adsabs/AstroCLIMB huggingface dataset:
Paper: Prograde and Retrograde Gas Flow around Disk-embedded Companions: Dependence on Eccentricity, Mass, and Disk Properties
Authors: Yi-Xian Chen, Avery Bailey, James Stone, Zhaohuan Zhu
Figure caption: Simulation results from the parameter survey. For each q  t  (horizontal axis) and h 0 (color), we vary eccentricity (vertical axis) and locate the transition eccentricity as a function of e  t  (solid lines with error bars) to be between the largest e for prograde CSD rotation outcome (squares) and the smallest e for retrograde CSD rotation outcome (circles).
Paper: Most Planets Might Have More than 5 Myr of Time to Form
Authors: Susanne Pfalzner, Shahrzad Dehghani, Arnaud Michel
Figure caption: Disk fraction vs. cluster age. Top left: distinction between areas of different density. Clusters generally used are shown in black, compact, dense clusters in green, and sparse clusters in blue. The original fit by Haisch (dashed black line). Top right: fit using only clusters within 200 pc with the age range 1–20 Myr equitably covered (red line and symbols). Bottom left: clusters within 1000 pc. Symbols area proportional to the number of stars considered and the color representing the cluster distance. Bottom right: disk fractions color-coded according to cluster distance.
Paper: Most Planets Might Have More than 5 Myr of Time to Form
Authors: Susanne Pfalzner, Shahrzad Dehghani, Arnaud Michel
Figure caption: Disk fraction vs. cluster age. Fits for mass-dependent disk lifetimes based on the high-significance values of Upper Sco and UCL/LCC assuming an initial disk fraction of 100% (solid line) and 75% (dashed line).
Paper: Most Planets Might Have More than 5 Myr of Time to Form
Authors: Susanne Pfalzner, Shahrzad Dehghani, Arnaud Michel
Figure caption: Top: median disk lifetime as function of stellar mass assuming 100% initial disk fraction (dashed lines), 80% initial disk fraction (solid lines), and a lower Upper Sco age of 8 Myr instead of 11 Myr (dotted lines). The orange lines show the general trend including the uncertainty for higher-mass stars. Bottom: correlation between disk lifetime and properties of planetary system.
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: Planet-radius distribution (left) and planet size-ratio distribution (right) of model C assuming an initial atmospheric mass fraction of 0.3%. Planet radii are computed using the empirical MRR of Otegi et al. (2020). We use the high-density MRR equation of Otegi et al. (2020) to compute the sizes of rocky planets that experienced late impacts and the low-density equation for planets with water-rich compositions or rocky cores with atmospheres (avoided impacts). 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 of our simulations including 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: Planet-radius distribution (left) and planet size-ratio distribution (right) of model C assuming an initial atmospheric mass fractions of 0.1% (top panels), 1% (middle panels), and 5% (bottom panels). 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 of our simulations including 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: Planet-radius distribution (left) and planet size-ratio distribution (right) of model A assuming an initial atmospheric mass fractions of 0.1% (top panels), 1% (middle panels), and 5% (bottom panels). 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 of our simulations including 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: Planetary architecture of our systems at the end of the simulations when including the effects of photoevaporation. The assumed atmosphere-to-core-mass fraction is 0.3%. As in our nominal analysis, the MRR used to convert masses to planet radii comes from Zeng et al. (2019).
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: Ratio of orbital period ratios for adjacent triple of planets in the same planetary systems. Gray shows exoplanet data from Weiss et al. (2018). Blue and black show the results of our model C.
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: The S/N maps of SiO J = 5 → 4 (v = 0) and 13CO J = 2 → 1 toward η Car. Contours are from 5 to 10. The position of η Car is indicated by the red marker. The approximate beam size is shown in the bottom left corner. The insets show the average spectrum of each molecule, computed in a region of radius 2.″5. The dominant kinematic components are highlighted with Gaussian profiles. Since SiO appears next to the edge of the band, its spectrum is truncated above 140 km s−1.
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: Comparison of abundances of SiO and SiS measured in η Car (this work) and other star types with confirmed detections of the two species: C-rich stars (Massalkhi et al. 2019), O-rich stars (Massalkhi et al. 2020), S-type stars (Ramstedt et al. 2009; Danilovich et al. 2018; De Beck & Olofsson 2020), the yellow hypergiant IRC+10420 (Quintana-Lacaci et al. 2016), and the red supergiants VY CMa (Ziurys et al. 2007) and NML Cyg (Singh et al. 2021). Some relevant objects have been labeled for clarity. The size of the markers is proportional to the square root of ﹩\dot{M}﹩. The gray stars around η Car indicate the abundances of individual clumps. The dashed line represents [SiO/SiS] = 1.
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 clump F. Top panel: full band from 217.0 to 218.8 GHz, rebinned to a resolution of 2 km s−1. The insets show zoom-ins of the transitions detected (gray boxes on the full spectrum) at the original resolution, with a Gaussian (blue) or hyperfine (purple) fitting superimposed. The 13CN spectra have been smoothed to better highlight the hyperfine structure. All of the insets have the same flux density scale, with the different lines scaled appropriately for better visibility. Bottom panel: same as the top panel from 219.1 to 221.0 GHz.
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: Velocity-aligned spectra of the Si-bearing molecules detected in clump F. The SiN transitions at 218.006 and 218.512 GHz have been stacked to improve S/N. For each spectrum, a Gaussian fitting (blue) and the corresponding residual (gray) are shown. The relative scaling of the lines is the same as in Figure 2.
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: Comparison of the SiO and 13CO line profiles in clumps C, D, H, and J. Spectra have been smoothed to 2 km s−1. All panels have the same intensity scale.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The range of timescales and colors associated with an r-process detection for rCCSNe with β ej = 0.06, a moderate ψ mix = 0.3, and different values of M  rp. For each model, we find the earliest time, t RX2, at which an R − X color difference (relative to unenriched SNe) of ≥1 mag occurs for at least two X in the NIR bands (J, H, and K). We also record R − K at t = t 2RX. We display the maximum t RX2 (top panels) and the minimum (R − K)RX2 (bottom panels) in order to provide a conservative estimate of the strength and timing of the signal. Bins in which no models achieved Δ(R − X) ≥ 1 for two X are colored gray. Evidence of the r-process emerges sooner and is associated with bluer R − K for rCCSNe with lower t  R,pk and, to a lesser extent, brighter M  R . The value of M  rp primarily influences where in t  R,pk−M  R  space a signal is detectable; it has only a minor effect on t RX2 and (R − K)RX2.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The time frame, relative to explosion, required to constrain r-process production in collapsars depends on the properties of the rCCSN and on the bands used in the observation. Above, we show the cumulative fraction of models that have been observable, according to a two-color criterion, at any point before time t. We have coarsely binned the models in β ej and broken them down by mixing coordinate ψ mix. For higher-velocity rCCSNe (top panels), while detectability is particularly sensitive to ψ mix, most of the detectable models reveal themselves within ∼2 months of explosion. In contrast, the odds of a detection for lower-velocity rCCSNe (bottom panels) rise continually out to t = 200 days, when our simulations end. Regardless of velocity, color comparisons in R − H and R − J offer better prospects for detection than R − J and R − H, particularly for models with lower ψ mix.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The ideal observing cadence depends on Δt sig, the lifetime of the signal, which is sensitive to the mixing coordinate ψ mix. We focus here on rCCSNe with high velocities and define detectability as Δ(R − X) ≥ 1 for X = H and K. Top panel: the fraction of models detectable at a particular time since explosion, for different ψ mix. Regardless of ψ mix, the fractions reach their peak around 50 days. (However, the values of those peaks do depend on ψ mix.) Bottom panel: the fraction of models, f >, that have a signal duration ≥ Δt sig, as a function of mixing coordinate. For well-mixed models, Δt sig can exceed100 days, while signals for models with lower ψ mix are more ephemeral.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The maximum R − K color recorded for rCCSNe with β ej = 0.06, ψ mix = 0.3, and different r-process masses M  rp, after the r-process-free envelope has become optically thin. We show the bin-averaged values of both the color maxima (top panels) and the times at which they occur (bottom panels). In all panels, hatching indicates bins for which no models have Δ(R − X) ≥ 1 for at least two bands X ∈ {J, H, K} at any point before t = 200 days. In bins for which detections are possible for multiple r-process masses, the maximum R − K increases with M  rp, as does the time at which that maximum takes place. This suggests that long-term photometric follow-up can provide better constraints on M  rp than an initial detection alone.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The minimum observable mixing coordinate, ﹩{\psi }_{\min }﹩, depends on the intrinsic properties of the rCCSN and on the timescale and passbands of the observation. As elsewhere, an observable signal is one that produces an R − X color difference of at least 1 mag compared to an average of unenriched SNe in the same bin (β ej, t  R,pk, M  R ) at some point during the observation time frame. We define ﹩{\psi }_{\min }﹩ as the minimum ψ mix for which ≥ 50% of models in a bin are observable. In bins where no ψ mix meet this criterion, an inverted triangle indicates the maximum ψ mix within the bin. Black crosses indicate that a bin contained rCCSNe, but no unenriched SNe for comparison. All enriched models have M  rp = 0.03 M ⊙. Top panels: the effect of β ej. More deeply buried r-process material is more easily observed for faster expanding rCCSNe. Middle panels: the effect of observing time frame. If observations are restricted to times close to peak, the differences between enriched and unenriched SNe are difficult to discern, even for highly mixed ejecta. Prolonged observing campaigns provide more opportunities for detection. Bottom panels: the effect of passband. The signal is more easily observed when redder bands are considered in color calculations.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The effects of enrichment are strongest at redder wavelengths and when the r-process mass and/or the degree of mixing are high. Top three panels: the times (t Δ) at which select colors of rCCSNe with variable M  rp and ψ mix but uniform M ej, β ej, and M 56 (=4.0 M ⊙, 0.04, and 0.25 M ⊙, respectively) first differ meaningfully (Δ ≥ 1 mag) from an unenriched SN with the same explosion parameters. The divergence occurs earlier for higher M  rp and ψ mix, and for a larger fraction of the models as redder bands are considered. Models to the left of the dashed black lines in each panel are found, under the framework of Section 3.2, to have Δ(R − X) < 1 mag once the ejecta is fully transparent and therefore meet our detection threshold only in the photospheric phase. Bottom panel: the maximum difference (with respect to time) in V − R of the rCCSNe compared to the unenriched model. The effect is small in the optical bands; for no model does Δ(V − R) ever exceed 1 mag. All panels: dark gray shading marks parameter combinations disallowed by the requirement that r-process-enriched cores also contain 56Ni (ψ mix M ej ≥ ψ mix M 56 + M  rp).
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: Top panel: our optically thin emission models and the observations and/or calculations that inform them. Optically thin layers free of r-process material emit a spectrum ﹩{{ \mathcal F }}_{\nu }^{07\mathrm{gr}}﹩ (blue curve) constructed from the photometry of the SN Ic SN 2007gr (Hunter et al. 2009; Bianco et al. 2014) 120 days after B-band maximum. The photometry-derived fluxes used in the spline fit are plotted as blue crosses. Observations of kn170817 43 days after the merger (Kasliwal et al. 2022; orange markers) are consistent with a blackbody at T ≤ 440 K (dashed orange curve) or with the more complex spectrum (solid black line) predicted by Hotokezaka et al. (2021) for r-process compositions in the nebular phase. We adopt a scaled 2500 K blackbody SED (dotted-dashed pink curve) to approximate optically thin emission associated with r-process material. The frequencies of the UVOIR and NIR bands are shown on the top axis. The shaded region indicates the frequencies that will be accessible to the JWST. Bottom panel: AB magnitudes calculated from a blackbody at T = 2500 K (plus signs) and from the spectrum of (Hotokezaka et al. 2021; diamonds), both scaled so M  V  = 0. The simpler blackbody function nevertheless faithfully reproduces the colors of the more complex spectrum.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: Increased mixing enhances emission in the NIR relative to the optical. All models above have M ej = 4.0 M ⊙, β ej = 0.04, M 56 = 0.25 M ⊙, and M  rp =0.08 M ⊙. Top panels: mixing redistributes energy among luminosity components, with higher ψ mix favoring L ph and ﹩{L}_{\mathrm{neb}}^{r{\rm{p}}}﹩ over ﹩{L}_{\mathrm{neb}}^{\mathrm{sn}}﹩. (Note that ﹩{L}_{\mathrm{neb}}^{\mathrm{sn}}﹩ and ﹩{L}_{\mathrm{neb}}^{r{\rm{p}}}﹩ refer to luminosity components with distinct SEDs, rather than components emitted from r-process-rich or -free regions. As described in Section 3.2, enriched ejecta contributes energy to both ﹩{L}_{\mathrm{neb}}^{\mathrm{sn}}﹩ and ﹩{L}_{\mathrm{neb}}^{r{\rm{p}}}﹩.) The dotted black lines indicate ﹩t={\tau }_{\mathrm{tr}}﹩, the time at which the outer r-process-free layers become transparent. The evolution of L ph slows at this point in response to the higher opacity of the core. Bottom panels: select broadband light curves showing the redistribution of energy from bluer to redder wavelengths.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The effect of r-process enrichment (M  rp = 0.03 M ⊙, variable ψ mix) on R − X for four explosion models with M ej, β ej, and M 56 corresponding either to literature-reported averages or to particular events representing extrema in the distribution of inferred SN Ic-BL properties (see Table 4 for details). We show the full color evolution for each model (top panels), as well as the maximum color and the time at which it occurs (bottom panels). In all panels, we plot predictions for r-process-free models with the same explosion properties for comparison. For all but the lowest ψ mix, the presence of r-process material enhances R − X, producing either a secondary maximum or a delayed global maximum relative to the unenriched cases. Significantly, the strongest enhancement can be transient in nature and may occur well before the rCCSN reaches its asymptotic colors. The impact is strongest for the highest-velocity models (the typical and low-mass SNe Ic-BL) but can be significant even for a typical SN Ic if ψ mix is high.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: SNe with similar observed properties near peak do not exhibit perfectly uniform color evolution. Having binned the r-process-free SNe according to t  R,pk, M  R , and β ej and averaged their R − X color evolution, we determine ﹩{\sigma }_{\max }﹩, the maximum standard deviation in each bin for any R − X, with respect to time. The cumulative distribution function of ﹩{\sigma }_{\max }﹩ is shown above for bins of constant central β ej. For typical SN Ic/Ic-BL velocities (0.03 ≲ β ej ≲ 0.1), most bins have σ  R−X  ≲ 0.4 mag at all times, less than our r-process detection threshold Δ(R − X) ≥ 1 mag. Furthermore, ﹩{\sigma }_{\max }﹩ is not necessarily indicative of σ  R−X  when a detection occurs (i.e., when Δ(R − X) ≥ 1 mag). In practice, the uncertainty at these times is often much less than the maximum value.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The presence of r-process material alters the SN light curves even near optical peak. As a result, r-process-free models with matching explosion parameters are not necessarily ideal points of comparison for rCCSNe. Above, we show how models with fixed (M ej, β ej, M 56) = (4.0 M ⊙, 0.04, 0.25 M ⊙) are distributed in t  R,pk and M  R , where t  R,pk (M  R ) is the rise time (peak magnitude) in R band. The histogram cell containing the r-process-free model with the same M ej, β ej, and M 56 is marked with a fuchsia cross. It contains only a minority of the enriched models.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: The same as Figure 12, but showing the impact of the r-process mass M  rp on ﹩{\psi }_{\min }﹩, for fixed β ej = 0.06 and observing window t obs ≤ 4t  R,pk. Detectability is determined with respect to R − K. The minimum detectable mixing coordinate (﹩{\psi }_{\min }﹩) is largely insensitive to the quantity of r-process material, at least within the range of M  rp we consider; a factor of five increase in M  rp produces only a modest reduction in ﹩{\psi }_{\min }﹩.
Paper: Signatures of r-process Enrichment in Supernovae from Collapsars
Authors: Jennifer Barnes, Brian D. Metzger
Figure caption: A comparison of model photometry (solid lines) and observations (markers) shows that our approach is well suited for modeling SNe Ic at a range of kinetic energies. SN 2007gr (top panel) is classified as an ordinary SN Ic (Madison & Li 2007), while SN 2002ap (bottom panel) is an SN Ic-BL (Filippenko & Chornock 2002; Gal-Yam et al. 2002; Meikle et al. 2002). The model parameters for each SN are given in Table 2. Photometry is from Bianco et al. (2014), courtesy of the OSC (Guillochon et al. 2017), and from Yoshii et al. (2003) and references therein. To improve readability, in these plots only we calculate magnitudes using the Vega system.
Paper: Disks of Stars in the Galactic Center Triggered by Tidal Disruption Events
Authors: Rosalba Perna, Evgeni Grishin
Figure caption: Sketch of the jet/cocoon system, as the overpressured cocoon engulfs gas clouds.
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: Top panel: Eddington ratio distribution functions for active galactic nuclei (AGN) in ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\,=﹩ 20–22 and ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\,=﹩ 22–25 bins, as well as for type I and type II AGN (from A22). Shaded regions show 1σ uncertainties. Bottom panel: ratio of obscured to overall space densities as a function of λ Edd. The red line shows ratio of ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\,=﹩ 22–25 AGN over all AGN, and the orange line shows ratio of type II AGN/all AGN. Black vertical lines show effective Eddington limits for ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\geqslant 22﹩ gas according to Fabian et al. (2008). At low Eddington ratios (λ Edd < −1.7), this ratio is high because gas is retained, while for higher Eddington ratios, gas is blown away. We suggest that at low-λ Edd this ratio is equal to the pure geometric covering factor of the torus, while at high λ Edd, it is a time-averaged covering factor. We calculate the torus opening angle at low-λ Edd and the covering factor decay rate at high λ Edd using these ratios.