adsabs/AstroCLIMB huggingface dataset:
Paper: Multiwavelength Observations of the Apparently Nonrepeating FRB 20250316A
Authors: Ye Li, Hui Sun, Lei Qian, Dong-Yue Li, Yan-Long Hua, Li-Ping Xin, Cheng-Kui Li, Yi-Han Wang, Jia-Rui Niu, Tian-Rui Sun, Zhu-Heng Yao, Jin-Jun Geng, Chi-Chuan Jin, Nanda Rea, Yuan Liu, Zhi-Chen Pan, Tao An, Vadim Burwitz, Zhi-Ming Cai, Jin-Huang Cao, Yong Chen, Hua-Qing Cheng, Wei-Wei Cui, Hua Feng, Peter Friedrich, Da-Wei Han, Jing-Wei Hu, Lei Hu, Yu-Xiang Huang, Shu-Mei Jia, Ji-An Jiang, Bin Li, Feng Li, Ming Liang, Yi-Fang Liang, Hao Liu, He-Yang Liu, Hua-Qiu Liu, Norbert Meidinger, Hai-Wu Pan, Arne Rau, Xin-Wen Shu, Chun Sun, Lian Tao, Jin-Long Tang, Zhen Wan, Hai-Ren Wang, Jian Wang, Jing Wang, Yun-Fei Xu, Yongquan Xue, Xuan Yang, Da-Zhi Yao, Yuhan Yao, Wen Zhao, Xiao-Fan Zhao, Hong-Fei Zhang, Jia-Heng Zhang, Juan Zhang, Mo Zhang, Song-Bo Zhang, Wen-Da Zhang, Xiao-Ling Zhang, Yong-He Zhang, Yong-Kun Zhang, Xian-Zhong Zheng, Yu-Hao Zhu, Ying-Xi Zuo, Sheng-Li Sun, Jian-Yan Wei, Wei-Wei Zhu, Peng Jiang, Weimin Yuan, Xue-Feng Wu, Bing Zhang
Figure caption: Left: upper limits on the persistent X-ray luminosity from the Chandra observation at the position of FRB 20250316A (red arrow). For comparison, the observed luminosities of LMXBs, HMXBs, magnetars, and ULXs are overplotted. Upper limits on the persistent X-ray luminosity from other one-off FRBs (filled arrows) and a repeating FRB (open arrow) are also shown. Right panel: multiwavelength constraints of FRB 20250316A. The predictions of afterglow models (Y. Wang et al. 2026) with different parameters are overplotted. Blue and orange lines are for X-ray and optical, respectively.
Paper: Multiwavelength Observations of the Apparently Nonrepeating FRB 20250316A
Authors: Ye Li, Hui Sun, Lei Qian, Dong-Yue Li, Yan-Long Hua, Li-Ping Xin, Cheng-Kui Li, Yi-Han Wang, Jia-Rui Niu, Tian-Rui Sun, Zhu-Heng Yao, Jin-Jun Geng, Chi-Chuan Jin, Nanda Rea, Yuan Liu, Zhi-Chen Pan, Tao An, Vadim Burwitz, Zhi-Ming Cai, Jin-Huang Cao, Yong Chen, Hua-Qing Cheng, Wei-Wei Cui, Hua Feng, Peter Friedrich, Da-Wei Han, Jing-Wei Hu, Lei Hu, Yu-Xiang Huang, Shu-Mei Jia, Ji-An Jiang, Bin Li, Feng Li, Ming Liang, Yi-Fang Liang, Hao Liu, He-Yang Liu, Hua-Qiu Liu, Norbert Meidinger, Hai-Wu Pan, Arne Rau, Xin-Wen Shu, Chun Sun, Lian Tao, Jin-Long Tang, Zhen Wan, Hai-Ren Wang, Jian Wang, Jing Wang, Yun-Fei Xu, Yongquan Xue, Xuan Yang, Da-Zhi Yao, Yuhan Yao, Wen Zhao, Xiao-Fan Zhao, Hong-Fei Zhang, Jia-Heng Zhang, Juan Zhang, Mo Zhang, Song-Bo Zhang, Wen-Da Zhang, Xiao-Ling Zhang, Yong-He Zhang, Yong-Kun Zhang, Xian-Zhong Zheng, Yu-Hao Zhu, Ying-Xi Zuo, Sheng-Li Sun, Jian-Yan Wei, Wei-Wei Zhu, Peng Jiang, Weimin Yuan, Xue-Feng Wu, Bing Zhang
Figure caption: Left: CHIME FRB rate and the FAST 3σ upper limit compared with the spectral energy functions of repeating FRBs. A typical power law with a slope of −1.5 is plotted as a red solid line. The blue lines present the spectral energy functions of repeating FRBs, scaled to match the rate of FRB 20250316A at its spectral energy. Right: the FRB rate (>5 Jy ms) of FRB 20250316A estimated with multiple telescopes, assuming energy function slopes of −1.5 (red region) and −1.0 (gray region), compared with the CHIME-detected FRB rate (blue histogram).
Paper: 3D Modeling of Moist Convective Inhibition in Idealized Sub-Neptune Atmospheres
Authors: Namrah Habib, Raymond T. Pierrehumbert
Figure caption: CM1 Radiative fluxes and estimated radiative timescale for initially adiabatic simulations. Column (a) shows the difference of the upward and downward longwave infrared flux, I+ − I−, and column (b) shows the temperature tendency, ﹩\frac{dT}{dt}﹩, calculated by the TWOSTR numerical package in CM1. Column (c) plots the final state CM1 profile in blue and the temperature profile from the python time-stepping calculation, which adjusts the final CM1 state toward radiative equilibrium (RE) in black. The calculated radiative-equilibrium profile provides an indication of the radiative relaxation timescale and the temperature for the layer where convection is inhibited.
Paper: 3D Modeling of Moist Convective Inhibition in Idealized Sub-Neptune Atmospheres
Authors: Namrah Habib, Raymond T. Pierrehumbert
Figure caption: Radiative fluxes for the initially isothermal compositional convection CM1 simulations. Column (a) shows the difference of the upward and downward longwave infrared flux, I+ − I−, and column (b) shows the temperature tendency, ﹩\frac{dT}{dt}﹩, calculated by the TWOSTR numerical package in CM1. Column (c) plots the final state CM1 profile in blue and the temperature profile from the python time-stepping calculation, which adjusts the final CM1 state toward radiative equilibrium (RE) in black.
Paper: 3D Modeling of Moist Convective Inhibition in Idealized Sub-Neptune Atmospheres
Authors: Namrah Habib, Raymond T. Pierrehumbert
Figure caption: Lapse rates for all six CM1 simulations with radiation. In each panel, the dry-adiabatic lapse rate is shown by the gray dotted line, the moist adiabatic lapse rate is given by the blue dashed line, and the gray gas radiative-equilibrium lapse rate is shown by the green dashed line for comparison. The black line shows the lapse rate at the final time step for the respective simulation.
Paper: An AI Superresolution Field Emulator for Cosmological Hydrodynamics: The Lyα Forest
Authors: Fatemeh Hafezianzadeh, Xiaowen Zhang, Yueying Ni, Rupert A. C. Croft, Tiziana DiMatteo, Mahdi Qezlou, Simeon Bird
Figure caption: Schematic overview of the proposed two-stage framework. The upper panel illustrates the overall model architecture and training process, including Stage 1 (left, purple box) and Stage 2 (right, green box). The lower panels show the detailed generator architectures for each stage: the SR-Generator (yellow box) used in Stage 1 and the Emu-Generator (orange box) used in Stage 2.
Paper: An AI Superresolution Field Emulator for Cosmological Hydrodynamics: The Lyα Forest
Authors: Fatemeh Hafezianzadeh, Xiaowen Zhang, Yueying Ni, Rupert A. C. Croft, Tiziana DiMatteo, Mahdi Qezlou, Simeon Bird
Figure caption: Comparison of gas distributions in the LR-HydroSim, HR-HydroSim, and HydroEmu simulations. The left column shows the full simulation volumes, where the color represents temperature and intensity indicates density. A representative sight line is highlighted by the red box and magnified in the right column. The corresponding Lyα flux profile along the sight line is overplotted in orange. The HydroEmulator prediction closely reproduces both the thermal structure and absorption features observed in the HR-HydroSim.
Paper: An AI Superresolution Field Emulator for Cosmological Hydrodynamics: The Lyα Forest
Authors: Fatemeh Hafezianzadeh, Xiaowen Zhang, Yueying Ni, Rupert A. C. Croft, Tiziana DiMatteo, Mahdi Qezlou, Simeon Bird
Figure caption: Comparison between the HR-HydroSim simulation and the HydroEmu prediction along a randomly selected sight line. The top three panels show the hydrogen overdensity ﹩\rho /\bar{\rho }﹩, temperature T, and line-of-sight velocity vy in real (comoving) space, while the bottom two panels show the optical depth τ and transmitted flux in redshift (velocity) space. Solid red lines correspond to the HydroEmu predictions, while dashed dark blue lines represent the HR-HydroSim simulation results.
Paper: 3D Modeling of Moist Convective Inhibition in Idealized Sub-Neptune Atmospheres
Authors: Namrah Habib, Raymond T. Pierrehumbert
Figure caption: Potential temperature for a CM1 simulation initialized on a superadiabatic state but with no moisture, with the initial state shown by the blue line, and the final state shown by the black line. The dry superadiabat simulation was performed to benchmark the CM1 model performance.
Paper: An AI Superresolution Field Emulator for Cosmological Hydrodynamics: The Lyα Forest
Authors: Fatemeh Hafezianzadeh, Xiaowen Zhang, Yueying Ni, Rupert A. C. Croft, Tiziana DiMatteo, Mahdi Qezlou, Simeon Bird
Figure caption: Phase-space distribution of gas in the temperature–density plane for the HR-HydroSim (left) and the HydroEmu prediction (right). The dashed black line indicates the best-fit power-law relation to the IGM TDR, with T0 and γ denoting the temperature at mean density and the fit parameter. The color scale shows the logarithmic number of gas elements per bin.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: Comparison of fitting and binning methods that highlight the causes of different interpretations in G25a. In all panels, we plot the Hubble residual against SALT2 color, where the residual does not contain the γ term (i.e., before mass step correction). Column-wide comparison highlights the dependence on “measured” profiles on binning methods, and row-wide comparison demonstrates the effects of splits and fitting methods. Right column: equally populated binning, similar to G25a. Middle column: equally spaced binning, similar to BS21. Left column: equally spaced rolling binning, with the shaded region obtained through MC bootstrapping. Top row: single split point at ﹩{\mathrm{log}}_{10}(\frac{M* }{{M}_{\odot }})=10﹩, similar to G25a. The parameters α, β, γ are all fitted simultaneously (but γ is not applied), similarly to G25a. Middle row: same fit as the top row, but split into three, treating the intermediate population separately. Bottom row: same split as the middle row but with a two-parameter fit (no γ fitted). The difference between the middle and bottom rows is also shown in Figure 7.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: (Left) Hubble residuals as a function of host logmass, when split for blue and red colors at c = 0. We only fit α and β to compute the residuals plotted: no mass step (γ term) is added. We note there is no obvious “step” for the red SNe. (Right) A further split of the plot shown in panel 1(a), where now low mass (logmass < 9.5), medium mass (9.5 ≤ logmass < 10.3), and high mass (10.3 ≤  logmass) are all shown. This is consistent with the panel to the left that there is a smooth dependence on mass for the Hubble residuals of red SNe, and a consistent convergence for Hubble residuals of blue SNe.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: A conceptual illustration of the trends in residuals that the dust and progenitor hypotheses predict, over a range of SNe Ia color. Top panel: the predicted residuals of SNe Ia, split by their host property (e.g., stellar mass). Bottom panel: the predicted separation between the split populations (i.e., the separation between the solid curve and the dashed curve in the top panel). The progenitor hypothesis predicts a color-independent, constant offset, while the dust hypothesis predicts a color-dependent increase in the separation.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: The scatter of residuals in subsamples, split by their light curve parameters (c, x1) and host properties. The scatter size is measured with nMAD, 1.48 ·  Med(∣HR∣). Residuals (Hubble residual) are calculated with model 1 in Table 1. We bootstrap the residual values within each bin to reduce the effect of small number statistics. Note that the number of data points varies between bins, and the size of the difference may not translate to the significance of the difference. See Section 2.2 for discussions.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: The separation of the Hubble residuals between low-mass (logmass < 9.5; green curves in Figure 6) and high-mass (10.3 < logmass; red curves in Figure 6) populations, shown as a function of color. Dotted and solid curves represent the residuals calculated with and without the γ-parameter, respectively (see Section 3.3 for a discussion). The significant difference in the separation sizes, as highlighted in the figure, necessitates a color-dependent model instead of a mass step, which attempts to model this profile with a single horizontal line. See Section 3.1 for the binning method used to obtain the profiles.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: Comparison of correction methods and remaining residuals over host logmass, SN Ia color, and SN Ia stretch (x1) values. Top row: the residuals after applying the best-fit Tripp standardization (model 1). Middle row: the residuals after applying the mass step model (model 12). Bottom row: the residuals after applying the Host2D model (model 14).
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: The values of Δμ (Equation (5)). The solid line represents the median value used for the correction (Equation (6)), and the shaded region represents the 16th and 84th percentiles. Individual Hubble residual values (Equation (4)) are shown in the background in light gray.
Paper: Reassessing the ZTF Volume-limited Type Ia Supernova Sample and Its Implications for Continuous, Dust-dependent Models of Intrinsic Scatter
Authors: Yukei S. Murakami, Daniel Scolnic
Figure caption: Color-dependent residuals, split by “step” locations of host property tracers.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Phase-folded observations of V658 Car. Panel (A): TESS light curve, each color representing a different sector (see legend); the inset zooms in the second stellar eclipse, where the model were shifted to match the observed level. Panels (B), (C), and (D) illustrate the EW, line asymmetries, and peak separation of Hα, respectively. The orange crosses represent the standard quantities (V/R and PS, see text), and the blue dots represent the weighted quantities (Equations (1) and (2)). The orange and blue solid lines in panel (C) show the result of a sine fit to the data (see text). Panel (E): radial velocities, where the dots are the observations, and the solid lines are the best fit obtained. Orange (solid), pink (dotted), blue (solid), and black (dotted) lines correspond to, respectively, the Be star (absorption lines), the Hαwings (see Appendix A), the companion, and the traveling emission in Fe II 9997 Å line. The amplitude of the former two were scaled up by a factor of 6, for better visualization. The dashed gray line represents the radial velocity of the center of mass. Panels (F) and (G) show the intrinsic polarization level and angle, respectively. The dots show the observations in the R band, and the dashed lines represent the corresponding average value. In panels (A), (B), (F), and (G), the solid lines represent our best model.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Top: phase-folded TESS light curve of V658 Car, each color representing a different sector (see legend). The main eclipses/attenuations are indicated. Bottom: SPH simulation for a binary system with α = 1 (viscosity parameter defined by N. I. Shakura & R. A. Sunyaev 1973), P = 30 days, and ratio of stellar masses of MBe/MsdOB = 6. ϕ indicates the corresponding observed orbital phase, with the system rotating counterclockwise. The white solid line correspond to the calculated Roche Lobe. More details about the simulation can be found in A. C. Rubio et al. (2025). Shown is the surface density, displaying the two-armed disk (dotted lines) and the transfer of mass from the Be disk to the companion. Considering the disk as Keplerian, we can map the physical positions of the double-peaked profile (red-dashed circle) and oscillating emission (green dot) in Fe II 9997 Å based on their peak velocities (see Section 3.2.3 for details). Since the latter varies over the orbital period, it is represented as a point, while the former remains stable and is therefore represented as a circle.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Dynamical spectral plots for V658 Car. The top panels present lines dominated by the Be star and/or its disk. The bottom panels present lines (or lack of) from the companion star and/or its disk. The red and cyan lines indicates the orbital velocity of the Be star and the companion, respectively. In this figure, we show selected single examples of each element for illustration. Appendix C contains more lines that show the same behavior.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Left: variation of Fe II 5316 Å across different phases in the same orbital cycle. We highlighted the appearance and motion of the traveling features with black arrows. Right: the Fe II 9997 Å line was fitted with a three-Gaussian profile (see Section 3.2.3). Here, we show the observed spectrum at phase 0.508 in orange and the best-fit oscillating Gaussian emission component in green. The blue line shows the subtraction of the latter from the former, revealing a nearly symmetric structure.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Variation of Hα, corrected for the Be radial velocity, across many orbital periods at the same orbital phase, 0.3 and 0.043 for the left and right, respectively. The blue line was observed by Bernard Heathcote, and made available by BESS. The orange and green lines represent NRES observations.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Partial EW of Hα for different velocity bins relative to the Be radial velocity. Black: line center (−150 to 150 km s−1). Pink: line peaks (−300 to −150 km s−1 and 150 to 300 km s−1). Blue: line wings (−750 to −300 km s−1 and 300 to 750 km s−1). The dots correspond to observations, while the lines are cubic splines to aid visualization of the variation outside the stellar eclipse.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: SED of V658 Car. The observations (UV from IUE, optical from GDR3, and IR from SOAR) were merged and presented in red to facilitate the visualization. Blue, vertical dotted line separates the different sources. The black line represents the solution obtained. The other lines represent each component of the model: Be star in blue; companion in orange; the sum of disk emission and scattering in magenta.
Paper: “X-Raying” a Be Star Disk: Fundamental Parameters of the Eclipsing Binary Be Star V658 Car
Authors: Tajan H. de Amorim, Alex C. Carciofi, Jonathan Labadie-Bartz, Ariane C. Silva, Felipe Navarete, Saul A. Rappaport, Pamela Querido, Amanda C. Rubio, Jon Bjorkman, Robert Gagliano, Ivan Terentev
Figure caption: Flowchart illustrating the modeling approach described in Section 4. Red lines indicate the inner loop, while the entire diagram represents the outer loop. See text for details.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Radial profiles of different quantities for halo A4 at z = 4. Top panel: projected H I and H2 column density profiles. Red solid and dashed lines show NH I, DLA = 2 × 1021 cm−2 and ﹩{N}_{{{\rm{H}}}_{2},{\rm{detec}}}=1{0}^{14}\,{{\rm{cm}}}^{-2}﹩, respectively. Middle panel: radial profiles of normalized LW-band flux ILW, dust metallicity ﹩{Z}_{d}^{\prime} ﹩, and atomic+molecular hydrogen density n. Bottom panel: Rmol as it is computed by our model (solid black) and using the optically thin approximation described in Section 3.1 (dashed black). The vertical dotted line marks radial distance at which the dust optical depth ﹩{\tau }_{d}=\left({N}_{{\rm{H}}\,{\rm\small{I}},{\rm{p}}}+2{N}_{{{\rm{H}}}_{2},{\rm{p}}}\right)\,{\sigma }_{{\rm{g}}}﹩ drops below 1, beyond which the Rmol computed from our model agrees with the optically thin approximation. Shaded regions show the interquartile range of the corresponding curves.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Total H2 column density, ﹩{N}_{{{\rm{H}}}_{2},{\rm{tot}}}﹩, as a function of total (atomic+molecular) hydrogen column density, Ntot, for our two-sided 1D models, for various densities n (top panel), LW-band fluxes ILW (middle panel), and dust abundances ﹩Z{{\prime} }_{d}﹩ (bottom panel). Colored curves show variations on our fiducial ISM model with n = 100 cm−3, ILW = 1, and ﹩Z{{\prime} }_{d}=0.1﹩. Black dashed lines show our representative high-z CGM model with n = 1 cm−3, ILW = 10, and ﹩Z{{\prime} }_{d}=0.1﹩. Gray dotted lines indicate constant ﹩{f}_{{{\rm{H}}}_{2}}\equiv 2{N}_{{{\rm{H}}}_{2,{\rm{tot}}}}/{N}_{{\rm{tot}}}﹩.
Paper: Molecular Hydrogen in High-redshift Damped Lyα Absorbers
Authors: Alon Gurman, Amiel Sternberg, Shmuel Bialy, Rachel K. Cochrane, Jonathan Stern
Figure caption: Top panel: H2 photodissociation rate for an F. Haardt & P. Madau (2012) UV background spectrum as a function of redshift. The right y-axis shows the value normalized to the solar neighborhood B. T. Draine (1978) field. The shaded regions show the redshift range we study and the corresponding range in ILW of 0.13–0.16 associated with the metagalactic field. Bottom panel: radial median profiles of ILW for each redshift. Shaded regions show the 25%–75% range and vertical dashed lines show the radial distance at which the median contribution from the galaxy and the metagalactic radiation field are equal.