adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Extent of Fe Kα Emission in Nearby Active Galactic Nuclei Using Multi-order Analysis of Chandra High Energy Transmission Grating Data
Authors: Megan Masterson, Christopher S. Reynolds
Figure caption: Left: simulation results for 10 individual simulations with σ  v  = 750 km s−1 and σ  θ  = 0.″4. Blue dotted lines show the input values of σ  v  and σ  θ . Black data points show the fit values for σ  v  and σ  θ  for each simulation. The red data point shows the fit values σ  v  and σ  θ  for a simultaneous fit to all 10 simulations with σ  v  and σ  θ  fixed to be the same between all simulations. All error bars show 1σ (68%) confidence. Right: calibration factor fits for the same 10 individual simulations with σ  v  = 750 km s−1 and σ  θ  = 0.″4 as in the left panel. The blue dotted line shows f = 1. Black data points show the fit values for f for each simulation. The red data dashed line shows the fit value for f for a simultaneous fit to all 10 simulations. The shaded red area shows 1σ error on this combined fit value for f. All error bars show 1σ (68%) confidence.
Paper: Probing the Extent of Fe Kα Emission in Nearby Active Galactic Nuclei Using Multi-order Analysis of Chandra High Energy Transmission Grating Data
Authors: Megan Masterson, Christopher S. Reynolds
Figure caption: Corner plots for each object in the sample. For each corner plot, the two histogram plots show the posterior distributions for σ  v  and σ  θ . The dashed vertical line shows the median chain value, reported in Table 2. The two dotted vertical lines show the 90% confidence bounds on the velocity widths and spatial extents. The other plot shows the density of chain steps in (σ  v , σ  θ ) space. The lines show lines of constant line width, σ  E,measured, in each order at the median values given in Table 2. The red dashed line corresponds to first order, blue solid line to second order, and orange dotted–dashed line to third order.
Paper: Probing the Extent of Fe Kα Emission in Nearby Active Galactic Nuclei Using Multi-order Analysis of Chandra High Energy Transmission Grating Data
Authors: Megan Masterson, Christopher S. Reynolds
Figure caption: Spectra for all seven objects in our sample with all ObsIDs combined together and corrected for redshift. Black lines with error bars indicate the first-order spectrum, decreased by a factor of 15 to roughly account for the difference in effective areas. Blue and orange lines with error bars indicate the second- and third-order spectra, respectively. For NGC 4151, only the first- and second-order spectra are shown. All first-order spectra are binned to a minimum signal-to-noise ratio of 3. For NGC 3783 and NGC 4151, the higher-order spectra are also binned to a minimum signal-to-noise ratio of 3. For Circinus, the higher-order spectra are binned to a minimum signal-to-noise ratio of 2. Due to low signal-to-noise ratio in the remaining objects, the higher-order spectra in the remaining objects are binned in groups of 5 bins. All binning is done solely for visual purposes in plotting. The models with fit parameters from Tables 2 and 4 averaged over all observations are overplotted in bold.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Comparison of the near-infrared spectra of V1515 Cyg and V1057 Cyg. Light gray and blue lines indicate V1057 Cyg observed with IRTF and NOTCam, respectively. Dark gray and red lines present V1515 Cyg observed with IRTF and NOTCam, respectively.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: FeH features around 1.62 μm. Black and red lines present V1515 Cyg and standard stellar spectrum (Rayner et al. 2009). The IRTF and NOTCam spectra are well matched with M6 and M9 dwarfs, respectively.
Paper: Probing the Extent of Fe Kα Emission in Nearby Active Galactic Nuclei Using Multi-order Analysis of Chandra High Energy Transmission Grating Data
Authors: Megan Masterson, Christopher S. Reynolds
Figure caption: Comparison of the distance of the emitting gas from the black hole, using two different measurements. The black dashed line shows equality between the two estimates. The distances measured by the spatial extent, r  θ , are consistently larger than the distances measured by the velocity width, r  v , under the assumption of gravitational motions for all seven objects in the sample. The values in this figure are reported in Table 2, and two possible explanations for the discrepancy are discussed in Section 4.1.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: CO bandhead of V1515 Cyg (upper spectra) and V1057 Cyg (lower spectra). Dashed lines indicate the integration range for EW.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: BPT diagram for the resolved NGC 5972 map as presented in Figure 11. The dashed line marks the separation between composite and star-forming, as proposed by Kauffmann et al. (2003). The solid line marks the transition between composite and AGN as proposed by Schawinski et al. (2007), and the dotted line marks the separation between Seyfert and LINER, as proposed by Kewley et al. (2001). The colored circles represent every spaxel in Figure 11, with star-forming emission shown in green, composite in blue, LINER in red, and Seyfert in orange.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Moment maps from a one-component Gaussian fit to the emission lines Hα (top panels) and [O III] (bottom panels). Left panels: moment 0 maps (flux distribution). Color bar in 10−17 erg s−1 cm−2 Å−1. Middle panels: moment 1 maps (velocity distribution). Color bar in km s−1. Right panels: moment 2 maps (velocity dispersion). Color bar in km s−1. All the maps are clipped at 3σ.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Resolved BPT diagram of NGC 5972; colors represent different sections of the BPT diagram as described in Figure 10. This map shows that the arms are dominated by Seyfert-like emission and are surrounded by a mixture of LINER-like and composite emission.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption:  V-band extinction map obtained from the Hα-to-Hβ flux ratio. This map shows the presence of a high dust obscuration, in the central region and along the southern arms.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Resolved [N II]/Hα flux ratio map. In this map we observe an excess of Hα over [N II] by a factor of ∼2 in particular knots over the arms (light-blue areas). This may be an indication of star formation in these areas.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Moment maps from the stellar components. Left panel: moment 1 map, showing kinematics dominated by disk rotation with perturbations observed in the N and S directions, color bar units in km s−1. Right panel: moment 2 map, color bar units in km s−1.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Light-weighted stellar age map, color bar in units of Gyr. The distribution of stellar age shows older populations in the central region, while younger populations are observed at larger radii.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Best-fitted ellipticity (top panel) and PA (bottom panel) for every fitted ellipse as a function of the radius in arcseconds. Different values of PA and ellipticity are observed in the inner ∼2.″5, while the values remain more or less constant outside this radius.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Flux distribution map from collapsing the cube around 9000 Å.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Left panels: examples of reduced χ 2 for arms “A,” “B,” and “C” from top to bottom. The reduced χ 2 distribution is shown in color and is obtained from the fitting of the simulation grid over U and n H. The blue stars shows the best values of (U, n H) from model 1, and the red stars are for model 2. Right panels: examples of the difference between emission-line ratios from the model and the CLOUDY simulations, in the same order as the left panels.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Left panel: moment 1 map for the [O III] emission line. Middle panel: kinematic model fitted to a data cube trimmed to contain only the [O III] emission line using the  3D  Barolo routine. The dashed line indicates the mean PA (14°) of the fit, while the dashed ellipse shows the extension of the inner disk. The solid line indicates the PA of the central feature, with the solid black circle indicating the extension of the nuclear feature. Right panel: residual map obtained from subtracting the fitted model from the moment 1 map.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: PVD extracted from the continuum-subtracted data cube along the major (top panel) and minor (bottom panel) axes, centered on the [O III] emission line. Red contours show the PVD from the best-fitted 3D model obtained with the  3D  Barolo routine.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Left panel: moment 1 for the stellar component obtained from the unbinned pPXF run. Middle panel: kinematic rotation model for the stellar component obtained from the 2DFIT task inside the routine  3D  Barolo. Right panel: residual map obtained from subtracting the kinematic model from the moment 1 map. All color bar units are in km s−1. The black star shows the kinematic center, and the black line marks the average PA of 2°.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Moment 0 map for the [S II] emission line; overplotted are the apertures on each arm, in red for arm “A,” yellow for “AT,” green for “B,” and blue for “C.” The color bar is in 10−20 erg s−1 cm−2Å−1 units, with an asinh scale to highlight the faint tidal tails.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Same as the right panel of Figure 14, but zoomed in at the central region.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: PVD extracted along PA = 150°; this angle crosses along the NW and SE arms. The red dots mark the best-fit model for the stellar component, and the blue dots mark the best-fit model for the ionized gas component as fitted to a data cube centered in the [O III] emission line.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Extracted spectra from the apertures shown in the top panel, spectral window centered on [O III] emission line. The x-axis corresponds to velocity in km s−1 and the y-axis to flux in 10−20 erg s−1 cm−2 Å. The red vertical line corresponds to the stellar best-fitted Barolo model, and the dashed vertical line corresponds to the receding velocity.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Moment 1 map for the [O III] emission line; overlaid in black are the apertures used to extract the spectra. Gray contours show the moment 0 distribution for the [O III] emission line.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The cumulative distributions of novae within our ﹩20^{\prime} \times 20^{\prime} ﹩ survey region compared with the cumulative distributions of M31 light from Model P of Courteau et al. (2011). The nova distribution is compared with the disk, bulge, total galaxy, and the best-fit disk+bulge (θ = 0.56) light in the upper left, upper right, lower left, and lower right panels, respectively, with corresponding K-S values comparing the nova and light distributions of ∼0, 0.053, 0.22, and 0.74.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The cumulative distributions of novae within our ﹩36^{\prime} \times 36^{\prime} ﹩ survey region of the 4 m mosaic images compared with the cumulative distribution of M31 light from Model P of Courteau et al. (2011). As with Figure 13, the nova distribution is compared with the disk, bulge, total galaxy, and the best-fit disk+bulge (θ = 0.56) light in the upper left, upper right, lower left, and lower right panels, respectively, with corresponding K-S values comparing the nova and light distributions of ∼0, 0.034, 0.26, and 0.90.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The cumulative nova density from survey A compared with the integrated background light of M31. Top panel: B light from de Vaucouleurs (1958). Bottom panel: R light from Kent (1987). The likelihoods that the nova density matches the background light are 0.57% and 5.5% for the B and R bands, respectively.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The cumulative nova density from survey B compared with the integrated background light of M31. Top panel: B light from de Vaucouleurs (1958). Bottom panel: R light from Kent (1987). The likelihoods that the nova density matches the background light are 1.5% and 10% for the B and R bands, respectively.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The results of our maximum likelihood analysis plotted as a function of the assumed disk-to-bulge nova density, θ. The relative bulge and disk surface brightness profiles are based on model P of Courteau et al. (2011). The analysis has been applied to the wider field 4 m survey (survey B), because its more extensive coverage (﹩36^{\prime} \times 36^{\prime} ﹩) provides a nearly equal balance between M31's bulge and disk populations. The most probable value is ﹩{\theta }_{\max }={0.56}_{-0.17}^{+0.23}﹩.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The spatial distribution of the 50 novae found within our ﹩36^{\prime} \times 36^{\prime} ﹩ field of survey B, superimposed on a DSS2 red image of M31.
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: For illustrative purposes, the flux as a function of time predicted by the SSC model as described in Section 3 is shown for arbitrary values of microphysical parameters for GRB 170206A. Red dashed–dotted, blue dotted, and green dashed lines show the theoretical light curves in the fast-cooling regime assuming different combinations of microphysical parameters ([ε  B  = 1.4 × 10−2, ε  e  = 2.6 × 10−2], [ε  B  = 6.5 × 10−3, ε  e  = 1.3 × 10−2] and [ε  B  = 5.7 × 10−4, ε  e  = 7.1 × 10−3], respectively) and different start times (﹩{t}_{\mathrm{start}}=0﹩, 3, and 11 s, respectively). Slow-cooling regime light curves, plotted with orange solid and black dashed−dotted lines, are derived assuming [ε  B  = 1.9 × 10−4, ε  e  = 8.0 × 10−3] and [ε  B  = 7.8 × 10−6, ε  e  = 4.5 × 10−2], respectively. For all the cases we assume a redshift of z = 0.3, n = 1 cm−3, and the isotropic energy of E iso = 3.6 × 1051 erg. Symbols represent flux upper limits at observation energy of 500 GeV derived from HAWC upper limits for fluences in the energy range of 80−800 GeV. The colors of symbols correspond to different spectral index assumptions: red for 0.7, green for 1.5, blue for 1.7, and violet for 2.2.
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: A comparison of similar variability signatures extracted by DHO and DRW. The black solid lines in each panel show the one-to-one correspondence. Top left: σ DHO vs. σ DRW; both characterize the asymptotic variability amplitude of the modeled system. Top right: driving white-noise amplitude (σ  ϵ ) of DHO and of DRW. Bottom left: τ decay of DHO vs. τ DRW; both report the e-folding decay timescale of its autocorrelation function. Bottom right: τ decay/τ perturb of DHO vs. τ DRW.