adsabs/AstroCLIMB huggingface dataset:
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Polar plots for the northern and southern CGM temperatures. Northern CGM figures mark the fields used in the stacked spectra with black rings. The NPS and Eridanus Enhancement are marked with cyan rings. The median temperature from Figure 3 is marked on each color bar, with an uncertainty that is equivalent to the average uncertainty (90% confidence interval).
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Stacked spectra of consistent fields in the northern CGM. Each detector is a different color (DPU 14, 54, and 38 are, respectively, black, orange, and cyan). The model for the CGM is two APECs, marked in solid black lines. Background and foreground components are marked in dashed lines. Model components that are identical between each detector are only shown once. The feature around 3 keV is due to the data filtering procedure as described in the text.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Box-whisker plots of warm (left) and hot (right) EM vs. angular distance from the Galactic center. Bin width is 20.°. For each bin, the northern and southern CGM are plotted on each side of the bin center-point. Boxes for the northern CGM are filled with cyan while the southern CGM boxes are unfilled. The box represents the two inner quartiles for each bin, and the orange line in each box is the median. The outer whiskers on each box are the two outer quartiles of the binned data.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Stacked CGM spectra after gain correction. Note that this also includes the edge component discussed in Appendix B.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Stacked CGM spectra before gain correction.
Paper: The Great Dimming of Betelgeuse: A Surface Mass Ejection and Its Consequences
Authors: Andrea K. Dupree, Klaus G. Strassmeier, Thomas Calderwood, Thomas Granzer, Michael Weber, Kateryna Kravchenko, Lynn D. Matthews, Miguel Montargès, James Tappin, William T. Thompson
Figure caption: Top panel: three TRES echelle spectra of the temperature sensitive V I (6251.83 Å) and Fe I (6252.57 Å) absorption lines from 2019 April 18 to 2020 February 3. The Fe I line becomes weaker relative to the V I transition during this time span. Note the broadening of the Fe I line on 2020 February 3 that appears to be blended at low T (see also Figure 3). Bottom panel: the V I/Fe I depth ratios clearly follow the behavior of the V magnitude indicating a decrease of the photospheric temperature. The dashed line marks a ∼400 day period.
Paper: The Great Dimming of Betelgeuse: A Surface Mass Ejection and Its Consequences
Authors: Andrea K. Dupree, Klaus G. Strassmeier, Thomas Calderwood, Thomas Granzer, Michael Weber, Kateryna Kravchenko, Lynn D. Matthews, Miguel Montargès, James Tappin, William T. Thompson
Figure caption: Top panel: V magnitude from the AAVSO (2022), STEREO, the Wasatonic Observatory, D. Corona, and daytime measures (DAY NOT). The broken line marks a ∼400 day period. This period is no longer present after the Great Dimming. Bottom panel: radial velocity of Betelgeuse from STELLA during 2018–2022.
Paper: The Great Dimming of Betelgeuse: A Surface Mass Ejection and Its Consequences
Authors: Andrea K. Dupree, Klaus G. Strassmeier, Thomas Calderwood, Thomas Granzer, Michael Weber, Kateryna Kravchenko, Lynn D. Matthews, Miguel Montargès, James Tappin, William T. Thompson
Figure caption: Mg II h flux obtained with STIS using a 25 × 100 mas aperture, and various offset positions. The aperture angle varies among the observations but is generally in the quadrant marked on the x-axis. The high chromospheric flux associated with the mass ejection event in 2019 September–November has not been observed subsequently. In 2022, STIS pointings were made at five positions on the disk: ±50 mas, ±25 mas, in the center. Optical and ultraviolet (FWHM) diameters are marked. The error bars represent the uncertainly in the STIS flux measurement.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Pearson r correlation coefficient and χ 2/N in g and r band calculated from ZTF light curves for three different binning timescales. We show the entire dwarf galaxy population with ZTF photometry in blue and the AGN control sample (from host galaxies of stellar mass M * > 3 × 109.75  M ⊙) in green. The cutoffs used for AGN candidate selection are shown with black dotted lines for each statistic. We required the three statistics to satisfy the cutoffs for all three binning timescales in order for a candidate to be selected.
Paper: The Great Dimming of Betelgeuse: A Surface Mass Ejection and Its Consequences
Authors: Andrea K. Dupree, Klaus G. Strassmeier, Thomas Calderwood, Thomas Granzer, Michael Weber, Kateryna Kravchenko, Lynn D. Matthews, Miguel Montargès, James Tappin, William T. Thompson
Figure caption: TRES spectra of Betelgeuse in 2019 April, a cooler supergiant (HD 156014), and a bright giant star (HD 175588). Note the systematic weakness of the absorption features as the effective temperature of the star decreases. At lower temperatures, the Fe I line at 6252.55 Å becomes blended with an unidentified absorption line. At the lowest temperature (3450 K), the unidentified line dominates the Fe I line, making the ratio measurement (V  I/Fe I) in Betelgeuse a lower limit when the star is faint.
Paper: The Great Dimming of Betelgeuse: A Surface Mass Ejection and Its Consequences
Authors: Andrea K. Dupree, Klaus G. Strassmeier, Thomas Calderwood, Thomas Granzer, Michael Weber, Kateryna Kravchenko, Lynn D. Matthews, Miguel Montargès, James Tappin, William T. Thompson
Figure caption: The chromospheric Ca II K-line, 3933 Å, from TRES echelle spectra, displays asymmetric emission wings (marked as a V (violet) and R (red) feature). The appearance of V ≤ R signals wind absorption from a differentially expanding atmosphere in 2019 January and March. The profile lost this asymmetry in 2019 September, mimicking the earlier profile on 2018 September 14.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Three examples of ZTF light curves that passed the variability criteria and were classified as variable AGN candidates.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: BPT diagram showing narrow line ratios derived from pPXF fitting of archival SDSS spectra of the ZTF-selected IMBH candidates (left) and SN candidates (right). Orange points show line ratios for IMBH candidates with broad Balmer lines in archival spectra, and blue points show those with narrow emission lines only. Gray contours show the population density with log scaling of the entire parent dwarf galaxy sample for line ratios derived from the NASA-Sloan Atlas. Classification regions are labeled in black text. We note that because pPXF determines narrow emission line strength after accounting for stellar absorption of those same lines, fluxes may appear to be slightly larger in the BPT diagram compared to the NSA-derived emission-lines fluxes of the dwarf galaxy population.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Pearson r correlation coefficient and χ 2/N in W1 and W2 band calculated from WISE forward-modeling light curves. We show the entire dwarf galaxy population with WISE photometry in blue and the AGN control sample (from host galaxies of stellar mass M * > 3 × 109.75  M ⊙) in green. The cutoffs used for AGN candidate selection are shown with black dotted lines for each statistic. We required the three statistics to satisfy the cutoffs in order for a candidate to be selected.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: BPT diagram showing narrow line ratios derived from pPXF fitting of archival SDSS spectra of the WISE-selected IMBH candidates. Orange points show line ratios for IMBH candidates with broad Balmer lines in archival spectra, and blue points show those with narrow emission lines only. Gray contours show the population density with log scaling of the entire parent dwarf galaxy sample for line ratios derived from the NASA-Sloan Atlas. Classification regions are labeled in black text.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Legacy survey cutouts of three WISE IMBH candidates (panels (a)–(c)) and two ZTF IMBH candidates (panels (d)–(e)) with host masses M * < 108.2 M ⊙ and the candidate with a FIRST radio detection (panel (f), radio position overlaid with a green circle). Blue circles show the central position for WISE or ZTF forced photometry.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Normalized galaxy mass and redshift distributions of variable IMBH candidates (top) and SN candidates (bottom) shown in green and the parent dwarf galaxy sample shown in blue. The subset of the parent dwarf galaxy for which ZTF photometry was produced for the optical IMBH search is shown in the hatched histogram. Redshifts and host galaxy mass measurements were derived from the NSA.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Normalized galaxy mass and redshift distributions of WISE IMBH candidates shown in green and the parent dwarf galaxy sample shown in blue. Redshifts and host galaxy mass measurements are derived from the NSA.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Three examples of ZTF light curves that passed the variability criteria and were classified as SN candidates.
Paper: Variability-selected Intermediate-mass Black Hole Candidates in Dwarf Galaxies from ZTF and WISE
Authors: Charlotte Ward, Suvi Gezari, Peter Nugent, Eric C. Bellm, Richard Dekany, Andrew Drake, Dmitry A. Duev, Matthew J. Graham, Mansi M. Kasliwal, Erik C. Kool, Frank J. Masci, Reed L. Riddle
Figure caption: Six examples of WISE forward-modeling light curves that passed the variability criteria and were classified as IMBH candidates.
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: Top: steady-state luminosity L pl (left panel) and rise time t rise (right panel) of SN precursor emission from wind-like mass ejection as a function of the wind mass-loss rate ﹩\dot{M}﹩ and velocity v w (equivalently, sonic radius for an assumed progenitor star mass M ⋆ = 10 M ⊙; top horizontal axis). The black and gray shaded regions are excluded, based on the wind kinetic luminosity being sub-Eddington and the total ejecta mass during the rise time exceeding the progenitor star mass (Equation (A9)). The other solid black lines correspond to M ej = 0.1M ⋆ and 0.01M ⋆. The thin shaded regions represent the mass-loss rate ﹩\dot{M}({v}_{{\rm{w}}})﹩ predicted by Quataert et al. (2016; Equation (18)) for a range of envelope masses M env/M ⋆ = 0.001 − 0.1. The black dashed line shows the critical mass-loss rate ﹩{\dot{M}}_{\mathrm{ion}}﹩ (Equation (A8) for T ion = 104 K) above which the drop in opacity from hydrogen recombination determines the transient rise time. Radiation pressure exceeds gas pressure at the sonic point to the right of the white line, i.e., across most of the parameter space. Bottom: the same as the top panels, but showing the ratios of steady-state luminosity L pl to the wind kinetic power ﹩{\dot{E}}_{{\rm{w}}}﹩ (Equation (A2); left panel) and to the maximum recombination luminosity L rec (Equation (21); right panel).
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: Optical light curves of the SN precursor emission in the wind mass-loss scenario for progenitor mass M ⋆ = 10 M ⊙. The thick black curve shows the fiducial case with wind mass-loss rate ﹩\dot{M}=1{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩ and wind velocity v w = 200 km s−1 (R s = 102 R ⊙). The wind duration is set to t w = 130 days, to match the SN2020tlf precursor duration (shown for comparison by the red points, along with the other precursors labeled as in Figure 1). The thin black curve shows the light curve from a single shell of thickness Δt = 4 days for the fiducial model, whose duration—being similar to that for all shells—controls the rise time of the total light curve. The colored lines show the light curve that results from increasing the wind mass-loss rate or speed relative to the fiducial model (while fixing t w). The black dashed curve shows the effect of tripling the “sonic” radius at which the wind thermal energy is initialized, to crudely mimic the effects of the reheating of the ejecta by internal shocks (Section 3.2.1).
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: The same as Figure 2, but showing light curves in the eruption scenario for different ejecta parameters, and compared with observed SN precursors (Figure 1). The blue, black, and red curves show models with a common ejecta mass M ej = M ⊙, but different ejecta velocities v ej = 200, 500, and 1000 km s−1, respectively. The yellow curve shows a model with v ej = 200 km s−1, but larger M ej = 3 M ⊙. The lighter shaded curves denote the bolometric luminosity. The stellar mass M ⋆ = 10 M ⊙ and radius R 0 = 103 R ⊙ are fixed for all models. The time of the eruption prior to the SN is set to t erupt = 140 days (except for the high-velocity models shown with the blue and red curves, for which t erupt = 100 and 50 days), to roughly match the onset of the observed precursor emission. The dependence of the predicted plateau luminosity and the duration of the ejecta properties broadly agree with the Popov analytic scalings (Equations (19) and (20)).
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: Sample of SN precursor light curves, showing the luminosity as a function of time relative to the onset of the SN (which we define by the luminosity rising abruptly by a factor of ≳ 10). The shaded region shows the characteristic timescale range before core collapse, corresponding to the core silicon burning in 13–20 M ⊙ stars (Woosley et al. 2002). The references to the light-curve data are given in Table 1.
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: The steady wind scenario is challenged in explaining the high luminosities of the SN precursor emission for reasonable ejecta masses. The black lines shows the maximum steady-state luminosity in the wind scenario as a function of wind velocity so as not to overproduce the total wind ejecta mass M ej (Equations (A10) and (A11)); specifically, the gray shaded region is excluded by the requirement M ej > M ⋆ = 10 M ⊙ (see the text for details). The colored circles represent the observed SN precursor luminosities and velocities (Table 1). The left-directed triangles show an estimate of the wind velocity (v engulf;  Equation (24)) invisible to flash spectroscopy observations (too-slow wind material would be overtaken by the SN shock prior to the observations).
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: Example SN precursor light-curve calculation in the eruptive mass-loss scenario. A solid black curve shows the optical light curve (bottom) and the evolution of the effective temperature (top) for a fiducial case with ejecta mass M ej = M ⊙, initial radius R 0 = R ⋆ = 103 R ⊙, and minimum ejecta velocity v ej = 1000 km s−1, for an assumed stellar mass M ⋆ = 10 M ⊙. The optical luminosity is calculated by excluding radiation of frequency > 1015 Hz from the bolometric light curve (the gray curve). The colored solid lines show the luminosity contributed by single shells with velocities v = 1000 to 1750 km s−1 (separated by 250 km s−1) and a shell width of dv = 2 km s−1. The dashed curves show an otherwise identical calculation, calculated following the original model of Matsumoto & Metzger (2022), which neglects the early-time suppression factor (Equation (7)) and uses a local estimate for the radial optical depth.
Paper: Supernova Precursor Emission and the Origin of Pre-explosion Stellar Mass Loss
Authors: Tatsuya Matsumoto, Brian D. Metzger
Figure caption: Contours of the characteristic optical precursor luminosity L pl (after subtracting the UV luminosity; left column) and duration t pl (right column) associated with eruptive mass-loss events in the space of ejecta velocity and mass, for different initial radii R 0 = 103, 102, and 10 R ⊙ (from top to bottom). The black shaded regions are excluded because the ejecta velocity is smaller than the surface escape speed for a star of mass M ⋆ = 10 M ⊙ and radius R ⋆ ≤ R 0. To the right of the white contours, the radiation pressure exceeds the gas pressure at the initial radius.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: SEDs obtained using RADMC-3D. The redshift of the model was assumed to be z = 2.0. Solid, dashed, and dotted lines represent PL DOGs, bump DOGs, and non-DOGs respectively. Following Narayanan et al. (2010), the bump DOGs and PL DOGs are classified by their intensities at 3.6, 4.5, and 7.9 μm: S 3.6 < S 4.5 and S 4.5 > S 7.9 for bump DOGs and S 3.6 < S 4.5 < S 7.9 for PL DOGs. Top panel: time evolution of the SED at θ = 0°. As the mass accretion rate increases, the SED becomes brighter in the mid-infrared. Bottom panel: comparison of the SEDs observed from θ = 0°, 30°, 60°, 75°, and 90° at 1107.0 Myr. The SED for θ > 60° becomes fainter in the mid-infrared. Note that the SEDs in the near-infrared are not sensitive for the viewing angles. This is because of the vertical distribution of the stars and gas. See Figure 11 in Appendix A.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Comparison of the time evolutions of F 24μm/F R and F 24μm in different viewing directions. From top to bottom, θ = 0°, 60°, and 75°. The plus signs (+) denote points that do not satisfy the DOG criteria. Squares (□) denote bump DOGs, and triangles (△) denote the PL DOGs. The redshift of the model was assumed to be z = 2.0. The blue and red dotted lines show the DOG criteria of F 24μm/F R = 982 and F 24μm = 0.3 mJy, respectively.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Gas density distribution (n H[cm−3]) in the first to third columns from the left and gas temperature (T[K]) in the rightmost column. From top to bottom, t = 1103.3, 1107.0, and 1115.0 Myr. Note that, here, the coordinates are shifted parallel to those in Figure 1 such that the origin is the center of gravity of the two BHs. Black circles denote the positions of the two BHs.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: The time evolution of the distance between the two BHs (top panel), total bolometric luminosity ﹩{L}_{\mathrm{AGN}s}=0.1\times {\dot{M}}_{\mathrm{gas}}{c}^{2}﹩ of the two AGNs (middle panel), and star formation rate (SFR) (bottom panel).
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Intensity distribution at 24 μm in the observed frame (z = 2.0) at t = 1107.0 Myr. Top panel: θ = 0°. Bottom panel: θ = 75°.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Infrared (8–1000 μm) luminosity of AGN origin vs. F 24μm for θ = 0°, 30°, 60°, and 90° during 1100–1115 Myr. L IR(AGN) does not include the contributions from stars. Plus signs denote time stamps that do not satisfy the DOG criteria. Squares denote bump DOGs, and triangles denote the PL DOGs. L IR(AGN) is positively correlated with F 24μm.
Paper: Origin and Evolution of Dust-obscured Galaxies in Galaxy Mergers
Authors: Naomichi Yutani, Yoshiki Toba, Shunsuke Baba, Keiichi Wada
Figure caption: Initial setup of the merger system. The two identical systems were merged. Each has a supermassive black hole (SMBH) of 108 M ⊙, a rotationally supported gas disk with a mass of 4 × 109 M ⊙ and angular momentum in the z-axis direction, and a spherical stellar system of 2 × 1010 M ⊙.