adsabs/AstroCLIMB huggingface dataset:
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: As in Figure 1 but for a star plunging closer to the black hole (β = 5). We show column density evolution for a 1 M ⊙ star on a parabolic orbit with β = 5, disrupted by a 106 M ⊙ Kerr black hole with spin a = 0.99. The initial orbital plane is misaligned by 60° to the black hole spin plane. The main panel shows the debris after 365 days projected in the x–y plane with a log color bar. Inset panels show stream evolution with a linear color bar between 0 and 1500 g cm−2. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Synthetic spectral energy distributions computed from the β = 1 calculation with the observer in the +z-direction (blue curves). Orange dotted curves show single-temperature blackbody fits to the optical band, while green dotted curves show blackbody fits to the soft X-ray band. The legend lists the luminosities (L tot, L bb, and L x), the optical blackbody temperature (T bb), and the X-ray temperature. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Disk formation in an isentropic simulation (radiatively efficient cooling) with a spinning black hole (a = 0.99, θ = 60°). The disk in this case is formed after 90 days and undergoes differential precession, which “tears” the disk into independent rings. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Disk formation in the core of the envelope when an adiabatic simulation is continued with radiatively efficient cooling. We resumed an adiabatic calculation (as in Figure 1) 1 yr after disruption assuming isentropic evolution. A narrow ring of material develops, similar to that obtained in the fully isentropic calculation (Figure 6). Each panel is 20 au × 20 au.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: As in Figure 10 but for the β = 5 calculation. Here the “bubble” is inflated on a shorter timescale, smothering the central engine in t < 30 days, but the retreat of the photosphere at t ≳ 240 days leads to soft X-ray emission as the hotter central regions become visible. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Numerical experiment where a stream is injected into an otherwise empty domain with a fixed injection speed but varying Mach numbers. Lateral expansion of the stream can be seen to depend solely on the Mach number of the flow. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Probability curves for P cc = 0.01 and 0.1 as a function of extragalactic DM (or excess DM) and localization radius for the faintest FRB host discovered to date (M  r  = −17 AB mag). Note that an FRB with an extragalactic DM ≈ 100 pc cm−3 can be associated with a dwarf, star-forming galaxy, like the FRB 20121102A host, with P cc of 0.01 and 0.1 using a localization precision of ≈10″ and ﹩1^{\prime} ﹩, respectively. The plot is produced using the formalism discussed in Section 2.1.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: As in Figure 14 but with a point mass placed at the origin and experimenting with different initial stream radii H for the same initial Mach number of M = 50. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Pan-STARRS r-band images of the baseband localization regions for FRB 20181223C (top left), FRB 20190418A (top right), FRB 20181220A (bottom left), and FRB 20190425A (bottom right). The 1σ and 2σ baseband localization regions are represented by dotted and solid cyan ellipses, respectively. While only one plausible host galaxy candidate is identified for FRB 20181220A, FRB 20190418A, and FRB 20190425A, we identify four potential host galaxy candidates within the localization area of FRB 20181223C. However, following our multiobject spectroscopic analysis discussed in Appendix B, only one galaxy satisfies the estimated maximum redshift limit for FRB 20181223C. Note that the bright disk galaxy (bottom middle) just outside the 2σ region is a spiral galaxy at z spec = 0.347, well above the maximum redshift estimated for FRB 20181223C, i.e., ﹩{z}_{\max }=0.085﹩ (see Table 1). Finally, the most probable host galaxies for the four FRBs are delineated by red boxes.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: SFHs of the four FRB host galaxies reported in this work. The x-axis is the look-back time (Gyr), such that the left panel shows the present day and the right panel shows the age of the Universe at the redshift of the galaxy. These SFHs are estimated using Prospector. For more details, see Appendix A.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Galactic-extinction-corrected spectra (in the observer’s frame) of the host galaxies for FRB 20181220A (left) and FRB 20190418A (right). The solid red lines depict the best-fitted line profiles estimated using Specutils for both galaxies, and the dotted vertical red lines denote the prominent nebular emission lines, Hα and [N II].
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: WISE color–color plot adapted from Wright et al. (2010) for our sample of local Universe FRB hosts. It illustrates how galaxies separate by type, showing the simple divisions for spheroidal and early-type disks, intermediate disks, and late-type disk galaxies (Jarrett et al. 2017). The infrared colors of all 18 local Universe FRB hosts support them being spiral or late-type galaxies. For a detailed description of each shaded region, kindly refer to Wright et al. (2010).
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Frequency vs. time (“waterfall”) plots of the dedispersed bursts detected from FRB 20181220A, FRB 20181223C, FRB 20190418A, and FRB 20190425A with saved baseband data. See Table 1 for their major burst properties. The waterfall plots are binned to have a temporal resolution of 0.39 ms and a spectral resolution of 0.391 MHz. Red lines represent bad frequency channels that were flagged in this analysis.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: The best-fitted SED model of the host galaxies of FRB 20181220A (top) and FRB 20181223C (bottom). The flux densities of the host galaxies in different wavelength bands are plotted along with the best-fit Prospector model spectrum. To assess the quality of the Prospector models, the modeled and actual photometry data are also shown. For more information, see Appendix A.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Comparison of the effective Poisson burst rates of the four low-DM FRBs studied in this work with those of published CHIME/FRB repeating sources with known hosts.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: The CFIS DR3 r-band image of the FRB 20220509G host (in ICRS reference frame). The star in close proximity to the FRB host is flagged for better visualization of the extended spiral arm features.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Same as Figure 9, but for the best-fitted SED model of the host galaxies of FRB 20190418A (top) and FRB 20190425A (bottom).
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Comparison of notable physical properties of the host galaxies of 18 local Universe FRBs and 83 SNe II. The sample of host galaxies of SNe II (represented as cyan stars) is taken from the Palomar Transient Factory (PTF) Core-collapse Supernova Host-galaxy catalog (Schulze et al. 2021). Our local Universe FRB sample consists of 7 repeating FRBs (bold crosses) and 11 apparently nonrepeating FRBs (circles). The four apparently nonrepeating FRBs presented in this work can be differentiated from other apparently nonrepeating FRBs via the crosses overlaid. Top: SFR vs. total stellar mass (M *) for local Universe FRBs and PTF SN II hosts. The background population of galaxies is taken from the SDSS MPA-JHU DR7 catalog (Brinchmann et al. 2004). The solid blue line represents the SFMS (Peng et al. 2010). Following the framework developed by Law-Smith et al. (2017), dashed lines are spaced 1σ = 0.5 dex apart (the median scatter in SFMS), with the green valley falling 1σ–3σ below the SFMS (the region between the lower blue dashed line and red dashed line). The galaxies below the red dashed line are found to be quiescent. These lines are used to define four regions that are shaded and labeled in the figure. Bottom: rest-frame color–magnitude diagram of the host galaxies of FRBs (stars) compared to those of Type II CCSNe (black circles). The rest-frame colors and absolute r-band magnitude of FRBs are taken from their discovery papers, or in cases where those values are missing, we estimate them using the host photometry magnitudes in the Pan-STARRS release 1 (PS1) survey catalog data (Chambers et al. 2016).
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Host galaxies of 18 local Universe FRBs used in this study, with black circles masking stars overlapping FRB 20210405I and FRB 20220509G hosts. For additional information, see Appendix C.
Paper: Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population
Authors: Mohit Bhardwaj, Daniele Michilli, Aida Yu. Kirichenko, Obinna Modilim, Kaitlyn Shin, Victoria M. Kaspi, Bridget C. Andersen, Tomas Cassanelli, Charanjot Brar, Shami Chatterjee, Amanda M. Cook, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Adaeze L. Ibik, J. F. Kaczmarek, Adam E. Lanman, Calvin Leung, K. W. Masui, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Ketan R. Sand, Paul Scholz, Kendrick M. Smith
Figure caption: Distribution of the host galaxies of the Pantheon SN Ia subsample according to their morphological classes as discussed in Appendix E. For more details on the classification scheme, see Pruzhinskaya et al. (2020).
Paper: GRB 211211A: The Case for an Engine-powered over r-process-powered Blue Kilonova
Authors: Hamid Hamidani, Masaomi Tanaka, Shigeo S. Kimura, Gavin P. Lamb, Kyohei Kawaguchi
Figure caption: SED of GRB 211211A and its time evolution. Five epochs are shown: 1 hr (dark purple), 5 hr (purple), 10 hr (blue), 1.4 days (orange), and 4.2 days (red). Filled circles indicate detections, while triangles indicate upper limits. Central values for the X-ray’s photon index (dashed lines) and the corresponding uncertainty (bow ties) are shown (see the Appendix). The afterglow model is shown at each epoch with a dotted line. Three r-process KN models are shown (using z = 0.0762): a low-opacity blue KN model (κ = 0.1 cm2 g−1 and M e = 0.04 M ⊙; light gray), a moderate-opacity blue KN model (κ = 1 cm2 g−1 and M e = 0.04 M ⊙; dark gray), and a red KN model (κ = 10 cm2 g−1 and M e = 0.04 M ⊙; black). The inability of r-process-powered blue KN models to explain both early observations without overproducing late emission is apparent. Also, the inconsistency of the low-opacity model (light gray) with the color of early data is apparent. IR/optical/UV data points were taken from Rastinejad et al. (2022) and Troja et al. (2022), and X-ray data were taken from Troja et al. (2022). For clarity, the data are scaled at each epoch by the following factors: 100, 10−0.8, 10−1.6, 10−2.4, and 10−3.2 (same as in Troja et al. 2022). For a similar plot, see Figure 2 in Troja et al. (2022) and Extended Data Figure 2 in Rastinejad et al. (2022).
Paper: GRB 211211A: The Case for an Engine-powered over r-process-powered Blue Kilonova
Authors: Hamid Hamidani, Masaomi Tanaka, Shigeo S. Kimura, Gavin P. Lamb, Kyohei Kawaguchi
Figure caption: The bolometric luminosity for a blue KN model (blue line; κ = 1 cm2 g−1 and M e = 0.05 M ⊙) that can explain the early KN emission in GRB 211211A (but overpredicts late KN emission) and a red KN model (red line; κ = 10 cm2 g−1 and M e = 0.04 M ⊙) that can explain the late KN emission in GRB 211211A (but underpredicts late KN emission). The observed KN emission in GRB 211211A (dark gray squares for our fit and dark gray circles for Troja et al. 2022; see Table 1) and AT 2017gfo (gray circles; data from Waxman et al. 2018) are shown. Dotted, dashed, and dotted–dashed lines highlight time-evolving power-law functions with indices of −0.3, −1.0, and −1.3, respectively. This illustrates the difficulty of r-process-powered KN models in explaining the fast time evolution of the KN emission in GRB 211211A. Other parameters of the KN models are β 0 = 0.05, β m = 0.4, and n = 2.
Paper: GRB 211211A: The Case for an Engine-powered over r-process-powered Blue Kilonova
Authors: Hamid Hamidani, Masaomi Tanaka, Shigeo S. Kimura, Gavin P. Lamb, Kyohei Kawaguchi
Figure caption: Time evolution of r-process-powered KN light curve. The early blue KN emission (thick blue line) is ∝ t −0.3, as it is mostly powered by diffusion emission (thin blue line; first term in Equation (5)). After a transitional phase, later emission (thick red line) follows the deposition rate of thermal energy through the r-process (thin red line in the optically thin part and dashed line in the whole ejecta) as ∝t −1.3 (second term in Equation (5)) and asymptotically as ∝t −2.3−t −2.8 (for a similar figure, see Figure 4 in Kasen & Barnes 2019; also see Waxman et al. 2019; Hotokezaka & Nakar 2020).
Paper: GRB 211211A: The Case for an Engine-powered over r-process-powered Blue Kilonova
Authors: Hamid Hamidani, Masaomi Tanaka, Shigeo S. Kimura, Gavin P. Lamb, Kyohei Kawaguchi
Figure caption: The ejecta mass (M e) and opacity (κ) parameter space for r-process-powered KN models. The area constrained by the thick blue line (as indicated by the blue arrow) is where KN models are at least as bright as the early (5–10 hr) blue KN emission observed in GRB 211211A (within 1σ); blue stripes indicate the parameter space where this is not the case (ruled out). The area constrained by the thick red line (as indicated by the red arrow) is where the KN models do not overpredict the late-time red emission (1.4–4.2 days; see Figure 3); red stripes indicate the parameter space where this is not satisfied (ruled out). There is no eligible parameter space where both the early and late emission of the KN in GRB 211211A can be explained by a combination of two r-process-powered KN models. Diamond symbols indicate the three KN models shown in Figure 3. The other parameters are taken as β 0 = 0.05, β m = 0.4, and n = 2 (found to have limited effects on the results).
Paper: GRB 211211A: The Case for an Engine-powered over r-process-powered Blue Kilonova
Authors: Hamid Hamidani, Masaomi Tanaka, Shigeo S. Kimura, Gavin P. Lamb, Kyohei Kawaguchi
Figure caption: Same as Figure 2. The bolometric luminosity of our alternative central engine model, where a low-power jet launched by late engine activity interacts with the lanthanide-rich ejecta to explain the early (<1 day) KN emission in GRB 211211A (blue line), while the r-process explains the late (1−4 days) red KN emission (red line) (see Figure 6 for the SED). This model can explain GRB 211211A data with only one red ejecta component. The parameters of the jet in the central engine model are jet isotropic equivalent luminosity L iso,0 = 1047 erg s−1 and jet opening angle θ 0 = 7.°5.