adsabs/AstroCLIMB huggingface dataset:
Paper: High Spectral Resolution Observations of Propynal (HCCCHO) toward TMC-1 from the GOTHAM Large Program on the GBT
Authors: Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Corner plot generated from the MCMC analysis of the physical parameters of HCCCHO with 50,000 iterations. Covariance between the parameters is displayed in the off-diagonal panels, while marginalized posterior distributions are shown in the panels on the diagonal. The vertical lines on the posterior distributions denote the 16th, 50th, and 84th confidence intervals.
Paper: Light Echoes of Protoplanetary Disks
Authors: Austin J. King, Benjamin C. Bromley
Figure caption: MCMC echo fits: each of the panels above show the parameter space fit of the modeled echo light curve from Figure 2. The top two panels show fits for disk-like structure. The bottom panels show the same information for ring-like structure. The two left panels represent a near face-on disk (i = 5°) and the two right panels represent a disk inclination of i = 45°. We show confidence boundaries of 1σ  (light blue) and 3σ  (cyan) and true parameters are denoted with a black “+.”
Paper: High Spectral Resolution Observations of Propynal (HCCCHO) toward TMC-1 from the GOTHAM Large Program on the GBT
Authors: Anthony J. Remijan, Zachary T. P. Fried, Ilsa R. Cooke, Gabi Wenzel, Ryan Loomis, Christopher N. Shingledecker, Andrew Lipnicky, Ci Xue, Michael C. McCarthy, Brett A. McGuire
Figure caption: Velocity-stacked spectra and matched-filter response of HCCCHO toward TMC-1. Left: the line profile of propynal determined from the MCMC analysis (red) overplotted with the velocity-stacked spectrum from the GOTHAM data (black). Right: matched-filter impulse response of the stacked spectrum, determined by cross-correlating the observed and simulated velocity stacks.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Sky map of the simulated PTA’s sensitivity, where each pixel across the sky is colored by the expected signal-to-noise ratio (SNR) of a CW signal coming from that sky location, fixed at d  L  = 150 Mpc, and averaged across different binary parameter values (GW frequencies of 2 nHz, 6 nHz, and 20 nHz; chirp masses of 108 M ⊙ and 109 M ⊙; and 100 random draws of ﹩\cos \iota ﹩, ψ, and Φ0). Pulsar positions are represented by the white stars. We inject into a total of nine galaxies, grouped into high (purple markers), mid (light blue markers), and low (orange markers) sky sensitivity regions. These three groups are demarcated by ellipses of the same color. In each sensitivity region, we inject into one galaxy at each of the near, mid, and far distance regimes, corresponding to <100 Mpc (circles), 100−300 Mpc (squares), >300 Mpc (triangles), respectively.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Sky maps of the 90% credible level localization areas recovered for the SNR = 15 injections, shown by the orange two-dimensional histograms outlined by black contours. The host galaxy IDs for each injection are listed at the top of each map. From left to right, the columns correspond to signals localized in regions of the sky with high, mid, and low sensitivity. From top to bottom, the rows correspond to injections with increasing distance ranges of d  L  < 100 Mpc, 100 Mpc < d  L  < 300 Mpc, and d  L  > 300 Mpc. The rows also roughly correspond to different chirp mass ranges, with the lowest chirp masses in the top row and increasing with each successive row. The blue stars represent the pulsar positions.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Sky maps of the 90% credible level localization areas recovered for the SNR = 8 injections, organized in the same manner as Figure 3. Note that the black contours enclose all regions included in the localization area, except for the middle center, bottom center, and bottom right sky maps, where the contours instead indicate excluded regions.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Tension metric examples as computed with tensiometer. The total binary mass posterior for the SNR = 15 injection into galaxy J19231198−2709494 is shown in red. The true galaxy’s total SMBH mass estimate (derived from the M BH–M bulge relation), with a tension of 0.04σ, is shown in yellow. Example distributions with 1σ, 2σ, and 3σ tension with the posterior are indicated by successively lighter-colored dashed lines.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: 90% credible area as a function of the injected SNR. The solid purple, dashed–dotted light blue, and dashed orange curves correspond to each of the three galaxy hosts in the 100−300 Mpc distance range, located in the high (J19231198−2709494), mid (J13010676+3950290), and low (J08475906+3147083) sensitivity regions of the sky, respectively. Uncertainties on the localization areas are ∼13 deg2 at most (at the lowest SNR) and therefore do not appear in the figure. The marker sizes reflect the injected chirp masses, with larger markers indicating higher chirp masses. The dotted gray line shows the expected 1/SNR2 scaling relation.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Zoomed-in localization areas for the SNR = 15 simulation set, arranged in the same layout as in Figure 3. The probability density maps are shown in orange, with darker regions having higher probabilities, and the 90% credible regions are outlined by the black contours. All possible host galaxies in NANOGrav’s catalog that fall within the contours are represented by open circles, while galaxies passing the mass cut appear as blue circles, and galaxies passing both the mass and distance cuts appear as yellow–green circles. The true galaxy is highlighted with white crosshairs. For ease of viewing, the cuts shown here correspond to the 1σ numbers listed under the f bulge = 0.31 columns in Table 5. The median localization area ΔΩ and the number of galaxies N gxy within the area of one representative bootstrapped sky location posterior are provided in the top left corner of each panel.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: 90% credible area as a function of the injected chirp mass of the binary, fixed at SNR = 20 for the galaxy J08475906+3147083. The full signal injections are shown by the solid yellow line, with lighter (or more yellow) markers representing lower chirp masses and darker (or more blue) markers representing higher chirp masses. The Earth-term-only injections are shown by the dashed red line. Uncertainties on the localization areas are all <1 deg2.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Obtaining a 1G BH mass distribution from the IMF. The progenitor IMF (bottom panel) gets transformed through the M I to M BH mapping (top right panel), resulting in a distribution for ﹩{dN}/{{dM}}_{1{\rm{G}}}﹩ of BHs in 1G systems. We label parameters underlying the 1G BBH mass distribution: a and b are the low-mass and high-mass spectral indices of the progenitor IMF, respectively, and ﹩{M}_{\mathrm{tr}}﹩ and ﹩{M}_{\mathrm{BH},\max }﹩ (dashed lines) control the onset of the nonlinearity and the maximum of the quadratic part of the mapping, respectively. The blue shaded region is the 90% credible region of the lognormal mapping for our choice of σ (see Equation (5) and preceding equations for the functional form). We vary these parameters in our fit to the LIGO–Virgo data, together with the parameters for the second-generation (2G) population (see Section 3.2).
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: 90% credible area for each of the SNR = 15 injections, shown as a function of the interpolated median angular separation between the source and the 10 nearest pulsars on the sky. Uncertainties on the localization areas are ∼2 deg2 at most. As in Figure 1, the sources’ colors correspond to the different sensitivity regions, and their marker shapes correspond to the different distance ranges.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Zoomed-in localization areas for the SNR = 8 simulation set, including only those localization areas that are well constrained, i.e., the entire left column and first two panels in the right column of Figure 4. Each panel is formatted in the same manner as in Figure 9. For ease of viewing, these cuts correspond to the 1σ numbers listed under the f bulge = 0.31 columns in Table 6.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Cumulative distribution of SMBH mass tension values for galaxies in the SNR = 8 localization region for source J04122834+2742065 (shown in the top right panel of Figure 10). Because a small percentage of galaxies have infinite sigma tension with the GW posterior, the distributions do not reach a cumulative fraction of 1. The solid dark blue and light blue curves correspond to all unknown-type galaxies having SMBH masses estimated with f bulge = 1 and f bulge = 0.31, respectively. The tension value for the true galaxy is indicated by the vertical dashed line.
Paper: Identifying the Host Galaxies of Supermassive Black Hole Binaries Found by Pulsar Timing Arrays
Authors: Polina Petrov, Stephen R. Taylor, Maria Charisi, Chung-Pei Ma
Figure caption: Distribution of pulsar-term frequencies for the injected binary chirp masses in Figure 7. The color scale corresponding to the different chirp masses is the same as in Figure 7. The injected Earth-term frequency of 20 nHz is indicated by the dashed red line.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: BH mass spectrum following our model in Equation (7) for different choices of (clockwise from top left) ﹩{M}_{\mathrm{tr}}﹩, ﹩{M}_{\mathrm{BH},\max }﹩, f pl, and σ. For the top left figure, we consider constant difference between ﹩{M}_{\mathrm{tr}}﹩ and ﹩{M}_{\mathrm{BH},\max }﹩. Unless being varied, we assume the following fiducial parameters: ﹩a=2,b=1,c=2.5,{M}_{\mathrm{tr}}=35{M}_{\odot },{M}_{\mathrm{BH},\max }\,=45{M}_{\odot },\sigma =0.05﹩, and f pl = 0.04.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Mass spectrum derived from our model (green) with no evolution of the mass distribution with redshift compared to the POWERLAW + PEAK mass spectrum informed by the same events (blue). We do not include redshift evolution of the mass distribution in this comparison as the models in LIGO Scientific Collaboration et al. (2023a) do not include mass–redshift correlations. POWERLAW + PEAK results were obtained using GWPopulation (C. Talbot et al. 2019). Top: comparison of the primary mass distributions. Bottom: comparison of the mass ratio distributions.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Representation of the M I–M BH relationship of the nonevolving ﹩\tfrac{{dN}}{{{dM}}_{1{\rm{G}}}}﹩ model in Section 3.2. Bottom panel: inferred distribution for the IMF of M I in merging binaries. Top right panel: 1σ credible region of the 95th percentile (higher blue shaded region) and 5th percentile (lower blue shaded region) for the inferred M I–M BH mapping. The dotted line is a single representative draw from the posterior.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Posterior for selected mass distribution population parameters from the evolving mass distribution model in Section 3.4 (magenta). One-dimensional posteriors from the nonevolving mass model overplotted in green for reference.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Posterior for selected mass distribution parameters using the model outlined in Section 3.2. Dark- and light-green shaded regions are the 1σ and 2σ contours, enclosing 39% and 86% of the probability, respectively. The prior distribution is shaded gray for reference. We find that widening the prior does not meaningfully increase the posterior support for the PPISN feature at higher masses.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Inferred mass distribution parameters using the evolving mass model in Section 3.4, but adopting a wider prior on ﹩{\dot{M}}_{\mathrm{tr}}﹩. The prior distribution is shaded gray for reference.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Model for a redshift-dependent mass distribution evaluated at selected redshifts assuming ﹩{\dot{M}}_{\mathrm{PISN}}=5\,{M}_{\odot }﹩ in Equation (10). All other parameters are the same as the fiducial set in Figure 2.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Draws from the nonevolving mass distribution posterior, evaluated at z = 0.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Redshift distribution parameters inferred with the evolving mass distribution model in Section 3.4. The prior distribution is shaded gray for reference.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: HST/WFC3 (∼1 arcmin2) image of SDSS1029 in the F160W band. The 26 spectroscopically confirmed multiple images included in our analysis are marked with circles, color-coded per system. Spectroscopic cluster members are marked with blue crosses. The two line-of-sight galaxies included in our multiplane strong-lensing modeling are highlighted with orange crosses. The seven objects for which the light distribution is modeled are indicated with cyan dashed circles and labeled following Section 3.3. The arc mask, which encompasses the light of the three QSO multiple images and the host galaxy, is shown in green.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: Zoom-in around the strongly lensed QSO host galaxy in the WFC3/F160W band. Left: the cyan regions show the lensmasks, encompassing the seven luminous objects for which the light distribution is modeled. In total, the lensmasks contain ∼9.3 × 104 HST pixels. Right: the red regions indicate the areas where the observational uncertainties associated with the science image are boosted (by a factor of 10) when modeling the extended surface brightness of the lensed arc (see Section 3.4). The number of boosted pixels represents ∼20% of the arc mask (in green).
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: Best-fit models for the surface-brightness distribution of the seven perturbing objects (following the labeling from Figure 1). From left to right: the observed HST F160W-band imaging, the best-fit model of their surface-brightness distribution, and the normalized residuals in a range from −5σ to 5σ. Angular scales of 1″ are shown in the middle panels. North is up and east is left.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Top: relationship between σ  C12 and lower edge of the upper mass gap, reproduced from data release of R. Farmer et al. (2020). Center: posterior distribution of 12C(α, γ)16O reaction rate, in terms of standard deviations away from the median reaction rate in STARLIB (A. L. Sallaska et al. 2013), computed by evaluating the fit in the top panel for the samples of ﹩{M}_{\mathrm{BH},\max }﹩ in the posterior in Figure 7. Bottom: inferred distribution of S 300, extrapolated from the distribution of σ  C12 as calculated from the fit in the top panel. Constraints on S 300 from R. J. deBoer et al. (2017) plotted for comparison, showing tension with the values implied from our results.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: Best-fitting source surface-brightness reconstruction of the QSO host galaxy and modeling. Top left: best-fitting source surface-brightness reconstruction of the QSO host galaxy on the source plane within an area of ﹩\sim 3.5\,{\mathrm{arcsec}}^{2}﹩, at z = 2.1992. Bottom left: reprojected source onto a rectangular, isotropic grid. The bars show angular scales of 0.″5 along the horizontal and vertical axes for both the reconstructed and reprojected source. Top right: best-fitting surface-brightness distribution model of the reconstructed source (shown in the top left panel), obtained with a single Sérsic profile. Bottom right: normalized residuals in a range between −5σ and 5σ.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: Best-fit surface-brightness reconstruction of the QSO host galaxy at z = 2.1992. From left to right: the observed HST F160W-band image over a ∼11″ × 29″ field of view (or ∼73 kpc × 192 kpc at the galaxy cluster redshift), the best-fit model, and the normalized residuals in a range between −5σ and 5σ. North is up and east is left.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: RGB image constructed with the HST passbands F435W (blue), F814W (green), and F160W (red) of the central region of SDSS1029, where we display the isodensity contours [0.65, 0.85, 1.35] of the convergence for D ls/D s = 1. The green and magenta contours correspond, respectively, to the best-fit position-based Lenstool model (Model 1 in A22) and the GLEE best-fit extended model presented in this work.
Paper: Physical Models for the Astrophysical Population of Black Holes: Application to the Bump in the Mass Distribution of Gravitational-wave Sources
Authors: Jacob Golomb, Maximiliano Isi, Will M. Farr
Figure caption: Selected population-level parameters from the evolving mass distribution analysis, without reweighting spins (pink, as presented in Section 4.2) and with reweighting spins to a fiducial population estimate (blue). The near-identical posteriors show that the spin population assumptions in this work do not cause a bias.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: 1σ and 2σ confidence levels of the joint 2D probability distributions of the velocity dispersion and truncation radius of the foreground spiral galaxy (SP; left) and the hidden galaxy (GX; right) from the position-based Lenstool and the extended GLEE lens models, in green and magenta, respectively. The black lines denote levels of equal total mass in solar mass units. In the adopted cosmology, 1″ corresponds to a physical scale of 6.18 kpc and 7.04 kpc at the redshifts of SP and GX, respectively. We note that both galaxies are modeled instead at the lens cluster redshift (z = 0.588) in the position-based Lenstool model by A22.
Paper: The Next Step in Galaxy Cluster Strong Lensing: Modeling the Surface Brightness of Multiply Imaged Sources 
Authors: Ana Acebron, Claudio Grillo, Sherry H. Suyu, Giuseppe Angora, Pietro Bergamini, Gabriel B. Caminha, Sebastian Ertl, Amata Mercurio, Mario Nonino, Piero Rosati, Han Wang, Andrea Bolamperti, Massimo Meneghetti, Stefan Schuldt, Eros Vanzella
Figure caption: Results from the [O II] gas kinematic analysis of the foreground spiral galaxy, SP. Left: HST color cutout centered on SP. Middle: rest-frame velocity field of SP derived from the [O II] emission line and using a systemic redshift of 0.511 for the center of the galaxy. Right: derived rotation velocities projected along the kinematic major axis, indicated with the pink solid line on the velocity map.