adsabs/AstroCLIMB huggingface dataset:
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: Masses of the parent BHs of the primaries of three considered BBH events, along with selected high-mass GW events from the GWTC-3 catalog. Contours represent 90% credibility regions on the posteriors of component masses.
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: Same as Figure 6, except the 1g+3g chain is from a cluster with escape speed V esc = 400 km s−1 and metallicity Z = 0.0225.
Paper: Probing the Dust Grain Alignment Mechanisms in Spiral Galaxies with M51 as the Case Study
Authors: Enrique Lopez-Rodriguez, Le Ngoc Tram
Figure caption: Timescales of the various grain alignment mechanisms as a function of the dust grain size, a, for the arms (top) and interarms (bottom). The timescales of Larmor (B-RAT; τ Lar; black), radiative precession (k-RAT, τ k−RAT, blue), gas damping (randomization; τ gas, green), and mechanical alignment (τ mech, red) are shown. The timescales for arm 1 (solid line), arm 2 (dashed line), and interarm (dotted line) are shown. The typical dust grain sizes (0.005–0.2 μm) in the diffuse ISM are shown as a yellow-shaded region. The dust grain sizes at which the dust grains become aligned, a align (orange), and disrupted by the incident radiation, a disp (gray), are shown. The dominant dust alignment mechanism is given by the shortest timescale, i.e., B-RAT (τ Lar) dominates in both arms and interarms.
Paper: Probing the Dust Grain Alignment Mechanisms in Spiral Galaxies with M51 as the Case Study
Authors: Enrique Lopez-Rodriguez, Le Ngoc Tram
Figure caption: M51's maps of the physical parameters to estimate the timescales of the dust grain alignment mechanisms. B-field strength (B, top left) by A. Fletcher et al. (2011) with contours starting at 7 μG and increasing in steps of 2 μG, energy density of the radiation field (u rad, top right) as estimated by Equation (6) with contours starting at ﹩{\mathrm{log}}_{10}({u}_{\mathrm{rad}}\,[\mathrm{erg}\,{\mathrm{cm}}^{-3}])=-12﹩ and increasing in steps of 0.2, dust temperature estimated using the modified blackbody function fitting procedure within the 70−350 μm spectral energy distribution (Section 2.1; T  d , bottom left) with contours starting at 18 K and increasing in steps of 1 K, and the mask (bottom right) of the arms and interarms as estimated by A. S. Borlaff et al. (2021).
Paper: TIC 435850195: The Second Triaxial Tidally Tilted Pulsator
Authors: Rahul Jayaraman, Saul A. Rappaport, Brian Powell, Gerald Handler, Mark Omohundro, Robert Gagliano, Veselin Kostov, Jim Fuller, Donald W. Kurtz, Valencia Zhang, George Ricker
Figure caption: Simulated Y 10y  (left panel) and Y 11x  modes (middle panel) for a star similar to TIC 435850195. These show that at the inclination angle of the system, roughly 75° (indicated in blue), we expect to see a central peak that is approximately half the amplitude of the sidelobes for any Y 11x  modes that may be present. In contrast, we observe only a frequency doublet of pulsations, regardless of inclination angle, for a Y 10y  mode. The right panel shows a vertical zoom-in on the periodogram for the Y 11x  modes to highlight the Fourier peaks arising from eclipse mapping (also called spatial filtration), further discussed in Section 5.3. Note the differing x-axis scales between the middle and right panels.
Paper: TIC 435850195: The Second Triaxial Tidally Tilted Pulsator
Authors: Rahul Jayaraman, Saul A. Rappaport, Brian Powell, Gerald Handler, Mark Omohundro, Robert Gagliano, Veselin Kostov, Jim Fuller, Donald W. Kurtz, Valencia Zhang, George Ricker
Figure caption: As Figure 8, but for the six highest-amplitude Y 10y  modes in TIC 435850195. These modes have amplitude minima at the primary eclipse (phases 0, 1, and 2) and amplitude maxima at the ELV maxima (phases 0.25, 0.75, 1.25, and 1.75). These modes also undergo a π phase shift at minimum amplitude. In every way, they are identical to the Y 10x  modes, except for being shifted by 90° in orbital phase. The phases for mode 12 have uncertainties of 0.243 and 0.125, which may partially explain why the calculated pulsation amplitude minima and maxima are slightly offset from the times of eclipse and ELV maxima.
Paper: Probing the Dust Grain Alignment Mechanisms in Spiral Galaxies with M51 as the Case Study
Authors: Enrique Lopez-Rodriguez, Le Ngoc Tram
Figure caption: Aligned (top) and disrupted (bottom) dust grain sizes across the disk of M51. The contours show the radiation field, u rad, (white), starting at 10−12 erg cm−3 and increasing in steps of 2.07 × 10−12 erg cm−3, and the magnetic field strength, B, (gray) starting at 10 μG and increasing in steps of 2 μG.
Paper: Probing the Dust Grain Alignment Mechanisms in Spiral Galaxies with M51 as the Case Study
Authors: Enrique Lopez-Rodriguez, Le Ngoc Tram
Figure caption: Dust temperature comparison map. Positive percentage differences indicate larger dust temperatures estimated using the modified blackbody fitting to the Herschel data. Negative percentage differences indicate larger dust temperatures estimated using the radiation field map (Equation (5)).
Paper: TIC 435850195: The Second Triaxial Tidally Tilted Pulsator
Authors: Rahul Jayaraman, Saul A. Rappaport, Brian Powell, Gerald Handler, Mark Omohundro, Robert Gagliano, Veselin Kostov, Jim Fuller, Donald W. Kurtz, Valencia Zhang, George Ricker
Figure caption: A comparison of the ratios of the central peak to the sidelobe amplitudes for Y 11x  modes to the limits obtained from the Y 10y  modes in TIC 435850195. The red lines correspond to the ratio of the 2σ detection threshold to the mean amplitude of each Y 10y  doublet. The blue shaded area corresponds to the 1σ uncertainty for the inclination angle of the system, from our light-curve fit.
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: Panel (a): compactness parameter (ℓ) as a function of the dimensionless coronal temperature (Θ e ), from the beginning (green) to the end of our observation (red) after the outburst; the orange-filled circle marks 650 days after the outburst. The Swift observations are labeled with crosses, while the XMM-Newton observations are labeled with filled circles. The low S/N of the Swift/XRT observations results in loose constraints on the coronal temperature; therefore, we did not show the error bars for the Swift observations. The black dashed line shows the threshold between the dominance of Compton cooling and bremsstrahlung cooling (e.g., A. C. Fabian et al. 2015). We also mark the threshold for thermal e −–p (black dotted line) and e −–e − (black dashed–dotted line) (A. C. Fabian 1994) coupling. The pair-production lines (B. E. Stern et al. 1995) are shown with different assumptions for corona geometry: slab (blue solid line), sphere (blue dotted line, and hemisphere (blue dashed line). The black-filled star shows the hyper-Eddington AGN IRAS 04416+1215 (A. Tortosa et al. 2022), while the blue error bars denote the median value of the X-ray-selected AGN sample of C. Ricci et al. (2018). Panel (b): evolution track of 1ES 1927+654 in the Θ e –ℓ plane, color-coded by the time after the outburst, from green to red. The color code of the points, as well as the lines, are the same as for panel (a). The red-filled star shows the Θ e  and ℓ values in 2011 May, before the outburst.
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: Optical to X-ray slope (α OX) as a function of Eddington ratio (λ E) in stages III and IV, color-coded by the time since the outburst (2017 December 23), from the beginning (green) to the end (red); the orange-filled circle marks 650 days after the outburst. The red-filled star shows the value in 2011 May, before the outburst. The cyan line plots the α OX–L 2500 correlation for type 1 AGNs (E. Lusso et al. 2010). The changing-look AGNs that were observed previously are represented by diamonds (J. J. Ruan et al. 2019) and crosses (Q. Yang et al. 2023), with gray denoting faint states and cyan denoting bright states. The background gray (faint states) and cyan (bright points) points represent the predicted AGN accretion state based on X-ray binaries (M. A. Sobolewska et al. 2011). The gray squares show the intermediate-mass black holes in R. Dong et al. (2012). The four black lines correspond to four different states of the accretion disk, discussed in Section 5.3: sparse-dotted line for the ADAF, dashed–dotted line for the gas pressure-dominated thin disk (S-curve lower), middle dashed–dotted line for the radiation pressure-dominated thin disk (S-curve middle), and right dashed line for the slim disk (S-curve upper). T 1 marks the break point of 1ES 1927+654, while T 2 gives the break point of the changing-look AGNs in J. J. Ruan et al. (2019).
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: The optical to X-ray slope (α OX) as a function of the monochromatic luminosity at 2500 Å (L 2500), color-coded by the time since the optical outburst, from the beginning (green) to the end (red); the orange-filled circle marks 650 days after the outburst. The red-filled star shows the pre-outburst value. The blue line shows the α OX–L 2500 correlation for X-ray-selected type 1 AGNs (E. Lusso et al. 2010), with the cyan shaded region indicating the scatter.
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: Evolution of (a) the hard X-ray photon index (Γ) and (b) the plasma optical depth (τ) after the outburst. The x-axis shows the time since the optical outburst on 2017 December 23. In panel (a), the green error bars are derived from our broadband SED fitting (Section 3.1). The red curve shows Γ derived from the NICER observations (M. Masterson et al. 2022), binned to 100 days; the 2σ range for each bin is shown as a red shaded region. The green-filled star and the horizontal dashed line mark the pre-outburst photon index. In panel (b), the blue horizontal line shows the median τ for BASS AGNs (C. Ricci et al. 2018). The green-filled star and the horizontal dashed line mark the pre-outburst plasma optical depth. The vertical dashed lines separate the four evolution epochs discussed in Section 4.1.
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: The coronal plasma optical depth (τ) as a function of dimensionless mass accretion rate (﹩\dot{m}﹩), color-coded by the time since the optical outburst (2017 December 23), from the beginning (green) to the end (red); the orange-filled circle marks 650 days after the outburst. The red-filled star shows the value in 2011 May before the outburst. The black dotted line shows a power-law fit to the observations for the data on the left branch (t > 650 days), with ﹩\mathrm{log}\tau =-2.5\mathrm{log}\dot{m}-1.7﹩. The black dashed line gives a fit with an opposite slope for the data on the right branch (t < 650 days).
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: Optical depth (τ) of the X-ray corona as a function of the Eddington ratio (λ E), color-coded by the time since the outburst (2017 December 23), from the beginning (green) to the end (red); the orange-filled circle marks 650 days after the outburst. The red-filled star shows the value in 2011 May, before the outburst. The blue curve gives the median of the Swift/BAT AGN sample from C. Ricci et al. (2018), where the cyan shaded area corresponds to the median absolute deviation. Blue-filled diamonds show the super-Eddington AGNs analyzed by A. Tortosa et al. (2023), with arrows indicating upper limits. The four black lines correspond to the four different states of the accretion disk discussed in Section 5.3: sparse-dotted line for the ADAF, dashed–dotted line for the gas pressure-dominated thin disk (S-curve lower), middle dashed–dotted line for the radiation pressure-dominated thin disk (S-curve middle), and right dashed line for the slim disk (S-curve upper).
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: The optical bolometric correction (κ 5100) as a function of the dimensionless mass accretion rate (﹩\dot{m}﹩), from the beginning (green) to the end (red); the orange-filled circle marks 650 days after the outburst. The red-filled star shows the pre-outburst value. The black line shows the expected ﹩{\kappa }_{5100}-\dot{m}﹩ correlation for a relativistic thin accretion disk (Equation (3)). The blue line shows the observed κ 5100 for type 1 AGNs (G. T. Richards et al. 2006), with the cyan shaded region indicating the scatter.
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: Cartoon showing the evolution of the accretion flow during the changing-look event in 1ES 1927+654. The four stages are defined in Section 4.1. The evolution of the disk–corona system in each stage is summarized in the text boxes.
Paper: The Interplay between the Disk and Corona of the Changing-look Active Galactic Nucleus 1ES 1927+654
Authors: Ruancun Li, Claudio Ricci, Luis C. Ho, Benny Trakhtenbrot, Erin Kara, Megan Masterson, Iair Arcavi
Figure caption: The optical to X-ray slope (α OX) vs. the coronal plasma optical depth (τ), color-coded by the time since the optical outburst (2017 December 23), from the beginning (green) to the end (red); the orange-filled circle marks 650 days after the outburst. The red-filled star shows the value in May 2011, before the outburst. The black line shows the best-fit relation ﹩\mathrm{log}{\alpha }_{\mathrm{OX}}=0.43\mathrm{log}\tau +0.87﹩, with the gray shaded region indicating the 1σ  uncertainty.
Paper: Cross-correlating Dark Sirens and Galaxies: Constraints on H 0 from GWTC-3 of LIGO–Virgo–KAGRA
Authors: Suvodip Mukherjee, Alex Krolewski, Benjamin D. Wandelt, Joseph Silk
Figure caption: The luminosity distance of the eight selected GW sources from GWTC-3.
Paper: The Impact of Mass-dependent Stochasticity at Cosmic Dawn
Authors: Viola Gelli, Charlotte Mason, Christopher C. Hayward
Figure caption: Left: M UV–M  h  relation at z = 9, populated with galaxies following the halo mass function and colored with the product f esc ξ ion (assuming an exponentially increasing f esc and linearly increasing ξ ion with ΔM UV), showing how up-scattered galaxies will contribute the most to the number density of ionizing photons. Center: escape fraction f esc and ionizing photon production efficiency ξ ion as a function of ΔM UV. For the escape fraction, we show three different cases of constant, linear, and exponential increase toward up-scattered galaxies. Right: Redshift evolution of the fraction of neutral hydrogen in the IGM for the same three scenarios, as well as for the case without scatter, assuming fixed f esc = 0.08 and ﹩{\mathrm{log}}_{10}{\xi }_{\mathrm{ion}}/(\mathrm{Hz}\,{\mathrm{erg}}^{-1})=25.7﹩. We also plot measurements from observations of: the evolution of the Lyα equivalent width (EW, C. A. Mason et al. 2018, 2019; P. Bolan et al. 2022; M. Nakane et al. 2024), the clustering of Lyα emitters (LAE; M. Ouchi et al. 2010; E. Sobacchi & A. Mesinger 2015), Lyα forest dark pixel fraction (I. D. McGreer et al. 2015), and quasar damping wings (F. B. Davies et al. 2018; B. Greig et al. 2019).
Paper: The Impact of Mass-dependent Stochasticity at Cosmic Dawn
Authors: Viola Gelli, Charlotte Mason, Christopher C. Hayward
Figure caption: Examples of star formation histories (left) and continuum spectral energy distributions (right) for three galaxies at z = 10 with same UV magnitude M UV = −20.
Paper: The Impact of Mass-dependent Stochasticity at Cosmic Dawn
Authors: Viola Gelli, Charlotte Mason, Christopher C. Hayward
Figure caption: UVLF at z = 7, 10, 14 for different halo mass functions (left) and transfer functions (right).
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Patches of the sky (yellow) from which Galactic synchrotron foregrounds are randomly drawn to form an ensemble of foreground realizations.
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Cylindrical 21cm–[C II] cross-spectrum with theory and instrument regions overplotted. The yellow lines correspond to the theoretically predicted crossover scale for a fiducial reionization scenario (solid yellow line at k ∼ 1.5 h Mpc−1) and for high-mass reionization (dashed yellow line at k ∼ 0.03 h Mpc−1). The modes accessible by HERA and CCAT-Prime are boxed off with the jointly accessible modes visible in the crosshatched region. With only limited Fourier space overlap, cross-correlation measurements may suffer from sensitivity limitations in addition to systematics.
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Simulated [C II] field (left) and 21 cm field (right) over 6° × 6° with 1′ resolution. In the middle panel, we plot the input theory auto-spectra for 21 cm (solid pink) and [C II] (solid turquoise) and also the input theory cross-spectrum (solid alternating pink and turquoise). The spectra estimated from the simulation cubes are plotted with hollow circle markers for 21 cm (pink), [C II] (turquoise), and their cross (purple). The correspondence between the spectra from simulated cubes and the input theory spectra validates our approach for generating cosmological realizations with the correct statistical properties.
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Brightness of [C II] and relevant CO emission lines as functions of emission redshift z emit and observed frequency. At all observed frequencies considered in this paper, CO interlopers will be a strong contaminant to [C II] observations and at the highest redshifts (z > 6) the CO(2–1) transition is a particularly strong nuisance.
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Top: example 21 cm foregrounds from our simulation pipeline at 200 MHz. The full-sky map shows the Galactic synchotron contribution with the HERA observing stripe superimposed. Each observation is simulated over a 6 × 6 deg2 simulation patch to capture bright foreground sources caught in low-level side lobes of an instrument’s PSF, in contrast to the smaller 2 × 2 deg2 analysis patch. Bottom: example realizations from different constituent components of 21 cm foregrounds described in Section 4.1.
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Flowchart depicting our end-to-end cross-correlation pipeline. Processes run from top to bottom and left to right. This pipeline produces correlated cosmological fields, simulates 21 cm foreground contaminants, simulates CO line interlopers (i.e., [C II] foregrounds), models both single-dish instruments and interferometers, and finally estimates auto- and cross-spectra.
Paper: Forecasts and Statistical Insights for Line Intensity Mapping Cross-correlations: A Case Study with 21 cm × [C II]
Authors: Hannah Fronenberg, Adrian Liu
Figure caption: Top: HERA-array layout assumed for the forecasts in this paper. Bottom: the resulting PSF.
Paper: Convective Magnetic Flux Emergence Simulations from the Deep Solar Interior to the Photosphere: Comprehensive Study of Flux Tube Twist
Authors: Shin Toriumi, Hideyuki Hotta, Kanya Kusano
Figure caption: (Top panels) Temporal evolutions of the Poynting flux in the photosphere, S  z , and the injected magnetic energy, E mag. (Bottom panels) Their peak values as a function of the initial flux tube twist, q/q cr.
Paper: No Evidence for a Dip in the Binary Black Hole Mass Spectrum
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane, Ilya Mandel
Figure caption: Posterior distributions for mass-related population hyperparameters inferred using GWTC-3 data. Blue shows the results when a gap is included, while orange shows the results when a gap is not included. The contours on the two-dimensional panels give the 50%, 90%, and 99% credible intervals.
Paper: No Evidence for a Dip in the Binary Black Hole Mass Spectrum
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane, Ilya Mandel
Figure caption: Log-scale histograms of the masses of all black holes (both m 1 and m 2) in each mock catalog used in Section 4. The colored histograms show the true mass values for the events in a given catalog, while the simulated mass posteriors associated with the events are shown in gray. Note that the cumulative density of the posterior distributions for all events in a given catalog is not represented by the height of the gray distributions (these are normalized per event).
Paper: No Evidence for a Dip in the Binary Black Hole Mass Spectrum
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane, Ilya Mandel
Figure caption: Posterior distributions for gap-related population hyperparameters inferred from mock catalogs with 50, 100, 150, and 200 perfectly measured (zero-uncertainty) events. Each color shows the results for an individual catalog, while the true values are shown by gray dashed lines. The contours on the two-dimensional panels give 90% credible intervals. The legends give the natural log one-dimensional Bayes factors and differences in maximum natural log-likelihoods comparing the gap and no-gap hypotheses for each mock catalog, as well as the natural log Bayes factor comparing the empty-gap to no-gap scenarios. Note that the vertical axes in the marginal posterior distributions are scaled differently for each corner plot.
Paper: No Evidence for a Dip in the Binary Black Hole Mass Spectrum
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane, Ilya Mandel
Figure caption: Toy gap models with (red) and without (gray) a strong preference for mass ratios near unity. The left panel shows identical power-law chirp mass distributions with gaps at ≈10M ⊙–12M ⊙ for both models. The right panel compares the distributions for primary (solid) and secondary (dashed) masses, corresponding to the two models.