adsabs/AstroCLIMB huggingface dataset:
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: The Spearman correlation coefficients (ρ) between the 2PCF signals and the galaxy formation redshifts defined in different ways and at different galactocentric distances. Following Figure 1, we adopt TNG50, TNG100, and TNG300 to continuously cover the full mass range, with the name of the simulation and the mass range of ﹩{\mathrm{log}}_{10}{M}_{200c}/{M}_{\odot }﹩ indicated by texts of each panel. We only show the results at redshift z = 0. In each panel, dotted blue, dashed–dotted orange, and dashed green curves refer to the Spearman correlation coefficients with z 1/4, z 1/2, and z 3/4. Here z 1/4, z 1/2, and z 3/4 are defined as the redshifts at which the galaxies have accreted one-fourth, half, and three-fourths of their total ex situ stellar mass at redshift z = 0. Negative correlation coefficients mean the clustering strength revealed by the 2PCF signals and the galaxy formation redshifts are anticorrelated, i.e., the clustering decreases with the increase in the formation redshifts.
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: The ex situ stellar mass accretion histories of galaxy systems in four different halo mass (M 200c ) bins, as indicated by the legend. The curves are medians taken over the assembly histories of galaxies in the same mass bin and are normalized to be unity at redshift z = 0. The gray dashed vertical lines mark the positions of redshifts z = 0.5, 1.0, and 1.5. The plot is based on TNG50.
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: The 2PCF signals as a function of galactocentric distances, r, scaled by R 200c . This figure is based on TNG50. We plot in each panel 2PCF measurements at the same redshift/snapshot. Different symbols connected by lines with varying colors in the same panel refer to the median 2PCFs for galaxies in four mass bins of M 200c  (see the legend). Galaxies are no longer divided into bins according to their formation redshifts.
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: Similar to Figure 4, but each panel shows the median 2PCFs in the same mass bin of M 200c , while different color curves refer to the measurements at different redshifts (see the legend).
Paper: The Mass and Redshift Dependence of Halo Star Clustering
Authors: Zhenlin Tan, Wenting Wang, Jiaxin He, Yike Zhang, Vicente Rodriguez-Gomez, Jiaxin Han, Zhaozhou Li, Xiaohu Yang
Figure caption: The velocity anisotropy (β) of subhalos, different symbols, and colors indicate different simulations. Here β is calculated using subhalos with galactocentric distances of 0.1R 200c  < r < R 200c . The number of subhalos within a single halo in this range should exceed 10, and the number of dark matter particles within a single subhalo should exceed 20 in order to exclude the effect of small-mass dark matter structures.
Paper: AGN STORM 2. X. The Origin of the Interband Continuum Delays in Mrk 817 
Authors: Hagai Netzer, Michael R. Goad, Aaron J. Barth, Edward M. Cackett, Keith Horne, Chen Hu, Erin Kara, Kirk T. Korista, Gerard A. Kriss, Collin Lewin, John Montano, Nahum Arav, Ehud Behar, Michael S. Brotherton, Doron Chelouche, Gisella De Rosa, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Yasaman Homayouni, Dragana Ilić, Shai Kaspi, Andjelka B. Kovačević, Hermine Landt, Luka Č. Popović, Thaisa Storchi-Bergmann, Jian-Min Wang, Fatima Zaidouni
Figure caption: The measured lag (ICCF centroid) for the DC component of Model 2 relative to the driving continuum light curve, here plotted as a function of the characteristic timescale of the driving continuum, for fixed light-curve durations of 500, 1000, and 2000 days, each with 1 day sampling. In all cases, the measured ICCF centroid shows a strong dependence on T char, for small T char. Only for long light-curve durations does the ICCF centroid approach the MER, and then only for the largest T char.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the central galaxy kinematics, q   ϕ  (Δr cen/R vir ∣  θ ) and q   ϕ  (Δv cen/V vir ∣  θ ), on  θ  h (M vir, c, and λ, from top to bottom) in IllustrisTNG (red) and SIMBA (blue). The y-axis denotes the probability density on a linear scale. The parameters that do not appear in the legends are kept at the fiducial values. The dashed lines mark the medians of the distributions. We find a significant dependence of q   ϕ  (Δr cen/R vir ∣  θ ) not only on M vir but also on c and λ for both IllustrisTNG and SIMBA: q   ϕ  (Δr cen/R vir ∣  θ ) is skewed toward lower Δr cen/R vir for higher M vir and c, while the trend is reversed for λ. The trends in both simulation suites are consistent with each other; however, q   ϕ  (Δr cen/R vir ∣  θ ) is broader in SIMBA than in IllustrisTNG.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the satellite galaxy kinematics, q   ϕ  (Δr sat/R vir ∣  θ ) and q   ϕ  (Δv sat/V vir ∣  θ ), on  θ  h (M vir, c, and λ, from top to bottom) in IllustrisTNG (red) and SIMBA (blue). The parameters that do not appear in the legends are kept at the fiducial values. For reference, we include NFW profiles using the three values of c (dashed; ﹩\mathrm{log}c﹩ panel). q   ϕ  (Δr sat/R vir ∣  θ ) differs between IllustrisTNG and SIMBA. They also differ from the NFW profiles (Section 5.2). In addition, q   ϕ  (Δv sat/V vir ∣  θ ) contains both the infalling and orbiting populations of satellite galaxies (Appendix C). Overall, the effect of  θ  h on the satellite kinematics is small, except for the effect of λ on Δv sat/V vir, which changes the infalling fraction.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the central galaxy kinematics, q   ϕ  (Δr cen/R vir ∣  θ ) and q   ϕ  (Δv cen/V vir ∣  θ ), on Ωm (top) and σ 8 (bottom) in IllustrisTNG (red) and SIMBA (blue). The parameters that do not appear in the legends are kept at the fiducial values. The dashed lines mark the medians of the distributions. In both IllustrisTNG and SIMBA, q   ϕ  (Δr cen/R vir ∣  θ ) is slightly skewed to higher Δr cen/R vir at higher Ωm. Overall, we find no strong dependence of galaxy kinematics on the cosmological parameters.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: The distribution of host halo properties, M vir, λ, c, for central galaxies (blue) and satellite galaxies (gray) in the SIMBA hydrodynamic suite. The contours are marked for 68th, 95th, and 99th percentiles. In total, we have 359,494 central galaxies and 22,244 satellite galaxies with M * > 109 M ⊙ in SIMBA. IllustrisTNG has a similar distribution, with 276,527 central and 34,695 satellite galaxies. The black dashed lines mark the fiducial values of the halo properties. We examine the distribution of galaxy kinematics at the points marked in orange (crosses) to identify the dependence on each halo property.
Paper: Investigating the Kinematics of Central and Satellite Galaxies Using Normalizing Flows
Authors: K. J. Kwon, ChangHoon Hahn
Figure caption: Dependence of the central galaxy kinematics, q   ϕ  (Δr cen/R vir ∣  θ ) and q   ϕ  (Δv cen/V vir ∣  θ ), on the baryonic feedback parameters. The distributions vary a single feedback parameter as indicated in the legend (blue, orange, green, and red), while the rest are kept at the fiducial values. We include the distributions at  θ  fid for reference (gray). The dashed lines mark the medians of the distributions. The baryonic feedback parameters do not largely impact the central galaxy kinematics.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The observed L X in the S band is compared with (left, red line) the expected L X,LMXB, and (right, dashed red line) the expected L X,HMXB. The data points are color-coded by z.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The ratio of L X(S) and L X ,PL(S) plotted against L X(B). The data points are color-coded by z. The horizontal red line indicates ratio = 1, and the blue vertical line indicates L X(B) = 1042 erg s−1, which marks the canonical boundary between normal galaxies and AGNs.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Same as Figure 9, but with L X,GAS in the S band determined with Method B in Section 4.2, subtracting the power-law component converted from the H band to the S band.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Left: the S-band (0.5–1.2 keV) XLF of galaxies with z < 0.6. Right: XLF separately built in three redshift bins: z = 0.1 (0.0–0.2), z = 0.3 (0.2–0.4), and z = 0.5 (0.4–0.6).
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Same as Figure 9, but with L X,GAS in the S band determined with Method A in Section 4.1, subtracting L X,LMXB and L X,HMXB based on the scaling relations.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The X-ray luminosity (left) in the S band (0.5–1.2 keV) and (right) H band (2–7 keV) plotted against redshift. The K-correction for the APEC (power-law) component is applied for the S (H) band. The galaxies with spec-z and photo-z are red and blue points, respectively.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The B-band (0.5–7.0 keV) XLF of galaxies. Also plotted are previously measured XLFs by Norman et al. (2004), Georgantopoulos et al. (2005), and D.-W. Kim et al. (2006). The dashed line with a slope of −1 (log ϕ = −1 ∗ log L X + 37.4) is for visibility. The same line is drawn in all XLF Figures below. Note that the X-ray luminosity includes all X-ray emission components (AGN, X-ray binaries, and hot gas).
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: The sky coverage area is plotted as a function of the X-ray flux for the S (0.5–1.2 keV) and B (0.5–7 keV) energy bands.
Paper: Luminosity Evolution of the Hot Gas in Normal Galaxies from the Near Universe to z = 0.5
Authors: Dong-Woo Kim, Giuseppina Fabbiano
Figure caption: Comparison of L X,GAS estimated by two methods. The solid and dotted lines indicate y = x and y = 3x, respectively.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Temperature and ionization equilibration processes in a solar-abundance plasma shock-heated with V sh = 1000 km s−1 and β = 0.01: (a) Electron and ion temperatures as a function of τ. Only the temperatures of several representative elements are plotted, although all the atoms from H to Ni are included in the calculation. (b) Ion fraction of oxygen for our model (solid lines) and nei model (dashed lines) and (c) their ratio as a function of τ. The ratios are plotted only when the ion fractions are greater than 10−2. Panels (d) and (e) are the same as (b) and (c), respectively, but for iron.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Synthesized spectra of a solar-abundance plasma in the 0.5–2.0 keV band, predicted by our model (solid line) and the nei (dashed line) model with the identical electron temperature of 0.91 keV and τ of 1011 cm−3 s: Panel (a) shows the theoretical spectra, whereas panels (b) and (c) show the spectra convolved with the instrumental response matrices of XRISM Resolve (Microcalorimeter) and XMM–Newton MOS (CCD), respectively.
Paper: A Self-consistent Model of Shock-heated Plasma in Nonequilibrium States for Direct Parameter Constraints from X-Ray Observations
Authors: Yuken Ohshiro, Shunsuke Suzuki, Yoshizumi Okada, Hiromasa Suzuki, Hiroya Yamaguchi
Figure caption: Immediate postshock temperatures of each particle species as a function of β in a solar-abundance plasma heated by a shock wave with a velocity of V sh = 1000 km s−1.
Paper: Constraining Quasar Feedback from Analysis of the Hydrostatic Equilibrium of the Molecular Gas in Their Host Galaxies
Authors: Qinyue Fei, Ran Wang, Juan Molina, Luis C. Ho, Jinyi Shangguan, Franz E. Bauer, Ezequiel Treister
Figure caption: The stellar mass vs. SFR for both quasar host galaxies and inactive galaxies. Black and white circles denote quasars with CO detections (A. S. Evans et al. 2006; J. Shangguan et al. 2020a), and red points indicate three targets with spatially resolved CO observations (J. Molina et al. 2021, 2023) that are used in this work. The EDGE–CALIFA data are represented by light-blue and dark-blue squares, with the latter corresponding to a subsample chosen for comparison with the quasar hosts. Additionally, we include the xCOLD GASS sample (A. Saintonge et al. 2017) as gray triangles. The solid line on the plot represents the main sequence of star-forming galaxies at z ∼ 0. Saintonge et al. (2016), while the gray-shaded band illustrates its ±0.4 dex uncertainties. The typical uncertainties associated with the host galaxy measurements are depicted by the error bar in the bottom-right corner of the plot.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show a comparison between two 3 M ⊕ models (30% in black and 10% in gray) initially having substantially larger RCB radii (compared to Figure 9) that are the same as the sonic point radii, both without core luminosity, similar to the setup shown in J. E. Owen & Y. Wu (2016). The advective cooling timescale is always comparable to the mass-loss timescale. Consequently, advective cooling starts to efficiently remove the planetary interior energy at the time that the H/He mass fraction begins to decline after 10−3 yr, resulting in a more pronounced enhancement in the post-boil-off mass fraction between models with different initial mass fraction, compared to the models that initially have a smaller radius. However, we suggest in Appendix B that the final mass fraction difference is also due to the initial entropy effect (Figure B2), rather than only the advective cooling effect (Figure B3). We argue that those cases with the extreme initial radii discussed here do not occur given self-consistent initial entropies (∼10k  b /atom) and initial mass fractions (≤20%).
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: The distributions of the final planetary radius and envelope mass fraction by 3 Gyr from the models discussed in the text. The fully numerical model with a Rayleigh core mass distribution in blue shows a flat distribution in <2.0 M ⊕ with no significant radius gap. The semianalytical model in yellow uses initial conditions from our numerical boil-off calculation and the GSS18 core mass distribution that has a high-mass tail. It does not exhibit a radius gap but instead a peak at 1.5 and 2.0 M ⊕. The fully analytical model that calculates both the boil-off and long-lived mass-loss (bolometric-driven) phases self-consistently is shown in red. As a comparison, similar model setups but with the long-lived escape turned off are shown in dashed black and dashed gray for both analytical and semianalytical models, respectively, showing no significant long-lived mass loss. All of the analytical models have the radius defined at the RCB, while the numerical model has a radiative atmosphere.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the temperature of the isothermal core T  c  and, at the bottom of the envelope, T  b  (top panel), H/He mass fraction (middle), and RCB radius (bottom), in the presence of a coupled (red) and decoupled core evolution (black). This is for a planet with a 3.6 M ⊕ core initially with 10% envelope mass receiving 100 F ⊕ stellar flux. The decoupled core evolution ceases once the core temperature drops to match the temperature at the bottom of the envelope, leading to a coupled subsequent core evolution. In the top panel, the core temperature (black) under the decoupled evolution declines quickly and connects to the temperature at the bottom of the envelope (gray) within the transition phase (which starts after the dotted line) until the boil-off is ended (with circles) and therefore switches to a coupled core evolution. The prolonged transition phase of 10 Myr, which is regarded as the core-enhanced part of the late boil-off, leads to a slight enhancement of the mass loss, after which the long-lived Parker wind is inefficient owing to the efficient thermal cooling and contraction, similar to the behavior of red.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: To demonstrate the importance of the radiative atmosphere, we show a comparison between the distribution of 20 mbar radii in blue (the same blue distribution in Figure 20) and RCB radii in red. Without a radiative atmosphere, the red model has a radius peak that is greatly shifted to a much smaller radius at around 1.5–2.0 R ⊕, without any radius gap feature, which is reminiscent of the semianalytical model in Figure 20. The radius cutoff also shrinks by 20%, coincidentally similar to that from the analytical model that has a different core mass distribution and no radiative atmosphere (orange, with GSS18 setup). We then illustrate the core mass distribution effect by incorporating the high-mass tail into our numerical model (black), which leads to an unrealistic flat distribution that extends outside 5 M ⊕.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: The final distributions of the planet radiii and H/He mass fractions with a range of different physics choices used in the analytical model. By including the ﹩{\dot{E}}_{\mathrm{adv}}﹩ term that is missing from the GSS18 model (yellow) with all other conditions the same, there is no sign of a radius gap in the range of 1.5−2.0 R ⊕ (red). A decoupled isothermal Parker wind with the ﹩{\dot{E}}_{\mathrm{adv}}﹩ term (black) yields a very similar final distribution to the original one (yellow), but with a dramatic shift in the mass-loss timescale (Figure 12). The blue distribution corresponds to the fully analytical model that additionally has our boil-off initial conditions, showing a bimodal distribution but with a less prominent radius gap.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: We show the importance of the radiative atmosphere for the GSS18 analytical model by attaching a layer of isothermal radiative atmosphere on top of the RCB and calculating the distribution of 20 mbar radii in black. As a comparison, the radius distribution without it is shown in blue, the same as the black in Figure 20, which exhibits a shape far from the observations. We find that the existence of the radiative atmosphere enlarges the planet radii for low-mass planets by 20%–30%, which shifts the peaks from 1.5–2.0 R ⊕ to a more reasonable 2.0–2.5 R ⊕.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: The evolution of radius and envelope mass fraction between a H/He (black) and a pure H2 (gray) atmosphere, for our nominal planets that have 3 M ⊕ cores with 5% initial mass fractions and 100 F ⊕ insolations, both with the physics improved. A pure H2 atmosphere assumed in GSS18 is much more susceptible to the isothermal Parker wind as discussed in the text. The plot is based on the GSS18 analytical model, but a similar effect also affects other models with the isothermal Parker wind, including our numerical model.
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: By varying the envelope mass fraction, we show the total energy difference (black) of adiabatic envelopes between steps and compare it to the analytical estimate that corresponds to the energy needed to lift H/He mass from the surface of the planet (RCB). The agreement between the two quantities is consistent with our analytical assessment in Equation (17).
Paper: Assessing Core-powered Mass Loss in the Context of Early Boil-off: Minimal Long-lived Mass Loss for the Sub-Neptune Population
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay
Figure caption: From our implementation of the analytical model, we show the distribution of the final planet radius and envelope mass fraction with (blue) and without (black) mass loss using the same original GSS18 analytical setup. A similar bimodal distribution is replicated.
Paper: X-Ray Spectra of Black Hole X-Ray Binaries with Returning Radiation
Authors: Temurbek Mirzaev, Cosimo Bambi, Askar B. Abdikamalov, Jiachen Jiang, Honghui Liu, Shafqat Riaz, Swarnim Shashank
Figure caption: Synthetic reflection spectra of the whole disk as observed far from the source. The inclination angle of the disk with respect to the line of sight of the observer is i = 45°. Yellow solid curves describe the Comptonized spectra from the corona. Black solid curves describe the thermal spectra of the disk. Blue dashed curves describe the reflection spectra produced by the direct radiation from the corona and the returning radiation of the thermal spectrum of the disk (i.e., we do not include higher-order disk reflection). Red dashed curves are for our final results for the reflection spectra (i.e., we include higher-order disk reflection). In the top panels, the Eddington-scaled luminosity of the source is λ = 0.01. In the bottom panels, we have λ = 0.1. In the left panels, the luminosity of the source is dominated by the corona (ρ = L corona/L disk = 100). In the right panels, there is no corona, and therefore, the reflection spectrum is produced by the returning radiation of the thermal component (ρ = 0). In the central panels, the luminosity of the corona and of the disk are equivalent (ρ = 1). See the text for more details.