adsabs/AstroCLIMB huggingface dataset:
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Gini–M20 diagram (top panel) and C–A diagram (bottom panel) for our S-PLUS sample, including all 47 metal-poor dwarf galaxy candidates (circles). Hexagon symbols highlight the galaxies followed up with GMOS. High Gini and M20 values imply that a galaxy is in a merger phase. Similarly, high concentration and asymmetry values indicate perturbed morphologies. The yellow lines show the separation between mergers (or perturbed) and noninteracting galaxies as established by J. M. Lotz et al. (2008) and A. C. Krabbe et al. (2024) for the Gini–M20 and C–A diagrams, respectively. Galaxy 2 and 6 lie above the threshold values that separate major merger (and perturbed) candidates from noninteracting galaxies in both diagnostic diagrams.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Offsets from the mass–metallicity (x-axis) and from the luminosity–metallicity relations for the sample of dwarf galaxies selected in different photometric surveys (SDSS, DES, S-PLUS). The offsets are calculated from the relation found in the Local Volume Legacy (D. A. Berg et al. 2012). The yellow shaded area shows the 1σ scatter of the L–Z and M–Z relation in the LVL. Two out of six galaxies selected from S-PLUS (hexagons) show the largest offsets in both relations compared with the galaxies in the other surveys.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Specific star formation rate vs. stellar mass. The S-PLUS galaxies (hexagon symbols) are compared to metal-poor dwarfs selected in other photometric surveys, such as the SDSS (H18, circles) and DES (L23, squares).
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Legacy g-band images of two galaxies in our sample, ID 2 (left panel) and ID 6 (right panel), with C, A, G, and M20 indices, indicating that the galaxies are in an interaction or merging phase.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Legacy g-band images of other galaxies with C, A, G, and M20 indices indicate that the galaxies are in an interaction or merging phase.
Paper: The Southern Photometrical Local Universe Survey (S-PLUS): Searching for Metal-poor Dwarf Galaxies
Authors: M. Grossi, D. R. Gonçalves, A. C. Krabbe, L. A. Gutiérrez Soto, E. Telles, L. S. Ribeiro, T. S. Gonçalves, A. E. de Araujo-Carvalho, A. R. Lopes, A. V. Smith Castelli, M. E. De Rossi, C. Lima-Dias, G. Limberg, C. E. Ferreira Lopes, J. A. Hernandez-Jimenez, P. K. Humire, A. L. Chies Santos, L. Lomelí-Núñez, S. Torres-Flores, F. R. Herpich, G. B. Oliveira Schwarz, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Hα line profiles of the four targets observed with GMOS, summed over the extent of the emission from all the star-forming knots.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Comparisons between true redshifts ztrue and predicted photometric redshifts zphot from the 7DS mock catalog under different input conditions. From top to bottom: best-fit photometric redshifts from IMS Y5 (40 bands, no prior), WTS Y5 (20 bands, no prior), WTS Y5 (40 bands, no prior), WTS Y5 (40 bands, with a m625 prior), and RIS (40 bands, no prior).
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Examples of matched SEDs and zPDF from 7DS and PS1. (a) A quiescent galaxy at ztrue = 0.377 with a Balmer break. (b) A star-forming galaxy at ztrue = 0.118 with emission lines. The original SED from EL-COSMOS is shown as a gray line. The orange line is the best-fit photo-z from PS1, and the blue line is from WTS Y5.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Comparisons between true redshifts and predicted photometric redshifts from the 7DS mock catalog with the combination of other surveys. From top to bottom: photometric redshifts from WTS Y5 + PS1, WTS Y5 + VIKING, and WTS Y5 + SPHEREx all-sky.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: A mr − m625 color as a function of true redshifts (middle panel). Adjacent colors of m613 (top panel) and m638 (bottom panel) are also described.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: A comparison of photo-zs obtained from PS1 and 7DS for a given magnitude bin at 20 ≤ m625 ≤ 22. No priors are applied for both results.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Top panel: simulated filter transmission curves. Bottom panel: an example of the EL-COSMOS SED (gray line) and its 7DS-like mock (data points).
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Overall photo-z metrics for WTS Y5 and combinations with other surveys. Left panel: catastrophic failure η as a function of NMAD σNMAD. The size of the markers represents the magnitude range (19, 20, 21, 22) in increasing order. Right panel: bias b as a function of true redshift. The area smaller than the benchmarking values, σNMAD = 0.01, η = 0.10, and b = 0.01, is shaded in gray.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: An illustration of the redshifted SED at z = 0.5, 1.0, 1.5, 2.0, 2.5, and 3.0 and wavelength window filters from 7DS (40 medium-band filters, 4000–8875 Å), Euclid (J and H), and SPHEREx (96 LVFs, 0.75–5.0 μm) as a function of redshift.
Paper: Photometric Redshift Forecast for the 7-Dimensional Sky Survey
Authors: Eunhee Ko, 은희 고, Myungshin Im, Yujin Yang, Ji Hoon Kim, Seong-Kook Lee, Gregory S.-H. Paek
Figure caption: Examples of matched SEDs and zPDF from 7DS alone and in combination with (a) VIKING and (b) SPHEREx.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: Zoomed-in views of several protostellar outflows or candidate sources in the Oph A region. The approximate locations (northwest, west, etc.) are labeled above each panel. (a) Bipolar jet associated with [GY92] 20, traced by two solid curves in the JWST F470N image. The jet from GSS 30 extending northward is indicated by a dotted curve. (b) Jets from GSS 30 IRS 1/2/3 as seen in the F470N image, overlaid with high-velocity CO components. Cyan contours show CO integrated intensities in the velocity range of –26.5 to –4.5 km s−1, and magenta contours represent the range of –9.5 to 25.5 km s−1. Contour levels for cyan are at (2.5, 5, 7.5, 10, 12.5, 15) × σ, with 1σ = 0.234 Jy beam−1 km s−1. Magenta contours are at (2.5, 5) × σ, with 1σ = 0.2 Jy beam−1 km s−1. (c) Same as panel (b), but showing low-velocity CO components from the GSS 30 IRS 1/2/3 outflows. Blue contours integrate over –1–0 km s−1, and red contours cover 6.5 to 8.5 km s−1. Both use contour levels of (6, 12, 18, 24, 36, 48, 60) ×σ, where 1σ = 0.07 Jy beam−1 km s−1. (d) Possible blueshifted CO component associated with ALMA Oph A 3. Gray contours show the 1.3 mm dust continuum emission, drawn at 3, 5, 7σ, etc. (e) JWST F470N image overlaid with CO blueshifted components near VLA 1623W, [GY92] 21, and [GY92] 23. Contours are at 3, 6, 9σ, etc., with 1σ = 43 mJy beam−1 km s−1. (f) Blueshifted CO integrated intensity (2.1–2.5 km s−1) around VLA 1623W, [GY92] 21, and [GY92] 23. Dashed ellipses mark the outflow components from [GY92] 21 and [GY92] 23. The dashed line shows the disk orientation of [GY92] 21.
Paper: Evidence of Time-dependent Diffusive Shock Acceleration in the 2022 September 5 Solar Energetic Particle Event
Authors: Xiaohang Chen, Lulu Zhao, Joe Giacalone, Nishtha Sachdeva, Igor V. Sokolov, Gábor Tóth, Christina M. S. Cohen, David Lario, Fan Guo, Athanasios Kouloumvakos, Tamas I. Gombosi, Zhenguang Huang, Ward B. Manchester, Bart van der Holst, Weihao Liu, David J. McComas, Matthew E. Hill, George C. Ho
Figure caption: Overview of the PSP observations on 2022 September 5 from 16:00 to 18:15 UT. (a) Magnetic field magnitude and components in the RTN coordinate system, with the heliocentric distance of PSP shown along the top x-axis in solar radii. Energy spectrograms for proton intensities from (b) HET-A, (c) LET-A, and (d) EPI-Lo of all the looking directions. (e) Energy spectrograms for EPI-Lo plotted against inverse velocity. The vertical dotted line indicates the CME eruption time. The gray and red dashed lines represent the regular velocity dispersion and IVA, respectively.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: 12CO channel maps around the S1-GSS 30 (from the northern part of the Oph A ridge to the west) region in the velocity range from 0 to 6 km s−1. The 1.3 mm dust continuum emission is indicated in blue contours. A dotted circle in the last panel indicates a part of the redshifted outflow component of [GY92]30, whereas the blueshifted component is shown in the first panel. In the lower-left panel, the JWST F470N image is presented, and the protostellar jet from [GY92]30 is clearly seen. Two open white boxes are the areas where 12CO and C18O flux densities presented in Figure 8 are computed.
Paper: Evidence of Time-dependent Diffusive Shock Acceleration in the 2022 September 5 Solar Energetic Particle Event
Authors: Xiaohang Chen, Lulu Zhao, Joe Giacalone, Nishtha Sachdeva, Igor V. Sokolov, Gábor Tóth, Christina M. S. Cohen, David Lario, Fan Guo, Athanasios Kouloumvakos, Tamas I. Gombosi, Zhenguang Huang, Ward B. Manchester, Bart van der Holst, Weihao Liu, David J. McComas, Matthew E. Hill, George C. Ho
Figure caption: Longitudinal spacecraft constellation and magnetic connectivity at 16:00 UT on 2022 September 5, generated with the Solar-MACH tool (J. Gieseler et al. 2023). The colored markers indicate the locations of STEREO-A (red), Earth (green), PSP (purple), and SolO (blue). The black arrow denotes the longitude of the parent active region. The colored lines and dashed black line from the active region represent the nominal Parker spirals of 400 km s−1 solar wind.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: (a) C18O moment-0 map with the two lines along which we took position–velocity maps, (b) and (c): C18O position–velocity maps along the A–B and C–D lines indicated in panel (a), respectively. The two dashed lines in panel (a) highlight the prominent striations, which are visible even in the integrated intensity image. These striations are most clearly observed in the 3.8 km s−1 channel. The arrows in panels (b) and (c) point to the same striations.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: 12CO and C18O integrated flux densities as a function of velocity at the east (a) and west (c) areas. The enlarged views of panels (a) and (c) are shown in panels (b) and (d). The red and blue colors represent the 12CO and C18O profiles, respectively. The areas taken are presented in Figure 7.
Paper: Unveiling Stellar Feedback and Cloud Structure in the ρ Ophiuchi-A Region Using ALMA and JWST: Discovery of Substellar Cores, C18O Striations, and Protostellar Outflows
Authors: Fumitaka Nakamura, Ryohei Kawabe, Shuo Huang, Kazuya Saigo, Naomi Hirano, Shigehisa Takakuwa, Takeshi Kamazaki, Motohide Tamura, James Di Francesco, Rachel Friesen, Kazunari Iwasaki, Chihomi Hara
Figure caption: C18O velocity channel maps (3.0 –3.8 km s−1) and striations in the S1 bubble. Contours show the 1.3 mm dust continuum emission. Some striations are indicated in the boxes in the channel maps of 3.2 and 3.4 km s−1, where the striations are prominent (see also Figures 10(b) and (c)). The magnetic field orientation in the bubble (N. Lê et al. 2024) is indicated by an arrow in the panel of 3.2 km s−1. For comparison, we also present the JWST F470N image with the 1.3 mm dust continuum emission and C18O integrated intensity map in the bottom-left panel.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: Upper panel: median r-band projected surface brightness profiles of our simulated clusters “observed” at z = 0.25 along with a high-richness sample of DES Y1 clusters at z = 0.25 from Y. Zhang et al. (2019). The solid brown curve shows the median simulated cluster profiles using the fiducial M/Lr with error bars showing the range of surface brightnesses allowed by the error bars on the observed ICL colors used to obtain the M/Lr. The shaded band around the solid curve spans the 16th to 84th percentiles of the simulated cluster sample. We further show a lower-redshift z = 0.025 median surface brightness profile using the fiducial M/Lr. The median and 16th to 84th percentiles of Rsp⋆,1 and Rsp⋆,2 for the cluster sample are indicated as vertical lines and shaded bands. Lower panel: radial limits of the indicated surveys calculated by comparing the surface brightness limits for each survey to the median surface brightness profile in the relevant band. Each point indicates the radial limit using the fiducial M/L with error bars propagating the error on the M/L. Radial limits are shown corresponding to both wide and deep surface brightness limits as well as for z = 0.025 and 0.25. Lower-redshift clusters allow for a small gain in probing the outskirts of the ICL. These limits in the radial reach of these surveys indicate that Rsp⋆,2 is within the reach of these surveys, particularly the Nancy Grace Roman Space Telescope, while Rsp⋆,1 is potentially too faint to observe with existing survey strategies.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: For each present-day cluster property, curves and violin plots illustrate the timescales at which major mergers most affect the property, thereby affording the property the most classification power about mergers at that time. Upper panel: Matthews correlation coefficients (MCC) of cuts in cluster properties optimized to best classify clusters as either having had at least one major merger or no major mergers in time windows of width 1 dynamical time centered on T. The shaded bands indicate the jackknife-estimated standard error. Horizontal line segments at the top of the plot indicate the time windows corresponding to the most “impactful” cut, the one which maximizes the MCC between the true and expected merger classifications. Lower panels: violin plots showing the distributions of each present-day property for clusters that experienced a merger around time T (dark) and for those which did not (light). The solid lines indicate the optimized cut between the distributions. When two violins are well separated, this means that the present-day property is impacted by the merger history at that time and that the optimized cut between them will correspond to a higher MCC. The tracers of merger history proposed in this work, Rsp⋆,1 and Rsp⋆,2, are similarly capable of classifying clusters that have merged and not merged at slightly different timescales. They are slightly less capable than the known tracer of relaxedness, xoff, but substantially more capable than cvir and M⋆1,2.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: Spearman’s correlation coefficients between present-day cluster properties and the MAH as a function of time. Time T is measured in units of number of dynamical times (where T = 0 indicates the present day) and the corresponding scale factors are included in the upper x-axis for reference. The shaded bands indicate the jackknife-estimated standard error (see Section 5.1 for further details). We plot our proposed tracers of the MAH (solid lines): the primary stellar splashback Rsp⋆,1 and the secondary stellar splashback Rsp⋆,2. Traditional tracers of the MAH are shown for comparison (dashed lines): the central offset xoff, the concentration cvir, and the stellar mass gap M⋆1,2. Rsp⋆,1 is highly correlated with m(T), with a peak 1.16 dynamical times ago. Rsp⋆,2 is strongly correlated to a slightly lesser degree and peaks more recently, 0.73 dynamical times ago. xoff is correlated similarly to Rsp⋆,2, but M⋆1,2 and cvir are both substantially less correlated with MAH than the stellar splashback tracers.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: An example of the stellar density maps, phase-space distributions, and radial stellar mass density profiles and our separation of particle populations for a cluster following the methods described in Section 4.1. In the left column, we show the projected stellar mass density map of the cluster and indicate the relevant radii. In the central column, we show the density of stellar mass in radial velocity phase space separated into particles on infall, first orbit, and second orbit. As particles are only star-tagged after crossing Rvir, the infall panel is lacking any stars outside that radius. In the right column, we show the profiles and corresponding log derivatives of particles on all orbits, on first orbit, and on second orbit. The dashed circles and vertical lines indicate the resulting measured primary and secondary stellar splashback radii for this cluster.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: Predictions of the MULTICAM model for MAH as a function of the primary and secondary stellar splashback radii, Rsp⋆,1 and Rsp⋆,2, created by generating 500 samples for each pair of Rsp⋆,1 and Rsp⋆,2. Upper panels: the median m(T) of the 500 predicted samples generated by MULTICAM at three epochs (columns) as a function of the primary and secondary splashback, Rsp⋆,1 and Rsp⋆,2. Lower panels: the median m(T) of the predicted MAH samples at three epochs (columns) as a function of Rsp⋆,1 for three selected Rsp⋆,2 values. The RMSE scatter around the median for Rsp⋆,2 = 0.7 is shown as a shaded band around the curve. The lack of smoothness in the contours and the curves is a result of the stochasticity inherent in generating a finite number of samples. The sensitivity of the predictions to each stellar splashback radius varies depending on epoch, corresponding to the varying of correlation strengths in Figure 4.
Paper: Memoirs of Mass Accretion: Probing the Edges of Intracluster Light in Simulated Galaxy Clusters
Authors: Tara Dacunha, Phil Mansfield, Risa H. Wechsler
Figure caption: Upper panel: MCC of the optimized linear cut best separating clusters that merged and did not merge in a window of 1.0 dynamical time around T. The shaded band indicates the standard error on the MCC as determined by jackknife resampling. The vertical dotted line indicates the timescale at which the MCC curve begins to peak (T = –0.57). For comparison, the MCC curves of Rsp⋆,1 and Rsp⋆,2 from Figure 7 are overplotted. Lower panel: the scattered points and contours corresponding to the Rsp⋆,1 and Rsp⋆,2 values of clusters that merged and did not merge around that peak time of T = –0.57. The contours indicate six linearly spaced levels of density of the scatter points in the space, found using a kernel density estimator. The black dashed line indicates the optimized linear cut between the red and green distributions with the highest MCC.