adsabs/AstroCLIMB huggingface dataset:
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Time after CC at which the gravitational instabilities in the collapsar disk first set in (top panel) and the period over which the gravitational instabilities are continuously excited during the fallback process (bottom panel), shown in the space of {r b, f K} for the fiducial progenitor model 250.25, with p = 4.5. The white space indicates the models that do not experience gravitational instabilities during fallback accretion. The red contours indicate the inferred primary mass of GW190521 [M ⊙], together with its 90% confidence limits. The cyan contours delineate the final BH masses of 60 M ⊙ and 130 M ⊙, which approximately correspond to the lower and upper end of the PI mass gap.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: A one-zone chemical evolution calculation showing the contribution to the total Galactic r-process content (stars and interstellar medium gas) from superKNe relative to ordinary collapsars and neutron star mergers as a function of Galactic age. The underlying model and parameters for neutron star mergers as well as ordinary collapsars are as in Siegel (2019; see their Methods and Extended Data in Figures 9 and 10), except for an updated local neutron star merger rate of ∼300 Gpc−3yr−1 (The LIGO Scientific Collaboration et al. 2021) and an efficiency factor f NS = 1. SuperKNe are assumed to follow the cosmic SFR, with the same cutoff distribution at high metallicities as long GRBs (ordinary collapsars; see Siegel 2019 for details), corresponding to our fiducial local rate of 10 Gpc−3 yr−1 in the absence of a cutoff. We assume a moderate average yield of 5 M ⊙ of r-process material per superKN event. As a result of the cutoff and Galactic outflows, the cumulative collapsar and superKN contribution decreases slightly at late times. The horizontal dashed line and the gray shaded area (±0.5 dex) indicate an estimate of the total present-day Galactic r-process content, assuming that the solar abundance pattern (A ≥ 69) generalizes to the entire Galactic stellar and gas mass of ≈ 6.6 × 1010 M ⊙ (McMillan 2017). The vertical dotted–dashed line indicates the time of formation of the solar system.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The disk frequency evolution (Equation (18)) for three progenitor models (250.25, 220.25, and 200.25), with rotation parameters p = 4.5, r b = 1.5 × 109 cm and an overall small (f K = 0.3;  top) or large (f K = 0.6;  bottom) Keplerian angular momentum parameter. The plots show twice the orbital angular frequency, which corresponds to the gravitational-wave frequency of the m = 2 density mode of the gravitationally unstable disk. The frequency evolution is largely controlled by f K, with all models reflecting the “sad trombone” nature of the gravitational-wave signal.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The detection horizons of gravitational waves from our fiducial model shown in Figure 2, with p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, for CE (top), ET (center), and DECIGO (bottom), assuming optimal matched filtering and an S/N of 8. For progenitors with medium to low rotation, these detectors may be able to detect gravitational waves from superKN collapsars at distances of typically a few hundred Mpc up to a few Gpc. These estimates are based on the corresponding physical frequency regime, as indicated in Figure 10. The sharp decrease in the detection horizon for CE at ﹩\mathrm{log}{r}_{{\rm{b}}}\gtrsim 9.4﹩ is due to the low-frequency emission below 10 Hz (below CE’s sensitivity band). The contours delineate the final BH masses, as in previous figures.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The same as Figure 12, but for the progenitor model 250.25, with p = 4.5, r b = 1.5 × 109 cm, and different values of the Keplerian fraction, f K = 0.2, 0.4, and 0.6. The relatively low to medium angular momentum models (here, f K ≈ 0.2) generate stronger signals in all detectors (detection horizon ∼400 Mpc with aLIGO at an S/N of 8), compared to cases with higher angular momentum (large values of f K). The f K = 0.6 model would only be detectable by BBO at a distance up to 100 Mpc with an S/N of 8 (see Figure 23).
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Amplitude spectral density of the gravitational-wave emission from the collapsar disk, shown for three progenitor models (250.25, 220.25, and 200.25) and the stellar rotation parameters p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, at an assumed source distance of 200 Mpc. The shaded region for each curve shows the unphysical frequency regime above the maximum disk frequency, as plotted in Figure 10, which is ignored in the S/N calculations. Shown for comparison are the measured or predicted noise curves for aLIGO, CE, ET, DECIGO, and BBO, with sensitivity curve data from https://dcc.ligo.org/LIGO-T1500293/public and Yagi & Seto (2011).
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Convergence test for model 250.25. Top: the relative error in computing the total mass of the star M ⋆, using a grid discretized in both polar angle and radius, showing that at the fiducial angular resolution of n  θ  = 1001, the relative error ≲0.0018 is dominated by the radial resolution of the progenitor model. Bottom: the total stellar mass, as computed by the numerical integration of Equations (9)–(14) with fixed angular resolution (n  θ  = 1001), varying the time step. For sufficiently high temporal resolutions, the relative error of ≲0.002 is again dominated by the radial discretization of the progenitor model, consistent with the error budget shown in the top panel.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Plus and cross-polarization strain amplitudes of the l = m = 2 mode of the gravitational waves resulting from the gravitationally unstable collapsar disk in the fiducial model shown in Figure 2, with p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, assuming a face-on orientation of the accretion disk (ι = 0). The emission starts a few seconds after the onset of the collapse and persists for several seconds, until the viscous draining of the disk dominates the fallback accretion, with the disk becoming stable again at around 9 s after the onset of the collapse.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The average ratio of p ej/p fb (see Equation (C1)) during the first 100 s for model 250.25, with p = 4.5 and setting θ fb = 45°. Disk winds can overcome the ram pressure of the infalling material in the polar directions and break out of the star, even without the help of the GRB jet.
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: Top panel: modeled spectra considering three independent data sets: XRT (in red), BAT+GBM+KW (in orange), and LAT (in blue). The models are shown in the ν F  ν  representation. Two distinguished time epochs are chosen: the first one dominated fully by the prompt emission (94–118 s; on the left), and the second one (118–241 s; on the right) with the separate prompt emission (8 keV–100 MeV) and afterglow components (in X-rays and high energies). We show the energy-dependent flux uncertainty regions (“butterflies”) derived from Swift/XRT and Fermi/LAT data analysis in red and blue, respectively. Bottom panel: Swift/BAT (15–150 keV), Fermi/GBM (8 keV–40 MeV), and KW (13–750 keV) count rate light curves; Fermi/LAT flux light curve (0.1–1 GeV); and photon indices measured from the Swift/XRT (0.5–10 keV) and Fermi/LAT (0.1–1 GeV) time-resolved spectra.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: Hα profile (left) and spectral energy distribution (right) of J1515−2527. The ALLWISE data point at 22 μm, signified as a triangle, is an upper limit. The disagreement between the synthetic spectrum and the optical photometry may be a result of the observations being taken at different times; regardless, our interest is primarily in the infrared, where the model and data correspond well. We estimate A  V  = 0 for this system.
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: The joint X-ray to high-energy spectrum of GRB 220101A at 94–118 s modeled by the Band function with the high-energy spectral cutoff E cutoff (Band+cutoff). We show the spectrum in the count representation (top panel), that in the spectral energy density representation (SED; middle panel), and the residuals between the data and best-fit model (bottom panel). We show the data points and relative errors with different colors, depending on the instruments, while the 3σ upper limits are shown with arrow markers. The joint Band model fit is shown with a black dashed line.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: Same as Figure 11, but for J1915−2847. The left panel shows observations from different nights (red and blue), as well as their mean (black). We estimate A  V  = 0 for this system as well.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption: Spectral cutouts of J0542−1535, J0749−0317, and J2004−2342. The target spectrum (black) is depicted alongside a system of similar spectral type for comparison, J1141+4245 (gray). All targets are roughly type M4.
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: Constraints on the R  γ –Γ0 prompt emission region. The gray points are drawn from the R  γ –Γ0 distribution after considering only the condition on the cutoff (first scenario), corresponding to the allowed parameter space derived from the opacity argument (requiring τ  γ γ  = 1 at E cutoff). We show the lower limits on Γ0 from the maximum synchrotron emitted energy (purple line) and from external shock deceleration (blue line) and the upper limits on Γ0 from the cutoff observation in prompt emission (green line), GeV afterglow emission at coasting and deceleration phase (orange line), and jet transparency requirement (red line). These upper/lower limits are reported with a 1σ confidence level. The blue shaded areas correspond to the R  γ –Γ0 parameter contours at 1σ, 2σ, and 3σ confidence levels. The contour plot and relative 1σ estimate of R  γ  and Γ0 (in yellow) are both obtained in the last scenario, which takes into account all the conditions on R  γ –Γ0 parameters.
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: Corner plot showing the parameter marginalized posterior distributions and contours from the MCMC performed for the afterglow analysis. The best-fit values and priors are shown in Table 2. The parameters fitted in the MCMC are the isotropic equivalent energy E kin, the jet opening angle θ  j , the circumburst medium density n, the electron distribution index p, absorption of optical emission A  R , and the constant fraction of the shock energy that goes to electrons ϵ  e  and into magnetic energy density ϵ  B .
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: Optical (r band; in orange), X-ray (0.5–10 keV; in red), and high-energy (0.1–1 GeV; in blue) light curves of GRB 220101A. Lines correspond to the afterglow model by the propagation of the forward shock in a homogeneous circumburst medium. Early X-ray (<134 s) and high-energy data (<118 s) are not considered for the modeling of the joint light curves.
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: Corner plot showing the parameter contours obtained from the MCMC of the prompt fit parameters, namely the low- and high-energy slopes α and β, respectively, the characteristic energy E ch, the cutoff energy E cutoff, and the flux integrated between 0.1 keV and 0.25 GeV. The 1σ contour region is shown in dark blue, while in light blue we show the 2σ contour region.
Paper: Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A
Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks
Figure caption: Distribution of simulated test statistics, obtained by fitting 103 fake spectra during the prompt time bin (930–118 s) with Band (null model) and Band+cutoff (alternative model). Fake spectra are produced by using as an input the Band model and its relative best-fit parameters obtained from the fit of the real data. The red dashed line represents a probability density of 0.01.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Microlensing parallax vs. Einstein crossing time for OGLE-detectable microlensing events (described in the first paragraph of Section 4.3) as a function of lens type. Regardless of IFMR, black hole (BH) lensing events are characterized by their long t  E  and low π  E  as compared to other types of lenses. The addition of the more massive Spera15 BH lenses allows for even smaller microlensing parallaxes, indicating that events with very low π  E  even at shorter t  E  are likely to be good BH microlensing candidates.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: A histogram of Einstein crossing times for OGLE-detectable microlensing events. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The solid lines indicate all lens types while the dashed lines indicate the distribution of the black hole lensing events. As t  E  ∝﹩\sqrt{{M}_{L}}﹩ the slight excess of long-duration events of the Spera15 IFMR can be attributed to the more massive BHs it produces as compared to the Raithel18 and SukhboldN20 IFMRs.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: A histogram of Einstein crossing times for microlensing events detectable by a Roman-style survey. The number of events is scaled to the number of events Roman is expected to detect during its 5 yr microlensing survey, as described in Section 4.5. The solid lines indicate all lens types while the dashed lines indicate the distribution of the black hole lensing events.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: A histogram of microlensing parallaxes for microlensing events detectable by a Roman-style survey. The number of events is scaled to the number of events Roman is expected to detect during its 5 yr microlensing survey, as described in Section 4.5. The solid lines indicate all lens types while the dashed lines indicate the distribution of the black hole lensing events.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: A histogram of microlensing parallax for OGLE-detectable microlensing events. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The solid lines indicate all lens types while the dashed lines indicate the distribution of the black hole lensing events. As π  E  ∝ ﹩1/\sqrt{{M}_{L}}﹩ the excess of low-π  E  events of the Spera15 IFMR can be attributed to the more massive BHs it produces as compared to the Raithel18 and SukhboldN20 IFMRs.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: A histogram of Einstein crossing times for OGLE-detectable microlensing events as a function of lens type for each IFMR. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The largest differences between the IFMRs are found at long Einstein crossing times (≳150 days) as that is where the overall distribution is dominated by BH lenses.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: A histogram of microlensing parallax for OGLE-detectable microlensing events as a function of lens type for each IFMR. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The largest differences between the IFMRs are found at small microlensing parallaxes (≲0.02) as that is where the overall distribution is dominated by BH lenses.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Einstein crossing time distributions for microlensing events detectable by a Roman-style survey, for constant-valued vs. Maxwellian NS/BH birth kicks. The number of events is scaled to the number of events Roman is expected to detect during its 5 yr microlensing survey, as described in Section 4.5. The effect of the different birth kicks does not significantly change the t  E  distribution.
Paper: The Impact of Initial–Final Mass Relations on Black Hole Microlensing
Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev
Figure caption: Mass distribution of black hole lenses from OGLE-detectable microlensing events. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The Spera15 IFMR produces much more massive BHs than the Raithel18 and SukhboldN20 IFMRs, and this is reflected in the detected lens masses. The SukhboldN20 IFMR produces the fewest BH lensing events overall.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Fractional difference α 1 − 1 between the average diameter of peak brightness in a 1.3 mm black hole image and the diameter of the black hole shadow (i.e., twice the critical impact parameter) shown against the fractional FWHM of the bright ring in the image, for a broad range of black hole spins, observer inclinations, and plasma model parameters (see text for details). The left and right panels correspond to positive and negative black hole spins, respectively. The purple-filled area shows the minimum fractional width of the ring imposed by the 15 G λ Butterworth filter that has been applied to the image to mimic the finite resolution of the EHT. The red-filled area represents configurations in which the fractional diameter difference is larger than the fractional FWHM of the bright ring; the dashed red line corresponds to the fractional diameter difference being equal to the fractional HWHM of the bright ring. If configurations existed in the red-filled area, their black hole shadows would have been disjoint from the bright rings. All the images fall near the vertical dashed line at a 1 − 1 = 0, demonstrating that, in all cases, the diameter of the black hole shadow is very close to that of peak brightness. The fact that all images fall within the white area demonstrates that the bright rings always encompass the critical impact parameters.