adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Structure and Evolution of BASS Active Galactic Nuclei through Eddington Ratios
Authors: Tonima Tasnim Ananna, C. Megan Urry, Claudio Ricci, Priyamvada Natarajan, Ryan C. Hickox, Benny Trakhtenbrot, Ezequiel Treister, Anna K. Weigel, Yoshihiro Ueda, Michael J. Koss, F. E. Bauer, Matthew J. Temple, Mislav Baloković, Richard Mushotzky, Connor Auge, David B. Sanders, Darshan Kakkad, Lia F. Sartori, Stefano Marchesi, Fiona Harrison, Daniel Stern, Kyuseok Oh, Turgay Caglar, Meredith C. Powell, Stephanie A. Podjed, Julian E. Mejía-Restrepo
Figure caption: Decline of the covering factor after an active galactic nuclei (AGN) reaches high enough λ Edd that radiation pressure exceeds the gravitational pull on obscuring matter (at ﹩\mathrm{log}\,{\lambda }_{\mathrm{Edd}}\geqslant -1.7﹩; Fabian et al. 2008), shown for two different assumed temporal dependences (dashed and solid black lines represent sigmoid and exponential functions, respectively, as in Equation (4)), evaluated for two different definitions of obscured vs. unobscured classes (sorted by ﹩\mathrm{log}\,{N}_{{\rm{H}}}﹩ or spectral line width). The colored lines show the decay for a 1000 AGN starting from different covering factors (see Section 2.2). Assuming that the ratio of obscured to overall AGN is a time-averaged covering factor (see bottom panel of Figure 2), we use an ensemble sampler to constrain the model parameters (shown in legend). All black lines and associated shaded regions show covering factor decay for ﹩-1\leqslant \mathrm{log}\,{\lambda }_{\mathrm{Edd}}\leqslant 0.5﹩. Exponential decay functions at two lower Eddington ratios are shown using blue lines: blue dotted lines show results for ﹩\mathrm{log}\,{\lambda }_{\mathrm{Edd}}\,=\,﹩−1.5 and blue dashed lines show results for ﹩\mathrm{log}\,{\lambda }_{\mathrm{Edd}}\,=\,﹩−1.2. The residual covering factor is higher at lower λ Edd.
Paper: Probing the Structure and Evolution of BASS Active Galactic Nuclei through Eddington Ratios
Authors: Tonima Tasnim Ananna, C. Megan Urry, Claudio Ricci, Priyamvada Natarajan, Ryan C. Hickox, Benny Trakhtenbrot, Ezequiel Treister, Anna K. Weigel, Yoshihiro Ueda, Michael J. Koss, F. E. Bauer, Matthew J. Temple, Mislav Baloković, Richard Mushotzky, Connor Auge, David B. Sanders, Darshan Kakkad, Lia F. Sartori, Stefano Marchesi, Fiona Harrison, Daniel Stern, Kyuseok Oh, Turgay Caglar, Meredith C. Powell, Stephanie A. Podjed, Julian E. Mejía-Restrepo
Figure caption: Schematic diagram of AGN circumnuclear structure at low and high Eddington ratios. Top panel: for λ Edd < −2, radiation pressure is too low to remove dust and gas around the AGN, so the covering factor remains high and differences between obscured and unobscured AGN are likely due to viewing angle. That is, because 80% of AGN have ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\gt 22﹩, the torus rises to 56◦ above the equatorial plane; since optical broad lines’ emission are seen in 60% of AGN, the densest gas lies below 37°. Bottom panel: at high λ Edd, radiation pressure removes the obscuring matter, leaving at most a small persistent covering factor (<5%). We find that BLR is visible from nearly all angles after 30% of the time at this λ Edd, which may indicate that the height of the BLR region rises above that of the depleted torus.
Paper: Probing the Structure and Evolution of BASS Active Galactic Nuclei through Eddington Ratios
Authors: Tonima Tasnim Ananna, C. Megan Urry, Claudio Ricci, Priyamvada Natarajan, Ryan C. Hickox, Benny Trakhtenbrot, Ezequiel Treister, Anna K. Weigel, Yoshihiro Ueda, Michael J. Koss, F. E. Bauer, Matthew J. Temple, Mislav Baloković, Richard Mushotzky, Connor Auge, David B. Sanders, Darshan Kakkad, Lia F. Sartori, Stefano Marchesi, Fiona Harrison, Daniel Stern, Kyuseok Oh, Turgay Caglar, Meredith C. Powell, Stephanie A. Podjed, Julian E. Mejía-Restrepo
Figure caption: The distribution of type I (green crosses) and type II (orange crosses) AGN in column density-Eddington ratio space. There are 276 obscured AGN (﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\geqslant 22﹩), compared to 220 type II AGN (narrow lines). Similarly, there are 301 AGN with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\lt 22﹩, and 366 type I AGN, some of which have high column densities.
Paper: Tidally-induced Magnetar Super Flare at the Eve of Coalescence with Its Compact Companion
Authors: Zhen Zhang, Shu-Xu Yi, Shuang-Nan Zhang, Shao-Lin Xiong, Shuo Xiao
Figure caption: The ratio η between the tidal force arisen from the companion and the critical distorting force that the crust can sustain, as a function of time; t  c  is the coalescence instance. When η surpasses unity, the crust is thought to be destructed. Different colors correspond to different ρ eff, and the orbital frequencies at the critical points are labeled.
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: Architecture of planetary systems at the end of our simulations, i.e., after dynamical instabilities have taken place. The horizontal axis shows the orbital period and the y-axis the planetary radius as calculated from the MRRs of Zeng et al. (2019). Planets are shown as individual dots. We only show planets with orbital periods shorter than 100 days. In all these models, more than ∼95% of the resonant chains became unstable after gas disk dispersal. Models A, B, and C are shown from left to right. Points are color-coded according to the planets’ number of late giant impacts (top row of panels), masses (middle row of panels), and ice-mass fractions (right column). We ignore the effects of photoevaporation and/or other subsequent atmospheric mass loss in all these cases (see the Appendix for simulations where the effects of photoevaporation are included). The dashed lines in the bottom panels show the exoplanet radius valley slope, calculated as ﹩R={10}^{-0.11{\mathrm{log}}_{10}(P)+0.4}﹩ (Gupta & Schlichting 2019; Van Eylen et al. 2019). The green background contours show the kernel density distribution of the planets in our simulations (dots of the figure).
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: Left: planet-radius distribution. Right: planet size-ratio distribution of adjacent planet pairs. These distributions are computed after dynamical instabilities and the breaking of the resonant chains. Exoplanets are shown in gray. Blue shows the outcome of our planet-formation simulations. Red shows the outcome of our planet-formation simulations including the effects of photoevaporation. From top to bottom, the panel rows show models A, B, and C. For all models, we use the MRR of Zeng et al. (2019) assuming an uncertainty of 7% in size and an initial atmosphere-to-core-mass ratio of 0.3%. We build these histograms accounting for uncertainties in radius by generating the possible radius of each planet 100 times.
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: Architecture of planetary systems at the end of the gas disk dispersal phase, i.e., before the onset of dynamical instabilities and the breaking of resonant chains. Planet sizes are calculated assuming primordial atmosphere-to-core-mass ratios of 0.3%. The horizontal axis shows the orbital period and the y-axis shows the planetary radius as calculated from the MRR from Zeng et al. (2019). Planets are shown as individual dots. Panels show the results of all simulations and all planets (P < 100 days) produced in each model. From top to bottom, it shows models A, B, and C, respectively. Individual planets are color-coded according to their masses (left-column) and ice/water-mass fractions (right-column panels).
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: Final planetary systems produced in Model-C. Each line shows one planetary systems. The color coding indicates the planet’s composition. A black ring around the dot indicates the presence of an atmosphere, and the full size of the dot scales with its radius. When determining the final planet sizes, we include atmospheric stripping by photoevaporation after the giant-impact phase. Planets’ atmospheric masses, when present, are assumed to correspond to 0.3% of the core mass.
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: Left: planet-radius distribution. Right: planet size-ratio distribution of adjacent planet pairs. Observations are shown in gray. Blue shows the outcome of our planet-formation simulations. Red shows the outcome of our planet-formation simulations modeling the effects of photoevaporation. Black shows the synthetic transit observations of our simulations. Green shows the synthetic transit observations when we include the effects of photoevaporation. From top-to-bottom, the panel-rows show models A, B, and C. For all models, we use the MRR of Zeng et al. (2019) assuming an uncertainty of 7% in size and an initial atmosphere-to-core-mass ratio of 0.3%.
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: Fraction of planets of different types produced in our simulations of model C that match the radius valley and peas-in-a-pod feature. The left-hand-side pie chart shows the relative fractions when the effects of photoevaporation are ignored. The right-hand-side panel shows the relative fraction when we include the effects of photoevaporation.
Paper: The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
Authors: André Izidoro, Hilke E. Schlichting, Andrea Isella, Rajdeep Dasgupta, Christian Zimmermann, Bertram Bitsch
Figure caption: The same as Figure 2 but for model D.
Paper: First Detection of Silicon-bearing Molecules in η Car
Authors: C. Bordiu, J. R. Rizzo, F. Bufano, G. Quintana-Lacaci, C. Buemi, P. Leto, F. Cavallaro, L. Cerrigone, A. Ingallinera, S. Loru, S. Riggi, C. Trigilio, G. Umana, E. Sciacca
Figure caption: Beam-averaged spectra of η Car between 219.100 and 220.950 GHz extracted from the clumps indicated in Figure 1. The spectra have been smoothed to a resolution of ∼5 km s−1. In each panel, the markers indicate the frequency of the 13CO J = 2 → 1 transition shifted to the velocity of the strongest SiO component.
Paper: First Detection of Silicon-bearing Molecules in η Car
Authors: C. Bordiu, J. R. Rizzo, F. Bufano, G. Quintana-Lacaci, C. Buemi, P. Leto, F. Cavallaro, L. Cerrigone, A. Ingallinera, S. Loru, S. Riggi, C. Trigilio, G. Umana, E. Sciacca
Figure caption: Beam-averaged spectra of η Car between 217.000 and 218.850 GHz extracted from the clumps indicated in Figure 1. The spectra have been smoothed to a resolution of ∼5 km s−1. In each panel, the markers indicate the frequencies of the transitions listed in Table 1 shifted to the velocity of the strongest SiO component.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption:  R-process signatures may be detectable in the photospheric phase if ejecta velocities are high—even for low mixing coordinates ψ mix. Colored regions indicate the minimum mixing coordinate (﹩{\psi }_{\min }﹩) for which M  rp = 0.05 M ⊙ produces a detectable signal, as a function of M ej and E k. Lines of constant β ej are overplotted. As described in the text, to be observable, a signal must fulfill both (a) ﹩{\tau }_{\mathrm{tr}}\leqslant 3{\tau }_{\mathrm{pk}}﹩ and (b) ﹩{{ \mathcal R }}_{{\rm{L}}}\geqslant 0.3﹩ at any time ﹩{\tau }_{\mathrm{tr}}\leqslant t\leqslant 3{\tau }_{\mathrm{pk}}﹩. A deeply buried r-process core (small ψ mix) is difficult to observe except in cases of low M ej and/or high E k. For typical SN Ib/c parameters (M ej/M ⊙ ∼ a few, β ej ∼ 0.03), r-process detection will be challenging unless mixing is extensive. On the other hand, the higher velocities of SNe Ic-BL, including GRB-SNe, should facilitate detection, even for low ψ mix. Scatter markers show E k and M ej for a handful of observed SNe (with error bars omitted to improve readability) from Cano et al. (2017).
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: A schematic illustration of our r-process collapsar model, with the main model parameters and emission components highlighted. All models are defined by their total mass, M ej, and kinetic energy, E k (which together define a characteristic velocity β ej), as well as a 56Ni mass, M 56. For the r-process-enriched models, a central core of mass M mix ≤ M ej is defined, and some mass M  rp ≤ M mix within that core is presumed to be composed of r-process elements. The mixing coordinate ψ mix is the ratio of M mix to M ej. The photosphere, defined as the surface at which τ = 2/3, separates the optically thick and optically thin regions. Emission from the optically thick layers inside the photosphere takes the form of a blackbody, in contrast to emission from the optically thin (nebular) layers.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption:  R-process signals will be easier to see if the peak time of the enriched inner layers (τ  rp) is close to the time at which the outer layers become transparent (﹩{\tau }_{\mathrm{tr}}﹩). This is the case only for certain combinations of the mixing coordinate ψ mix (=M mix/M ej), the r-process mass fraction ζ (=M  rp/M mix), and the velocity β ej. The curves above denote the contours where ﹩{\tau }_{r{\rm{p}}}={\tau }_{\mathrm{tr}}﹩ for different values of β ej. For higher β ej, ﹩{\tau }_{r{\rm{p}}}\approx {\tau }_{\mathrm{tr}}﹩ even for low ψ mix and/or low ζ. In contrast, for lower β ej, the signal is weaker absent significant mixing.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The addition of r-process material alters the optical−NIR colors of the nebular phase compared to SNe with no r-process enrichment. The magnitude of the effect depends on the mixing coordinate ψ mix and on the nebular-phase r-process SED, which we model here as a blackbody of effective temperature T  rp. The signal is most apparent for high ψ mix and for 1000 K ≲ T  rp ≲ 2000 K.
Paper: A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter
Authors: James Gurian, Michael Ryan, Sarah Schon, Donghui Jeong, Sarah Shandera
Figure caption: The minimum temperature of a 108 M ⊙ atomic dark-matter halo at z = 10 with r  α  = 1 and ξ = 5 × 10−3, under constant-density evolution (left) and adiabatic collapse (right). The region that does not cool substantially is shaded in dark gray. Light blue/gray corresponds to cooling to the atomic limit, while dark blue indicates molecular cooling. Molecular cooling is more efficient under adiabatic collapse because the compressional heating and increasing density promote molecule formation. Contours of equal suppression of the halo mass function compared to CDM are shown (dashed): to the left of these contours CDM-like virialized halos are very rare.
Paper: A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter
Authors: James Gurian, Michael Ryan, Sarah Schon, Donghui Jeong, Sarah Shandera
Figure caption: The opacity-limited minimum fragment mass for a 108 M ⊙ atomic dark-matter halo at z = 10 with r  α  = 1 and ξ = 5 × 10−3 (as Figure 1), under constant-density evolution (left) and adiabatic collapse (right). The region that fails to cool significantly (gray) and the halo-mass-suppression isocontours (dashed) are again shown. The result is plotted as a fraction of the Chandrasekhar mass, M  C . The value of M  C  is shown on right-hand vertical axes.
Paper: A Lower Bound on the Mass of Compact Objects from Dissipative Dark Matter
Authors: James Gurian, Michael Ryan, Sarah Schon, Donghui Jeong, Sarah Shandera
Figure caption: The halo mass function for two representative choices of parameters (see Figure 1). The bottom color band of each curve indicates the minimum temperature of those halos that collapse under hydrostatic evolution, while the top band illustrates the adiabatic density case. The black region fails to cool.
Paper: Opening the Era of Quasar-host Studies at High Redshift with JWST
Authors: Xuheng Ding, John D. Silverman, Masafusa Onoue
Figure caption: Science-grade images (first and third columns) and host galaxy images (second and fourth columns) for the four quasars at z > 2 with the F200W and F444W filters. In each case, the host galaxy image (i.e., data minus quasar) is produced by subtracting the best-fit PSF. The redshift of each quasar is indicated in each panel. The pixel units are in megajanskys per steradian (MJy sr−1). For the LW (e.g., F444W) filter; AEGIS 477 happens to be located at the edge of FOV in module B; only the right-side part of the quasar is observed.
Paper: Opening the Era of Quasar-host Studies at High Redshift with JWST
Authors: Xuheng Ding, John D. Silverman, Masafusa Onoue
Figure caption: Left: UVJ diagram for the five quasar systems, together with the sample from CANDELS at 1.6 < z < 3.5. Two systems whose 4000 Å break is not constrained by JWST are filled in white. Right: galaxy size–M * distribution and relations. The Sérsic index values are presented by the symbol color. For SDSS1420B, R eff is labeled using an arrow to indicate an upper limit. We also show the best-fit relation reported in van der Wel et al. (2014) for the star-forming (blue line) and quiescent (red line) at z ∼ 2.2. We also include six broad-line AGNs at 1.6 < z < 1.7 from Ding et al. (2020) based on HST/WFC3 imaging.
Paper: Opening the Era of Quasar-host Studies at High Redshift with JWST
Authors: Xuheng Ding, John D. Silverman, Masafusa Onoue
Figure caption: SED fitting of the host galaxy photometry based on gsf (Morishita et al. 2019) software. The red data points with errors indicate the host flux only, i.e., the quasar emission has been removed. The red arrow represents an upper limit. The blue diamonds show the predictions using the best-fit model. The inferred M * is also shown in the figure with 16%, 50%, and 84% confidence levels, along with the age and SFRs, both with lower and upper limits.
Paper: Opening the Era of Quasar-host Studies at High Redshift with JWST
Authors: Xuheng Ding, John D. Silverman, Masafusa Onoue
Figure caption: Two-dimensional decomposition of SDSS1420A based on imaging data from HST (a) and JWST (b); two filters are selected for each telescope. The panels are as follows from left to right: original data, model (quasar + galaxies) convolved with the PSF, data—quasar (host galaxy only), normalized residual image, and 1D surface brightness profile (top) and the corresponding residual (bottom).
Paper: Opening the Era of Quasar-host Studies at High Redshift with JWST
Authors: Xuheng Ding, John D. Silverman, Masafusa Onoue
Figure caption: Spatially resolved host properties of SDSS1420A. The top panels are (left) the original quasar color image from combining three JWST filters as indicated and (right) the color image of the host galaxy after the central quasar is subtracted in each filter. The bottom panels from left to right are (1) the stellar mass map, (2) the SFR map, and (3) the age map. In the panels, three regions are indicated with a radius of 2 kpc, 4 kpc, and 8 kpc. The 2 kpc region is applied as a mask in the bottom panels.
Paper: Opening the Era of Quasar-host Studies at High Redshift with JWST
Authors: Xuheng Ding, John D. Silverman, Masafusa Onoue
Figure caption: Surface brightness (SB) profiles (annuli) of nine select PSFs are shown as a function of radius (based on stars detected by JWST) per filter and compared with the simulated PSF model from webbpsf. The vertical lines indicate the FWHM values of the PSF stars (averaged) and PSF model by webbpsf. We only show the inner regions (<7 pixels) of these profiles that are key for quasar subtraction. The PSFs in our library demonstrate very stable performance, while the simulated PSF models by JWST are too narrow (i.e., peaking at the center) for all the filters.
Paper: The Luminosity Function of Tidal Disruption Flares for the ZTF-I Survey
Authors: Zheyu Lin, Ning Jiang, Xu Kong, Shifeng Huang, Zesen Lin, Jiazheng Zhu, Yibo Wang
Figure caption: The TDF LF based on 33 ZTF-I TDFs following the procedures of van Velzen (2018). The volumetric rates for limiting magnitudes r = 19.5, 20.0, and 20.5 are shown in blue, orange, and green, respectively. The orange and green markers are slightly shifted for the convenience of display. The blue solid and dashed represents the fitting result to a power-law and a Gaussian model for r = 19.5, respectively. For comparison, the previous TDF LF by van Velzen (2018) based on 13 TDFs is displayed in pink. Remarkably, the brightest source among 13 TDFs, ASASSN-15lh, is marked in black. It is outstandingly bright while its origin remains unclear. Therefore, we adopt the fitting parameters for both with and without (w/o) this source. As 7 out of 13 TDFs in van Velzen (2018) have only postpeak light curves, their ﹩{z}_{\max }﹩ should be underestimated. Consequently, their volumetric rates are overestimated. To evaluate this effect, we multiply their peak luminosity for a factor of 1.2, 1.5, 2.0. The data points and error bars in pink, cyan, brown, and olive correspond to multiplication factors (×) of 1.0, 1.2, 1.5, and 2.0, respectively. Left: LF for rest-frame g-band peak luminosity L  g . The sources are binned into eight bins separated by equivalent log L  g . The number of sources in these eight bins is {2, 0, 4, 6, 8, 8, 0, 5}. While for the sources of van Velzen (2018), the sources are binned into seven bins separated by equivalent log L  g . The number of sources in these seven bins for the multiplication factor of 1.0 (pink) is {4, 2, 3, 3, 0, 0, 1}. When the multiplication factors for postpeak sources are applied, the original power-law profile (solid and dashed pink line) can still describe the LF, while the Gaussian profile (dashed pink line) cannot. Right: LF for blackbody luminosity L bb. The sources are binned into seven bins separated by equivalent log L bb. The number of sources in these seven bins is {5, 7, 9, 6, 1, 2, 3}. While for the sources of van Velzen (2018), the sources also are binned into seven bins separated by equivalent log L bb. The number of sources in these seven bins for the multiplication factor of 1.0 (pink) is {2, 4, 4, 2, 0, 0, 1}. When the multiplication factors for postpeak sources are applied, the original power-law profile (solid and dashed pink line) can still describe the LF.