adsabs/AstroCLIMB huggingface dataset:
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The density (left panels) and temperature (right panels) distribution near the BH (yellow dot) at four different times. Note the stationary spiral shock structure that appears around 2t 0.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The distribution of the total energy E + E therm, normalized by the local gravitational potential E grav = − GM •/r, at ϕ = 0° (left, near the nozzle shock) and 180◦ (right, near the apocenter shock) at t = 3t 0.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: Circularization efficiency η, defined in Equation (8), as a function of time. The red line shows the time average of η, estimated as ﹩\eta (t)={\int }_{0}^{t}{{dt}}^{{\prime} }\eta ({t}^{{\prime} })/{\int }_{0}^{t}{{dt}}^{{\prime} }﹩.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The temperature distribution (left) at t = t 0 in the equatorial plane. The right panel shows a zoom-in of the region demarcated by the green box in the left panel near where two streams collide. The arrows indicate the motion of gas. Notice the different color scales in the left and right panels.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: SEDs sorted into five panels based on UV and MIR emission properties (see Table 2). Each SED is normalized at rest-frame wavelength 1 μm and colored by the intrinsic 0.5–10 keV X-ray luminosity. The numbers indicate the number of AGNs in each panel and their percentage of the total sample. From top to bottom, the UV and MIR slopes change from falling to rising. Note: 8 sources out of 1246 (0.6%) are not included, as they fall outside the continuum slope limits, likely due to noise in the photometric data. Removing these sources has little no effect on the total analysis, as they are such a small fraction of the total sample.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The 0.25 μm (top), 6 μm (middle), and 100 μm (bottom) as a function of the intrinsic 0.5–10 keV X-ray luminosity for all 1246 AGNs in the sample. The black squares show the median X-ray luminosity in bins of 0.5 dex along the x-axis. The vertical error bars show the 25th–75th percentile spread in each bin, and the horizontal error bars show the width of the bin. The black dashed line is a fit to these median points. The blue line shows the relation between the X-ray and UV luminosity from Just et al. (2007), derived from unobscured AGNs. The red line shows the relation between the X-ray luminosity and the 6 μm luminosity derived from Stern (2015). The upper limits in the FIR are shown by downward-pointing arrows, and the crosses show the sources from Stripe 82X that utilize image stacking. The emission at shorter wavelengths (UV–MIR) is AGN dominated in this sample, though the UV is heavily affected by dust. The weaker correlation at 100 μm likely means that this emission is not entirely dominated by the AGN across the full luminosity range.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The SEDs normalized at 1 μm for the sources within our sample that match the criteria outlined in Section 3.1 and Table 1. The color of each SED is the intrinsic 0.5–10 keV X-ray luminosity. The solid black line is interpolation of the median SED in the X-ray and in the UV−MIR region. The dashed black line is the interpolation of the median SED of the detections and the 1σ upper limits in the FIR normalized at 1 μm. The normalized FIR upper limits for individual sources are shown in gray. A wide range of emission properties in the X-ray, UV, MIR, and FIR can be seen around the total median SED.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: SEDs separated into three bins of increasing intrinsic 0.5–10 keV X-ray luminosity. Each SED is normalized at 1 μm, with the normalization of other bins scaled to the normalization of the central bin. The color of each SED is the intrinsic 0.5–10 keV X-ray luminosity with the same color bar found in Figure 3. The solid black line is the median SED for the sources in each bin. The dashed black line is the median of the detections and the 1σ upper limits. The FIR upper limits for individual sources are shown in gray. An evolution in the median SED can be seen with L X; however, a large spread in the range of each emission property is still visible in each bin.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Distributions of intrinsic X-ray luminosity for AGNs in each panel from Figure 12. The dashed black line shows the median X-ray luminosity of each panel. A clear trend can be seen, with the mean X-ray luminosity decreasing from the first panel to the fourth and fifth panels.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The X-ray bolometric correction, L bol/L X, as a function of the integrated bolometric luminosity. The black squares show the mean in bins of L bol, with the error bars showing the 1σ spread in the y-direction and the width of the bin in the x-direction. The red and blue lines show bolometric corrections derived by Duras et al. (2020) and Hopkins et al. (2007), respectively. The average bolometric luminosity calculated in this work is systematically higher at high bolometric luminosities than the literature values.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The distribution of obscuring column density, N H, for the measured estimates (∼56% of the sample) and the upper limits (∼32% of the sample). The total sample is shown in gray, while the measured estimates are shown as the hatched histogram. Most show signs of moderate to heavy obscuration.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Median SEDs for the five panels shown in Figure 12. The FIR median lines include the 1σ upper limits for sources without FIR detections. The gray line shows an unobscured AGN template from Assef et al. (2010). Sources from the third through fifth panels have similar 1 μm luminosities, while the second and first panel sources have increasingly larger 1 μm luminosities, likely due to contributions from the AGN. Sources from the first panel are more luminous at all wavelengths from the X-ray to MIR than the sources from the other four panels.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Distributions of 1 μm luminosities for the 1246 AGNs in our sample, separated according to the five SED shapes defined in Table 2 and shown in Figure 12. The median redshift of each panel is displayed in each panel, and the dashed black line shows the median 1 μm luminosity of each panel. The sources in the first panel have 1 μm luminosities 3 times higher than the other panels, indicating AGN dominance.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The distribution of the total bolometric luminosity found by integrating the X-ray to FIR SED of each AGN. The black dashed line shows the mean of log L bol/(erg s−1) = 45.2 distribution, and the shaded region shows the 1σ spread ±0.51 dex.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: SEDs separated into three redshift bins. Each SED is normalized at 1 μm, with the normalization of each bin scaled to the normalization of the central bin. The color of each SED is the intrinsic 0.5–10 keV X-ray luminosity with the same color bar found in Figure 3. The solid black line is the median SED for the sources in each bin. The dashed black line is the median of the detections, stacked fluxes, and 1σ upper limits in the FIR. The FIR upper limits for individual sources are shown in gray. No major change in the median SED can be seen between the three redshift bins.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The intrinsic 0.5–10 keV X-ray luminosity as a function of spectroscopic redshift for the sources in the AHA survey. The red crosses are the sources from the largest and shallowest layers of the wedding cake, the Stripe 82X survey; the blue plus signs are from the middle layer, COSMOS; and the gray circles are from the GOODS-N/S fields. Only sources with confirmed multiwavelength counterparts that have been observed with Herschel are shown.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Distribution of the 1 μm luminosities for the 1246 AGNs in our sample separated into three redshift bins. The mean of each distribution is shown as a vertical dashed line with the same corresponding color as the histogram (log L 1 μm/(erg s−1) = 44.02, 44.27, and 44.42 for each redshift bin in increasing order).
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: A distribution of the 1 μm luminosities for the 1246 AGNs in our sample. The mean of the distribution is shown as a vertical dashed line, and the shaded region shows the 1σ spread about the average. The 1σ distribution spans ± 0.46 dex around the mean of log L(1μm)/(erg s−1) = 44.2.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: Left: the photosphere temperature distribution dL/dT at four different times t/t 0 = 0.5, 1, 2, and 3. Right: the angular distribution of the temperature at t = 3t 0.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: Radial total energy (E + E therm) flux integrated over a spherical shell at given r, normalized by the Eddington luminosity L Edd, at four different times. Positive values mean net positive (or negative) energy carried by gas moving radially outward (or inward).
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Histogram of the intrinsic 0.5–10 keV X-ray luminosity for the 1246 sources in our final sample. The gray histogram is the total sample; the histograms of the sources from each AHA field (Stripe 82X—red; COSMOS—blue; GOODS-N/s—black) are also shown. The median of each distribution from the respective AHA fields is shown as a vertical dashed line in the same corresponding color.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The azimuthally integrated density distribution at t/t 0 = 0.5, 1, 2, and 3.
Paper: Shocks Power Tidal Disruption Events
Authors: Taeho Ryu, Julian Krolik, Tsvi Piran, Scott C. Noble, Mark Avara
Figure caption: The rate at which gas is expelled through the inner radial boundary at r = 40r g, divided by ﹩{\dot{M}}_{0}﹩, as a function of t/t 0.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Top: ratio of UV (0.1–0.36  μm) to total bolometric luminosity as a function of bolometric luminosity, for the AHA AGN sample. Sources are colored according to their panel in Figure 12; medians are shown as large circles, and error bars indicate the 75th and 25th percentiles of the distributions. Middle: same as the top panel, but for MIR luminosity (3–30  μm). Bottom: same as the other two panels, but for FIR luminosity (30–500  μm). The upper limits in the FIR are shown by downward-pointing arrows, and the crosses show the sources from Stripe 82X that utilize image stacking.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Ratio of UV (top), MIR (middle), and FIR (bottom) luminosity to intrinsic 0.5–10 keV X-ray luminosity as a function of intrinsic 0.5–10 keV X-ray luminosity. Colors correspond to the five panels in Figure 12. The median of each of the five panels is shown as a large circle, and error bars show the 75th and 25th percentiles of each distribution. The dashed line in the bottom panel is a fit to the data. The upper limits in the FIR are shown by downward-pointing arrows, and the crosses show the sources from Stripe 82X that utilize image stacking.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Left: distributions of the calculated bolometric luminosity (integrated X-ray to FIR minus the galaxy contribution) for AGNs in each panel from Figure 12. The dashed black line shows the median of each panel. A clear trend can be seen as the median bolometric luminosity decreasing from the first panel (blue) to the fifth panel (red). Right: ratio between the calculated AGN bolometric luminosity and intrinsic X-ray luminosity as a function of the SED shape defined in Table 2. The dashed black line shows the median ratios of each panel. This ratio is remarkably constant, independent of SED shape, indicating that X-ray luminosity is an excellent marker of total AGN power—and that accretion power dominates the energetics of these sources.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Ratio of UV (0.25  μm) luminosity to MIR (6  μm) luminosity as a function of MIR (6  μm) luminosity. Sources are colored based on which of the five panels in Figure 12 they fall into. The median of each of the five panels is shown as a large circle with the corresponding color for each panel, with the error bars showing the 75th and 25th percentiles of the distribution for each panel. Sources in the third panel have significantly weaker UV emission for a given MIR emission compared to the rest of the sample, likely driven by obscuration around the SMBH.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: The distributions of the estimated column density, N H, for sources in each panel from Figure 12. The dashed black line is the median column density in each distribution for each panel. The total sample is shown in each respective color, while the measured estimates, without upper limits, are shown as the hatched histograms. AGNs from the first and second panels are mostly unobscured, while sources in the bottom three panels show a wide range of N H values, from unobscured to Compton-thick.
Paper: The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei
Authors: Connor Auge, David Sanders, Ezequiel Treister, C. Megan Urry, Allison Kirkpatrick, Nico Cappelluti, Tonima Tasnim Ananna, Médéric Boquien, Mislav Baloković, Francesca Civano, Brandon Coleman, Aritra Ghosh, Jeyhan Kartaltepe, Michael Koss, Stephanie LaMassa, Stefano Marchesi, Alessandro, Peca, Meredith Powell, Benny Trakhtenbrot, Tracey Jane Turner
Figure caption: Top: stacked images of the first three bins from the 250 μm images. Bottom: histograms of the flux measurements made from 10,000 bootstrapped stacks for the corresponding images in the top row.