adsabs/AstroCLIMB huggingface dataset:
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Radial profiles of the (left) surface density Σ and (right) azimuthal velocity at the midplane vϕ, normalized by the initial azimuthal velocity vϕ,init. While we present the azimuthal velocity at the midplane only, we confirm that the velocity at other heights shows a similar trend and good agreement between grid-based codes, with smaller velocity perturbations near the planet in the Phantom simulation due to the shallower gap.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: The (top) radial and (middle) azimuthal location of the planet inferred by DISCMINER (global peak in Figure 8) for synthetic 12CO cubes generated with different combinations of hydrodynamic and radiative transfer codes. The bottom panel shows the peak residual velocity at the inferred planet location.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: (Left panel) Folded velocity residual maps (see A. F. Izquierdo et al. 2023, 2025) computed for the 12CO synthetic cube created with FARGO3D and mcfost, as an example. The green circle and cross indicate the location of peak and clustered residuals, whereas the black circle shows the correct planet location (100 au and −45°). (Middle panel) Peak residual velocity as a function of azimuthal angle. (Right panel) Peak residual velocity as a function of radius.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Azimuthally averaged temperature profiles in an r − θ plane from various combinations of hydrodynamic and radiative transfer codes (shown in the upper left corner of each panel). The black contours show where T = 20 K. The white areas in the upper left and lower left corners of the bottom panels is due to the lack of SPH particles there.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Azimuthal distribution of the density at (top panels) R = 1.3 and (bottom panels) R = 0.7. From left to right, each panel shows the density at the midplane, at Z/R = 0.1, and at Z/R = 0.3, respectively. The scatter seen in the Phantom simulation is due to the finite number of particles used in the simulation and is expected.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 10, but for the meridional velocity vθ.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 10, but for the azimuthal velocity vϕ/〈vϕ〉.
Paper: exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes
Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Same as Figure 10, but for the radial velocity vr.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison of the data, frank model, CLEAN-imaged frank model, residuals, and polar plots for each disk (here showing AA Tau and CQ Tau and continued in Appendix A). (Top to bottom, left to right) First panel: fiducial continuum image of the observed data obtained with robust −0.5, with the synthesized beam’s FWHM shown as an ellipse in the lower left corner. The asinh function was applied to the color scale to visually enhance the fainter emission. Second panel: image of the frank model swept over 2π and reprojected, with normalized intensity and an asinh stretch. Each gap is marked by a dashed arc labeled “D” with its distance from the star in au, while solid arcs labeled “B” indicate the rings. The dotted line corresponds with the PA measured on gas data with discminer (A. F. Izquierdo et al. 2025) and defines the ϕ = 0 angle of the polar plots, increasing counterclockwise (note possible PA differences with the one measured from galario and used in frank; see Appendix C). Third panel: frank model sampled at the same uv-points of the observation and imaged with CLEAN as the observed data. The color scale is the same as the data panel. Fourth panel: residuals obtained subtracting the frank model from the data. The residual visibilities were calculated at the same uv-points of the ALMA observations and imaged with CLEAN as the observed data. The color scale shows the residuals in units of the observed noise (σrms). Rings and gaps are marked with solid and dashed ellipses, respectively. Fifth panel: polar plot of the data continuum image. Sixth panel: polar plot of the nonaxisymmetric residuals. The locations of rings and gaps are marked by solid and dashed horizontal lines, respectively.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gallery of residuals plots generated by subtracting the frank model (sampled at the same uv-points of the observations) from the data and then imaged with CLEAN and robust −0.5. The source order is from the least to the most nonaxisymmetric, according to the NAI presented in Section 4.2 and reported in the lower right corner of each panel and in Table A1. The color scale represents the values of residual SNR in units of the observed noise (σrms) for the respective observation, and the same extremes are applied to each plot. Note that the spatial scales are different for every disk. Rings and gaps are marked with solid and dashed ellipses, respectively, while the synthesized beam is indicated by the ellipse in the lower left corner.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Comparison between the continuum emission and the 12CO velocity kinks identified by C. Pinte et al. (2024). The left panels show the continuum emission from the fiducial CLEAN data images, and the middle panels display the frank residuals. Dashed–dotted ellipses represent R90, while solid circles indicate the positions of the velocity kinks, deprojected onto the midplane. Ellipses in the lower left corner indicate the synthesized beam. The right panels show the intensity radial profile of the azimuthally averaged fiducial CLEAN images (black) and the frank model (red). Vertical blue dashed–dotted lines represent R90, while the vertical green dotted lines indicate the radial location deprojected onto the midplane of the planet candidates generating the kinks (Rcand). The green shaded area in the intensity profile and the size of the green circles in the 2D images represent the uncertainty due to the gas image beam size (C. Pinte et al. 2025). The purple shaded area represents intensity values below 5 times the rms noise (σrms) measured in the CLEAN image.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gallery of radial intensity profiles on a log-linear scale of the deprojected and azimuthally averaged CLEAN data (black solid line) and the frank model (red solid line). Sources are arranged alphabetically. The gray shading represents CLEAN data uncertainty, calculated as the 1σ scatter per radial bin, divided by the square root of the number of beams in the associated annulus. The red shading indicates the 1σ uncertainty of the frank model, estimated via bootstrapping, considering small variations of the disk geometrical parameters (see Section 3.2). The black scale bar in the top right corner of each panel shows the FWHM, averaged between the major and minor axes of the CLEAN synthesized beam. Radial positions of rings and gaps are marked, with each gap labeled with a dashed line and a “D” (for dark) followed by the distance from the central star in au. Solid lines with “B” labels (for bright) denote the rings. A vertical blue dashed–dotted line indicates R90, the radial location within which axisymmetric substructures are defined.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gallery showing the fits of the continuum extended emission with an exponential function in a log-lin scale. The intensity radial profiles are from the azimuthally averaged CLEAN images with robust −0.5. The blue vertical dashed–dotted line indicates R90, while the purple shaded area represents intensity values below 5 times the rms noise σrms measured in the CLEAN image. The rms noise is properly scaled accounting for the radial dependence of the azimuthal average, that is, dividing the σrms by the square root of the number of beams within the corresponding radial annulus. The orange line shows the best fit using the exponential model ﹩I(R)={I}_{0}\exp [-R/{\lambda }_{{\rm{out}}}]﹩ of the region between R90 and the radius where the intensity intersects the 5 × σrms line.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: From left to right: radius enclosing 90% of the continuum emission (R90 dust), radius enclosing 90% of the 12CO emission (﹩{R}_{9{0\,}^{12}{\rm{CO}}}﹩; M. Galloway-Sprietsma et al. 2025), and their ratio (Rgas/Rdust) as a function of the parameter λout from the exponential model of the continuum extended emission ﹩I(R)={I}_{0}\exp [-R/{\lambda }_{{\rm{out}}}]﹩. Uncertainties on R90 dust are present but smaller than the data points. The color scale indicates the number of beams resolving the outer disk falloff, with values of σfit/σbeam (Table 4) displayed on a logarithmic scale.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Gallery of fiducial continuum images at 0.9 mm (331.6 GHz) of the exoALMA sample, obtained with the CLEAN algorithm and robust of −0.5. The source order is alphabetical. All images are shown on the same angular scales. The FWHM of the synthesized beams and the 20 au scale bars are indicated in the lower left and right corners of each plot, respectively. The color scale ranges from null to peak intensity for each disk. An asinh stretch is applied to the color scale to visually enhance the fainter emission. A linear stretch version is presented in Figure A1.
Paper: exoALMA. IV. Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
Authors: Pietro Curone, Stefano Facchini, Sean M. Andrews, Leonardo Testi, Myriam Benisty, Ian Czekala, Jane Huang, John D. Ilee, Andrea Isella, Giuseppe Lodato, Ryan A. Loomis, Jochen Stadler, Andrew J. Winter, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Daniele Fasano, Mario Flock, Misato Fukagawa, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Francois Menard, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Richard Teague, Gaylor Wafflard-Fernandez, David J. Wilner, Lisa Wölfer, Hsi-Wei Yen, Tomohiro C. Yoshida, Brianna Zawadzki
Figure caption: Mass accretion rate and NIR excess as function of the NAI (higher values indicating more asymmetric disks). Left plot: log–log plot of the mass accretion rate, normalized for the correlation with the stellar mass assuming ﹩\dot{M}\propto {M}_{\star }^{1.8}﹩ (C. F. Manara et al. 2023), as a function of the NAI (defined in Section 4.2). Right panel: lin–log plot of NIR excess vs. the NAI. Downward-pointing triangles represent upper limits. Values of the NIR excess are reported in Table D1.
Paper: Coincident Multimessenger Bursts from Eccentric Supermassive Binary Black Holes
Authors: Vikram Manikantan, Vasileios Paschalidis, Gabriele Bozzola
Figure caption: Left: specific luminosity of synchrotron emission on a color scale vs time for a 107 M⊙ binary accreting at 10% Eddington. The y-axis is the frequency of the SED, and the x-axis is the time, with the color bar indicating the specific luminosity, Lν. Right: PSD of the Fourier transform of the frequency-binned SED time series. We perform the Fourier transform for the time period t > 4000 M (t > 54.7 hr). The plots demonstrate that only the optically thin region νem ≳ 1014 Hz of the synchrotron SED has clear periodicity on the orbital timescale of f ∼ forb, which matches its mass accretion rate periodicity and Poynting luminosity periodicity. There is no clear periodicity in the optically thick regime.
Paper: Coincident Multimessenger Bursts from Eccentric Supermassive Binary Black Holes
Authors: Vikram Manikantan, Vasileios Paschalidis, Gabriele Bozzola
Figure caption: Contours of rest-mass density (ρ0) normalized to the initial maximum density ﹩{\rho }_{0,{\rm{m}}ax}=2.6\times 1{0}^{-11}(\langle \dot{M}\rangle /0.1{\dot{M}}_{{\rm{edd}}}){(M/1{0}^{7}{M}_{\odot })}^{-1}{(\eta /0.1)}^{-1}{\rm{g}}\,{{\rm{cm}}}^{-3}﹩, where ﹩\dot{M}﹩ is the accretion rate and ﹩{\dot{M}}_{{\rm{edd}}}﹩ is the Eddington accretion rate for a gravitational mass M and radiative efficiency η. The left panel corresponds to the binary just after apocenter (t/M = 4120); the center show the binary as it approaches pericenter (t/M = 4220); and the right panel shows the binary at pericenter (t/M = 4300). We indicate the BH horizons with black disks. In the left panel, tidal streams circularize to form minidisks. In the center panel, these minidisks begin to accrete, and in the right panel, they are depleted at pericenter. Once in a quasi-steady-state, the binary exists in the cavity with density ρ0/ρ0,max ∼ 10−3–10−2.
Paper: Coincident Multimessenger Bursts from Eccentric Supermassive Binary Black Holes
Authors: Vikram Manikantan, Vasileios Paschalidis, Gabriele Bozzola
Figure caption: Left: rest-mass accretion rates onto both BHs (solid black line) and onto the individual black holes (dashed and dotted–dashed lines), all normalized by the total average for 3000 < t/M < 5500. Right: power spectral density (PSD) of the Fourier transform of the total rest-mass accretion rate, with the frequency normalized to the BBH orbital frequency. The Fourier transform is performed on the time period t = 3000–5500 M. The dominant frequency for accretion is f ∼ forb and is insensitive to the time interval over which we perform the Fourier transform.
Paper: Coincident Multimessenger Bursts from Eccentric Supermassive Binary Black Holes
Authors: Vikram Manikantan, Vasileios Paschalidis, Gabriele Bozzola
Figure caption: SED of the jet synchrotron emission at “low” (thick black line) and “high” (thin red line) states at t = [44, 40] hr in Figure 4. The synchrotron self-absorption frequencies (vertical, translucent black and red lines) are νssa = [7.1, 9.3] × 1013 Hz, and the peak specific luminosities are Lν = [1.0, 1.8] × 1023 erg s−1 Hz−1 for the low and high states, respectively.
Paper: Coincident Multimessenger Bursts from Eccentric Supermassive Binary Black Holes
Authors: Vikram Manikantan, Vasileios Paschalidis, Gabriele Bozzola
Figure caption: Top row: amplitude of the ℓ = 2, m = 2 mode of the gravitational-wave (GW) strain, ∣h22∣, normalized by the distance r/M vs retarded time tret. Middle: outgoing Poynting luminosity normalized by the rest-mass accretion rate vs tret. Bottom: synchrotron luminosity integrated in the optically thin regime 8 × 1013 Hz < νem < 8 × 1014 Hz vs. tret. We denote the location of GW bursts with vertical translucent gray lines on both the GW and EM panels. The lightcurves shows almost perfect alignment between GW, Poynting flux, and EM bursts.