adsabs/AstroCLIMB huggingface dataset:
Paper: Examining the Potential for Methyl Halide Accumulation and Detectability in Possible Hycean-type Atmospheres
Authors: Michaela Leung, Shang-Min Tsai, Edward W. Schwieterman, Daniel Angerhausen, Janina Hansen
Figure caption: (a) Comparison of stellar surface spectra for both the Sun and GJ 436, used here as a stand-in for K2-18, an M2.8V star (top), and photochemical cross sections for CH3X gases and DMS (bottom). (b) Comparison of photolysis rates for CH3X gases for Earth-like biological production flux levels simulated using K2-18b parameters. (c) Comparison of mixing ratio profiles for 1D (dashed) and 2D (solid, shaded by longitude) simulations using Earth-like flux levels. Modest enhancements of CH3Cl are shown, with similar ratios of the other gases. The largest mixing ratio range is seen for CH3I, which shows some longitudinal dependency. (d) Mixing ratios similar to (c) for 50× Earth-like flux, around where fluxes become potentially spectrally detectable. Enhancements of 5–10× are seen for all gases compared to 1D results.
Paper: Examining the Potential for Methyl Halide Accumulation and Detectability in Possible Hycean-type Atmospheres
Authors: Michaela Leung, Shang-Min Tsai, Edward W. Schwieterman, Daniel Angerhausen, Janina Hansen
Figure caption: (a) Emission spectra of K2-18 b for various CH3X biological production flux levels using photochemical profiles as input. The largest feature can be seen at 10 μm, with smaller features appearing at 7 and 13.7 μm. (b) Distance distribution of warm sub-Neptunes and super-Earths around M- and FGK-type stars detectable with LIFE in the current baseline setup. For details on the exoplanet classification, see R. K. Kopparapu et al. (2018). The 5 pc distance assumed here is the typical distance for more than a dozen expected targets. (c) Detectability of various levels of CH3X (primarily CH3Cl) biological production fluxes in the emission spectrum of a “K2 18b-like” planet at 5 pc, after 24 hrs of observation with LIFE. Top: planetary emission for atmospheres with and without various levels of CH3Cl. The gray area represents the 1σ sensitivity; the gray error bars show an individual simulated observation. Bottom: statistical significance of the detected differences between atmospheric models with various levels of CH3X (see legend).
Paper: Examining the Potential for Methyl Halide Accumulation and Detectability in Possible Hycean-type Atmospheres
Authors: Michaela Leung, Shang-Min Tsai, Edward W. Schwieterman, Daniel Angerhausen, Janina Hansen
Figure caption: Top left: simulated observations using JWST NIRSpec PRISM instrument. Optimal detection for CH3X gases in 5 transits (3σ, 14 for 5σ) at the 4.0 μm CH3Cl feature, which does not have strong CH4 interference, as seen for other CH3Cl features in this spectral range (i.e., 3.3 μm). Error bars are shown for 5 transits. Top right: simulated observations using JWST MIRI-LRS instrument. Both features are more difficult to detect due to instrumental constraints, but detection is possible for the 10 μm band in tens of transits. For the “No Flux” scenario, C2H6 features are present near 3.3 μm, between 6 and 8 μm and beyond 12 μm, confounding the detection of methyl halide gases in these ranges. The presence of methyl halide gases at biological production levels appears to suppress C2H6 abundances; see Section 5 for further discussion. Concentrations of other gases such as CO and H2CO are also reduced when high levels of methyl radicals are introduced. Error bars shown are for 5 transits. Bottom: bar chart comparing number of transits necessary to detect each feature based on simulated noise for two confidence levels.
Paper: First-principles Measurement of Ion and Electron Energization in Collisionless Accretion Flows
Authors: Evgeny A. Gorbunov, Fabio Bacchini, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Different MRI-driven electron–ion turbulence properties. (a) and (b): particle energy distribution functions during the turbulence stage; (c): turbulent spectra for the poloidal magnetic field ﹩{B}_{{\rm{pol}}}\equiv \sqrt{{B}_{x}^{2}+{B}_{z}^{2}}﹩ and the toroidal magnetic field By, averaged over t = 10.5P0–12.5P0. Perpendicular wavenumbers are normalized by the initial relativistic electron skin depth ﹩{d}_{e,0}^{{\rm{R}}}﹩ (d): temporal evolution of the total 〈α〉-parameter (black line) and total stresses, normalized by the average total pressure 〈p〉. (e) and (f): Reynolds and anisotropic stresses for different species; (g) and (h): distribution of (p⊥/p∥, β∥) for (g) electrons and (h) ions at t = 10.5P0. The approximate firehose (p⊥,j/p∥,j > 1 − 2/β∥,j) and mirror instability (﹩{p}_{\perp ,j}/{p}_{\parallel ,j}\gt 1/2(1+\sqrt{1+4/{\beta }_{\parallel ,j}})﹩) thresholds are indicated in dashed–dotted and dashed lines, respectively.
Paper: First-principles Measurement of Ion and Electron Energization in Collisionless Accretion Flows
Authors: Evgeny A. Gorbunov, Fabio Bacchini, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: (a) The evolution of dimensionless parameters typically used for heating ratios in the simulation run; (b) Measured heating ratio evolution over time (blue line) vs. the heating ratios obtained from G. G. Howes (2010), V. Zhdankin et al. (2019), V. Zhdankin (2021), and Y. Kawazura et al. (2022), along with the heating ratio fitted with our formula, Equation (8).
Paper: First-principles Measurement of Ion and Electron Energization in Collisionless Accretion Flows
Authors: Evgeny A. Gorbunov, Fabio Bacchini, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Structure of the (a) Bx, (b) By, and (c) Bz magnetic-field components during the turbulent stage, at t = 12P0; (d) Energy evolution of magnetic-field components and kinetic energies of ions and electrons, normalized by the total energy at t = 0. The dashed line depicts a moment after which the RR force was turned off.
Paper: First-principles Measurement of Ion and Electron Energization in Collisionless Accretion Flows
Authors: Evgeny A. Gorbunov, Fabio Bacchini, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Scatterplot of Qi/Qe vs. 〈ρi〉/〈ρe〉. The later times of the simulation are shown in lighter colors. The heating ratio proposed in this work is shown by the black dashed line, and the red solid line represents V. Zhdankin (2021) formula for the heating ratio with solenoidal driving.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: Upper: the background is the 850 μm dust emission with NH3 contours overlaid. The orbital model from J. M. D. Kruijssen et al. (2015) is shown as dashed lines (Streams 1, 2, 3, and 4; see the center plot for the color legend) and our proposed streams are shown as solid lines (Streams A, B, and C). Center: the PV plot of our three streams and the four from J. M. D. Kruijssen et al. (2015). The mean velocity of the clumps is plotted with the error bars reflecting the standard deviation. A best-fit line is plotted through each of our three streams. Lower: an artist’s impression of the CMZ flows as seen from just out of the Galactic plane “above” us. This shows the various flows and interprets the velocity structures we see. Our Streams A, B, and C are shown with arrows denoting the flow of material. White lines represent the magnetic fields, which are aligned with the streams except in areas of active star formation, such as in Stream B, where the field lines are now perpendicular to the stream. Question marks denote the areas that are not addressed in this Letter.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: Upper panel: the identified clumps from the clump-finding algorithm. Each clump is shown as a different color. Contours are of the 850 μm Stokes I emission from this work. Contour levels are 200, 400, 800, 1500, 2500, and 5000 mJy beam−1. Lower panel: each of the clumps from the upper figure is represented by colored circles and crosses positioned at the centroids of the clumps. The colors represent the mean peak velocity component of that clump (see Appendix C). Circles denote the points used to fit the final splines while crosses denote those omitted. The contours are the same as the upper panel. The gold stream in the lower left quadrant was not used as we have limited emission in that region.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: CDFs of our observations, random distribution, and 3D alignment models. Both figures show 3D alignment models as black (100% preferentially parallel and 100% preferentially perpendicular) and gray (50% preferentially parallel, 50% preferentially perpendicular model) dashed lines with the random distribution CDF in solid black. Preferentially parallel is Δθ3D < 30° and preferentially perpendicular is Δθ3D > 60°. The model CDFs are of the projected 2D angle difference (see the text for details). Left: the observed CDF of all data points is plotted in red. It shows a clear agreement with the model CDF having a majority of preferentially parallel alignment, although it tends toward the 50% parallel, 50% perpendicular CDF around ∣Δθ∣ ≈ 35°. The p-value of the one-sample KS test is 0.007, which indicates it is not similar to a random distribution. Right: the observed CDF of the eastern half of the CMZ (Stream B) is plotted in blue and of the western half (Streams A and C) in red. The western half shows a clear agreement with the parallel alignment CDF, and a KS test gives a p-value of 0.002 indicating it is nonrandom. The eastern half initially shows good agreement with the 50% parallel, 50% perpendicular distribution but becomes indistinguishable from the random distribution at ∣Δθ∣ ≳ 40°. Comparing the blue CDF to the 50/50 model and random CDF yields p-values of 0.35 and 0.66, respectively, meaning the eastern distribution could be drawn from either.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: In the first three plots, Sgr A* is marked with a star and in all plots a contour value of 200 mJy beam−1 is plotted. Upper: 850 μm Stokes I continuum. The main molecular clouds are labeled. Upper middle: 850 μm Stokes Q continuum with the color map spanning ±10 δQrms, the rms noise in Stokes Q. Lower middle: 850 μm Stokes U continuum with the color map spanning ±10 δUrms, the rms noise in Stokes U. Lower: 850 μm Stokes I continuum with B-field vectors overlaid. The vectors are all uniform in length, binned to 14″ and follow the SNR cuts stated in Section 3.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: The lower plot shows the number of velocity features fit per pixel with contours matching Figure B1 overlaid. An inset is shown of a region and four pixels are chosen, which show one, two, three, and four component fits. For plots (a) and (c), fits 1 and 2 and 2 and 3, respectively, are fit with double Gaussians, while all the rest are single Gaussians. A red dashed line shows the total Gaussian and the gray spectra show the residual spectra once all the Gaussian fits have been removed. The centroid velocity of the Gaussian fit with highest amplitude was used in each pixel.
Paper: The Miscibility of Hydrogen and Water in Planetary Atmospheres and Interiors
Authors: Akash Gupta, Lars Stixrude, Hilke E. Schlichting
Figure caption: Simulation snapshots of the two-phase system at 1000 K and 10 GPa. Oxygen atoms are denoted by red spheres and hydrogen atoms by blue spheres. The Gibbs dividing surface is illustrated by the green–blue surface, separating H-rich from H-poor phases (A. P. Willard & D. Chandler 2010). The initial condition is on the left and an equilibrated snapshot at 200 ps in the center. The rightmost panel shows the spatial variation of the H2 concentration x of the equilibrated portion of the simulation over a 5 ps interval, and the dashed line results from a fit to Equation (A1).
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: Background image is the 850 μm SCUBA-2 map from H. Parsons et al. (2018). Overlaid are 6﹩^{\prime} \rm{}\,\rm{}\,﹩ diameter circles showing the pointings observed toward the CMZ. The green solid circles are the BISTRO-3 fields. The red solid circles are the three fields observed as part of M17AP074. The cyan dashed circles are those fields observed as part of M20AP023 (X. Lu et al. 2024).
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: A plot showing the identified structures using astrodendro. The background image is the 850 μm dust emission map. The black contour shows the 200 mJy beam−1 base of the astrodendro structure. The colored contours correspond to the branch and leaf index. The magnetic field vectors used to calculate circular means within each of the structures are plotted as white, uniform length vectors.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: A(Li) vs. age of RC stars. The projection of the evolution lines on the timeline is the timescale of the meridional circulation. At the start of the core He burning, vin, RC is, respectively, 1.0, 10, 30, 50, and 100 km s−1.
Paper: The Critical Role of Dark Matter Halos in Driving Star Formation 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Luis C. Ho, Alvio Renzini, Yong Shi, Emanuele Daddi, Dingyi Zhao, Chengpeng Zhang, Zeyu Gao, Di Li, Cheqiu Lyu, Filippo Mannucci, Roberto Maiolino, Tao Wang, Feng Yuan
Figure caption: Distribution of galaxies on the SFE–sSFR plane. The dots show the location of central spiral galaxies in the ALFALFA-SDSS matched sample on the SFEH I–sSFR plane, with the grayscale representing the M*. The purple diagonal lines indicate four different values of constant μH I of 1%, 10%, 100% and 10. The gray thick line indicates the best-fitted ﹩{\mathrm{SFE}}_{{{\rm{H}}}_{2}}﹩–sSFR relation found in J. Dou et al. (2021a), which is called the FFR of molecular gas. The background color represents the value of log (﹩{M}_{{{\rm{H}}}_{2}}﹩/MH I) estimated from the FFR.
Paper: The Critical Role of Dark Matter Halos in Driving Star Formation 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Luis C. Ho, Alvio Renzini, Yong Shi, Emanuele Daddi, Dingyi Zhao, Chengpeng Zhang, Zeyu Gao, Di Li, Cheqiu Lyu, Filippo Mannucci, Roberto Maiolino, Tao Wang, Feng Yuan
Figure caption: The SFE–Mhalo relation (left panels) and (﹩{M}_{{{\rm{H}}}_{2}}﹩/MH I)–Mhalo relation (right panels) for central spirals in the ALFALFA-SDSS matched sample. Level contours represent the number density of galaxies, with values normalized. Left: blue contours show the SFEH I–Mhalo relation for star-forming galaxies, while red contours represent passive galaxies. In the upper left panel, star-forming galaxies are defined by log sSFR  >  −2 Gyr−1, and red ones are those with log sSFR  <  −2 Gyr−1. In the lower left panel, a stricter criterion is applied: star-forming galaxies are defined by log sSFR  >  −1 Gyr−1 and passive galaxies by log sSFR  <  −2.5 Gyr−1. The horizontal dashed line indicates the molecular gas FFR for the SFMS galaxies. Right: the (﹩{M}_{{{\rm{H}}}_{2}}﹩/MH I)–Mhalo relation is calculated using the molecular gas FFR. The same definitions for star-forming and passive galaxies are applied in the right panels as in the corresponding left panels. The horizontal dashed line indicates the position where the H I depletion timescale is equal to that of H2.
Paper: The Critical Role of Dark Matter Halos in Driving Star Formation 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Luis C. Ho, Alvio Renzini, Yong Shi, Emanuele Daddi, Dingyi Zhao, Chengpeng Zhang, Zeyu Gao, Di Li, Cheqiu Lyu, Filippo Mannucci, Roberto Maiolino, Tao Wang, Feng Yuan
Figure caption: Upper: the average disk radius (log Rdisk) on the SFEH I–Mhalo plane (upper left panel) and (﹩{M}_{{{\rm{H}}}_{2}}﹩/MH I)–Mhalo plane (upper right panel) for central spirals in the ALFALFA-SDSS matched sample. Lower: the average log SFEH I (lower left panel) and log (M﹩{}_{{{\rm{H}}}_{2}}﹩/MH I) (lower right panel) on the Rdisk–Mhalo plane. All panels are obtained by using a moving box of size 0.5 dex in both the x-axis and y-axis.
Paper: Discovery of a Low-mass Strong-lens System in SMACS J0723.3−7327
Authors: Limeng Deng, Yiping Shu, Lei Wang, Guoliang Li, Gabriel Bartosch Caminha, Jiang Dong, Zizhao He, Han Qu, Ruibiao Luo
Figure caption: Color composite image of SMACS J0723 generated from JWST NIRCam data in six filters (F090W, F150W, F200W, F277W, F356W, and F444W). The inset figure provides an enlarged view of the strong-lens system studied in this work.
Paper: Upper Limits on the Mass of Cool Gas in the Circumgalactic Medium of Dwarf Galaxies
Authors: Yakov Faerman, Yong Zheng, 永 郑, Benjamin D. Oppenheimer
Figure caption: Cool CGM mass vs. halo mass. The shaded bands around our upper limits shows the uncertainties due to unknown gas metallicity and redshift range (vertical and diagonal hatching, respectively). Horizontal error bars for our results indicate the halo mass bin widths, and for all other results the range of halo masses in each sample. Dashed lines show fixed fractions of the halo cosmological baryon mass budget, ﹩{M}_{{\rm{b,cosm}}}=\frac{{{\rm{\Omega }}}_{b}}{{{\rm{\Omega }}}_{m}}{M}_{{\rm{200m}}}﹩ (see Sections 2.4 and 3.4).
Paper: Upper Limits on the Mass of Cool Gas in the Circumgalactic Medium of Dwarf Galaxies
Authors: Yakov Faerman, Yong Zheng, 永 郑, Benjamin D. Oppenheimer
Figure caption: Our models fitted to the H I column densities measured in absorption, after binning the data in halo mass. Top: comparison to observations. Markers: observed H I column densities (full and empty markers show measurements and limits, respectively), dotted curves are power-law fits to the column density profile to guide the eye (upper limits are ignored for this fitting), and solid black curves are our models. Dashed curves show the model total hydrogen columns (scaled down by a factor of 103) for the volume-filling (fV = 1) scenario. Bottom: gas thermal properties—density (left panel), temperature (middle), and pressure (right). The blue, black, and red curves correspond to the halo mass bins, from low to high, respectively. Solid and dotted curves are for the nominal and clumpy models, respectively (see text in Section 2.4 and Table 1 for model description and parameters).
Paper: Upper Limits on the Mass of Cool Gas in the Circumgalactic Medium of Dwarf Galaxies
Authors: Yakov Faerman, Yong Zheng, 永 郑, Benjamin D. Oppenheimer
Figure caption: The H I column density for a path length of 150 kpc as a function of gas density and temperature (solid contours). The thick dotted curve shows the gas equilibrium temperature, and the thin dashed lines show the gas thermal pressure. The shaded regions show diffuse gas in different regimes. The cool CGM (shaded blue) is addressed in Section 2, and can form fairly large column densities, mainly as a function of gas density (and volume filling fraction). At low densities, the IGM (shaded gray) has low H I ion fractions, but with a path length of up to 1 Mpc can form NHI ≲ 1014 cm−2. The warm/hot CGM (shaded red) can span a wide range of temperatures and densities, depending on its formation mechanism (winds vs. accretion). Column densities comparable to the observed values (≈1014 cm−2) can form at relatively low temperatures (T < 3 × 105 K) or higher densities and pressures (see text in Section 3.5).
Paper: Upper Limits on the Mass of Cool Gas in the Circumgalactic Medium of Dwarf Galaxies
Authors: Yakov Faerman, Yong Zheng, 永 郑, Benjamin D. Oppenheimer
Figure caption: The effect of the volume filling fraction on the gas properties for a given H I column density profile (and fixed density slope, an). The three models have fV between unity (solid black) and 0.01 (dotted red) and the gas total mass varies to produce the same H I column density profile (right panel), roughly following the measured column densities (markers). Volume-filling gas (solid black curve) has lower volume densities (left panel) and higher temperatures (middle) (see text in Section 2.3).