adsabs/AstroCLIMB huggingface dataset:
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Distribution (2D histogram) of source detection as a function of instrumental magnitude and QF (top), ﹩{\mathrm{log}}_{10}{\hat{\chi }}_{r}^{2}﹩ (middle), fracflux (bottom). Detections shown are in r band for a typical line of sight (0.°5 radius) toward the Galactic plane (ℓ, b) = (−65°, 0°), with no cut on photometricity. Edge case sources with negative flux are excluded. The color scale is in log-density, and each panel has its own normalization (light, white, low; dark, blue, high density). Quality cuts are shown as green-dashed lines.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Classification of the DECaPS2 r-band imaging by crowdsource nebulosity CNN. Three of the four possible classes are shown as increasing opacity RGB color (nebulosity, light neb, and error), and the fourth class (normal) can be inferred by taking the complement. Each NSide = 512 HEALPix pixel displays the mean probability of each class over all photometric detections in the region. The probability associated with each source detection is the class probability of the pixel closest to the center of the source.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: DECaPS2 objects grouped by the bluest and reddest bands in which that object has an OK detection. The number of objects (in millions) is shown, and each entry is colored based on its relative proportion of the sample (logarithmic color scale, white low, black high). Sources with no OK detections are shown as an inset. The top panel uses the usual definition of OK detection while the bottom panel additionally requires fracflux > 0.75.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Color–magnitude diagrams (CMDs) in i vs. i − z for a beam of radius 0.°5 on a grid of Galactic latitude and longitude over the survey footprint. Each CMD color scale is in log-density and has its own normalization (light, white, low; dark, blue, high density). The features associated with blue main-sequence stars in the disk (A), red clump stars (B), and red-giant-branch stars (C) are labeled. Reddening vector showing effect of dust plotted in (−116°, 1°) for reference.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Time-invariant flat-field across the full DECam field of view produced during photometric calibration of DECaPS2. Each panel shows a different photometric band and the median and σ IQR in millimagnitudes of the flat-field are in the bottom left and right corners, respectively. Gaps between CCDs of order 200 pixels are not shown in this large-scale representation. The sky orientation shown for the focal plane is north up, west right.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Median r − i color for sources in the DECaPS2 catalog across the survey footprint (NSide = 512). This figure employs a cut requiring sources to be brighter than 19th magnitude in the i band and be detected in r band.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: High-resolution coverage map of the DECaSP2 survey footprint showing the number of photometric g-band visits. Small-scale variations in coverage resulting from the tiling strategy and CCD failures are visible.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Median g-band ﹩{\chi }_{r}^{2}﹩ (top) and fracflux (bottom) over all objects in the survey footprint.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Zoomed-in version of Figure 2 at the scale of the focal plane of DECam.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Top left: median Z-score for unblended, injected z-band sources as a function of the injected S/N for both flux and cflux. Top right: median Z-score for injected sources with moderate S/N as a function of distance to a source in the original image. Bottom left: additional dependence on the neighbor S/N is shown. Bottom right: converts the bottom left panel into a 2D histogram of the median Z-score bias vs. the median fracflux for the given injected-neighbor source distance. Color scale is logarithmic density (light, white, low; dark, blue, high density) with gray indicating 0 density.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Same as Figure 21 for Z-score σ IQR instead of the median Z-score.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Left: median fracflux as a function of the neighbor S/N and distance between the injected source and neighbor. Middle: IQR of the distance between the recovered location for an injection and the nearest neighbor on the same axes. Right: line cut along the green-dashed line in the middle panel showing the median distance between the recovered location for an injection and the nearest neighbor vs. the between the true injected location and the nearest neighbor. Perfect location recovery would fall along the 1:1 line (gray, dashed).
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Top: single-exposure g-band image of M62 with labeled radii in steps of ﹩1\buildrel{\,\prime}\over{.} 2﹩. Color scale is arcsinh stretched around the median with high and low counts in black and white, respectively. Middle: CMD in g vs. g − r for all sources within ﹩6^{\prime} ﹩ of the center of M62 using flux (left) and cflux (right). Color scale shows log density (light, white, low; dark, blue, high) on a common scale. Bottom: line cut along the green-dashed line in middle panels showing the sharper main sequence given by cflux.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Variation of the photometric depth (top) and reliable separation (bottom) in i band across the survey footprint. Both are determined by a threshold of −169 mmag bias on recovered injected sources. The average depth from Figure 19 and the median reliable separation over the survey footprint are indicated on the respective color bar by a green line.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Top: image (g-band) stamps cut from annuli around M62 between the indicated radii. Each image is arcsinh stretched around the median with its own color scale (black high and white low counts) to emphasize the increasing degree of blending toward the center of the globular cluster. Bottom: CMDs in g vs. g − r for sources found in the indicated annuli. Color scale shows log density (light, white, low; dark, blue, high) on a common scale in units of sources per square-degree.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: CMD in r vs. r − i using flux (left) and cflux (right) for selected sources near the Vela supernova remnant impacted by nebulosity (see text for exact cuts). Color scale shows log density (light, white, low; dark, blue, high) on a common scale. Reddening vector (right) showing effect of dust plotted for reference. cflux shifts stars with overestimated r-band flux toward a simple reddened main sequence.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: Color map of the multiplicative underestimation of error as measured by σ IQR for z-band flux and cflux over the survey footprint. The color scale is log2 to emphasize the large range of values while maintaining interpretability. Top and bottom compare results for flux and cflux, respectively.
Paper: The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Andrew K. Saydjari, Edward F. Schlafly, Dustin Lang, Aaron M. Meisner, Gregory M. Green, Catherine Zucker, Ioana Zelko, Joshua S. Speagle, 佳士 沈, Tansu Daylan, Albert Lee, Francisco Valdes, David Schlegel, Douglas P. Finkbeiner
Figure caption: The ratio of the additional uncertainty CLOUDCOVERR.JL introduces as the result of correlations to diagonal Poisson uncertainty from the background sky counts (Equation (9)), shown over the survey footprint. Each HEALPix pixel shows an outlier-clipped mean with a further requirement that sources have the CLOUDCOVERR.JL flag dnt = 0.
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: Trends in the peak energetic particle flux and frequency of IS⊙IS energetic particle enhancements. Blue dashed line shows the radial distance of Parker Solar Probe as a function of time. Overlayed on that line are circles indicating the peak event flux (both as circle size and color; see color bar at the top of the figure) of each energetic particle enhancement. The border of the circle in magenta and cyan indicates that the event was observed in EPI-Lo and EPI-Hi, respectively. Black circles indicate the monthly sunspot number. Black crosses in the lower panel show the time of each of the enhancements.
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: The SEP event observed beginning on 2021 May 28 (Event Catalog number 2021-148). (a) EPI-Hi LETA proton flux spectrogram, (b) EPI-Hi LETA proton flux time series summed over energies 1–10 MeV, (c) EPI-Lo proton flux spectrogram averaged over all EPI-Lo apertures, (d) EPI-Lo proton flux time series summed over all apertures and energies ∼78–200 keV. Black vertical dashed lines in panels (b) and (d) indicate the start time identified in the Event Catalog. Brown vertical dashed lines in panels (b)and (d) represent the time of the maximum flux in EPI-Hi and EPI-Lo (separately). Orange vertical dashed line in panels (b) and (d) represent the identified end time of the event in the Event Catalog. Cyan horizontal dashed line in panels (b) and (d) represent the baseline flux calculated as the average over the 12 hr preceding the event. Gray regions indicate data gaps (see text for details).
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: Total number of days IS⊙IS has been observing and number of days in which IS⊙IS has observed events as a function of heliocentric distance (binned in 0.1 au increments).
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: Daily averaged time intensity profiles of ∼1–10 MeV protons from EPI-Hi/LET A (panel (a)) and ∼78–200 keV protons from EPI-Lo over the course of the Parker Solar Probe mission to the time of writing.
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: Trace of Parker Solar Probe Orbit 10 with overlay of energetic ion count rates from EPI-Hi LETA (outside of orbit trace) and EPI-Lo (inside of orbit trace) following the format developed by McComas et al. (2019). Noteworthy events mentioned in the text are circled.
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: Power-law spectral indices of a subset of IS⊙IS events observed to have dispersive onsets as a function of spacecraft heliocentric distance. Spectra are fit separately for EPI-Lo and EPI-Hi due to ongoing intercalibration work. Both populations show a positive correlation between spectral index and heliocentric distance indicated by the Pearson correlation coefficients (CC) shown on the plot. Both the color and size of each of the markers indicate the time (in days since the start of the mission) of the event.
Paper: A Living Catalog of Parker Solar Probe IS⊙IS Energetic Particle Enhancements
Authors: J. G. Mitchell, C. M. S. Cohen, T. J. Eddy, C. J. Joyce, J. S. Rankin, M. M. Shen, G. A. de Nolfo, E. R. Christian, D. J. McComas, R. L. McNutt, M. E. Wiedenbeck, N. A. Schwadron, M. E. Hill, A. W. Labrador, R. A. Leske, R. A. Mewaldt, D. G. Mitchell, J. R. Szalay
Figure caption: Fraction of total observing time in which IS⊙IS observed particle enhancements as a function of heliocentric distance.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Integrated halo baryon density (left), temperature (center), and entropy (right) normalized to the corresponding nonlinear scale defined in Equation (65) for redshifts listed in the legend. Each marker denotes the mean value for all halos in a given redshift and mass bin consisting of at least 10 halos. We only include results from bins containing more than one redshift sample. The solid black line traces the mean value of each bin for all redshifts, while the shaded gray band shows the corresponding standard deviation. The dashed–dotted black line represents a least-squares regression fit of the data for each quantity. The bottom panel shows the ratio of all measurements to the mean curve, where the horizontal dashed lines indicate a ±1%, ±5%, and ±2% spread for the left, center, and right panels, respectively.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Top panel: radial profiles of the baryon fraction normalized to the universal mean at z = 0 for the gravity-only scale-free simulation. The solid colored lines trace the median profile for halos stacked in five mass bins. The legend lists the bin widths in units of ﹩\mathrm{log}({M}_{200})﹩. For the most massive bin, we also show the 25th and 75th percentiles from the stack as error bars. The vertical dotted lines indicate the location of the convergence length R conv = 24.4 h −1 kpc for each mass bin of the corresponding color. Bottom: global baryon mass fraction in units of the universal mean as a function of M 200 at z = 0. The red circles denote the median in each bin, while the error bars show the 25th and 75th percentiles of the distribution. The vertical dashed black line indicates the converged mass scale M conv = 3 × 1011 h −1  M ⊙. In both panels, the gray shaded band highlights ±1% deviations from the universal mean.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Radial profiles showing density (left), temperature (center), and entropy (right) for the Santa Barbara cluster (Frenk et al. 1999) at redshift z = 0 for a number of Lagrangian (CRK-HACC, GADGET-2, DISPH), Eulerian (Nyx, SAMR), and hybrid (GIZMO, AREPO) solvers. In the case of AREPO, we show results from both the strict energy conservation and dual entropy formulations. The lower (upper) set of data points in the left panel corresponds to the baryon (dark matter) density profile, while the vertical dotted line in each panel denotes R 200 = 2.75 Mpc. Notably, the CRK-HACC measurements are consistent with the grid-based approaches.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Radial profiles showing density (left), temperature (center), and entropy (right) for the nIFTy cluster (Sembolini et al. 2016) at redshift z = 0 for a variety of Lagrangian (CRK-HACC, GADGET-2, G2-ANARCHY, G3-X-ART, G3-SPHS, G3-MAGNETICUM), Eulerian (RAMSES, ART), and hybrid (AREPO) solvers. The lower set of data points in the left panel corresponds to the baryon density profile from the nonradiative run, while the upper set of points corresponds to the total matter density profile in the gravity-only run. In each panel, the vertical dotted line denotes the halo radius, R 200 = 2.41 Mpc, identified with CRK-HACC. As opposed to the discrepancies seen in Figure 10, most of the methods are in closer relative agreement for the nIFTy comparison. The CRK-HACC results are again consistent with the mesh-codes, and are among the grouping of modern SPH codes.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Stacked radial profiles of baryon density (left), temperature (center), and entropy (right) normalized to the nonlinear scale (Equation (65)) for redshifts detailed in the legend. We show results for three separate M/M * mass bins, which are separately labeled in each plot. The markers denote the mean stack for halos at a fixed redshift within a given mass bin, while the solid black line and gray shading trace the combined stack and its standard deviation. The bottom panels show the ratio with the combined stack profile of the middle mass bin, where the horizontal dashed lines indicate a ±5% spread.
Paper: Simulating Hydrodynamics in Cosmology with CRK-HACC
Authors: Nicholas Frontiere, J. D. Emberson, Michael Buehlmann, Joseph Adamo, Salman Habib, Katrin Heitmann, Claude-André Faucher-Giguère
Figure caption: Radial profiles showing density (left), temperature (center), and entropy (right) for the Argonne cluster run at redshift z = 0. The lower (upper) set of data points in the left panel correspond to the baryon (dark matter) density profile, while the vertical dotted line in each panel denotes R 200 = 2.52 Mpc found by CRK-HACC. As in Figure 10, the CRK-HACC solutions are closely consistent with the Eulerian approach (Nyx), where the results appear to be numerically converged.