adsabs/AstroCLIMB huggingface dataset:
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: 21 cm line spectra toward the IC 443 shocked clumps B, C, and G. Each spectrum is from a position centered on the clump, with nearby background subtracted. At low velocities, indicated by the vertical gray dashed lines, the spectrum is strongly contaminated by absorption of the SNR synchrotron emission by cold foreground gas and should be ignored.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Observed H2 S(5) and S(1) spectra of IC 443 B (top) and IC 443 C (bottom) with scaled model spectra. The models are labeled with their name from Table 3. The sum of models (black curve) matches the overall velocity distribution. The bulk of the modeled S(5) flux is from shocks into gas with moderate densities, while the S(1) line is mostly from shocks into high-density gas, although all models contribute to both lines.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Distribution of MaNGA galaxies on the diagram of redshift vs. r-band absolute magnitude. The spatial resolution, corresponding to the physical scale of a typical PSF FWHM of 2.″5, is also shown along the ordinate. The galaxies populate two branches, corresponding to the MaNGA primary and secondary samples. To ensure sufficient spatial resolution, we limit our sample galaxies at redshift z < 0.05 with axial ratios b/a > 0.5.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Color images of a random sample of MaNGA star-forming galaxies, illustrating the difference between compact and extended galaxies. Images are composed from gri bands. Within each mass bin, two compact galaxies are displayed on the left, while two extended galaxies are shown on the right. All images are scaled to cover 30 kpc on each side.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Selection of star formation galaxies. Star formation galaxies are selected by requiring their locations on the SFMS with a width of 0.5 dex, and the fractions of the star formation spaxels are larger than 50%.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Sample distribution in the mass–size plane. The selected star-forming galaxies are separated into different mass–size bins. The solid line is the mass–size relation for late-type galaxies in SDSS (S. Shen et al. 2003).
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Distribution of star formation residual Δlog SFR, H I mass log M H I , dust extinction A V, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩, and stellar spin ﹩{\lambda }_{{R}_{{\rm{e}}}}﹩ as a function of radius residual Δlog R e. Δlog SFR and Δlog R e represent the residuals from the SFMS and the mass–size relation, respectively. Gray dots are the star-forming galaxies selected in our sample. Larger symbols show the median values for compact and extended galaxies, with different colors indicating different mass bins. Error bars indicate their median errors. The Pearson correlation coefficient r and the p-values are listed in the top right corner of each panel.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Radial profiles of sSFR (left) and the stellar mass density (Σ*)–sSFR relationship (right) in different mass–size bins. The color of the lines represents different stellar mass bins. In each mass bin, dotted lines with filled dots are the median profiles from compact galaxies, while solid lines with open circles are the median profiles from extended galaxies. The shaded region represents the error on the median profile. In the right panel, gray dashed lines are the linear fits to the Σ*–sSFR relationships (only the fits for three lower mass bins in compact galaxies are shown for clarity). A constant sSFR is indicated as the dotted gray line (B. C. Hsieh et al. 2017).
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: (a) The changes of D  n (4000) as a function of stellar mass with corresponding errors. The central values that change with different stellar masses are shown in solid lines, and the trends at R e are shown in dashed lines. Compact and extended galaxies are separated into filled coral dots and open green circles, accordingly. (b) The changes of EW(Hδ) as a function of stellar mass. (c) D  n (4000) vs. EW(Hδ) diagram. The gray solid lines are the predictions of the G. Bruzual & S. Charlot (2003) model with declining star formation history.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Upper left: the metallicity residuals at fixed M * as a function of local stellar mass density Σ*. The best-fit curve is shown as a solid line, following the formula provided in the lower right corner. Upper right: the residuals of metallicity at fixed M * and Σ* as a function of ΔsSFR. Symbols are the same as in Figure 9. See the text for more details on how these metallicity residuals are calculated. Lower: same as the upper panels but for ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      DOP16.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Radial profiles of ΣSFR, Σ*, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      PG16, and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      DOP16 in different mass–size bins. The color of the lines represents different stellar mass bins. In each mass bin, dotted lines with filled circles are the median profile from compact galaxies, while solid lines with open circles are the median profiles from extended galaxies. The shaded region represents the error on the median profile. The gray dashed line is the linear fit to the median profile (in radial range >0.5R e) in each mass–size bin.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Radial profiles of Σ*, ΣSFR, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      PG16, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      DOP16, A V, D  n (4000), EW(Hδ  A ), and EW(Hα) for each mass–size bin. Gray lines show the profiles for individual galaxies, with radius measured in steps of 0.2 R e along the semimajor axis. The median profiles are color-coded by stellar mass, with solid lines representing extended galaxies and dotted lines representing compact galaxies. The shaded regions indicate the errors on the median profiles.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: The metallicity as a function of stellar mass density (Σ*) in different mass–size bins. Both ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      PG16 (left) and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      DOP16 (right) are shown. The color of the lines represents different stellar mass bins. Symbols are the same as in Figure 9. Gray dashed lines are the linear fits to the Σ*–12 + log(O/H) relationships. The best-fit rMZR in J. K. Barrera-Ballesteros et al. (2016) is indicated by the dotted line.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Same as Figure 5 but for central stellar velocity dispersion σ *,cen and Sérsic index n.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: The fitting coefficients for the Σ*, ΣSFR, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      PG16, and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩                      DOP16 profiles as a function of stellar mass. Compact and extended galaxies are shown in coral and green dots accordingly with their errors.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Upper panels: the Σ* and ΣSFR profiles in the convolved extended galaxies (purple lines) compared with the original profiles in compact and extended galaxies (dotted lines with filled dots and solid lines with open circles, respectively) in the lowest mass bin. Lower panels: the sSFR profiles and their relations with Σ*.
Paper: Radial Profiles of Σ*, ΣSFR, Gas Metallicity, and Their Correlations across the Galactic Mass–Size Plane
Authors: Lin Lin, Shiyin Shen, Hassen M. Yesuf, Ye-Wei Mao, Lei Hao
Figure caption: Same as Figure 13 but for A V, D  n (4000), EW(Hδ  A ), and EW(Hα).
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Evolution of observed parameters during the flare, with aligned X-axes. Row 1: flux rope eruption observed by AIA 131 Å; the yellow line shows the upper limit of the plot in row 2. Row 2: growth of the fan structure, observed by the IRIS 1330 Å SJI. Diagonal black dots show the movement of the rastering slit, and larger black squares are an artifact of the SJI. Row 3: time series of GOES 1–8 Å, STIX 6–12 keV, STIX 12–25 keV, STIX 25–50 keV, and IRIS Fe XXI intensity. Row 4: IRIS Fe XXI nonthermal velocity and Doppler velocity. The vertical gray lines in rows 3–4 mark the time period analyzed in this study.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Detrended time series over a 100 s period, for the parameters presented in Figure 2. The data cover a subset of the Figure 2 time range, spanning the area between the vertical gray lines. The scale of the top and middle plots is a percentage of the maximum value.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Wavelet analysis (Morlet) of the full time-series range plotted in Figure 2, cropped to the Figure 5 time range of interest for comparison. The vertical dashed lines in some wavelet plots show the start/end time of those observations, with the plot extended to show the ease of comparison to other parameters (the wavelet analysis is applied to the nonextended time series). The orange lines show the cone of influence for the wavelet. For some parameters, the boundaries of the cone of influence sit outside of the time range plotted here (but the data are within the cone). In the right column, we show the global wavelet spectrum, with the red line showing the 95% confidence interval.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Top row: LOS integrated maps of simulated Fe XXI parameters. Second row: time series of mean emission over the yellow box in the above row, with a smoothed curve overplotted in gray. Third row: comparison between detrended oscillations in both simulated and observed Fe XXI emission. Bottom row: FFT of the detrended simulated Fe XXI time series.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Left/Center: global FFT of the raw STIX 6–12 keV (left) and GOES 1–8 Å (center) time series shown in Figure 2. The vertical dashed lines mark a local spike at 48 s. The solid and dashed green lines show the power-law confidence fit and 2σ level, respectively. Right: relative locations of Solar Orbiter and Earth observatories (GOES/SDO/IRIS), relative to the Sun.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Example IRIS Fe XXI 1354.8 Å spectral map, from the peak of Fe XXI intensity emission. Four example pixels are chosen to demonstrate the quality of the single Gaussian fit.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption:  12CO v = 1–0 line stack in the stellar reference frame. The continuum is marked with a dashed gray line. A Gaussian fit to the profile is overplotted in red. A deep (∼40%), blueshifted absorption feature centered at −5.9 km s−1 (marked by a dashed black line) can be clearly seen. No significant emission is present. The portion of the spectrum from −51 to −29 km s−1 has been masked out due to telluric absorption.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Schematic showing the data points used in the SliRM moving average for the first three time steps of an eight-step raster.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption: Individual 12CO v = 1–0 transitions with detections. Zero velocity is marked in an orange dashed line, and transitions are labeled. Gaussian fits to the data are plotted in red. The reported velocities are in the stellar reference frame. We did not include P6 in our subsequent analysis, and so do not plot its Gaussian fit here, but we do include it in our stacked line profile in Figure 4. Gaps in the line profiles are due to removal of telluric absorption features.
Paper: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
Authors: Ryan J. French, Laura A. Hayes, Maria D. Kazachenko, Katharine K. Reeves, Chengcai Shen, Juraj Lörinčík
Figure caption: Subsection of Figure 6, showing Fe XXI intensity wavelet analysis. The 1330 Å SJI wavelet is overplot in orange.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption: A comparison of features between the sky transmission, standard star, CX Tau raw, and CX Tau standard-corrected spectra. The sky transmission spectrum is taken from Gemini, and therefore has a higher spectral resolution than the Keck data. All wavelengths are in the observed reference frame. Regions where the sky transmission falls below 70% are marked in gray vertical sections. Orange dashed lines show the wavelength of empirically identified absorption features.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption:  M-band (4.64–4.74 μm) spectrum of CX Tau. 12CO (v = 1–0) rovibrational transitions along the P- and R-branches are labeled and marked in orange. No clear CO emission features can be seen, but there is persistent, narrow absorption at low energy levels.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption: The emission surface of rotational CO (J = 2–1) determined from ALMA observations by S. Facchini et al. (2019), constructed using the disksurf software tool. The points are color coded by the gas temperature under the (good) assumption that the CO is optically thick. The arrows shows the viewing direction given the disk inclination of 55° (note that the plot aspect ratio is not unity).
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption: Rotation diagram of 12CO (v = 0–1). The solid line is the line of best fit assuming a two-temperature component model.
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Relation between remnant spin and kick in quasi-circular BH mergers. The left panel assumes an isotropic spin prior allowing for orbital precession and mass ratios q ≤ 6 while the central and right ones are restricted to aligned spins, parallel to the orbital angular momentum of the binary, and mass ratios q ≤ 2 and q ≤ 6, respectively. The color code denotes the probability density.
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Posterior distributions for the ancestral masses and birth kicks of the primary component BH of GW190521. We show the posterior two-dimensional 68% and 90% credible regions, together with the corresponding one-dimensional posterior distributions. The left panel corresponds to a p(θ anc) distribution allowing for precessing ancestors while the central and right panels correspond to aligned-spin ancestors, respectively restricted to mass ratios q ≤ 2 and q ≤ 6. Results obtained under the original LVK analysis of GW190521 are shown in blue while those obtained under the eccentric merger analysis by I. M. Romero-Shaw et al. (2020) are shown in orange. Prior distributions are shown in gray.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption: JWST-MIRI image of the H2 S(1) transition at ∼17.02 μm. The location of the central protostar is marked with a white star. The region within 1.22 λ / D ≅ 0.″66 is marked in a white circle and all pixels that are located at least partially inside have been masked out of the image for our analysis purposes, as continuum subtraction within this region is highly uncertain. The cold rotational CO components from S. Facchini et al. (2019) are plotted in blue contours.
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Ancestral spin magnitudes. Posterior distributions for the spin magnitudes of the ancestral BBHs of GW190521. The left panels correspond to our precessing distribution p(θ anc) for the ancestors while the right panels correspond to our aligned-spin ones. The blue and orange distributions correspond, respectively, to a quasi-circular and eccentric scenario for GW190521. Prior distributions are represented in gray.
Paper: Gone with the Molecular Wind: Photoevaporation in the Compact Dust Disk around CX Tau
Authors: Alexa R. Anderson, Jonathan P. Williams, Geoff A. Blake, Klaus M. Pontoppidan, Colette Salyk, A. C. Adwin Boogert, Clara Ross, L. Ilsedore Cleeves
Figure caption: JWST-MIRI image of the [Ne II] transition at ∼12.8 μm. The location of the central protostar is marked with a white star. The region within 1.22 λ / D ≅ 0.″5 is marked in a white circle and all pixels that are located at least partially inside have been masked out of the image for our analysis purposes, as continuum subtraction within this region is highly uncertain.
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Posterior distributions for the ancestral masses and birth kicks of the secondary component BH of GW190521. Same as Figure 3 but for the secondary component of GW190521.
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Spin magnitudes for the GW190521 component BHs. The left (right) panel corresponds to the primary (secondary) BH. Blue distributions correspond to the quasi-circular precessing scenario for GW190521, originally reported by the LVK collaboration (R. Abbott et al. 2020a), while the orange ones correspond to the eccentric nonprecessing scenario described in I. M. Romero-Shaw et al. (2020).
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Viability of the components of GW190521 as the result of a merger of stellar-origin BHs as a function of the escape velocity of the host environment. The left (right) panel corresponds to the primary (secondary) BH. Solid (dashed) curves correspond to a quasi-circular (eccentric) interpretation for GW190521. Blue (red) curves correspond to our precessing (aligned-spin) p(θ anc) distribution for the ancestor BHs. We highlight typical maximal values for four different types of host environments, namely globular clusters, the Milky Way, nuclear star clusters, and elliptical galaxies.
Paper: Kicking Time Back in Black Hole Mergers: Ancestral Masses, Spins, Birth Recoils, and Hierarchical-formation Viability of GW190521
Authors: Carlos Araújo-Álvarez, Henry W. Y. Wong, Anna Liu, Juan Calderón Bustillo
Figure caption: Ancestral effective-spin parameters. Same as Figure 5 for the effective spin χ eff and effective spin-precession χ  p  parameters of the ancestral BH binaries of GW190521.