adsabs/AstroCLIMB huggingface dataset:
Paper: Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49
Authors: Anindya Saha, Anandmayee Tej, Hong-Li Liu, Tie Liu, Guido Garay, Paul F. Goldsmith, Chang Won Lee, Jinhua He, Mika Juvela, Leonardo Bronfman, Tapas Baug, Enrique Vázquez-Semadeni, Patricio Sanhueza, Shanghuo Li, James O. Chibueze, N. K. Bhadari, Lokesh K. Dewangan, Swagat Ranjan Das, Feng-Wei Xu, Namitha Issac, Jihye Hwang, L. Viktor Tóth
Figure caption: (a) Effective line-of-sight excitation temperature map generated using HCO+. (b) Column-density map toward G24.47, generated using molecular transitions H13CO+ and HCO+. The ellipses represent the apertures of identified molecular cores. In both panels, the overlaid contours show the H40α emission with contour levels starting at 2σ (σ = 0.04 Jy beam−1 km s−1) in steps of 1σ. These contours are smoothed over 5 pixels using Gaussian kernel. The beam size of 2.″5 is indicated at the bottom left.
Paper: Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49
Authors: Anindya Saha, Anandmayee Tej, Hong-Li Liu, Tie Liu, Guido Garay, Paul F. Goldsmith, Chang Won Lee, Jinhua He, Mika Juvela, Leonardo Bronfman, Tapas Baug, Enrique Vázquez-Semadeni, Patricio Sanhueza, Shanghuo Li, James O. Chibueze, N. K. Bhadari, Lokesh K. Dewangan, Swagat Ranjan Das, Feng-Wei Xu, Namitha Issac, Jihye Hwang, L. Viktor Tóth
Figure caption: Channel maps of HCO+ overlaid with H40α contours (Gaussian smoothed over 5 pixels) with levels starting at 2σ (σ = 0.04 Jy beam−1 km s−1) in steps of 1σ. Each panel shows the velocity-integrated intensity within a velocity range of 1 km s−1. The velocity range is mentioned in the top left of each panel.
Paper: Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49
Authors: Anindya Saha, Anandmayee Tej, Hong-Li Liu, Tie Liu, Guido Garay, Paul F. Goldsmith, Chang Won Lee, Jinhua He, Mika Juvela, Leonardo Bronfman, Tapas Baug, Enrique Vázquez-Semadeni, Patricio Sanhueza, Shanghuo Li, James O. Chibueze, N. K. Bhadari, Lokesh K. Dewangan, Swagat Ranjan Das, Feng-Wei Xu, Namitha Issac, Jihye Hwang, L. Viktor Tóth
Figure caption: A schematic of the hierarchical triggering of multi-epoch massive star formation in G24.47.
Paper: Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49
Authors: Anindya Saha, Anandmayee Tej, Hong-Li Liu, Tie Liu, Guido Garay, Paul F. Goldsmith, Chang Won Lee, Jinhua He, Mika Juvela, Leonardo Bronfman, Tapas Baug, Enrique Vázquez-Semadeni, Patricio Sanhueza, Shanghuo Li, James O. Chibueze, N. K. Bhadari, Lokesh K. Dewangan, Swagat Ranjan Das, Feng-Wei Xu, Namitha Issac, Jihye Hwang, L. Viktor Tóth
Figure caption: Morphology of the region associated with G24.47. (a) Spitzer-IRAC color-composite image overlaid with VLA 4.86 GHz contours at [3, 7, 20, 50, 90, 110, 120] × σ (=0.4 mJy beam−1). (b) VLA 4.86 GHz map overlaid with ATOMS H40α contours (Gaussian smoothed over 5 pixels) starting at 2σ (=0.04 Jy beam−1 km s−1) in steps of 1σ. The displayed ellipses are identified VLA cores with their central positions (X) marked. The insets show the H40α spectra (boxcar smoothed by four channels; velocity resolution of 6.0 km s−1) of the cores along with their respective Gaussian fits. The LSR velocity of 101.5 km s−1 is indicated in each. (c) ALMA 3 mm map overlaid with the H40α contours displayed in (b). The displayed ellipses are identified 3 mm cores with their central positions (+) marked. (d) Moment-zero map (3 pixel smoothed using Gaussian kernel) of H13CO+ in the velocity range 93.0 to 113.0 km s−1. The displayed ellipses are identified molecular cores with their central positions (+) marked. Ellipses drawn in the lower left corner of (b), (c), and (d) represent the beams of the respective maps displayed.
Paper: Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49
Authors: Anindya Saha, Anandmayee Tej, Hong-Li Liu, Tie Liu, Guido Garay, Paul F. Goldsmith, Chang Won Lee, Jinhua He, Mika Juvela, Leonardo Bronfman, Tapas Baug, Enrique Vázquez-Semadeni, Patricio Sanhueza, Shanghuo Li, James O. Chibueze, N. K. Bhadari, Lokesh K. Dewangan, Swagat Ranjan Das, Feng-Wei Xu, Namitha Issac, Jihye Hwang, L. Viktor Tóth
Figure caption: Moment-zero (left three columns) and moment-one (rightmost column) maps of HCO+ and H40α observed toward G24.47 are shown in panels (a)–(d) and (e)–(h), respectively. The velocity ranges used to obtain the moment-zero maps are given in the top left of each panel. The color bar indicates the flux scale in Jansky per beam kilometer per second and kilometer per second for moment-zero and moment-one maps, respectively. The overlaid contours (in panels (a)–(d)) show the H40α emission (presented as color scale in panel (e)) with contour levels starting at 2σ (σ = 0.04 Jy beam−1 km s−1) in steps of 1σ. These contours are smoothed over 5 pixels using Gaussian kernel. The moment-zero maps (in panels (e)–(g)) are smoothed across 3 pixels using Gaussian kernel. The beam is indicated at the bottom left corner in each panel.
Paper: Direct Observational Evidence of Multi-epoch Massive Star Formation in G24.47+0.49
Authors: Anindya Saha, Anandmayee Tej, Hong-Li Liu, Tie Liu, Guido Garay, Paul F. Goldsmith, Chang Won Lee, Jinhua He, Mika Juvela, Leonardo Bronfman, Tapas Baug, Enrique Vázquez-Semadeni, Patricio Sanhueza, Shanghuo Li, James O. Chibueze, N. K. Bhadari, Lokesh K. Dewangan, Swagat Ranjan Das, Feng-Wei Xu, Namitha Issac, Jihye Hwang, L. Viktor Tóth
Figure caption: (a) Spectra (averaged over entire molecular ring) of H13CO+ (1–0), HCO+ (1–0), and H40α toward G24.47 are shown in red, green, and blue lines, respectively. H13CO+ (1–0) and H40α spectra are scaled up by factors of 3 and 30, respectively. H40α spectrum is boxcar smoothed by four channels, resulting in a velocity resolution of 6.0 km s−1. (b) PV diagram of HCO+ along the PV cut in east–west direction, centered on the ALMA phase center (marked in panel (c)). The contours start at 3σ (σ = 3.0 mJy beam−1) in steps of 6σ. The circular velocity structure is indicated by the white dashed line. The black dashed–dotted line marks the LSR velocity of 101.5 km s−1 in panels (a) and (b). (c) Moment-zero map of HCO+; this panel is same as Figure 2(a).
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: The Gaia DR3 AMRF (﹩{ \mathcal A }﹩) as a function of the primary mass. The maximal possible AMRF values for an MS secondary (﹩{{ \mathcal A }}_{\mathrm{MS}}﹩) and an MS close binary (﹩{{ \mathcal A }}_{\mathrm{TR}}﹩) companion are marked by the dotted and dashed lines, respectively. The underlying light gray density plot shows the measured values from Gaia DR3 (after applying some quality cuts on the astrometric solutions; see Shahaf et al. 2023). Our selected volume-limited samples of high-probability MS+WD systems with different primary masses (see legend) are plotted with purple markers and gray error bars. Note that because of the primary mass uncertainty, there is some overlap between the samples. The expected AMRF values of WD companions of different masses are marked by blue shaded stripes, ranging from 0.2 M ⊙ (light blue) to 1.4 M ⊙ (dark blue) in steps of 0.1 M ⊙.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Secondary mass distribution of the selected volume-limited samples with MS primaries of 0.5 M ⊙ ≤ M 1 < 0.6 M ⊙, 0.6 M ⊙ ≤ M 1 < 0.7 M ⊙, and 0.7 M ⊙ ≤ M 1 < 0.8 M ⊙ (purple shaded bars) and the full no-red-color-excess sample (dotted black). The observed distribution of the full 40 pc WD sample of O’Brien et al. (2024; solid black) and the magnitude-limited 100 pc hydrogen-dominated (DA) WD samples of Jiménez-Esteban et al. (2023; solid red) and Kilic et al. (2020; solid blue) are plotted for reference. The inset panel zooms in on the high-mass end of the distribution.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Period–eccentricity relation of the selected samples (purple markers with black error bars). Systems of higher multiplicity (see Section 4.3) are marked by a red square. The two-dimensional histogram of a class I (PrI > 0.9) subsample with the same constraints on the primary mass, orbital separation, and distance is plotted in blue shades for reference.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Mass–period relation of the selected samples (purple markers indicating different primary mass ranges as in Figure 1; see legend) and the full no-red-color-excess sample (blue dots). Systems of higher multiplicity (see Section 4.3) are marked by a red square. The solid lines show the theoretical relation from Chen et al. (2013) for different metallicities (from top to bottom, Z = 0.02, 0.01, 0.004, and 0.001), while the dashed lines show the relation from Rappaport et al. (1995) for Z = 0.02 and 0.004. The y-axis shows the orbital period, P, times (1 − e)3/2, where e is the eccentricity (see Joss et al. 1987 for a derivation of this relation).
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Histograms of the parallax error, cosine of the inclination angle, transverse velocity, projected semimajor axis, period, eccentricity, metallicity, primary mass, and mass ratio (from right to left, top to bottom) of the selected volume-limited samples and the reference full no-red-color-excess sample. The dips in the period around 1 and 2 yr are a result of Gaia’s mission duration.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Cumulative number of systems as a function of the probed volume (solid line) for a variety of photometric primary mass bins (top: 0.5 M ⊙ ≤ M 1 < 0.6 M ⊙; middle: 0.6 M ⊙ ≤ M 1 < 0.7 M ⊙; bottom: 0.7 M ⊙ ≤ M 1 < 0.8 M ⊙). The dashed line shows the expected number assuming a constant space density (calculated based on the total number of systems per sample at a maximal distance of 225 pc), and the gray region highlights its Poisson uncertainty. The dotted red line marks the selected maximal distance for each sample.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: The WD mass distributions of our samples (purple shaded bars) compared to those of WDs orbiting mild barium giants (black solid line) and strong barium giants (red dashed line) from Escorza & De Rosa (2023).
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: The cumulative fraction of massive WDs, relative to the full distribution. See Appendix B for the fitting procedure used to estimate the high-mass fraction.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Dereddened absolute Gaia G-band magnitude of the tertiary companions vs. that of the corresponding inner binary. Systems where the tertiary has a redder (bluer) G BP−G RP color are marked by red circles (blue triangles). The dashed black line corresponds to equal absolute magnitudes.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Gaia dereddened color–magnitude diagram for the tertiary companions in the higher-multiplicity systems in our sample (marked by red circles). The number density of the Gaia 100 pc sample is shown in gray scale for reference.
Paper: A Deficit of Massive White Dwarfs in Gaia Astrometric Binaries
Authors: Na'ama Hallakoun, Sahar Shahaf, Tsevi Mazeh, Silvia Toonen, Sagi Ben-Ami
Figure caption: Double-Gaussian fit to the mass distribution of our final samples (top three panels), the 40 pc field sample of O’Brien et al. (2024; fourth panel), and the 100 pc field samples of Jiménez-Esteban et al. (2023; fifth panel) and Kilic et al. (2020; bottom panel). The bar plot shows the underlying observed distribution. The solid line shows the fitted function, while the dashed lines show the individual Gaussian components of the fit.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Corner plot of the posterior distribution for the parameters L 0, θ  c , and θ  v , assuming a top-hat jet structure. In the off-diagonal plots, the dashed and solid lines indicate the 50% and 90% credible regions. In the middle panel P(θ  v ), we report in red the prior π(θ  v ) derived from the GW analysis. The vertical dotted lines identify the 1σ credible interval (16th and 84th percentiles), while the dashed lines are the median (50th percentile). For the other posteriors, P(L 0) and P(θ  c ), the vertical dashed and solid lines report the 50th and 90th percentiles of each posterior, respectively. The gray scale in the off-diagonal plots indicates the posterior density, where darker corresponds to larger values. The excluded regions are outside the gray areas.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Upper left panel: joint Swift-BAT+Fermi-GBM flux upper limit sky map in the 15–350 keV band. The upper limits are relative to a timescale of 1 s, computed at 5σ confidence level. For the individual contributions from the two telescopes, see Figure 11. Upper right panel: joint Swift-BAT+Fermi-GBM sky map of the bolometric luminosity upper limit. The luminosity is computed in the rest-frame energy range 1 keV–10 MeV. In both upper panels, the solid and dashed lines are the GW localization contours at 90% and 50% credibility, respectively. Lower panel: weighted distribution of the luminosity upper limit, where the weight is given by the GW probability density of the single pixel. The vertical dashed line represents the weighted average over the sky of the luminosity upper limit.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Posterior distribution of the luminosity profile L(θ  v ), assuming different angular structures. The color density is produced by randomly extracting L 0, θ  c , s, and L off from the relative posterior samples, which are then given as input to compute the luminosity profile L(θ  v ) for each extraction. For each subplot, the solid (dashed) lines indicate the 90% (50%) upper limits.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption:  L 0–θ  c  posterior probability (taken from the lower left panel of Figure 2) compared with estimates from Rouco Escorial et al. (2023) of isotropic luminosities and opening angles of a sample of short GRBs. The green point is relative to GW170817, for which the on-axis isotropic luminosity is taken from Salafia et al. (2019) and the opening angle from Ghirlanda et al. (2019). The solid and dashed lines are 90% and 50% exclusion regions derived from the present analysis under the assumption of a top-hat jet structure.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Upper-limit sky map in the 15–350 keV band for Swift-BAT (left) and Fermi-GBM (right). The upper limits are relative to a timescale of 1 s, computed at a 5σ confidence level. Solid and dashed lines are the GW contours at 90% and 50% credibility, respectively. The white region is the position of the Earth, for which no upper limits are available.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Regions of the L 0–θ  c  plane excluded by the condition M ej < 0.052 M ⊙. The exclusion lines are computed for different values of α, defined in the text. The dashed and solid black lines are the 50% and 90% exclusion regions reported from Figure 2.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Posterior distribution of the efficiency factor η, which is the fraction of accretion power that is converted in the beaming-corrected luminosity of the jet. The posterior is produced for the EoSs H4 and DD2, assuming an accretion timescale of 1 s and 0.1 s.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Same as Figure 2 but assuming a power-law profile for the jet structure with an off-axis slope s = 2 (top) and s = 4 (bottom).
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Same as Figure 2 but for a power-law model with s as a free parameter (top panel) and the top-hat+isotropic component (bottom panel). For the panel of the posterior distribution of s, the solid line reports the 10th percentile.
Paper: Constraining Possible γ-Ray Burst Emission from GW230529 Using Swift-BAT and Fermi-GBM
Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov, Michelle C. Hui, Rahul Kashyap, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Hiroyuki Nakano, Giacomo Principe, Oliver J. Roberts, Bangalore Sathyaprakash, Lijing Shao, Eleonora Troja, Péter Veres, Colleen A. Wilson-Hodge
Figure caption: Same as Figure 2 but assuming a Gaussian profile for the jet structure.