adsabs/AstroCLIMB huggingface dataset:
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Comparison of the BASS AGN to the velocity dispersions of the HETMGS survey (van den Bosch et al. 2015), which was designed to select the most massive BHs (and highest velocity dispersions) at all redshifts that could be dynamically resolved. For both samples, the redshift range is limited to 0.02 < z < 0.04 to avoid the low-mass galaxies at low redshifts in HETMGS that can be resolved.
Paper: BASS. XXVI. DR2 Host Galaxy Stellar Velocity Dispersions
Authors: Michael J. Koss, Benny Trakhtenbrot, Claudio Ricci, Kyuseok Oh, Franz E. Bauer, Daniel Stern, Turgay Caglar, Jakob S. den Brok, Richard Mushotzky, Federica Ricci, Julian E. Mejía-Restrepo, Isabella Lamperti, Ezequiel Treister, Rudolf E. Bär, Fiona Harrison, Meredith C. Powell, George C. Privon, Rogério Riffel, Alejandra F. Rojas, Kevin Schawinski, C. Megan Urry
Figure caption: Examples of excluded X-Shooter templates from the hierarchical clustering analysis. Left: UVB templates that were excluded due to emission line features. Left middle: UVB templates that were excluded because of low S/N or because they were only found in one spectrum. The numbers on the left and right sides of the figure indicate the number of spectra the features were found in in the clustering analysis. Right middle and right: Examples of excluded X-Shooter VIS templates from hierarchical clustering analysis.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: The results of WOC (DM, BCG+ICL; left) and ζ MHD (DM, BCG+ICL; right) for different galaxy clusters for different smoothing factors (upper panel), decentering (middle panel), and binning (lower panel). A smoothing factor of 17 is used for the decentering and binning tests. The labels are in the order of formation time (z  m/2), where cluster 1 formed early (dynamically relaxed) and cluster 6 formed late (dynamically young). Note that for spatially matched distributions, the WOC would be close to 1, and the MHD would be close to 0. The range of the MHD result is indefinite, i.e., the ζ-value is unbounded for the case of nonmatching distributions. We thus take the logarithm of ζ MHD, to allow for a qualitative visual comparison between the trends of the MHD and WOC methods. The MHD method results using the largest contour are plotted as solid lines, while those using all the contours are plotted as dashed faint lines.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: Overlapping area fractions as a function of brightest area. The results for different convolution factors for the dark matter vs. BCG+ICL of cluster 1 (upper panel), the dark matter vs. different components of cluster 1 (middle panel), and the dark matter vs. BCG+ICL of different galaxy clusters (lower panel) are plotted. For the x-axis (area of brightest pixels), the corresponding physical scales of the radial profiles of dark matter are marked together in the upper panel. Additionally, the pixel areas for 100 kpc and 200 kpc contour levels are marked as vertical gray dashed lines in the lower panel. The upturn at the largest area is an artifact of the image size and the zero values in the images, and is marked as the blue hatched region.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: The characteristics of the original WOC (upper panel), MHD (middle panel), and WOC M  (lower panel) methods when varying the parameters of the compared NFW mock images. The results of fixing the four parameters for the reference distribution (Map 1 in Table 2), and varying the concentration rate (first column), offset (second column), ellipticity (third column), and PA (fourth column) of the Map 2 results, are shown (the thick black lines). For each plot, when taking a different concentration (red line), offset (green line), ellipticity (blue line), and PA (magenta line), the values of the Map 2 cases are overplotted. The parameter sets of the mock images are summarized in Table 2.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: The intermediary steps used for measurements with the WOC (third row) and MHD (fourth and fifth rows) methods, for cluster 6 (third and fourth rows) and cluster 1 (fifth row). The raw data images of the dark matter and BCG+ICL of cluster 6 are plotted in the first and second rows, respectively. All of the panels have a box size of 1.5 × 1.5 h −2 Mpc2. For both methods, the distributions of the dark matter and BCG+ICL are marked with blue and orange colors, respectively. The three levels of the dark matter and BCG+ICL distributions are plotted in the left (first level), middle (second level), and right (third level) panels. In the MHD method, when there were several contours for one level (marked by the dotted line), the largest contour (the solid line) was selected to compare with the contour of the other component.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: Galaxy clusters simulated in the GRT simulations. Projected images in 2.5 × 2.5 h −2 Mpc2 boxes for dark matter (first column), all stellar particles (second column), member galaxies excluding the BCG (third column), and the BCG+ICL (fourth column) are shown. Throughout this work, the comparison of the spatial distribution between dark matter and galaxies is conducted using all member galaxies, including the BCG, but we show satellite galaxies without the BCG as an aid to visualizing the relative distributions of the galaxies and BCG+ICL. The mass growth histories of each cluster are plotted in the fifth column. The major merging events (with mass ratios smaller than 1:5) are marked as red triangles.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: The measuring process of the WOC method for cluster 1, simulated in GRT simulations. All panels have a box size of 1.5 × 1.5 h −2 Mpc2. The dark-matter distribution in cluster 1 (first row) was compared with all stellar particles (second row; cluster galaxies including BCG+ICL), member galaxies (third row; cluster galaxies including BCG), and BCG+ICL (fourth row). In the three lower panels, the distributions of dark matter and the other compared components are marked with blue and orange colors, respectively. We measured the overlap areas of the three levels, in the order from highest to lowest, as the first (left), second (middle), and third (right) levels, and gave them weights to calculate the WOC.
Paper: Comparison of Spatial Distributions of Intracluster Light and Dark Matter
Authors: Jaewon Yoo, Jongwan Ko, Cristiano G. Sabiu, Jihye Shin, Kyungwon Chun, Ho Seong Hwang, Juhan Kim, M. James Jee, Hyowon Kim, Rory Smith
Figure caption: WOC method idea. We measure the overlap areas of the contours between two distributions at various density threshold levels. We calculate the fraction of the overlapping area and give weight, using the signal strength, to quantify their overall similarity as a normalized number between 0 and 1. For further details, see Section 3.1.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Top: an  example 1D spectrum of a low-mass galaxy (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\approx 8.3)﹩) in the EGS field. The blue shows the coadded spectrum of all 1D extractions, and the green shows the continuum-subtracted spectrum, though the observed difference between the two is small, as the estimated continuum (orange line) is quite small for such a low-mass galaxy. The redshift routine searched the continuum-subtracted spectrum for significant residual flux peaks in order to identify emission lines. The error spectrum is shown in purple, generally only visible when coinciding with stronger skylines, which are more common at the redder wavelengths. The vertical dotted red lines show common strong skylines that were excluded from the emission-line detections. Vertical dashed black lines show common strong emission lines (e.g., [O III]4959,5007; Hβ; [O II]3727,3729). Green vertical dashed lines show the locations of weak emission lines that may serve as metallicity indicators ([Ne III] and [O III]4363), and dashed blue lines indicate typically weak helium lines. Magenta dashed lines indicate the locations of the Ca H and K absorption lines, typically only seen in higher-mass galaxies with stronger continua and older stellar populations. Middle:  an example spectrum for a high-mass galaxy (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\approx 10.4)﹩) in EGS that nonetheless exhibits some indicators of star formation, with detectable [O II]3727,3729 emission and Hβ and Hγ Balmer lines. This galaxy lies outside primary CANDELS photometric coverage, and so lacks some photometric and color information. Bottom: another massive galaxy (log(M⋆/M⊙ ) ≈ 10.5)) in EGS that is quiescent, with no visible Balmer emission. This galaxy’s redshift is determined via the Ca H and K absorption lines.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The four fields targeted in the various HALO7D observations, clockwise from top left: COSMOS, EGS, GOODS-South, GOODS-North. Black shaded regions indicate coverage from the CANDELS catalogs in these fields (Dahlen et al. 2013; Guo et al. 2013; Santini et al. 2015; Kocevski et al. 2017; Barro et al. 2019) with measured photometry and redshifts. The colored points indicate the locations of HALO7D target galaxies. We obtained successful redshift fits for points with colored outlines (gold or magenta), and were unable to measure redshifts in HALO7D spectra for the points with black outlines. HALO7D targets in the COSMOS and EGS fields included a number of galaxies outside the regular CANDELS coverage, as can be seen where the HALO7D targets do not overlap the black CANDELS region. We obtained photometry for these galaxies from the COSMOS/UltraVista (Muzzin et al. 2013) and EGS/IRAC (Barro et al. 2011a, 2011b) catalogs.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Overview of the HALO7D galaxies with redshift fits. The galaxies are sorted in ascending redshift from bottom to top. Note that the y-axis scale is not linear, as the sample is not uniformly distributed in redshift. The axis labels indicate a few example redshift locations to give a sense of this distribution. The brightness at each wavelength in each row is scaled to the flux of the DEIMOS spectrum.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: RGB images of example HALO7D galaxies matching the three categories of target described in Figure 2. The photometric bands used are F606W (blue), F814W/F850LP (green), and F160W (red), taken from CANDELS (Guo et al. 2013; Barro et al. 2019) and 3D-HST (Skelton et al. 2014). Each image has a diameter of 60 HST pixels, for a diameter of 3.″6. Dashed lines indicate the placement of spectroscopic slits.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Top: photometric redshifts z  p  (primarily from CANDELS, Dahlen et al. 2013; EGS/IRAC, Barro et al. 2011a, 2011b; and COSMOS/UltraVista, Muzzin et al. 2013) compared to the redshift from HALO7D spectra z  h7, colored by the stellar mass. Bottom: the difference in redshift between z  h7 and z  p , colored by the stellar mass. The solid black points show the median difference as a function of z  h7.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The redshift and stellar mass distribution of HALO7D redshift catalog. The black vertical dashed line demarcates the separation between the low-mass and high-mass samples at ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=9.5﹩. The points are colored by the number of significant features detected, counting the pair of Ca H and K absorption lines and the [O II]3727,3729 doublet each as a single feature. The top panel gives a histogram of the mass distribution of the overall sample with good redshifts, separated by the redshift fit quality, z  Q .
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Top panel: histogram of z  h7, redshifts from this work where there is a good fit with z > 0. Middle panel: other catalog spectroscopic redshifts z  s  compared to z  h7, colored according to the number of features detected; galaxies without spectroscopic redshifts from other catalogs are set to z  s  = 0, and galaxies without a good fit from HALO7D spectra are set to z  h7 = 0. Bottom: redshift difference between z  s  and z  h7, normalized by 1 + z  s .
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Each pair of panels gives the F606W AB magnitude histograms and success fractions for one of the four HALO7D fields. The top panels give magnitude histograms for the whole target sample (white), the sample with usable extracted spectra (red), and the sample with good redshift fits (blue). The bottom panels give the success fractions as a function of magnitude. The red dashed line is the fraction of usable spectra out of the target sample in a given magnitude bin. The solid blue line gives the fraction of spectra with good redshift fits out of the total target sample.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Each pair of panels gives the stellar mass histograms and success fractions for one of the four HALO7D fields. The top panels give mass histograms for the whole target sample (white), the sample with usable extracted spectra (red), and the sample with good redshift fits (blue). The bottom panels give the success fractions as a function of stellar mass. The red dashed line is the fraction of usable spectra out of the target sample in a given mass bin. The solid blue line gives the fraction of spectra with good redshift fits out of the total target sample.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The distribution of total exposure time in the coadded spectra, measured in hours. The histogram is broken down by the assigned z  Q  redshift quality. This demonstrates the benefits of the depth of the observations, as the lowest-quality flag, z  Q  = 0, is overrepresented among galaxies with low exposure times, and the highest-quality flags are overrepresented among the highest exposure times.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The emission-line flux distributions as a function of redshift, and colored by the stellar mass. The top row gives ionized oxygen emission lines, and the bottom row hydrogen Balmer series emission. Fluxes are not corrected for dust extinction or stellar absorption.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The absolute difference between the photometric redshift z  p  and the HALO7D redshift z  h7, plotted against (left) the F606W AB magnitude, (middle) the F160W AB magnitude, and (right) the stellar mass. Red points give the median absolute difference in bins of magnitude or mass, and blue points give the σ NMAD.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The distribution of z  h7 in each of the HALO7D fields.
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: The SFR (top panel) and sSFR (bottom panel) of the sample as function of the stellar mass. In the left column, the vertical dashed line separates the dwarf sample from the massive galaxy sample, and individual HALO7D galaxies are given by black points, with dwarf galaxies filled and massive galaxies empty. Purple diamonds give the median SFR/sSFR for each mass bin, with error bars giving the standard deviation in the bin. We compare this with star-forming CANDELS/3D-HST galaxies (Whitaker et al. 2014) at comparable redshifts (0.5 < z < 1.0 blue, 1.0 < z < 1.5 green). These curves are each separated into parts, representing SFR measurements from stacking analysis (dotted) and individual SFRs (solid line). In the lower-left panel, we also include relations from AEGIS (magenta; Noeske et al. 2007), DEEP2/3 (orange; Guo et al. 2016b), and FIGS (cyan; Pharo et al. 2020). In the right column, the HALO7D points are colored by Sérsic index n as determined in the CANDELS galaxy morphology catalogs from van der Wel et al. (2012).
Paper: The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations
Authors: John Pharo, Yicheng Guo, Guillermo Barro Calvo, Timothy Carleton, S. M. Faber, Puragra Guhathakurta, Susan A. Kassin, David C. Koo, Jack Lonergan, Teja Teppala, Weichen Wang, Hassen M. Yesuf, Fuyan Bian, Romeel Davé, John C. Forbes, Dusan Keres, Pablo Perez-Gonzalez, Alec Martin, A. J. Puleo, Lauryn Williams, Benjamin Winningham
Figure caption: Left: the distribution of Sérsic indices from van der Wel et al. (2012) for the low-mass (blue) and high-mass HALO7D samples. Right: the star formation rate residual Δlog sSFR vs. the radius residual Δlog r  e  for the dwarf galaxy sample, colored by Sérsic index n. The residuals are measured from the sSFR and size medians of the mass bins shown in Figure 14. A Spearman rank correlation test finds a correlation coefficient consistent with 0 and no significant correlation measure. The color range of n is restricted to best show possible variation among the predominantly low-n dwarf sample.