adsabs/AstroCLIMB huggingface dataset:
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: Variation of L0 with respect to different parameters. In the upper left panel, the magenta stars represent the cases with ﹩\dot{m}=1﹩, while the cyan stars correspond to ﹩\dot{m}=0.5﹩. In the other panels, the magenta stars indicate the case of q = 0.003, whereas the cyan stars represent q = 0.01. For all panels, the remaining disk parameters, not explicitly shown, are set to the following values: ﹩\dot{m}=1﹩, α = 0.01, a = 100Rg, and q = 0.003. The dashed lines indicate the power-law model that best fits the values. This figure shows that L0 is a power-law function of q, ﹩\dot{m}﹩, ad, and α, and the power-law index is different for different parameters.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: Disk solutions of gas inflow velocity V, temperature T, specific angular momentum L, as well as viscous torque Tϕr, surface density Σ and scale high H/r, for cases of q = 0 (cyan solid line), q = 0.01 (magenta dashed line), and q = 0.1 (blue dot dashed line). The other disk parameters are ﹩\dot{m}=1﹩, Mp = 108M⊙, a = 100Rg, and α = 0.01.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: The impact of varying q, α, a, and ﹩\dot{m}﹩ on the disk solution of Tϕr. The chosen values for the fiducial disk parameters are q = 3 × 10−3, α = 0.01, Mp = 108M⊙, a = 100Rg, and ﹩\dot{m}=1﹩. In each panel, we illustrate the behavior of Tϕr as only a specific parameter is varied, while keeping all other disk parameters fixed at their fiducial values.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: Radiation efficiency of thin disks vs. slim disks. The disk parameters are set to α = 0.1, Mp = 108M⊙, and ad = 100Rg for the slim disks. A break is inserted in the y-axis from 0.065 to 0.4 for better readability.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: The upper two and the lower left panels show the profiles of V, H/r, and Tϕr, while the lower right panel shows the variation of L0 as the viscous parameter α changes. The disk parameters are Mp = 108M⊙, ﹩\dot{m}=1﹩, a = 200Rg, q = 0.003, and α = 0.01.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: The disk spectra for different q values. The other disk parameters are ﹩\dot{m}=1﹩, Mp = 108M⊙, a = 100Rg, and α = 0.01.
Paper: Detection of the Extended Gamma-Ray Emission around PSR J1627-4706 with Fermi-LAT
Authors: Weixiong Ding, Yang Wang, Xiaolei Guo, Yuliang Xin
Figure caption: The 2° × 2° TS maps for photons above 5 GeV. Left: the excess map by subtracting the components from diffuse backgrounds and 4FGL-DR4 sources. Right: the residual map with an additional extended GeV source being subtracted for SrcX, assuming a 2D-Gaussian spatial template. The maps are smoothed with a Gaussian kernel with σ = 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩02. The green cross indicates the best-fit position for SrcX as a point source. The cyan dashed circle shows the size of R68 for the 2D-Gaussian template. The magenta and white diamonds represent the positions of PSR J1627-4706 and PSR J1624-4721, respectively. The 4FGL-DR4 catalog point sources in this region are marked by the red pluses. The color bar represents the TS value for each pixel.
Paper: Detection of the Extended Gamma-Ray Emission around PSR J1627-4706 with Fermi-LAT
Authors: Weixiong Ding, Yang Wang, Xiaolei Guo, Yuliang Xin
Figure caption: The multiwavelength SED of the gamma-ray source. The top panels are for the leptonic models with the different values of gas density, and the bottom panel is for the hadronic model. The green solid and magenta dashed lines represent the synchrotron component and bremsstrahlung component, respectively. The blue, red, and green dotted lines show the ICS components for the different seed photons. The black solid curve represents the sum of the different radiation components in the gamma-ray band. In the bottom panel, the hadronic component is marked by the red dashed line. The cyan dotted–dashed line shows the differential sensitivity of CTA-South (50 hr; Cherenkov Telescope Array Consortium et al. 2019).
Paper: Detection of the Extended Gamma-Ray Emission around PSR J1627-4706 with Fermi-LAT
Authors: Weixiong Ding, Yang Wang, Xiaolei Guo, Yuliang Xin
Figure caption: Left: the 4.85 GHz radio map from the PMN survey. Right: integrated CO emission intensity (K km s−1) in the velocity range of −91 ∼ −68 km s−1. The green contours show the gamma-ray morphology in this region, and the 68% containment radius is marked by the cyan dashed circle. The magenta diamond represents the positions of PSR J1627-4706.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: Evolution of the binary separation with time. The disk parameters for the fiducial model are Mp = 108M⊙, ﹩\dot{m}=1﹩, α = 0.1, and q = 3 × 10−3. The vertical dotted lines show the critical radius where ﹩{\dot{a}}_{{\rm{tid}}}={\dot{a}}_{{\rm{gw}}}﹩ for the corresponding cases. This plot shows that the disk can help to shrink the separation effectively.
Paper: Detection of the Extended Gamma-Ray Emission around PSR J1627-4706 with Fermi-LAT
Authors: Weixiong Ding, Yang Wang, Xiaolei Guo, Yuliang Xin
Figure caption: The energy density in TeV-emitting PWN or pulsar halo, derived as ﹩{\epsilon }_{e}=\dot{E}{\tau }_{{\rm{c}}}/V﹩, is plotted against the pulsar’s spin-down luminosity (﹩\dot{E}﹩) and characteristic age (τc), following the scaling shown in Figure 2 of G. Giacinti et al. (2020). The color bar indicates the extent of gamma-ray emission for each source. Regions shaded in gray denote energy densities below the typical ISM value of 0.1 eV cm−3. PSR J1627-4706 is marked by the star, and the three identified pulsars halos are denoted by the diamond (Geminga), square (PSR B0656+14), and pentagon (PSR J0622+3749).
Paper: Detection of the Extended Gamma-Ray Emission around PSR J1627-4706 with Fermi-LAT
Authors: Weixiong Ding, Yang Wang, Xiaolei Guo, Yuliang Xin
Figure caption: Left: the SED of SrcX is shown as the black dots. The black arrow indicates the 95% upper limit, and the blue histograms show the TS value for each energy bin. The green solid and dashed lines represent the best-fit power-law spectrum and its 1σ statistical error in the energy range of 500 MeV to 1 TeV, respectively. Right: light curve of SrcX. The red solid and dashed lines represent the mean flux and its 2σ uncertainty range, respectively, derived from the entire dataset.
Paper: A Pseudo-Newtonian Stationary Circumbinary Slim Disk Model
Authors: Sixiang Wen, Vasileios Paschalidis
Figure caption: The impact of varying Bi on the disk solution. The chosen values for the disk parameters are q = 3 × 10−3, α = 0.1, Mp = 108M⊙, a = 300Rg, and ﹩\dot{m}=1﹩.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: z ∼ 7.05–7.15 JWST galaxy number counts around J1120+0641 (navy squares) and in the adjacent field (teal diamonds). For the adjacent field, we show counts incorporating the three medium-confidence candidates as open diamonds. For comparison, we plot very deep z ∼ 7 HST J125 counts in five legacy fields from R. J. Bouwens et al. (2015) in gray, scaled to only reflect galaxies between z = 7.05 and 7.15 (see Section 4.2 for details). Number counts derived from the two C. Simpson et al. (2014) candidates are shown as light green circles. With only HST data, the quasar field appears significantly underdense, but incorporating JWST data reveals a significant overdensity of galaxies at mF150W ≲ 28, beyond which the lack of completeness at the faint end of our sample becomes evident. Markers have been offset horizontally for visual clarity. Counts and errors are calculated via a Monte Carlo method; see Section 4.2 for details.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The SEDs and thumbnail images of the two C. Simpson et al. (2014) LBG candidates that overlap with our JWST data. LBG1 (left SED, upper row of thumbnails) is not picked up in our sample due to its nondetection in F405N. Its SED shape and flux place it at z ∼ 7, but it is likely not associated with the quasar directly. LBG2 (right SED, lower row of thumbnails) is exceedingly bright in the longer NIRCam bands, in agreement with its detection with Spitzer. Like C. Simpson et al. (2014), we believe this galaxy likely lies at z ∼ 2.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The field around J1120+0641, and the narrowband candidates identified. The surveyed JWST field in F410M is shown in black and white, with z ∼ 7 candidates marked with green circles. The footprint of the archival HST F814W observations is also shown, centered on the quasar position, which is marked with a white star. Some sources in the quasar field overlap one another and are indicated (“two sources”). The three candidates in the adjacent field with less certain redshift determinations are marked with lighter green squares. At lower left, we show the transmission curves of the HST/ACS and JWST/NIRCam filters observed, along with an example z = 7.1 spectrum. The [O III] λ5007 line shifts into the NIRCam F405N filter for a narrow redshift range around z ∼ 7.1.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: Examples of galaxies with elevated F405N or F410M that were removed from our sample in the visual inspection process. Candidate 048 (top) is classified as a spurious source: the underlying galaxy certainly exists, but its elevated narrowband flux is likely due to the bright detector artifact visible in the F405N image. Candidate 163 (bottom) is classified as a low-redshift source based on its angular size, brightness, and clearly resolved spiral structure.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The future of J1120+0641’s host galaxy. J1120+0641’s black hole and stellar mass at z = 7.08 is marked with a teal square. The lighter teal polygon marks the region where the host could land at z = 0, up to the maximum possible galaxy mass we derive, 2.5 × 1011 M⊙ (see Table 4). The lower boundary assumes no black hole growth, while the upper boundary assumes the black hole grows at the same rate as the host galaxy. The solid thick gray line is the local relationship between black hole and stellar mass from J. E. Greene et al. (2020), and we show similar relations from J. Kormendy & L. C. Ho (2013) and A. E. Reines & M. Volonteri (2015) as lighter, dashed and dotted–dashed lines respectively. We expect the host galaxy to grow to approximately 6 × 1010 M⊙ in stellar mass: this area of the polygon is shaded darker and labeled. With no further black hole growth and a mass of 6 × 1010 M⊙, J1120+0641 will reach an MBH/M* ratio of ∼2.5% at z = 0, still significantly above the local J. E. Greene et al. (2020) relation.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The fraction of zphot ∈ [7.0, 7.5] galaxies in JADES with an excess in F410M relative to F200W, as a function of F200W magnitude. The number of galaxies in each bin is indicated in white text. Our brightest z ∼ 7.1 source has an F200W magnitude of 26.6: at this magnitude and fainter, almost 100% of JADES sources have an F410M excess indicating the presence of [O III]. Visual inspection reveals that the small number of sources at brighter magnitudes (gray shaded region), which tend not to display this excess, are almost all faint stars with poor photometric redshift fits. Essentially all galaxies at z ∼ 7 have bright lines in our bands of interest, indicating that our narrowband selection does not leave out a significant population of lineless galaxies.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The thirteen z ∼ 7.1 sources detected in the field around J1120+0641 (in order of ID, see Table 1). Each source’s spectral energy distribution is shown in the rest frame in the left panel, along with the Prospector (light green) and Bagpipes (dark blue) best-fit spectra and 16%–84% confidence intervals. On the right are the source’s thumbnails in F814W and our JWST filter set. The narrowband filter F405N is shown in teal. Each band with a positive measured flux has the magnitude in the band listed in the lower right corner of the image.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The flux of J1120+0641’s host galaxy in the rest-UV/optical compared with a set of stellar SED models. The models include measurements from Table 3 (diamonds) compared with a set of stellar SED models (shades of green) to illustrate the low levels of extinction required to fit the data. The models include constant star formation for 350 Myr (from z ≥ 13), AV = 0.03; 250 Myr, 150 Myr, and 85 Myr, AV = 0.1, 0.15, and 0.25 respectively; and 350 Myr with the SFR for the most recent 10 Myr doubled and tripled, AV = 0.15 and 0.25 respectively. To simplify the figure, only the continua (no emission lines) are displayed.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: Three-line fit to the profile of the Hα line. The two broad components and flat continuum are as given by S. E. I. Bosman et al. (2024), where we also obtained the data; we have added a faint unresolved line contributed by the star formation, which reduces the χ2 of the fit. The residuals are shown in the lower panel.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The SED of J1120+0641, shifted to the rest frame. The solid black line is the template SED for a “normal” quasar, while the dashed line shows the behavior of a warm-dust-deficient source (which is identical at λ < 3 μm; J. Lyu et al. 2017). A composite spectrum of J1120+0641 from D. J. Mortlock et al. (2011), M. A. Marshall et al. (2025), and S. E. I. Bosman et al. (2024) is shown in light green. The green diamonds are photometry of the quasar from M. A. Stone et al. (2024) and M. Yue et al. (2024). The template has been fit to the spectrum by least squares in log space.
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The three medium-confidence z ∼ 7.1 sources detected in the adjacent field, as in Figure A1. Unlike the high-confidence sources in Figures A1 and A2, these sources are anomalously bright in the redder bands, leading to steep spectral slopes and high best-fit masses (see Table 1).
Paper: The z = 7.08 Quasar ULAS J1120+0641 May Never Reach a “Normal” Black Hole to Stellar Mass Ratio
Authors: Meredith A. Stone, George H. Rieke, Jianwei Lyu, 建伟 吕, Michael K. Florian, Kevin N. Hainline, Yang Sun, Yongda Zhu
Figure caption: The six high-confidence z ∼ 7.1 sources detected in the adjacent field, as in Figure A1. Because this field is offset from the quasar, these sources do not have archival F814W data.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: Comparisons between MONK and our Geant4 simulated spectra. The MONK simulations are performed under Kerr spacetime, with the geometry that a spherical corona locates above the accretion disk on the spin axis of the BH, the corona temperature is 20 keV, its height is 24 M (G = c = 1), its radial optical depth is 5, its bulk-motion velocity away from the disk plane is 0.4c, the inclination angle is 65°, and the inner radius of the disk is fixed at 6M. The BH parameters are a = 0.9, ﹩\dot{m}=0.1﹩, and M⊙ = 10. The corona radii are 18 M, 6 M, and 3 M in panels (a), (b), and (c), respectively. For Geant4 simulations, the same geometry and parameter values with MONK are shared to make comparisons, except that the spacetime in Geant4 simulations are flat. Additionally, in panel (a), the spectrum of a cylindrical geometry, with its geometry described in Section 2.2, is also plotted. For all simulations in this figure, only disk components and Compton components are calculated, but the reflections are not.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The spectra of return-to-disk photons in the eight radial bins (1Rin–3Rin, 3Rin–7Rin, 7Rin–12Rin, 12Rin–20Rin, 20Rin–30Rin, 30Rin–50Rin, 50Rin–100Rin, and 100Rin–200Rin). Panels (a) to (f) correspond to situations with jet velocities 0c, 0.1c, 0.2c, 0.4c, 0.7c, and 0.99c, respectively.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: A diagram of the simulated geometry, with some parameters marked on.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The densities of positions where return-to-disk photons exit the cylindrical corona on the surface of the corona. The left panel shows the densities at different radii on the bottom side of the cylindrical corona. The right panel shows the densities at different height on the lateral side of the cylindrical corona. The photon number is normalized to the seed photon number. The lines with different colors correspond to simulations with different jet velocities.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The reflection component spectra under different ionization parameters log(xi). The ionization parameter has little effect on the high-energy part of the reflection component spectra.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: A flow chart of the Comptonization MC program.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The unfolded spectrum of Swift J1727.8-1613 observed by Insight-HXMT compared with MC simulation results; the lower panel is the corresponding relative residual. The selected observation is NO. P061433802003, which was during VHS of its 2023 burst. The blue, orange, and green curves represent the low-energy (LE), medium-energy (ME), and high-energy (HE) data, respectively; the solid line, dashed–dotted line, and dotted line denote the MC spectrum, its Compton component, and its disk component, respectively. The mean squared error (MSE) of the log-transformed data is 0.000598, and the corresponding MC parameters are shown in Table 2.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The simulated spectra at inclination angle 85°. The red lines are the thermal component emitted by the accretion disk; the yellow lines are the Compton component; the green lines are the reflection component; the blue lines are the sum of all components, i.e., the observed spectra. Panels (a)–(f) correspond to jet velocity 0c, 0.1c, 0.2c, 0.4c, 0.7c, and 0.99c, respectively.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The simulated spectra at inclination angle 25°. The red lines are the thermal component emitted by the accretion disk; the yellow lines are the Compton component; the green lines are the reflection component; the blue lines are the sum of all components, i.e., the observed spectra. Panels (a)–(f) correspond to jet velocity 0c, 0.1c, 0.2c, 0.4c, 0.7c, and 0.99c, respectively.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The average scattering times and the total scattered photon counts between the cylindrical corona (blue solid line) and the spherical corona (yellow dashed line) under different jet velocities.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: Comparisons of the energy spectra of disk and Compton scattering between disk outer radii of 200Rin and 500Rin, in an energy range 0.1–200 keV. The left panel shows the energy spectra of direct disk radiation without Compton scattering with different outer disk radii. The right panel shows the energy spectra of pure Compton radiations with different outer disk radii.
Paper: Monte Carlo Simulation of the Compton Scattering and Disk Reflection of a Cylinder with Hot Electrons Moving Away from a Black Hole
Authors: Wei Meng, Yuan You, Shuang-Nan Zhang, Jia-Ying Cao
Figure caption: The influences of the jet velocity on return-to-disk photons. The left panel shows the spectra of return-to-disk photons under different jet velocities. The right panel shows the number of return-to-disk photons (red line) under different jet velocities, compared with the number of all scattered photons (blue line).