adsabs/AstroCLIMB huggingface dataset:
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Terms in the integrated angular momentum conservation Equation (25) for MHD-T in units of ﹩{\dot{M}}_{\mathrm{Edd}}﹩. The terms are averaged over the last 2 days of the simulation in azimuth and 10° from the midplane.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Mass-weighted eccentricity averaged within 10° from the midplane, over the azimuth, and over the last 2 days of the simulation.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Left: plot of energy losses in detector A1 vs. the sum of the energy losses in the detectors in which the particles come to rest for a sample of events entering the A-end of HET 2 for the period 2013/1–2021/365. As described in the text, this combination of energy losses is the basis for calculating the M1 estimate of the particle mass. The solid line separates the charge assignment into Z = 1 (below) and Z = 2 (above). The curves show the expected positions of energy loss pairs from the isotopes 1H (red), 2H (blue), 3H (cyan), 3He (magenta), and 4He (yellow) at an incidence angle of 13° for appropriate ranges of incident energies. Right: similar to left panel, except the plot is for energy losses from A2 vs. the sum in the following detectors. This combination of energy losses forms the basis of the M2 mass estimate of each particle.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Average of the two mass estimates for each particle identified as Z = 5, B, vs. total energy deposited in active layers of the detectors. The data are from the V1 HET 2 telescope, B end in low-gain mode. The curved lines are expected tracks for 10B (bottom) and 11B (upper) particles incident at an a average angle to the normal. The vertical lines represent energy bin edges as described in the text.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Cross section of a HET telescope (adapted from W. R. Cook 1981). The detectors and method of analysis of the energy losses in them are described in the text. Window A is a covering over the A-end telescope aperture consisting of a sheet of 1/4 mil aluminized mylar and a thinned-out section of thermal blanket material, amounting to 1/2 mil aluminized mylar plus 2 mils Sheldahl black-coated Kapton. Window B is similar, except the 1/4 mil aluminized mylar sheet is replaced by a 1 mil aluminized mylar sheet.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Plots and tables depicting the method for accounting for background in energy bins A, B, and C for 2H particles incident on window A of the A-end of HET 2. The method is described in the text.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Counts (in red) and net counts (in blue) vs. circle radius for energy bin A of 2H particles entering the A-end of HET 2. The blue curves represent the results for 15 different starting radii of the initial circle. The selected value for net counts is 248, which is in the approximate center of the plateau region.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: Methodology of deriving half-mass radii. Panels (A) and (B): measured SBP (black), convolved model from GALFIT (orange), and deconvolved model (dark blue) in two photometric bands (F227W and F444W, respectively). The residual between the flux from the original cutout and the convolved model is added to the deconvolved model (bright blue). This is considered the total flux. The lower panels display in red the magnitude of the residual correction to be small compared to the total flux. Panel (C): radial color profile derived from the total flux in F277W (A) and F444W (B). Panel (D): derived radial M*/LF444W profile using the color–M*/LF444W relation derived in Section 3.2. Panel (E): radial luminosity profile derived from the total flux measured in F444W. Panel (F): radial mass profile derived from multiplying the radial M*/LF444W profile (D) with the luminosity profile (E). Panel (G): curve of growth for mass (bright green) and total flux in F444W (dark green) with half-light and half-mass radii (dashed lines). The uncertainties of the half-mass radii are determined with Monte Carlo simulations.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: Left panel: star-forming (gray), old quiescent (red), and young quiescent (blue) galaxies in PRIMER. Since the most massive galaxies drive the rest-frame optical size difference, we select only galaxies that have masses greater than log(M*/M⊙) > 10 (black dashed line). The galaxies in this work are the blue and red symbols above this line. Right panel: selection of quiescent galaxies (only log(M*/M⊙) > 10 sample depicted) in the (U − V) vs. (V − J). The black solid line indicates the selection of K. E. Whitaker et al. (2013). The dotted line divides the sample into recently quenched (blue) and older (red) quiescent galaxies.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: Left panel: evolution of half-light radii measured at F150W of young (blue) and old (red) quiescent galaxies. Right panel: evolution of half-mass radii. Both populations grow in both light-weighted and mass-weighted sizes toward lower redshift, with no significant difference. In both panels, the dotted lines depict the logarithmic fits to the respective data whereas the error bars depict the standard error in the mean.
Paper: The Evolution of Half-mass Radii and Color Gradients for Young and Old Quiescent Galaxies at 0.5 < z < 3 with JWST/PRIMER
Authors: Maike Clausen, Ivelina G. Momcheva, Katherine E. Whitaker, Sam E. Cutler, Rachel S. Bezanson, James S. Dunlop, Norman A. Grogin, Anton M. Koekemoer, Derek J. McLeod, Ross J. McLure, Tim B. Miller, Erica J. Nelson, Arjen van der Wel, David A. Wake, Stijn Wuyts
Figure caption: M*/LF444W dependence on redshift. Data points are color-coded by the classification of a galaxy as young quiescent (blue) or old quiescent (red). The fit parameters for each redshift bin are listed in Table 1.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Energy spectra of the electrons, positrons, and protons downstream of the shock (400 c/ωpe ≤ x ≤ 800 c/ωpe) at ﹩t=1.72\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩ in the simulation with 64 particles per cell per species on a smaller spatial scale (4096 c/ωpe × 64 c/ωpe). The thermal distribution with a temperature of T = 5mec2/kB (dotted line) is also illustrated.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Spectral distribution of the polarization angle χ(k) in k space for the magnetic field in the downstream (1000 c/ωpe ≤ x ≤ 3300 c/ωpe) of the shock at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Energy spectra of the electrons, positrons, and protons in the downstream regions of the shock, i.e., 0 c/ωpe − 800 c/ωpe (dashed line), 800 c/ωpe − 1600 c/ωpe (solid line), 1600 c/ωpe − 2400 c/ωpe (dashed–dotted line), and 2400 c/ωpe − 3200 c/ωpe (dotted line) at ﹩t=6.25\times 1{0}^{3}{\omega }_{{\rm{pe}}}^{-1}﹩.
Paper: Kinetic Simulations of Particle Acceleration in Relativistic Perpendicular Electron–Positron Shocks with Proton Admixture
Authors: Huan Yu, Qi Xia, Jun Fang
Figure caption: Energy spectra of the positrons in the downstream region of the shock (200 c/ωpe − 800 c/ωpe) at ﹩t=2969\,{\omega }_{{\rm{pe}}}^{-1}﹩ (dashed line), ﹩4062\,{\omega }_{{\rm{pe}}}^{-1}﹩ (solid line), ﹩5000\,{\omega }_{{\rm{pe}}}^{-1}﹩ (dashed–dotted line), and ﹩6250\,{\omega }_{{\rm{pe}}}^{-1}﹩, respectively.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: The best-fit cases for four epochs of observation by Spitzer through IRAC imaging (solid black circles) and IRS spectroscopy. For day 125, we combined the optical data from CSP-I with the Spitzer spectrum. The epochs of day 125 and day 272 (+IRAC day 252) were fit using a blackbody (in dotted, purple line) for the optical component, along with a cool IR component (dashed, red line) from dust (sum of the two components given in blue). For epoch 629 (+IRAC day 634) and epoch 806 (+IRAC day 830), we assumed a combination of hot (in green) and cool IR (red) components. We suggest that the cool IR component for all the cases originates from some pre-existing dust in the circumstellar matter, which was formed in the winds of the progenitor before the explosion. The hot IR component is attributed to emission from newly formed dust in the ejecta. See Table 4 for the fitting parameters and Section 7 for a detailed description of the scenario.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: A summary of the location, composition, and mass of dust in SN 2005af two decades after the explosion is presented in a schematic diagram (see Sections 7 and 8 for details). The inner O/Mg/Si shell, marked in brown, is where silicate dust is formed. The He/C shell, marked in orange, is the site for amorphous carbon dust formation. The dusty region of the CSM, hosting the surviving pre-explosion dust, is marked in yellow.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: The best-fit model is presented for mid-IR fluxes (data given in Table 3) of SN 2005af obtained through JWST/MIRI, 6826 days post-explosion. We find that, at this epoch, dust is predominantly C-rich in composition. See Section 7.6 and Table 4 for the description.
Paper: Two Decades of Dust Evolution in SN 2005af through JWST, Spitzer, and Chemical Modeling
Authors: Arkaprabha Sarangi, Szanna Zsíros, Tamás Szalai, Laureano Martinez, Melissa Shahbandeh, Ori D. Fox, Schuyler D. Van Dyk, Alexei V. Filippenko, Melina Cecilia Bersten, Ilse De Looze, Chris Ashall, Tea Temim, Jacob E. Jencson, Armin Rest, Dan Milisavljevic, Luc Dessart, Eli Dwek, Nathan Smith, Samaporn Tinyanont, Thomas G. Brink, WeiKang Zheng, Geoffrey C. Clayton, Jennifer Andrews
Figure caption: JWST/MIRI composite image of SN 2005af, taken on 2023 July 21, which is 6826 days post-explosion. The white tick marks show the position of the supernova.
Paper: Open Cluster Study Using Gaia. I. Membership and Cluster Properties
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Comparison of cluster properties we estimate with those found in selected past studies (CG20; M. Netopil et al. 2016; D. Bossini et al. 2019; W. S. Dias et al. 2021; E. L. Hunt & S. Reffert 2023). Cluster names are shown along the horizontal axis. Orange dots, red triangles, violet “+,” black triangles, and green triangles represent values from CG20, D. Bossini et al. (2019), HUNT23, W. S. Dias et al. (2021), and M. Netopil et al. (2016), respectively. From small to large, the increasing size of the green triangles signifies [Fe/H] estimated using photometry, low-resolution spectroscopy, and high-resolution spectroscopy. Blue violins and horizontal lines denote the posterior distributions and the median, 5th percentile, and 95th percentile from our Bayesian parameter estimation.
Paper: Open Cluster Study Using Gaia. I. Membership and Cluster Properties
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Two-dimensional sections of μRA, μdec, and π of all sources (dots) within rproj/pc = 20 for example clusters representing three different levels of overlap with field stars and hence difficulty in identification. The cluster NGC 2632 (top) is well separated from the field stars and can be easily identified in all astrometric planes. For NGC 1039 (middle), the cluster has a higher overlap with the field stars. It is still identifiable in the planes involving π, but not easily identifiable without it. IC 4651 (bottom) has a very high degree of overlap with the field and it is not easy to identify separately from the field stars in any of the astrometric planes.
Paper: Open Cluster Study Using Gaia. I. Membership and Cluster Properties
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Same as Figure 9 but showing convergence of the posterior distributions at different stages of Bayesian parameter estimation for our example cluster NGC 2287. Black (red) shows the posterior distributions using walker positions between 40,000 and 50,000 (50,000 and 60,000) step counts. Clearly the distributions show excellent agreement indicating that our MCMC chains have sufficiently converged.
Paper: The Gamma-Ray Emission from Radio Galaxies and Their Contribution to the Isotropic Gamma-Ray Background
Authors: Antonio Circiello, Alex McDaniel, Mattia Di Mauro, Christopher Karwin, Nikita S. Khatiya, Marco Ajello, Fiorenza Donato, Dieter Hartmann, Andrew W. Strong
Figure caption: Source-count distribution for the RGs. The data points are obtained using the efficiency and flux values of the sources of the detected sample that are in L. Marcotulli et al. (2020). The dashed red line is obtained by fitting the source-count distribution obtained assuming the best-fit parameters for the Lγ–LC,5GHz correlation from the detected RGs to the data points. The green band is obtained fixing the parameter k = 1, and variating the α and β parameters from the detected RGs, within their 1σ uncertainties.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Left: the core-scale (∼10,000 au) magnetic field orientations around HH 211 observed with JCMT. The gray scale shows the 850 μm intensity, with contour levels at 0.09, 0.3, and 0.8 Jy beam−1. The beam size of the JCMT observation is shown by the blue circle in the bottom left of the panel. The cross indicates the position of the central protostar (C.-F. Lee et al. 2018b, 2023). Right: a zoomed-in view of the left panel overlaid with ALMA Band 3 observations. The green lines represent 0.025 and 0.08 mJy beam−1 levels in the ALMA Band 3 observations with a robust parameter of 2.0. Spatial scale bars are shown in the top-right corner of both panels.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Dust continuum around HH 211 in Band 3 (left) and Band 6 (right) with a robust parameter of 0.5. The contour levels are 5, 10, 20, 50, 100, 200, and 500 times the rms noise levels, where the rms noises are 0.009 mJy beam−1 in Band 3 and 0.045 mJy beam−1 in Band 6. The synthesized beam sizes are shown in the bottom left of both panels. The red and blue arrows indicate the redshifted and blueshifted jet directions, respectively (M. J. McCaughrean et al. 1994). Spatial scale bars are shown in the top-right corners of both panels.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Dust continuum around HH 211 in ALMA Band 3 (97.5 GHz) with a robust parameter of 2.0. The synthesized beam and spatial scale bar are shown in the bottom-left and bottom-right corners, respectively. The central coordinates are R.A. = 03h43m56﹩\mathop{.}\limits^{{\rm{s}}}﹩800, decl. = +32°00′50.00″.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Physical properties of the gas within the halos of the M+M sample. Particle data are binned by stellar mass and plotted in the corresponding column (labeled on the top of each column) according to the following ranges: M* = 106.0−7.5 M⊙ (left column), M* = 107.5−8.5 M⊙ (center column), and M* = 108.5−9.5 M⊙ (right column). Top row: gas density vs. temperature diagram (T(ngas)) for only CGM particles (0.15–1.0R200c). The orange dashed line represents the median virial temperature, while the black lines represent isobaric lines of 10−17, 10−16, and 10−15 Ba in thermal gas pressure. Also included are radial profiles as a function of normalized radial distance, r/R200c, of gas temperature (T(r), upper-middle row), gas density (ngas(r), lower-middle row), and gas metallicity relative to solar (Z(r)/Z⊙, bottom row). The gray shaded region denotes what is removed from the halo as the “disk,” i.e., not included in the phase diagram. The color bar for all panels shows the mass-weighted probability density. The definitions for the various CGM temperature ranges are also shown in the T(r) panels. Median conditions of the CGM (r = 0.15–1.0R200c) are shown in each panel; we find that with decreasing mass, typical CGM conditions become more diffuse, cooler, and less metal-enriched. Median CGM density and temperatures for each galaxy in the M+M sample can be found in Table 3.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Ion fractions (fion) for H I  (salmon) and a representative low ion (C II, light green), intermediate ion (C IV, dark green), and high ion (O VI, purple) as a function of radial separation from the galaxy. For each ion, we show the median values for the same three virial mass bins as Figure 10, with solid, dashed–dotted, and dashed lines representing high-, intermediate-, and low-mass galaxies. We see little variation in the shape of fion radial profiles with halo mass. However, with increasing distance from a galaxy, low ions (H I  and C II) become increasingly less abundant and intermediate/high ions (C IV  and O VI) become the dominant ionization stages; this is due to the radial dependence of the CGM’s physical properties (Figure 10).
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: CGM UV-observable (at z = 0–0.3) budgets for the M+M  sample. Left panel: median masses of individual ions with UV-detectable transitions in the CGM. Center panel: median total UV-observable mass in the CGM (Mele.,UV), defined as the summed mass of ions with UV-detectable transitions (explicitly written in the legend and plotted in the left panel). Right panel: corresponding UV-observable fraction/ionization correction (fele.,UV), defined as the UV-observable mass divided by total element mass (fele.,UV = Mele.,UV/Mele.). Each panel shows results for three stellar mass bins (log M*/M⊙ = 6.0–7.5, 7.5–8.5, and 8.5–9.5), and the error bars show the 16th–84th percentile range; markers are horizontally offset for clarity. Elements are represented as follows: hydrogen (salmon circles), silicon (blue squares), carbon (green triangles), and oxygen (purple diamonds). In the left panel, markers are rotated to distinguish between ions.
Paper: Marvelous Metals: Surveying the Circumgalactic Medium of Simulated Dwarf Galaxies
Authors: Daniel R. Piacitelli, Alyson M. Brooks, Charlotte Christensen, N. Nicole Sanchez, Yakov Faerman, Sijing Shen, Akaxia Cruz, Ben Keller, Thomas R. Quinn, James Wadsley
Figure caption: Fraction of CGM mass in the cool phase, T = 103.8–104.5 K (blue hexagons) and the warm phase, T = 104.5–105.5 K (orange triangles) as a function of stellar mass. For a given halo, the two phases are connected by a gray dashed line, and the dominant phase is bolded. The solid line and shaded region show the median CGM percent value and 16th–84th percentile range for the cool or warm phases in a bin size of 0.6 dex, plotted at the center of the bin. The dashed black line represents the sum of the median phase fractions, indicating the typical fraction of CGM mass not residing in the cool or warm gas phases (i.e., the cold or hot phases). The majority of CGM mass (>95%) resides in the cool and warm phases, and, for logM*/M⊙ > 7 galaxies, the cool and warm CGM comprise a median value of 30% and 70% of CGM mass, respectively. Table 3 provides the mass in the cool and warm CGM phase for each galaxy in the M+M sample.