adsabs/AstroCLIMB huggingface dataset:
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: VPDs of the PMs measured in the NGC 346–N66 region. Each point corresponds to the PM of one star. Only stars that meet the astrometry and photometry selection criteria are considered. Measurement using the F555W filter are shown in the left panel. The corresponding results for the F814W filter are shown in the right panel. Median errors along the X and Y directions are shown in the upper-right corner.
Paper: Constraints on the Very High Energy Gamma-Ray Emission from Short GRBs with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, K. P. Arunbabu, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Brisbois, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, S. Coutiño de León, C. de León, E. De la Fuente, R. Diaz Hernandez, S. Dichiara, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, N. Fraija, A. Galván-Gámez, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, B. Hona, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, A. Iriarte, V. Joshi, S. Kaufmann, A. Lara, W. H. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, S. S. Marinelli, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, R. Noriega-Papaqui, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, Z. Ren, C. D. Rho, D. Rosa-González, M. Rosenberg, J. R. Sacahui, H. Salazar, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, R. W. Springer, P. Surajbali, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou
Figure caption: Allowed density of the surrounding medium as a function of microphysical parameters related to the energy given to amplify the magnetic field (top panels) and to accelerate electrons (middle panels) and the energy given to accelerate electrons as a function of the energy to amplify the magnetic field (bottom panels), from left to right columns for GRB 181222A and GRB 170206A. Color scale indicates the percentage of cases remaining from the total cases per bin in the fast-cooling regime.
Paper: Constraints on the Very High Energy Gamma-Ray Emission from Short GRBs with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, K. P. Arunbabu, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Brisbois, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, S. Coutiño de León, C. de León, E. De la Fuente, R. Diaz Hernandez, S. Dichiara, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, N. Fraija, A. Galván-Gámez, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, B. Hona, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, A. Iriarte, V. Joshi, S. Kaufmann, A. Lara, W. H. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, S. S. Marinelli, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, R. Noriega-Papaqui, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, Z. Ren, C. D. Rho, D. Rosa-González, M. Rosenberg, J. R. Sacahui, H. Salazar, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, R. W. Springer, P. Surajbali, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou
Figure caption: Same as Figure 7, but for the slow-cooling regime.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The continuum spectra of the disks (left panel: M = 10 M ⊙, right panel: M = 108 M ⊙). The solid lines are the results calculated with α = 0.1, while the dashed lines are for α = 0.3. The colored lines correspond to different accretion rates at the outer radius r out = 1000: ﹩\dot{m}({r}_{\mathrm{out}})=1﹩ (red), 10 (green), 100 (blue), and 1000 (black), respectively.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The Eddington ratios of the disk as functions of the accretion rate at the outer radius of the disk r out = 1000 (black lines). The red lines indicate the least radiation power required to accelerate the gas from the disk surface to infinity. The solid lines indicate the results calculated with α = 0.1, while the dashed lines are for α = 0.3.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The properties of the disk-outflow systems with different values of α. The black lines are the results with α = 0.1, while the colored lines indicate the results for α = 0.05 (red), 0.3 (green), and 0.5 (blue). The calculations are carried out with ﹩\dot{m}({r}_{\mathrm{out}})=20﹩ and r out = 1000. The left panel: the radiation flux ﹩{\tilde{f}}_{\mathrm{rad}}﹩ (solid lines) and the kinetic power ﹩{\tilde{Q}}_{{\rm{w}}}﹩ tapped into the outflows (dotted lines) in the disk as functions of radius. The right panel: the vertical velocity v  z (H) of the gas at the disk surface z = H.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The continuum spectra of the disks surrounding BHs with M = 106 M ⊙. The solid lines indicate the disk spectra calculated with α = 0.1, while the dashed lines are for the spectra calculated with α = 0.3. The colored lines correspond to different accretion rates at the outer radius r out = 100: ﹩\dot{m}({r}_{\mathrm{out}})=1﹩ (red), 5 (green), 10 (blue), and 30 (black), respectively.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The properties of the disk-outflow systems with different values of γ. The black lines are the results with γ = 1.5, while the red and green lines are for γ = 1.4 and 1.6, respectively. The calculations are carried out with ﹩\dot{m}({r}_{\mathrm{out}})=20﹩, r out = 1000, and α = 0.1. The left panel: the radiation flux ﹩{\tilde{f}}_{\mathrm{rad}}﹩ (solid lines) and the kinetic power ﹩{\tilde{Q}}_{{\rm{w}}}﹩ tapped into the outflows (dotted lines) in the disk as functions of radius. The right panel: the vertical velocity v  z (H) of the gas at the disk surface z = H.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The fraction of radial energy advection f adv = Q adv/Q + varying with the radius of the disk. The results calculated with α = 0.1 are plotted as solid lines, while the dashed lines are for the results with α = 0.3. The colored lines are the results for different accretion rates, ﹩\dot{m}({r}_{\mathrm{out}})=1﹩ (red), 5 (green), 10 (blue), 100 (cyan), and 1000 (black), respectively.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The accretion rate ﹩{\dot{m}}_{\mathrm{out}}﹩ and the Eddington ratio λ evolve with time in the TDEs. The dotted line indicates the accretion rate at the outer radius of the disk evolving with time as ∝t −5/3. The solid line is the light curve of the disk emission with α = 0.1, while the dashed line is for the disk with α = 0.3. The outer radius of the disk r out = 100 is adopted in the calculations.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The vertical velocity v  z (H) of the gas at the disk surface z = H. The results calculated with α = 0.1 are plotted as solid lines, while the dashed lines are for the results with α = 0.3. The colored lines are the results for different accretion rates, ﹩\dot{m}({r}_{\mathrm{out}})=5﹩ (green), 10 (blue), 100 (cyan), and 1000 (black), respectively.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for NGC 4501. Black denotes Chandra data and the model for the AGN core. Red and green denote FPMA and FPMB data, respectively, and models for NuSTAR observation 60375002002, while blue and cyan denote FPMA and FPMB data, respectively, and models for NuSTAR observation 60375002004. The Chandra data and models for the extra point sources are depicted in light gray.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Chandra and NuSTAR FPMA (ObsID: 60375002002) images of NGC 4501. The larger, 40″ radius circle denotes the NuSTAR extraction region, while the smaller circles denote the Chandra extraction regions. Eight off-nuclear point sources are visible in the Chandra image; all but Src 5 are sufficiently bright that they are included in the X-ray spectral fitting.
Paper: NuSTAR Observations of AGNs with Low Observed X-Ray to [O III] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?
Authors: M. Lynne Saade, Murray Brightman, Daniel Stern, Matthew A. Malkan, Javier A. García
Figure caption: Unfolded spectrum and best-fit model for NGC 4922. Black, red, and green denote Chandra data (ObsIDs 4775, 15065, and 18201, respectively), while blue and cyan denote FPMA and FPMB data, respectively.