adsabs/AstroCLIMB huggingface dataset:
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: Percentage of the parameter space in each cooling case as a function of ϵ  B , ϵ  e , and n for fast (top), slow (middle), and transition cases (bottom) as defined in the text. Colors correspond to the keV fluences of 3.62 × 10−5 erg cm−2 for GRB 181222A (purple), 1.02 × 10−5 erg cm−2 for GRB 170206A (blue), 6.83 × 10−7 erg cm−2 for GRB 170709A (green), and 8.88 × 10−8 erg cm−2 for GRB 180103A (red). Solid lines correspond to the cases considered for the given regime and keV fluences, while dashed lines correspond to the cases consistent with a hypothetical flux upper limit of 10−10 erg cm−2 at 500 GeV.
Paper: Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk
Authors: Weixiang Yu, Gordon T. Richards, Michael S. Vogeley, Jackeline Moreno, Matthew J. Graham
Figure caption: The percentage of DHO fits removed by a cut of S BM > 2.6 as a function of the rest-frame effective wavelength of each photometric band. The shaded areas show the rest-frame coverage of the photometric bands centered at the C IV and Mg II emission lines. Some local peaks can be spotted at the wavelengths of emission lines (or within the shaded regions), e.g., at the C IV line for g and r bands, and at the Mg II line for r and z bands.
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: The 90% upper limits derived by HAWC for the sample of bursts with zenith angle less than 21° vs. the fluence observed during the prompt emission. The corresponding energy ranges are 15–150 keV (Swift-BAT; green), 10–1000 keV (Fermi-GBM; red), and 20–2000 keV (Konus-Wind; blue). HAWC upper limits are derived using a time window of T 90 (the same as referred to the fluence provided by the satellite) and assuming a power-law spectrum with index −0.5 and z = 0.3. The identity function is shown as a black dotted line. We show, from left to right, GRB 150423A, GRB 180103090, GRB 200514380, GRB 150710A, GRB 180617872, GRB 160406503, GRB 190905985, GRB 170709334, GRB 141205A, GRB 170206A, and GRB 181222841.
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: Distribution of the fluence 90% upper limits extracted in the first time window (0–2 s) for the 43 short GRB positions with respect to the zenith angle of the source. All these limits are derived between 80 and 800 GeV assuming a redshift of 0.3 and a spectral index of −0.5. The detector sensitivity is best up to ∼ 20°. Bursts considered in this work and included in this figure are reported in Table 1.
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: HAWC upper limits of the fluence extracted in the energy range 80–800 GeV for the GRB 170206A for different spectral indices and redshifts. The limits are calculated for spectral indices of −0.7 (triangles) and −2.2 (squares) and for redshifts of 0 (black), 0.3 (red), and 1 (blue). The dashed black line is the average flux measured by Fermi-GBM during the prompt emission.
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: Distribution of the significances after trial correction extracted for each GRB of the total sample on the 10 consecutive time windows. It is consistent with a normal distribution. The solid line represents a normal distribution with a mean of 0 and a standard deviation of 1. The normal distribution that fits the significance distribution has a mean of 0.09 ± 0.05 and a standard deviation of 0.95 ± 0.03, shown as a dashed line.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The viscously dissipated power, radiation flux, and the kinetic power tapped into the outflows in the disk as functions of radius. The results calculated with α = 0.1 are plotted in the left panel, while the right panel is 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. The radiation flux ﹩{\tilde{f}}_{\mathrm{rad}}﹩ (solid lines), the viscously dissipated power ﹩{\tilde{Q}}^{+}﹩ (dashed lines), and the kinetic power of the outflows ﹩{\tilde{Q}}_{{\rm{w}}}﹩ (dotted lines) from the unit area of the disk vary with radius with different values of the parameters are plotted. The magenta lines correspond to ﹩{\tilde{f}}_{\mathrm{rad}}={\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}\equiv 2\sqrt{3}/9{r}^{2}﹩. We note red dotted line is absent because ﹩{\tilde{f}}_{\mathrm{rad}}\lt {\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ is always satisfied in the disk, i.e., no outflow is driven from the disk, when ﹩\dot{m}({r}_{\mathrm{out}})=1﹩.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The accretion rates as functions of radius in the disks. The solid and dashed lines correspond to the results calculated with α = 0.1 and 0.3, respectively. The colored lines indicate the results of ﹩{\dot{m}}_{\mathrm{out}}=5﹩ (red), 10 (green), 100 (blue), 500 (cyan), and 1000 (black), respectively. The outer disk radius r out = 1000 is adopted.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The dynamics of the gas motion in the vertical direction of the disk. The left panel: the density distributions of the disk. The black lines indicate the results of ﹩{\tilde{f}}_{\mathrm{rad}}=0.2{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (solid), ﹩0.5{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (dashed), and ﹩{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (dotted), respectively. The colored lines are the results of the disk calculated with ﹩{\tilde{f}}_{\mathrm{rad}}=2{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩. The different values of the vertical optical depth, τ = 100 (red), 1000 (green), and 5000 (blue), are adopted, respectively. The right panel: the vertical velocities of the gas in the disk calculated with different values of τ and ﹩{\tilde{f}}_{\mathrm{rad}}﹩. The solid lines are the cases of τ = 100, while the dashed and dotted lines are for τ = 1000 and 5000, respectively. The results with different values of ﹩{\tilde{f}}_{\mathrm{rad}}﹩ are labeled with different colors, ﹩{\tilde{f}}_{\mathrm{rad}}=1.1{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (red), ﹩2{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (green), ﹩5{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (blue), and ﹩10{\tilde{f}}_{\mathrm{rad}}^{\mathrm{crit}}﹩ (black), respectively.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The rates of the angular momentum carried away by the outflows from the disk region between R and R out. The solid and dashed lines correspond to the cases with α = 0.1 and 0.3, respectively. The colored lines are the results for different accretion rates, ﹩\dot{m}({r}_{\mathrm{out}})=5﹩ (red), 10 (green), 100 (blue), 500 (cyan), and 1000 (black), respectively. The left panel contains the ratios of the angular momentum carried away by the outflows to that of the gas accreted by the BH, while the results normalized to the angular momentum rate of the gas accreted onto the outer edge of the disk r out = 1000 are plotted in the right panel.
Paper: A Supercritical Accretion Disk with Radiation-driven Outflows
Authors: Xinwu Cao, Wei-Min Gu
Figure caption: The specific angular momenta of the gas in the disks as functions of radius. The solid line indicates the angular momentum of the Keplerian rotation, while the dashed lines are the specific angular momentum of the disk with different values of model parameters. The colored lines indicate the results of ﹩{\dot{m}}_{\mathrm{out}}=5﹩ (red), 10 (green), 100 (blue), 500 (cyan), and 1000 (black), respectively. The outer disk radius r out = 1000, and the viscosity parameter α = 0.1, are adopted in the calculations.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Zoom-in on the flares from each observing epoch plotted in absolute flux on the same scale to enable a comparison between epochs. The solid gray lines mark the average flux outside of flare. The dashed gray lines in the Fe XXI plots mark the average flux from the last exposure of the 2015 February visit (i.e., following the candidate dimming). Fe XXI fluxes were computed using the “line ratio” method (green points in Figure 6) and Fe XII fluxes are from direct integration (orange points in Figure 6). Note in the top row that the Fe XXI flux at the start of the 2015 February visit is elevated well above other visits (gray lines), yet declines to a value (dashed line) well below the out-of-flare average for the other visits.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Solar context for the 2015 February event if interpreted as a CME. Black contours give the 1σ and 2σ bounds of solar CMEs. Blue contours give the 1σ and 2σ bounds of the MCMC samples for the Fe XXI+Fe XII mass and kinetic energy of the 2015 February event on ϵ Eri. The 2015 February event is consistent with solar CMEs, albeit on the high end of mass and energy.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Solar CME masses and kinetic energies from the SOHO/LASCO catalog (Gopalswamy et al. 2009) through 2021 January. Power-law fits to data above a threshold (selected by eye) are also shown and the equation of the fit provided in the lower left of each panel. The mass and energy estimates of many events are flagged as unreliable. We fit only the unflagged events, but plot curves both for all events and unflagged events. There was no mass or energy estimate for 41% of events in the LASCO catalog.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: 2017 August epoch, lightcurves of the HST observations from calibration program 15365. Point colors indicate the different methods used to measure the Fe line fluxes as demonstrated in Figures 4 and 5. The black lines are reference lightcurves from summing the flux of two of the brightest FUV lines. Possible dimming profiles explored by the MCMC sampler are shown as the translucent regions, matched to the color of the points fit.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: 2017 March epoch lightcurves of the HST observations from calibration program 14909. Point colors indicate the different methods used to measure the Fe line fluxes as demonstrated in Figures 4 and 5. The black lines are reference lightcurves from summing the flux of two of the brightest FUV lines. Possible dimming profiles explored by the MCMC sampler are shown as the translucent regions, matched to the color of the points fit.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Mass increase when considering a heterogeneous-density distribution of the form ﹩{dV}/{dn}\,\propto \,{n}^{\alpha }﹩ versus the homogeneous-density estimate adopted in the main body of this work. Each curve adopts a different value for α and shows the additional mass as the volume is integrated to increasingly low densities while preserving the observed line ratio. Large y-values mean significant mass could be present that is not accounted for if assuming a homogeneous density of n ref. For α ≤ −2, significant low-density mass could be hidden from a dimming mass estimate.
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: 2017 March epoch, MCMC chains from the fit to the Fe XXI data in Figure 11. Symbols are the pre-flare flux, F pre (10−15 erg s−1 cm−2); CME acceleration, a (m s−2); dimming depth, ﹩{\delta }_{\max }﹩ (relative units); and the white noise hyperparameter, σ (relative units).
Paper: Constraining the Physical Properties of Stellar Coronal Mass Ejections with Coronal Dimming: Application to Far-ultraviolet Data of ϵ Eridani
Authors: R. O. Parke Loyd, James Paul Mason, Meng Jin, Evgenya L. Shkolnik, Kevin France, Allison Youngblood, Jackie Villadsen, Christian Schneider, Adam C. Schneider, Joe Llama, Tahina Ramiaramanantsoa, Tyler Richey-Yowell
Figure caption: Derived ejected emitting masses that could explain the data in Figure 6 if a CME occurred. The left distribution is heavy-tailed and the 95% limit is beyond the plot range. Vertical gray lines are the 18th, 50th, and 84th percentiles.
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 model for Mrk 463. The model shown is the fit with all of the APEC parameters frozen (i.e., the fit that was used to recover the BORUS parameters). Black denotes Chandra observation 4913 of the eastern AGN. Red denotes Chandra observation 4913 of the western AGN. Green denotes Chandra observation 18194 of the eastern AGN. Blue denotes Chandra observation 18194 of the western AGN. Cyan and magenta represent NuSTAR FPMA and FPMB data, respectively. The Chandra observations of Source 1 and Source 2 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: Intrinsic 2–10 keV X-ray luminosities vs. 12 μm luminosities for the galaxies in our sample. The blue squares are the galaxies plotted with observed 2–10 keV luminosities. The black points with error bars use the intrinsic 2–10 keV luminosities. The red line is the mean L 2–10 vs. L 12μm relation for the complete reliable sample in Asmus et al. (2015). The scatter of this relation is 0.33 dex, which is depicted as the light red shaded region. L 2–10 errors were derived from our measurements as explained in Section 4. Errors on L 12μm are derived from the literature.
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 5005. Black denotes XMM-Newton pn data, red denotes XMM-Newton MOS1 data, green denotes XMM-Newton MOS2 data, blue denotes Chandra data, cyan denotes FPMA data, and magenta denotes FPMB data.
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: Intrinsic 2–10 keV X-ray luminosities vs. updated [O III] luminosities for the galaxies in our sample. The intrinsic luminosities are plotted alongside their former positions from Figure 1. The Mrk 463 2–10 keV luminosity is the combined luminosity of the eastern and western AGNs. IC 3639 has been moved slightly to the left to better distinguish it from NGC 6890.