adsabs/AstroCLIMB huggingface dataset:
Paper: Near- and Mid-ultraviolet Observations of X-6.3 Flare on 2024 February 22 Recorded by the Solar Ultraviolet Imaging Telescope on board Aditya-L1
Authors: Soumya Roy, Durgesh Tripathi, Sreejith Padinhatteeri, A. N. Ramaprakash, Abhilash R. Sarwade, Nived V. N., Janmejoy Sarkar, Rahul Gopalakrishnan, Rushikesh Deogaonkar, K. Sankarasubramanian, Sami K. Solanki, Dibyendu Nandy, Dipankar Banerjee
Figure caption: Reference fit (solid red) of the SoLEXS spectra (blue crosses) using an isothermal model. The bottom panel shows the fit residue.
Paper: Near- and Mid-ultraviolet Observations of X-6.3 Flare on 2024 February 22 Recorded by the Solar Ultraviolet Imaging Telescope on board Aditya-L1
Authors: Soumya Roy, Durgesh Tripathi, Sreejith Padinhatteeri, A. N. Ramaprakash, Abhilash R. Sarwade, Nived V. N., Janmejoy Sarkar, Rahul Gopalakrishnan, Rushikesh Deogaonkar, K. Sankarasubramanian, Sami K. Solanki, Dibyendu Nandy, Dipankar Banerjee
Figure caption: The flare as observed in all narrowband filters at the time of peak intensity in NB03. The overplotted black contours show 60% of the peak intensity observed in NB03.
Paper: Near- and Mid-ultraviolet Observations of X-6.3 Flare on 2024 February 22 Recorded by the Solar Ultraviolet Imaging Telescope on board Aditya-L1
Authors: Soumya Roy, Durgesh Tripathi, Sreejith Padinhatteeri, A. N. Ramaprakash, Abhilash R. Sarwade, Nived V. N., Janmejoy Sarkar, Rahul Gopalakrishnan, Rushikesh Deogaonkar, K. Sankarasubramanian, Sami K. Solanki, Dibyendu Nandy, Dipankar Banerjee
Figure caption: Coaligned and coregistered AIA 1600 and 1700 Å and GONG Hα observation near the NB03 peak in (a), (b), and (c), respectively. The overplotted contours show 60% of the peak intensity observed in NB3.
Paper: Fading Light, Fierce Winds: JWST Snapshot of a Sub-Eddington Quasar at Cosmic Dawn
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke, Meredith Stone, Jane Morrison, Stacey Alberts, Xiangyu Jin, Yongda Zhu, Weizhe Liu, 伟哲 刘, Jinyi Yang
Figure caption: The observed nuclear quasar spectrum of HSC J2239+0207 (blue line). A normal quasar template built from SDSS is also plotted in red as a comparison. We have highlighted various spectral features. We have plotted a galaxy template with stellar mass M* ∼ 1010 M⊙ (orange line) and show the resulting QSO+galaxy spectrum (green dashed line). All the templates have been smoothed to match the NIRSpec prism resolutions.
Paper: Electrodynamics and Dissipation in the Binary Magnetosphere of Premerger Neutron Stars
Authors: Jens F. Mahlmann, Andrei M. Beloborodov
Figure caption: Initial (static) state used in the simulation with aligned magnetic moments (χ1 = χ2 = 0∘). Top: black and blue curves show the magnetic field lines emerging from the two neutron stars. No field lines connect the stars in this configuration. The figure also indicates the energy release region (magenta box) that appears when the stars are spun up and the KH instability develops at the interface of their magnetospheres. Bottom: schematic picture of compressive wave emission from the interface region (red circle). Their relative amplitude b = δB/B is b0 in the emission region and grows as the waves propagate to the outer magnetosphere. The red contours show the approximate locations where such waves become nonlinear (b = δB/Bbg ∼ 1, leading to shocks), for the initial wave amplitudes b0 = 0.1 and b0 = 0.02. The shown magnetosphere is the initial state; the actual configuration changes after spinning up the stars, so the contours of b = 1 will also change.
Paper: Fading Light, Fierce Winds: JWST Snapshot of a Sub-Eddington Quasar at Cosmic Dawn
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke, Meredith Stone, Jane Morrison, Stacey Alberts, Xiangyu Jin, Yongda Zhu, Weizhe Liu, 伟哲 刘, Jinyi Yang
Figure caption: Top panel: the IFU reconstructed images of the quasar HSC J2239+0207. The postage stamps show images at the flux peak of the [O III] and Hα+[N II] emission and the adjacent emission-line-free continuum. We have highlighted the rectangular aperture used to extract the companion signals in green. Middle panel: the NIRSpec IFU prism spectra of the emission companion (green line) with the 1σ uncertainties (gray shaded regions). We also plot the observed spectrum of quasar HSC J2239+0207 as a comparison (blue line) and labeled the [O III], Hβ, [N II], and Hα wavelengths at the quasar redshift. Bottom panel: the NIRSpec IFU prism spectra of the companion (green line) compared to two stacked spectra for extreme emission-line galaxies (EELGs; dark yellow line) and non-EELGs (magenta line) at z > 5.7 from K. Boyett et al. (2024).
Paper: Fading Light, Fierce Winds: JWST Snapshot of a Sub-Eddington Quasar at Cosmic Dawn
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke, Meredith Stone, Jane Morrison, Stacey Alberts, Xiangyu Jin, Yongda Zhu, Weizhe Liu, 伟哲 刘, Jinyi Yang
Figure caption: PyQSOFit spectral decomposition results of the UV (top) and optical bands (bottom) of the HSC J2239+0207 NIRSpec prism spectrum. The integrated model (black dotted line) is composed of the AGN featureless continuum (dashed orange line), the iron emission model (thin blue line), the broad-line components (red lines), and the narrow-line components (yellow lines). The data are shown with the thick light-blue line. The wavelengths of some strong nebular emission lines are labeled with vertical gray dashed lines, and the gray horizontal bands on the top indicate the wavelength window used to fit the featureless continuum and iron models.
Paper: Fading Light, Fierce Winds: JWST Snapshot of a Sub-Eddington Quasar at Cosmic Dawn
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke, Meredith Stone, Jane Morrison, Stacey Alberts, Xiangyu Jin, Yongda Zhu, Weizhe Liu, 伟哲 刘, Jinyi Yang
Figure caption: Top panel: continuum-normalized spectrum of HSC J2239+0207. The dashed green vertical line denotes the Lyα wavelength (1215.7 Å), and the pink vertical line denotes the wavelength where the quasar flux (blue line) starts to drop below 10% of the quasar continuum (red dotted line). The wavelength difference between the two (δλ) gives the size of the quasar proximity zone. Bottom panels: the location of HSC J2239+0207 on the proximity zone vs. AGN luminosity (left) and redshift (right) plane, in comparison with the sample in A.-C. Eilers et al. (2017). Dashed lines are the best-fit correlations reported in A.-C. Eilers et al. (2017).
Paper: Fading Light, Fierce Winds: JWST Snapshot of a Sub-Eddington Quasar at Cosmic Dawn
Authors: Jianwei Lyu, 建伟 吕, George H. Rieke, Meredith Stone, Jane Morrison, Stacey Alberts, Xiangyu Jin, Yongda Zhu, Weizhe Liu, 伟哲 刘, Jinyi Yang
Figure caption: Normalized spectrum of HSC J2239+0207 for the BAL feature measurements. The x-axis indicates the velocity relative to the rest-frame wavelength of the ionic species indicated by the label. The solid (dashed) horizontal line represents a normalized flux level of 1.0 (0.9). BAL troughs defined as normalized flux < 0.9 are highlighted as yellow shaded regions. Vertical red solid lines indicate ﹩{\nu }_{{\rm{\max }}}﹩ and ﹩{\nu }_{{\rm{\min }}}﹩ for each BAL.
Paper: Erratum “Overestimation of Astrophysical Gamma-Ray Energies during Thunderstorms: Synergy of Galactic and Atmospheric Accelerators” (2024, ApJL, 975, L39)
Authors: A. Chilingarian, M. Zazyan
Figure caption: (a) Illustration of fitting procedure; (b)–(d) Relationship between “true” and estimated primary gamma-ray energies for different AEFs and H values.
Paper: Erratum “Overestimation of Astrophysical Gamma-Ray Energies during Thunderstorms: Synergy of Galactic and Atmospheric Accelerators” (2024, ApJL, 975, L39)
Authors: A. Chilingarian, M. Zazyan
Figure caption: The enhancement of EAS electrons after their propagation in various AEFs (Ez), which terminated at different heights H above the surface.
Paper: Electrodynamics and Dissipation in the Binary Magnetosphere of Premerger Neutron Stars
Authors: Jens F. Mahlmann, Andrei M. Beloborodov
Figure caption: Snapshots of the simulations with χ1 = χ2 = 0∘ (top panels) and χ1 = 0∘, χ2 = 30∘ (bottom panels). Left: selected closed magnetic field lines attached to the rotating stars and interacting in the interface region near the vertical midplane (yz-plane). Right: color plots of charge density ρ = ∇ · E/4π (related to drift velocity v/c = E × B/B2) and the velocity component vy, measured in the xy-plane. The cross-circles show where the rotating magnetic field lines puncture the plane. The snapshots of ρ and vy illustrate the motion of the magnetic field lines and show the vortices generated by KH instability in the interface layer (magenta box). The KH vortices create an effective drag between the magnetospheres, intermittently slowing down and releasing the field lines.
Paper: Electrodynamics and Dissipation in the Binary Magnetosphere of Premerger Neutron Stars
Authors: Jens F. Mahlmann, Andrei M. Beloborodov
Figure caption: 2D shear layers during the linear growth of the force-free KH instability for varying shear velocities βs0 and magnetic field orientations Ω. We display the normalized drift velocity βx/βs0 (left), the charge density ρ/ρ0 (middle), and the parallel electric field ﹩{E}_{\parallel }^{2}/{e}_{0}﹩ removed by enforcing the force-free condition E · B = 0 (right). Consistent with Equation (A19), some configurations will not have any instability (top row). For ﹩\cos {\rm{\Omega }}\gt 0﹩, the instability growth induces parallel electric fields that FFE constraint enforcement removes.
Paper: Electrodynamics and Dissipation in the Binary Magnetosphere of Premerger Neutron Stars
Authors: Jens F. Mahlmann, Andrei M. Beloborodov
Figure caption: Growth rates of the KH instability as a function of initial shear velocity βs0: theory (solid lines), predictions for specific simulations (black squares), and simulation measurements (black dots). Solid lines are drawn for different values of ﹩{\rm{\cos }}{\rm{\Omega }}\in \{0,1\}﹩ (see the color-coding). The instability growth is suppressed for ﹩{\rm{\cos }}{\rm{\Omega }}\lt {\beta }_{0}﹩
Paper: Electrodynamics and Dissipation in the Binary Magnetosphere of Premerger Neutron Stars
Authors: Jens F. Mahlmann, Andrei M. Beloborodov
Figure caption: Magnetic fields in 3D simulations of aligned rotator magnetospheres (Ωr*/c ≈ 0.2) next to a perfectly conducting wall at the right end of the domain. The dashed gray lines indicate the nominal light cylinder location. As the conducting wall approaches the star, the magnetosphere is increasingly compressed.
Paper: Electrodynamics and Dissipation in the Binary Magnetosphere of Premerger Neutron Stars
Authors: Jens F. Mahlmann, Andrei M. Beloborodov
Figure caption: Outgoing luminosity for compressed aligned rotator magnetospheres, normalized to L0 = μ2Ω4/c3. Stronger compression drives higher spindown luminosity. The thick black line denotes a reference model without compression.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Examples of our stacked spectra. The gray spectra are the zmedian = 3.443 (left), zmedian = 3.653 (middle), and zmedian = 4.083 (right) stacks, shifted to the observation frame. Overplotted are the best-fit models. The red spectrum is the T02 SED, and the blue spectrum at the top is the L15 SED, with the lighter blue region indicating the 1σ confidence region. The two SEDs are both shifted to zqso = 3.443, to be comparable with the leftmost stack. All five spectra are normalized at 1450 Å. Overplotted on the DESI stacked spectra are the best-fit models using the T02 SED. An illustration of the composite spectra and SED templates redward of Lyman-α is shown in Appendix A.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Parameter distributions of the DESI quasar sample analyzed here. Left: the distribution of angular positions, showing a roughly uniform distribution across the survey area. Middle: the distribution of quasar magnitude and color, colored with redshift. The x-axis is the g − z color, and the y-axis is the color defined in E. Chaussidon et al. (2023), which combines the optical grz bands and the infrared W1 and W2 bands. To better illustrate the stellar contaminants, we use red points to represent the stellar color from the early data release of the DESI Milky Way Survey (S. E. Koposov et al. 2024), filtered with RVS_WARN = 0 and RR_SPECTYPE = 0, as well as PRIMARY = TRUE (see their Section 5.1). Right: the distribution of redshift. Nbin means the number of quasar sightlines within the redshift bin.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Comparison between different ﹩{\lambda }_{{\rm{mfp}}}^{912}﹩ measurements. All the points and lines are normalized with our T02 power-law fitting in Table 1 (denoted as ﹩{\lambda }_{{\rm{mfp}}}^{912* }﹩ on the y-axis label) and are slightly shifted along the x-axis for a better display. The purple dashed–dotted line and green dashed line are the W14 power-law model and our ﹩{\lambda }_{{\rm{mfp}}}^{912* }﹩ model. The blue upward triangles are the original P09 results. With exactly the same data, we use our method (gray squares), our method with the ﹩{\lambda }_{{\rm{mfp}}}^{912}﹩ definition as 1/κ0 (purple pentagons), our method with γτ = 0 (orange hexagons), and our method with both the 1/κ0 definition and γτ = 0 (green downward triangles), respectively, to measure ﹩{\lambda }_{{\rm{mfp}}}^{912}﹩. Measurements with DESI stacks at the same redshift range are shown with red circles, for comparison. To better illustrate the uncertainty estimates, the blue, green, gray, and red dots are shaded with the same color within the 1σ range, while the purple and orange dots are not. Comparing the blue and green triangles, we believe that our method stays consistent with previous works in estimating both values and uncertainties. Correcting the γτ choice makes the P09 measurements consistent with ours (gray squares), while the z = 4.07 and z = 4.22 results deviate from our ﹩{\lambda }_{{\rm{mfp}}}^{912* }﹩ model for more than 1σ. The different ﹩{\lambda }_{{\rm{mfp}}}^{912}﹩ definition would generate ∼7% bias, and neglecting γτ would bias the result for ∼20%.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Measurements of different quasar SEDs compared with our default model. Left: measurements when we adjust the tilt index α in Equation (3) to 0.5 (blue upward triangles), 0.25 (orange downward triangles), −0.25 (green squares), and −0.5 (red hexagons), which show that except for an extreme tilt (∣α∣ ≳ 0.5), our default measurements would not bias more than 5% due to an incorrect spectral index. Right: measurements with different overall normalization. The blue upward triangles, orange downward triangles, and green squares represent the measurements when we shift the T02 SED by 0.85, 1.15, and 1.30. For comparison, we also draw the measurements with L15, represented by the red hexagons. The difference between the L15 and T02 measurements can then be explained for ∼70% by the overall height of the SED, and the remaining ∼30% may come from the shape fluctuations.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: The measured mean free path as a function of redshift, using the T02 SED. Left: the overall mean free path evolution at 2 ≲ z ≲ 5, with data points from P09 (blue upward triangles), M. Fumagalli et al. (2013; pink pengatons), J. M. O’Meara et al. (2013; green diamonds), W14 (black downward triangles), E. Lusso et al. (2018; orange hexagons), and this work (red circles). The violet dashed–dotted line and the green dashed line represent the best power-law fittings in W14 and this work, respectively. Right: the zoom-in plot at 3.1 ≤ z ≤ 4.7, to better display the differences between our work and P09. Our measurements are systematically lower than the interpolation of the W14 power law at z ≲ 4, which is mainly due to the improper handling of the Lyman-series opacity evolution in P09, and our power law is roughly consistent with other previous works.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: MCMC posteriors. Top left: the combined MCMC sampling of the parameter posterior for the zmedian = 3.443 composite spectrum. The blue lines show the median parameter values in marginal distributions that can be used as appropriate choices for the maximum posterior estimation. The dashed vertical lines denote the 16% and 84% quantiles. Top right: the mean free path distribution calculated from the parameter posterior sample in the top left panel, which is mostly Gaussian-shaped. Lower left: the parameter posterior at zmedian = 3.443 when the parameter γκ in Equation (4) is freed. Lower right: the broken-power-law parameter posterior when fitting the data points in Figure 6.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Comparison between our measurements and the previous f(NHI, z) models. The red circles, blue upward triangles and black downward triangles are the observational measurements from our work, the remeasured P09, and W14, respectively. The black, purple, and yellow lines are the mean free path calculations with the Equation (10) definition, using models from F. Haardt & P. Madau (2012), A. K. Inoue et al. (2014), and E. Puchwein et al. (2019), respectively. The green dashed–dotted line represents our best broken-power-law fitting. All three models in the literature overpredict the evolution speed of the mean free path.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: The best-fit broken power law of the current mean free path measurements at 2 ≲ z ≲ 6, using the functional form in Equation (12). The data points in P09 (blue upward triangles) are remeasured using our pipeline, as we do in Figure 5.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: The Lyman-series optical depth calculated using the f(NHI, z) model in J. X. Prochaska et al. (2014; P14), at the rest frame of three z = 3.5 (blue), 4.0 (orange), and 4.5 (green) quasars. The upper panel shows the optical depth accounting for all Lyman-series lines. The lower panel shows the ratio of the optical depth calculated from the P14 model and our Equation (4), with the black horizontal dashed lines representing 1.000, 0.995, and 0.990 and the red vertical dashed line representing the Lyman-limit wavelength (912 Å). The Lyman-series opacity blueward of the Lyman-limit wavelength clearly evolves, and our approximation of the Lyman-series optical depth in Equation (4) is shown to produce only <1% systematic error, and for most cases <0.5%.
Paper: Measuring the Mean Free Path of H I Ionizing Photons at 3.2 ≤ z ≤ 4.6 with DESI Y1 Quasars
Authors: Anning Gao, J. Xavier Prochaska, Zheng Cai, Siwei Zou, Cheng Zhao, Zechang Sun, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, A. de la Macorra, Arjun Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, S. Juneau, A. Kremin, P. Martini, A. Meisner, R. Miquel, J. Moustakas, A. Muñoz-Gutiérrez, J. A. Newman, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Marginalized parameter posterior of broken-power-law fitting when incorporating data from P. Gaikwad et al. (2023), F. B. Davies et al. (2024), and S. Satyavolu et al. (2024). The blue histograms are the normalized posterior, the blue vertical dashed–dotted lines indicate the maximum posterior estimation, and the blue titles are the parameter estimations, with the uncertainties defined in the way described in Section 4.3. For comparison, we also show the marginalized posterior from Section 4.3 with the gray lines.