adsabs/AstroCLIMB huggingface dataset:
Paper: Directly Tracing Cool Filamentary Accretion over >100 kpc into the Interstellar Medium of a Quasar Host at z = 1
Authors: Sean D. Johnson, Joop Schaye, Gregory L. Walth, Jennifer I-Hsiu Li, Gwen C. Rudie, Hsiao-Wen Chen, Mandy C. Chen, Benoît Epinat, Massimo Gaspari, Sebastiano Cantalupo, Wolfram Kollatschny, Zhuoqi (Will) Liu, Sowgat Muzahid
Figure caption: Summary of the redshift survey and galaxy group hosting TXS 0206−048. The grayscale image displays the reduced, coadded HST ACS+F814W image of the field centered on TXS 0206−048 with orientation and scale marked at the bottom right. The full ﹩1^{\prime} \times 1^{\prime} ﹩ MUSE FoV is marked by the black square with solid outline, and the 40″ × 40″ region shown in Figure 1 is marked with a dashed line. Galaxies in the group hosting TXS 0206−048 are labeled with red circles and labeled by their ID and velocity in km s−1 from Table 1. The approximate luminosity-weighted group center is marked with an asterisk. Galaxies with secure redshifts but foreground and background to the quasar host group are marked with blue and orange dashed symbols, respectively. The inset panel at the top right displays the line-of-sight velocity histogram for group members, including TXS 0206−048, with a black, solid line, while the best-fitting Gaussian with a mean line-of-sight velocity of μ = −130 km s−1 and a line-of-sight velocity dispersion of σ = 550 km s−1 is shown with a dashed gray line. The 1.4 GHz radio image from the FIRST survey is shown in the top right inset panel and confirms the core-dominated nature of this radio-loud quasar.
Paper: Directly Tracing Cool Filamentary Accretion over >100 kpc into the Interstellar Medium of a Quasar Host at z = 1
Authors: Sean D. Johnson, Joop Schaye, Gregory L. Walth, Jennifer I-Hsiu Li, Gwen C. Rudie, Hsiao-Wen Chen, Mandy C. Chen, Benoît Epinat, Massimo Gaspari, Sebastiano Cantalupo, Wolfram Kollatschny, Zhuoqi (Will) Liu, Sowgat Muzahid
Figure caption: Line-of-sight velocity of the Host nebula and N filament as a function of projected distance from the quasar compared with nearby galaxies. Points corresponding to the Host nebula are shown as blue pentagons and those corresponding to the N filament are shown as red squares. The N filament measurements are made following the filament contours seen in Figure 1 with 0.″6–1.″2 radius extraction apertures depending on the width of the filament at each location. The measurements for the Host nebula are made moving north from the quasar toward the N filament with 0.″6 radius extractions. Galaxies G2, G6, G9, and G11 overlap spatially with the N filament and their stellar velocities vs. projected distances are shown in black circles in the bottom panel for comparison with the nebulae the quasar marked by a blue star. Despite their spatial coincidence seen in Figure 1, the line-of-sight [O II] velocities of the N filament differ from nearby galaxies by ≳300 km s−1. The luminosity-weighted group velocity is indicated by the red dashed line.
Paper: Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744 
Authors: E. Vanzella, M. Castellano, P. Bergamini, T. Treu, A. Mercurio, C. Scarlata, P. Rosati, C. Grillo, A. Acebron, G. B. Caminha, M. Nonino, T. Nanayakkara, G. Roberts-Borsani, M. Bradac, X. Wang, G. Brammer, V. Strait, B. Vulcani, U. Meštrić, M. Meneghetti, F. Calura, Alaina Henry, A. Zanella, M. Trenti, K. Boyett, T. Morishita, A. Calabrò, K. Glazebrook, D. Marchesini, S. Birrer, L. Yang, T. Jones
Figure caption: Color composition of JWST/NIRISS imaging of a portion of the cluster A2744 (the bands used for the red, green, and blue channels are indicated at the top right). The highly magnified arclet is marked with a green rectangle in the main panel, along with its zoomed version (bottom left insets) where the compact star clusters, 3.1a, 3.2a, 3.3a and 3.1b, 3.2b, 3.3b are shown. The two red contours mark the locus for magnification ×100 bottom left inset, from top to bottom: the color image based on HST bands, the JWST/NIRISS color image, and the HST/F814W image with the green lines marking the locations at magnification μ  TOT  = 30 and 100; black crosses indicate the observed position of the knots and the red circles the predicted position from the lens model (Bergamini et al. 2022). Bottom right inset: the same color images are shown for the counterimage 3c. Top inset: the VLT/MUSE spectrum of the arclet reporting some of the relevant absorption and emission lines.
Paper: Early Results from GLASS-JWST. VI. Extreme Rest-optical Equivalent Widths Detected in NIRISS Wide Field Slitless Spectroscopy
Authors: K. Boyett, S. Mascia, L. Pentericci, N. Leethochawalit, M. Trenti, G. Brammer, G. Roberts-Borsani, V. Strait, T. Treu, M. Bradac, K. Glazebrook, A. Acebron, P. Bergamini, A. Calabrò, M. Castellano, A. Fontana, C. Grillo, A. Henry, T. Jones, D. Marchesini, C. Mason, A. Mercurio, T. Morishita, T. Nanayakkara, P. Rosati, C. Scarlata, E. Vanzella, B. Vulcani, X. Wang, C. Willott
Figure caption: NIRISS/WFSS Grizli-extracted 2D and 1D spectra for three example galaxies in our sample with large [O III]λ5007 EWs (these measurements are described in Section 3), to first demonstrate the typical high-quality spectra and then to show how far we can push the NIRISS data. In the 1D panels we mark the location of ≥5σ (dark blue) and ≥3σ (light blue) detected emission lines. Top: a galaxy with strong detections in each rest-optical emission line; ID 2707 (z = 1.82) with a rest-frame [O III]λ5007 EW = 1003 ± 37 Å. The quality of these NIRISS spectra also allows the detection of weaker rest-optical lines including Ne III]λ3869], Hδ, and the blended Hγ+[O III]λ4363. Middle: the galaxy in our full sample with the largest EW; ID 2314 (z = 2.93) with a rest-frame [O III]λ5007 EW = 1901 ± 787 Å. Here the EW signal-to-noise is <5, although we note both the line and broadband continuum are detected above this threshold. Bottom: the faintest galaxy (F150W total mag = 29.1 ± 0.2) in our full sample with a [O III]λ5007 EW measurement; ID 683 (z = 3.23) with a rest-frame [O III]λ5007 EW = 446 ± 109 Å.
Paper: Early Results from GLASS-JWST. VI. Extreme Rest-optical Equivalent Widths Detected in NIRISS Wide Field Slitless Spectroscopy
Authors: K. Boyett, S. Mascia, L. Pentericci, N. Leethochawalit, M. Trenti, G. Brammer, G. Roberts-Borsani, V. Strait, T. Treu, M. Bradac, K. Glazebrook, A. Acebron, P. Bergamini, A. Calabrò, M. Castellano, A. Fontana, C. Grillo, A. Henry, T. Jones, D. Marchesini, C. Mason, A. Mercurio, T. Morishita, T. Nanayakkara, P. Rosati, C. Scarlata, E. Vanzella, B. Vulcani, X. Wang, C. Willott
Figure caption: Left panel: the 1 < z < 3.4 NIRISS spectroscopic redshift distribution of 76 galaxies with NIRISS detections (>5σ) of Hα, [O III], Hβ, or [O II]. The distribution is split into three colors based on the set of emission lines that are covered by the observations at different redshifts (e.g., [O II] is only visible at z > 1.7 and Hα at z < 2.4). We note an apparent overdensity of 21 independent galaxies in the range 1.33 < z < 1.37. Right panel: the comparison of the NIRISS Grizli-derived and input spectroscopic redshifts, color coded by the number of >5σ NIRISS line detections. Excellent agreement is found in the sample, with the majority of targets having their previous redshifts confirmed through multiple NIRISS line detections. Only two galaxies (NIRISS ID:2808 and 1911, Δz > 0.5) are found to have previously misidentified redshifts solutions.
Paper: Early Results from GLASS-JWST. VI. Extreme Rest-optical Equivalent Widths Detected in NIRISS Wide Field Slitless Spectroscopy
Authors: K. Boyett, S. Mascia, L. Pentericci, N. Leethochawalit, M. Trenti, G. Brammer, G. Roberts-Borsani, V. Strait, T. Treu, M. Bradac, K. Glazebrook, A. Acebron, P. Bergamini, A. Calabrò, M. Castellano, A. Fontana, C. Grillo, A. Henry, T. Jones, D. Marchesini, C. Mason, A. Mercurio, T. Morishita, T. Nanayakkara, P. Rosati, C. Scarlata, E. Vanzella, B. Vulcani, X. Wang, C. Willott
Figure caption: Rest-optical EW properties of 1 < z < 3.4 SFGs. Left: the [O III]λ5007 rest-frame EW distribution of galaxies with NIRISS-detected (≥5σ) line emission. Stacked histograms show ≥5σ EW measurements (blue) and 5σ upper limits (orange), divided between 10 bins of equal logarithmic width. Right: the comparison of Hβ and [O III]λ5007 EWs, restricted to objects where both have ≥5σ measurements (in orange). We report a positive trend, in agreement with the overlaid z ∼ 2 galaxy sample presented by Tang et al. (2021b, 2022; in gray). We also overlay the best-fit curve (green) for the z ∼ 2.3 Sanders et al. (2020) sample, who utilize a second-order polynomial function. We use a linear function to model our data, which are shown in orange accompanied by the 2σ uncertainty for our data.
Paper: Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744 
Authors: E. Vanzella, M. Castellano, P. Bergamini, T. Treu, A. Mercurio, C. Scarlata, P. Rosati, C. Grillo, A. Acebron, G. B. Caminha, M. Nonino, T. Nanayakkara, G. Roberts-Borsani, M. Bradac, X. Wang, G. Brammer, V. Strait, B. Vulcani, U. Meštrić, M. Meneghetti, F. Calura, Alaina Henry, A. Zanella, M. Trenti, K. Boyett, T. Morishita, A. Calabrò, K. Glazebrook, D. Marchesini, S. Birrer, L. Yang, T. Jones
Figure caption: Cutouts of the arclet as observed with HST, JWST, and VLT filters. Small circles in the bottom left corner indicate the PSF size in each instrument/band (for Hubble and VLT they are taken from Merlin et al. 2016, whereas for JWST the PSFs are estimated with available nonsaturated stars).
Paper: Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744 
Authors: E. Vanzella, M. Castellano, P. Bergamini, T. Treu, A. Mercurio, C. Scarlata, P. Rosati, C. Grillo, A. Acebron, G. B. Caminha, M. Nonino, T. Nanayakkara, G. Roberts-Borsani, M. Bradac, X. Wang, G. Brammer, V. Strait, B. Vulcani, U. Meštrić, M. Meneghetti, F. Calura, Alaina Henry, A. Zanella, M. Trenti, K. Boyett, T. Morishita, A. Calabrò, K. Glazebrook, D. Marchesini, S. Birrer, L. Yang, T. Jones
Figure caption: The direct image of image 3c (NIRISS/CLEAR; left) and the detection of [OII]λ3727,3729 despite nearby contamination from other galaxies. The redshift of image 3c is consistent with the counterimages 3a and 3b.
Paper: SKYSURF-3: Testing Crowded Object Catalogs in the Hubble eXtreme Deep Field Mosaics to Study Sample Incompleteness from an Extragalactic Background Light Perspective
Authors: Darby M. Kramer, Timothy Carleton, Seth. H. Cohen, Rolf Jansen, Rogier A. Windhorst, Norman Grogin, Anton Koekemoer, John W. MacKenty, Nor Pirzkal
Figure caption: Left column: histograms of object counts per ﹩\tfrac{1}{2}﹩ mag bin per deg2 for the F435W, F606W, and F775W original and replicated images up to their completeness limits. AX Rep refers to the integer A replications of the XDF data, and AxXDF refers to that integer times the original XDF bin counts. Points are located at the centers of their bins. Spline fits show the general trends, and counts are plotted and listed up to their faintest complete magnitudes for the individual filters (e.g., up to m AB = 29 mag for F606W). Right column: the ratios per ﹩\tfrac{1}{2}﹩ mag bin of the replicated image bin counts over 2, 3, and 4 times the original image bin counts. These curves demonstrate the completeness of each replication. The faint horizontal blue line marks the expected ratio of 1, as a comparison to the actual values.
Paper: SKYSURF-3: Testing Crowded Object Catalogs in the Hubble eXtreme Deep Field Mosaics to Study Sample Incompleteness from an Extragalactic Background Light Perspective
Authors: Darby M. Kramer, Timothy Carleton, Seth. H. Cohen, Rolf Jansen, Rogier A. Windhorst, Norman Grogin, Anton Koekemoer, John W. MacKenty, Nor Pirzkal
Figure caption: Magnitude vs. half-light radius plot for the F606W original and replicated images. The black points are the original objects, and the other colors are the 2×, 3×, and 4× XDF replications’ objects. Each successive color has more transparent markers, and there are more blue marks than green, more green than red, and more red than black. This figure was modeled after Figure 3 in Windhorst et al. (2008) so features could be marked and compared. The pink band represents the natural confusion limit with a range between 1/25 and 1/50 objects per beam (see, e.g., Serjeant et al. 1997; Silva et al. 2005). The cyan dashed curve represents the 174.4ks surface brightness limit of the XDF F606W data. Its shape has been changed from Windhorst et al. (2008) as the curve is only intended to draw the eye to the trend and the cutoff of the objects, demonstrating the exposure time and resolution limits to observing these objects. The dark gray dashed line represents the limit below which point sources with fainter magnitudes cannot be resolved, as they blend in with the sky distribution. All curves have been shifted in magnitude to account for the m Vega to m AB conversion. This figure demonstrates that natural confusion (pink band) is an important completeness constraint for bright large objects that make up most of the IGL (m AB ≲ 28.5 mag). It also demonstrates that the three main limits on the original HUDF sample remain the the same for the replicated samples, validating our methods of replication, namely the point-source detection limit (horizontal gray dashed line), the surface brightness limit (slanted cyan dashed line) and the natural confusion limit due to statistical object overlap (pink band).
Paper: The Halo Bias inside Cosmic Voids
Authors: Giovanni Verza, Carmelita Carbone, Alessandro Renzi
Figure caption: The profile, δ h(r), for voids traced by halos with M ≥ 1013 h −1 M ⊙ at z = 0, 0.49, 1.05. The upper panels show the measured (black dots) halo density profile, ﹩{\delta }_{{\rm{h}}}^{{\rm{v}}}(r)﹩, and the models described in the text: ﹩{p}_{{\rm{v}}}(r),{q}_{{\rm{v}}}(r),{\delta }_{{\rm{m}}}^{{\rm{v}}}(r)﹩ is case (a) (blue solid lines); ﹩{p}_{{\rm{v}}}^{{\rm{A}}}(r),{q}_{{\rm{v}}}^{{\rm{A}}}(r),{\delta }_{{\rm{m}}}^{{\rm{A}}}(r)﹩ is case (b) (magenta dashed–double-dotted lines); ﹩{p}_{{\rm{U}}},{q}_{{\rm{U}}},{\delta }_{{\rm{m}}}^{{\rm{v}}}(r)﹩ is case (c) (orange dashed–dotted lines); ﹩{b}_{1}({p}_{{\rm{U}}},{q}_{{\rm{U}}}){\delta }_{}^{{\rm{v}}}(r)﹩ is case (d) (orange dashed lines); the linear fit is case (e) (green dotted lines). The middle panels show the relative values of the model with respect to the measurements. The shaded areas represent the uncertainty of the parameters that the models depend on. The lower panels show the ratios ﹩{\delta }_{{\rm{h}}}(r)/{\delta }_{{\rm{m}}}^{{\rm{v}}}(r)﹩, except for the magenta dashed–double-dotted lines, which represent ﹩{\delta }_{{\rm{h}}}(r)/{\delta }_{{\rm{m}}}^{{\rm{A}}}(r)﹩.
Paper: SKYSURF-3: Testing Crowded Object Catalogs in the Hubble eXtreme Deep Field Mosaics to Study Sample Incompleteness from an Extragalactic Background Light Perspective
Authors: Darby M. Kramer, Timothy Carleton, Seth. H. Cohen, Rolf Jansen, Rogier A. Windhorst, Norman Grogin, Anton Koekemoer, John W. MacKenty, Nor Pirzkal
Figure caption: Left column: histograms of object counts per ﹩\tfrac{1}{2}﹩ mag bin per deg2 for the F105W, F125W, and F160W original and replicated images up to their completeness limits. AX Rep refers to the integer A replications of the XDF data, and AxXDF refers to that integer times the original XDF bin counts. See Figure 3 for the ACS/WFC filters. The values in the legend are up to the completeness limit in each filter and replication. Right column: the ratios per ﹩\tfrac{1}{2}﹩ mag bin of the replicated image bin counts over 2, 3, and 4 times the original image bin counts. These curves demonstrate the completeness of each replication and how it varies with magnitude.
Paper: SKYSURF-3: Testing Crowded Object Catalogs in the Hubble eXtreme Deep Field Mosaics to Study Sample Incompleteness from an Extragalactic Background Light Perspective
Authors: Darby M. Kramer, Timothy Carleton, Seth. H. Cohen, Rolf Jansen, Rogier A. Windhorst, Norman Grogin, Anton Koekemoer, John W. MacKenty, Nor Pirzkal
Figure caption: A centered zoomed comparison of the four images used for the F606W analysis. Each detected object is marked with a green ellipse, the size of which corresponds to 2.5× the profile rms along major and minor axes to account for the Kron factor (Kron 1980). (a) Original XDF image with objects brighter than m AB ∼ 24 mag masked out. (b) The masked original image + a masked and once rotated original image. (c) The image of panel (b) + a masked and twice rotated original image. (d) The image of panel (c) + a masked and 3  times rotated original image. This process increases the surface density of objects brighter than the detection limit by integer factors in each iteration, while leaving the sky unchanged.
Paper: SKYSURF-3: Testing Crowded Object Catalogs in the Hubble eXtreme Deep Field Mosaics to Study Sample Incompleteness from an Extragalactic Background Light Perspective
Authors: Darby M. Kramer, Timothy Carleton, Seth. H. Cohen, Rolf Jansen, Rogier A. Windhorst, Norman Grogin, Anton Koekemoer, John W. MacKenty, Nor Pirzkal
Figure caption: Examples of square image regions excised for analysis from the XDF mosaics before the objects brighter than m AB ∼ 24 mag were masked out. (a) Exposure times in the WFC3/IR images, such as the F160W image shown here, vary significantly throughout a single mosaic. We therefore excised a large region with relatively uniform depth in the deepest part of the WFC3/IR mosaics—a 1401 × 1401 pixel region centered on pixel (2734,3072) in the XDF mosaics. (b) We similarly excised the largest square image regions with relatively uniform depth from the ACS/WFC mosaics, such as the F606W image shown here. Each ∼2870 × 2870 pixel region is centered on pixel (2625,2625) in the XDF mosaics.
Paper: Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
Authors: Samantha C. Wu, Jim Fuller
Figure caption: Properties of each binary system undergoing late-stage mass loss. Points are plotted as a function of the helium star’s initial mass, and colors correspond to the initial orbital period given in the legend. Dots represent mass loss up to the end of the solid lines in Figure 2, and open circles include the extrapolated mass loss shown as dotted lines in Figure 2. Top left: time before Si burning when late-stage MT ensues, t MT, as defined in Section 3.2. Bottom left: final mass of each stripped star after case BB and late-stage MT. Right: predicted mass (top) and radius (bottom) of CSM due to late-stage mass loss.
Paper: Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
Authors: Samantha C. Wu, Jim Fuller
Figure caption: Properties of the binary systems after a CEE, assuming unstable MT begins once ﹩\dot{M}\gt 5\times {10}^{-4}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ and that the inspiral ends once the NS unbinds the envelope down to the CO core. Points are plotted as in Figure 3 as a function of each stripped star’s initial He core mass. Top: values on the left axis show the final orbital period of each system after the CEE. The right axis values are the gravitational-wave merger timescales for a binary system consisting of two neutron stars orbiting at the periods of the left axis. Bottom: envelope mass unbound by the CEE.
Paper: Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
Authors: Samantha C. Wu, Jim Fuller
Figure caption: Left: evolution of the radius of single stripped stars as a function of time until Si burning. The legend labels the initial He core mass of each stripped star. Each star expands after He burning and throughout C burning, then contracts and reexpands during O/Ne burning. Right: time before Si burning of the stripped stars’ second expansion. Points are colored by the maximum orbital period at which the star will fill its Roche lobe in a binary with a 1.4 M ⊙ companion star.
Paper: Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
Authors: Samantha C. Wu, Jim Fuller
Figure caption: Dots and open circles are predicted mass vs. radius of CSM due to late-stage mass loss (Figure 3, Section 3.3). Star symbols are predicted mass and radius of material unbound during the CEE (Figure 4, Section 3.4). Colors indicate initial P orb as in Figure 3. Points with error bars are estimated CSM properties of USSNe (square diamonds) and type Ibn SNe (thin diamonds). All are given error bars of at least a factor of 2 in each direction to account for systematic uncertainties in the modeling.
Paper: Extreme Mass Loss in Low-mass Type Ib/c Supernova Progenitors
Authors: Samantha C. Wu, Jim Fuller
Figure caption: The mass-loss rates and accumulated mass loss of the helium star models, each of which is placed in a binary with a 1.4 M ⊙ compact companion at the initial orbital periods listed in the top panels. The legend indicates the initial mass of each helium star. For simulations that end before Si burning, we assume that ﹩\dot{M}﹩ remains steady until Si burning and extrapolate the accumulated mass loss until Si burning, shown as dotted lines.
Paper: Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei
Authors: Jia Ren, Ken Chen, Yun Wang, Zi-Gao Dai
Figure caption: The bolometric and multiband ν L  ν  light curves, where M2 is UVOT/M2, and W1 is WISE/W1, respectively. From top to bottom, the SMBH mass is 106, 107, and 108 M ⊙, respectively. Panels from left- to right-hand sides show the results for mergers occurring at 102, 103, and 104 r s of the active galactic nucleus (AGN) disk, respectively. The accretion rate of SMBHs is ﹩{\dot{M}}_{\bullet }=0.1{\dot{M}}_{\bullet ,\mathrm{Edd}}﹩, other parameters can be found in Section 3. The horizontal lines show the background ν L  ν  luminosities of AGN at different bands. We take the mean spectral energy distribution (SED) of quasars from Shang et al. (2011), with the use of the scaling law ζ(3000 Å) = 5.2 in the correlation of L bol,iso = ζ λ L  λ  (Runnoe et al. 2012).
Paper: Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei
Authors: Jia Ren, Ken Chen, Yun Wang, Zi-Gao Dai
Figure caption: From top to bottom, the optical depth, the propagated distance of the ejecta, the disk density in the position of the ejecta, the accelerated velocities, and the dynamics of the ejecta evolve, respectively. Three panels from left- to right-hand sides show the dynamics and other properties of ejecta at 0°, 45°, and 88° directions, respectively. The labels (a)–(e) mark five stages of the ejecta dynamics that are separated by vertical dashed–dotted lines. The blue solid, red dashed–dotted, and green dashed–dotted lines are the accelerated velocities from the pressure, the swept gas, and the gravity of the central compact remnant, respectively. Note that the pressure accelerates the ejecta and the last two terms decelerate the ejecta. The merger occurs in the disk radius as 103 r s with the mass of the SMBH being 107 M ⊙. To emphasize the main concern about dynamics, we have ignored the change of disk parameters, e.g., ρ 0 and P 0, during ejecta propagation.
Paper: Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei
Authors: Jia Ren, Ken Chen, Yun Wang, Zi-Gao Dai
Figure caption: The light curves under different AGN region environments, with gas densities of 10−24 g cm−3 (dashed–dotted lines) and 10−17 g cm−3 (solid lines), respectively. The mass of the SMBH is 107 M ⊙ with accretion rate ﹩{\dot{M}}_{\bullet }=0.1{\dot{M}}_{\bullet ,\mathrm{Edd}}﹩; merger occurring at 103 r s of the AGN disk; other parameters are the same as Figure 2 and fixed.