5, 4, 3, 2, 1.
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 relative total CPU time (speedup) and memory usage of our algorithm when compared to an image-based shift-and-stack search. The black solid line visualizes the single-epoch m50 = 23.7, while the dashed black line visualizes the theoretical maximum ﹩{m}_{50}^{{\rm{coadd}}}=26.2﹩ that could be achieved through optimal coaddition. The dotted black line visualizes the ﹩{m}_{50}^{{\rm{KBMOD}}}=25.47﹩ depth achieved in an image-based shift-and-stack approach, utilizing the KBMOD software.
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 relative core-search CPU time (speedup) and memory usage of our algorithm compared to an implementation of an image-based shift-and-stack search. The black lines represent the predicted scaling of speedup and memory with Δx2 and Δx−2, respectively.
Paper: Modeling the Optical Colors of Galactic Cirrus Clouds in the Stripe 82 Region
Authors: Kwang-Il Seon, Jongwan Ko, Woowon Byun, Jaehyun Lee, Young-Soo Jo
Figure caption: Mean scattered-light intensities as functions of ﹩{\tau }_{g}^{{\rm{h}}}﹩ for various Ms. The intensities are averaged over 10 random realizations of the density structure in the RT simulations. Standard deviations across the 10 samples are shown as error bars.