adsabs/AstroCLIMB huggingface dataset:
Paper: Unveiling Galaxy Chemical Enrichment Mechanisms Out to z ∼ 8 from Direct Determination of O and Ar Abundances from JWST/NIRSPEC Spectroscopy
Authors: Souradeep Bhattacharya, Magda Arnaboldi, Ortwin Gerhard, Chiaki Kobayashi, Kanak Saha
Figure caption: (Left) log(O/Ar) vs. 12 + log(Ar/H) for the 11 SFGs at z ∼ 1.3–7.7 and two candidate AGN hosts at z ∼ 4.5. The galaxies are colored by their redshift. The green and blue lines respectively show the sequence of mean values of low-redshift (z < 0.3) relatively lower-mass (<log(M*/M⊙) > = 7.23) and higher-mass (<log(M*/M⊙) > = 9.41) galaxies from SDSS (S. Bhattacharya et al. 2025, in preparation). Their standard deviations are shaded. The MW solar neighborhood GCE model (C. Kobayashi et al. 2020a) is shown as black dashed line. (Right) Same as the left panel but now the SFGs are colored by the age of the Universe at their redshift, and the AGN candidates are not plotted. Also plotted is a GCE model for an intermittent starburst scenario that follows the star formation history shown in the inset, colored by age of the Universe.
Paper: Unveiling Galaxy Chemical Enrichment Mechanisms Out to z ∼ 8 from Direct Determination of O and Ar Abundances from JWST/NIRSPEC Spectroscopy
Authors: Souradeep Bhattacharya, Magda Arnaboldi, Ortwin Gerhard, Chiaki Kobayashi, Kanak Saha
Figure caption: (a) [O III] λ4363 and ionized Ar lines in flux- and wavelength-calibrated archival 1D JWST/NIRSPEC spectra and 2D traces for the 10 galaxies analyzed here. Observed 1D spectra are shown in gray (with shaded 1σ uncertainty), best-fit 1D spectra in red, and the fitted continuum in black. For the Ar line regions, the color scale of the 2D traces is adjusted to the line fluxes for the highest-redshift (see Table 2) galaxies (left). The horizontal red lines enclose the pixels used by the MAST/JWST pipeline for constructing the 1D spectra. (b) The distribution in the 2D spectra of line flux to its error ratio (Flux/δFlux) around the detected Ar lines for the same five highest-redshift galaxies; the color scale is adapted for each 2D trace. Notice in particular that both [Ar IV] lines are detected for the z = 7.66 galaxy ERO 10612 (see also Table 1).
Paper: Unveiling Galaxy Chemical Enrichment Mechanisms Out to z ∼ 8 from Direct Determination of O and Ar Abundances from JWST/NIRSPEC Spectroscopy
Authors: Souradeep Bhattacharya, Magda Arnaboldi, Ortwin Gerhard, Chiaki Kobayashi, Kanak Saha
Figure caption: (a) 1D spectrum and flux error for CEERS 1651 as a function of rest-frame wavelength in a broad wavelength range around the detected [Ar III] λ7136 line. Emission lines with Gaussian-like profiles such as the ionized Ar and He I λ7281 lines are identified by ALFA; however, the He I λ7065 line is too weak to be identified. Noise peaks, given their non-Gaussian profiles, are not identified as emission lines. (b) The Flux/δFlux in the 1D spectra plotted as a function of rest-frame wavelength, in a wavelength range around the detected [Ar III] λ7136 line, for the four highest-redshift galaxies where the line is detected. The Flux/δFlux for the 1D stacked spectrum for these four galaxies is marked in black.
Paper: Unveiling Galaxy Chemical Enrichment Mechanisms Out to z ∼ 8 from Direct Determination of O and Ar Abundances from JWST/NIRSPEC Spectroscopy
Authors: Souradeep Bhattacharya, Magda Arnaboldi, Ortwin Gerhard, Chiaki Kobayashi, Kanak Saha
Figure caption: The 12 + log(O/H) abundances determined in this work compared to previously published values. The inset shows the same for the two sources with previously published 12 + log(Ar/H) determinations.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Top panel: long-term optical (ZTF), UV (Swift UVOT), and X-ray (Swift, NICER) light curves of AT2022upj. Although the X-ray emission at early times was faint, the source showed a delayed X-ray brightening ∼1 yr post-optical/UV peak. The first indication of QPEs occurred another ∼year after. Bottom panels: NICER X-ray light curve from 2024 December 12–2025 January 8 revealing quasiperiodic eruptions with 0.5–3.5 days recurrence times.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Correlation of QPE burst duration (Tdur) with recurrence time (Trec). The error bars show the diversity of timescales in each source (not measurement uncertainties). AT2022upj shows a relatively high scatter in both quantities. The top-left hatched region denotes Tdur ≥ Trec, which is an invalid region of parameter space. The bottom-right region denotes Tdur < 16 ks and Trec > 100 ks, which is rendered unobservable by current instrument capabilities.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Top panel: stacked Swift XRT spectrum (72,770 ks) of the late-time rise (between MJDs 60200–60600 in Figure 1). We show fits with a disk blackbody + power-law model (Table 1). Bottom panel: background-subtracted NICER spectra of QPE #4 (Figure 1) fit with a blackbody model for the rise, peak, and decline phases (Table 1).
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Top panel: inferred accretion disk surface density profiles Σ(r) at the times of the delayed X-ray rise (blue) and the emergence of QPEs (green). The inferred outer radius is consistent with viscously expanding over ∼few hundred days to the orbital radius corresponding to a 3 day QPE. Bottom panel: model light curves fit to the Swift UVW1, ZTF g-band, and Swft X-ray data. The presence of the optical/UV plateaus and delayed X-ray rise indicate the delayed formation, and viscous expansion, of an accretion disk.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Spectral evolution of the QPEs in AT2022upj for bursts #4 (red) and #6 (blue). The latter eruption shows a more complex eruption profile reminiscent of the overlapping bursts of eRO-QPE1, whereas burst #4 shows the more standard hysteresis behavior seen in QPEs (bottom-left panel).
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Numerical simulations of the QPE blind detection probability. Top panel: one realization of a mock light curve showing 10 randomly distributed observations each of 0.001Trec duration, of which one “detected” a QPE by measuring a point above the 5 × /8 × /10 × fquiesc threshold in red/green/blue, respectively. Middle panel: simulated detection probabilities, with 3 × 50 × 1000 realizations for various choices of detection threshold and total exposure time. We fix Nobs = 10. Bottom panel: same as above, for fixed Tobs = 0.1Trec and varying Nobs.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Posterior probability of the fraction of optical TDEs resulting in QPEs (q), marginalized over Trec, ﹩\mathrm{log}{L}_{{\rm{peak}}}﹩, τdelay, and τlife. In the legend, we report the maximum a posteriori estimate and 68% highest-density credible intervals. Full corner plots can be found in Appendix C.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Corner plot for the accretion disk model fit to the multiband light curve of AT2022upj. The resulting surface density profile and disk luminosity are shown in Figure 4.
Paper: Discovery of Quasiperiodic Eruptions in the Tidal Disruption Event and Extreme Coronal Line Emitter AT2022upj: Implications for the QPE/TDE Fraction and a Connection to ECLEs
Authors: Joheen Chakraborty, Erin Kara, Riccardo Arcodia, Johannes Buchner, Margherita Giustini, Lorena Hernández-García, Itai Linial, Megan Masterson, Giovanni Miniutti, Andrew Mummery, Christos Panagiotou, Erwan Quintin, Paula Sánchez-Sáez
Figure caption: Corner plot for sampling run of QPE/TDE fraction.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: The mid-infrared transmission spectrum of K2-18 b obtained with the JWST MIRI LRS instrument. The data points with error bars (in brown) show the observed spectrum as described in Section 2.1. The horizontal error bars correspond to the spectral bin width. The dark blue curve denotes the median retrieved spectral fit, while the two lighter shaded regions denote the 1σ and 2σ intervals. The prominent features of DMS and DMDS are identified. Both molecules have overlapping spectral features between 6.8 and 8 μm, with broader features between ∼9 and 10 μm for DMS and ∼10–11 μm for DMDS. The individual spectral contributions of these molecules are shown in Figure 4.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Spectral contributions of notable chemical species in the MIRI band. Each curve denotes the spectral contribution of a particular molecule to the model spectrum, as denoted in the legend. The mixing ratios of DMS and DMDS are set to a representative value of 5 × 10−4, while CH4 and CO2 are set to 10−2, consistent with constraints obtained from previous near-infrared observations (N. Madhusudhan et al. 2023b). The black line denotes the resulting transmission spectrum with all molecular contributions combined.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Leave-one-out analysis for the MIRI transmission spectrum of K2-18 b. The black data points with error bars show the observed transmission spectrum obtained using the JExoRES pipeline. The center shading of each data point denotes the corresponding elpd difference (Δelpd) between the canonical atmospheric model with DMS and DMDS and one with both molecules absent. The redder points denote higher and positive Δelpd, indicating that the canonical model is more capable of predicting them if they are absent from the fit than the atmospheric model without DMS and DMDS. Similarly, bluer points denote larger negative Δelpd values, indicating a preference against DMS and DMDS, while white points denote Δelpd values close to zero. Gold points denote the median retrieved spectrum (in blue) binned for each data point, while the dark and light cyan shaded regions denote the retrieved 1σ and 2σ contours, respectively.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Retrieved posterior probability distributions for DMDS and DMS from our canonical retrievals described in Section 3, using data from the JExoRES (top) and JexoPipe (bottom) pipelines. The posteriors shown in blue correspond to the canonical retrieval containing both DMDS and DMS, along with CH4 and CO2. The other two cases show the retrievals with only one of the two molecules, DMDS or DMS, included in the canonical retrieval, with all other parameters remaining unchanged. The orange distribution corresponds to the retrieval with only DMDS present, and the green distribution corresponds to the retrieval with only DMS present.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: The MIRI transmission spectrum of K2-18 b obtained using different treatments of the detector settling effect. We consider an exponential + a linear trend (dark gray and purple), an exponential + a quadratic trend (pink), and a quadratic trend alone (orange), as well as different numbers of integrations to mask at the start of the observation.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Demonstration of the stability of the MIRI transmission spectrum of K2-18 b using two independent data reduction pipelines. The spectra from the JExoRES and JexoPipe pipelines are shown in purple and orange, respectively, and are further described in Sections 2.1 and 2.2.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: MIRI transmission spectrum of K2-18 b using different bin widths. For our analysis, we do not consider the spectrum below 5.6 μm to be conservative, given that the choice of binning affects the spectrum in this region. Note that these spectra did not use GPs, as discussed in Appendix A.7, thus the error bars may be somewhat underestimated.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Comparisons between different spectral extraction methods. The dark gray points show the MIRI transmission spectrum of K2-18 b using the optimal extraction method, while the green points show the spectrum using box extraction.
Paper: New Constraints on DMS and DMDS in the Atmosphere of K2-18 b from JWST MIRI
Authors: Nikku Madhusudhan, Savvas Constantinou, Måns Holmberg, Subhajit Sarkar, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Effects of different nonlinearity corrections on the MIRI transmission spectrum of K2-18 b. The spectra with the standard and our custom nonlinearity corrections are shown in dark gray and yellow, respectively.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the computed GLS periodograms for the residuals of MAROON-X Red channel radial velocities. A β distribution for the planetary eccentricities has been used for all the planets.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the computed GLS periodograms for the combined residuals of MAROON-X Red channel and ESPRESSO radial velocities. A β distribution for the planetary eccentricities has been used for all planets.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: Top panels: phase-folded plots for planets Barnard b, c, d, and e based on joint fit between MAROON-X Red channel and ESPRESSO radial velocities. Bottom panel: residuals as a function of time for the 4-Planet model.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the computed GLS periodograms of raw radial velocities (red color for Red channel data and blue color for Blue channel data, chromatic index (CRX), differential line widths (dLW), and Hα index for MAROON-X Red and Blue channel data.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows a comparison of planetary architectures between Barnard’s Star and other compact M dwarf systems. Left panel: orbital periods of different planets with symbol sizes proportional to the planets’ masses. Right panel: mutual Hill separations between consecutive planets in the systems.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: Phase-folded plots for planets Barnard b, c, and d based on MAROON-X Red Channel data. The bottom panel shows the residuals of the 3-Planet model for MAROON-X Red channel radial velocities.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the computed GLS periodograms for the combined residuals of MAROON-X Red channel, Blue channel, and ESPRESSO radial velocities. A β distribution for the planetary eccentricities has been used for all planets.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the computed GLS periodograms for the combined residuals of MAROON-X Red and Blue channel radial velocities. A β distribution for the planetary eccentricities has been used for all planets.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: Phase-folded plots for planets Barnard b, c, d, and e based on joint fit between MAROON-X Red and Blue channel radial velocities.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the current sensitivity of detecting planets around Barnard’s Star using the MAROON-X Red channel and ESPRESSO data.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: This plot shows the global GP model for the 4-Keplerian model joint fit between the MAROON-X Red channel and ESPRESSO data sets.
Paper: Four Sub-Earth Planets Orbiting Barnard’s Star from MAROON-X and ESPRESSO
Authors: Ritvik Basant, Rafael Luque, Jacob L. Bean, Andreas Seifahrt, Madison Brady, Lily L. Zhao, Nina Brown, Tanya Das, Julian Stürmer, David Kasper, Rohan Gupta, Guđmundur Stefánsson
Figure caption: Phase-folded plots for planets Barnard b, c, d, and e using ESPRESSO data.
Paper: Disk Draining in LIGO Progenitor Black Hole Binaries and Its Significance to Electromagnetic Counterparts
Authors: Xiaoshan Huang, Sierra Dodd, Sophie Lund Schrøder, Shane W. Davis, Enrico Ramirez-Ruiz
Figure caption: Disk formation preceding the formation of the second BH in a LIGO binary. The panels show the gas column density in the orbital plane during the first orbit of the binary after the SN explosion. The plots are centered on the BH remnant from the exploding star, and the time stamps are given in units of the dynamical timescale of the stellar progenitor: t* = 0.07, 0.68, 2.25, 5.67 (from left to right). The length scale shown in all panels corresponds to the initial size of the pre-SN progenitor: R*. These simulations are used to inform the conditions of the gas in and around LIGO BH binaries near the time of merger.
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: The final distributions of eccentricities and orbital periods for the three planets obtained from the simulations in group 1. Panels (a), (b), and (c) illustrate the orbital period distributions of W1, W2, and W3, respectively. The colors represent the ﹩{Q}_{p}^{{\prime} }﹩ used for the planets, and the shapes of the dots indicate different migration timescales of the third planet, as shown in the legend in panel (a). The green dots and error bars represent the estimated values from observations. Panels (d), (e), and (f) show the number distributions of ﹩{Q}_{p}^{{\prime} }﹩ for the three planets. The light gray bars indicate the number distribution for runs in which SPSE planets are formed, while the dark gray bars represent the number distribution for the systems that formed USP planets.