adsabs/AstroCLIMB huggingface dataset:
Paper: Time Evolution Images of the Hypergiant RW Cephei during the Rebrightening Phase Following the Great Dimming
Authors: Narsireddy Anugu, Douglas R. Gies, Rachael M. Roettenbacher, John D. Monnier, Miguel Montargés, Antoine Mérand, Fabien Baron, Gail H. Schaefer, Katherine A. Shepard, Stefan Kraus, Matthew D. Anderson, Isabelle Codron, Tyler Gardner, Mayra Gutierrez, Rainer Köhler, Karolina Kubiak, Cyprien Lanthermann, Olli Majoinen, Nicholas J. Scott, Wolfgang Vollmann
Figure caption: The OITOOLS fitting residuals for the K-band (2.0−2.31 μm) visibilities (left) and closure phases (right). These are for the epoch 2023 June 21. The gray symbols with vertical error bars are the measurements, and the red dots represent the corresponding fits from the OITOOLS reconstructed images. The lower panels show the fitting residuals in standard deviation (σ%). See Section 5 for the image reconstruction procedures used.
Paper: Time Evolution Images of the Hypergiant RW Cephei during the Rebrightening Phase Following the Great Dimming
Authors: Narsireddy Anugu, Douglas R. Gies, Rachael M. Roettenbacher, John D. Monnier, Miguel Montargés, Antoine Mérand, Fabien Baron, Gail H. Schaefer, Katherine A. Shepard, Stefan Kraus, Matthew D. Anderson, Isabelle Codron, Tyler Gardner, Mayra Gutierrez, Rainer Köhler, Karolina Kubiak, Cyprien Lanthermann, Olli Majoinen, Nicholas J. Scott, Wolfgang Vollmann
Figure caption: The PMOIRED fit residuals (V 2 and T3PHI) of the MYSTIC K-band data (λ = 2.0−2.39 μm) for the epoch 2023 July 21 are shown. The black lines represent the interferometric data, while the red lines depict the analytical model fits. The CHARA baselines are indicated in each baseline box. For details on the PMOIRED model fitting procedures, refer to Section 4.
Paper: Time Evolution Images of the Hypergiant RW Cephei during the Rebrightening Phase Following the Great Dimming
Authors: Narsireddy Anugu, Douglas R. Gies, Rachael M. Roettenbacher, John D. Monnier, Miguel Montargés, Antoine Mérand, Fabien Baron, Gail H. Schaefer, Katherine A. Shepard, Stefan Kraus, Matthew D. Anderson, Isabelle Codron, Tyler Gardner, Mayra Gutierrez, Rainer Köhler, Karolina Kubiak, Cyprien Lanthermann, Olli Majoinen, Nicholas J. Scott, Wolfgang Vollmann
Figure caption: The u v-coverage of RW Cep observations for different epochs. The top panels are for MIRC-X, and the bottom panels are for MYSTIC. The u v-coordinates represent the projections of the baseline vectors on the plane of the sky of the target.
Paper: Time Evolution Images of the Hypergiant RW Cephei during the Rebrightening Phase Following the Great Dimming
Authors: Narsireddy Anugu, Douglas R. Gies, Rachael M. Roettenbacher, John D. Monnier, Miguel Montargés, Antoine Mérand, Fabien Baron, Gail H. Schaefer, Katherine A. Shepard, Stefan Kraus, Matthew D. Anderson, Isabelle Codron, Tyler Gardner, Mayra Gutierrez, Rainer Köhler, Karolina Kubiak, Cyprien Lanthermann, Olli Majoinen, Nicholas J. Scott, Wolfgang Vollmann
Figure caption: The K-band observations of RW Cep from 2023 July 21. The squared visibility and closure phases are presented in the top and bottom panels, respectively. The color bar represents the wavelength. The squared visibility in the CO band-head lines (2.3 μm) is smaller, indicating a larger angular size compared to that for the continuum.
Paper: Time Evolution Images of the Hypergiant RW Cephei during the Rebrightening Phase Following the Great Dimming
Authors: Narsireddy Anugu, Douglas R. Gies, Rachael M. Roettenbacher, John D. Monnier, Miguel Montargés, Antoine Mérand, Fabien Baron, Gail H. Schaefer, Katherine A. Shepard, Stefan Kraus, Matthew D. Anderson, Isabelle Codron, Tyler Gardner, Mayra Gutierrez, Rainer Köhler, Karolina Kubiak, Cyprien Lanthermann, Olli Majoinen, Nicholas J. Scott, Wolfgang Vollmann
Figure caption: Synthetic images reconstructed using the OITOOLS software. The synthetic observations replicate the same u v-coverage and signal-to-noise ratio as the real observations.
Paper: Time Evolution Images of the Hypergiant RW Cephei during the Rebrightening Phase Following the Great Dimming
Authors: Narsireddy Anugu, Douglas R. Gies, Rachael M. Roettenbacher, John D. Monnier, Miguel Montargés, Antoine Mérand, Fabien Baron, Gail H. Schaefer, Katherine A. Shepard, Stefan Kraus, Matthew D. Anderson, Isabelle Codron, Tyler Gardner, Mayra Gutierrez, Rainer Köhler, Karolina Kubiak, Cyprien Lanthermann, Olli Majoinen, Nicholas J. Scott, Wolfgang Vollmann
Figure caption: These ROTIR images are reconstructed from the synthetic observations, which replicate the same u v-coverage and signal-to-noise ratio as the real observations.
Paper: Evidence for Dust Depletion in a Misaligned Protoplanetary Disk with JWST
Authors: C. C. Espaillat, T. Thanathibodee, Z. Zhu, I. Rabago, J. Wendeborn, N. Calvet, L. Zamudio-Ruvalcaba, M. Volz, C. Pittman, M. McClure, J. F. Babb, R. Franco-Hernández, E. Macías, M. Reynolds, P.-G. Yan
Figure caption: Top: JWST spectrum of UX Tau A with some atomic lines, H2 lines, and PAH features identified. Bottom: MIR spectra of UX Tau A displaying MIR continuum variability over ∼19 yr (see legend). The JWST MIRI MRS spectrum is shown in black, and the other spectra are from Spitzer. We include WISE/NEOWISE W1 and W2 photometry, which are shown as magenta and teal circles. The stellar photosphere (dotted line) is adapted from C. Espaillat et al. (2011).
Paper: Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Gianna Cauzzi, Kevin Reardon
Figure caption: Pores’ rotation derived from VBI images and the changes in Lorentz force within the ViSP and HMI FOVs. Panel (a): pore rotation in VBI G band (red: pore A, cyan: pore B). White ellipses represent the best fit for each pore’s boundary; yellow dashed line indicates a reference angle. Panel (b): temporal evolution of pores’ rotation and the separation between them derived from VBI images. Panel (c): temporal evolution of positive (ϕ +) and negative (ϕ −) magnetic fluxes in the ViSP FOV. The GOES X-ray flux (1–8 Å) is shown in the gray line. Panel (d): temporal evolution of horizontal (δ F  h ) and radial (δ F  r ) component of Lorentz forces in the ViSP FOV (consisting of pores A and B; R1 region highlighted in panel (e)). Panels (f) and (g): temporal evolution of δ F  h  and δ F  r  derived from HMI in the regions R1 and R2 highlighted in panel (e).
Paper: Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Gianna Cauzzi, Kevin Reardon
Figure caption: Comparison of HMI ((a), (c)) and ViSP ((b), (d)) LOS magnetic field highlighted within the orange and red boxes in Figure 2. HMI LOS magnetic field contours are overlaid on the ViSP and HMI FOVs; the difference between two consecutive ticks corresponds to 5″. Solid, dashed, dotted, and dotted–dashed contours refer to the values of −500 G, −300 G, 500 G, and 300 G, respectively. (e) Scatterplot of LOS magnetic field derived from ViSP vs. HMI. r  s  is the Spearman correlation coefficient.
Paper: Evidence for Dust Depletion in a Misaligned Protoplanetary Disk with JWST
Authors: C. C. Espaillat, T. Thanathibodee, Z. Zhu, I. Rabago, J. Wendeborn, N. Calvet, L. Zamudio-Ruvalcaba, M. Volz, C. Pittman, M. McClure, J. F. Babb, R. Franco-Hernández, E. Macías, M. Reynolds, P.-G. Yan
Figure caption: TESS (black line/individual black dots) and ASAS-SN g-band (purple) light curves of UX Tau A. To facilitate comparison, the TESS data were scaled to match the ASAS-SN data. A vertical dotted line marks the time of the JWST observation.
Paper: Evidence for Dust Depletion in a Misaligned Protoplanetary Disk with JWST
Authors: C. C. Espaillat, T. Thanathibodee, Z. Zhu, I. Rabago, J. Wendeborn, N. Calvet, L. Zamudio-Ruvalcaba, M. Volz, C. Pittman, M. McClure, J. F. Babb, R. Franco-Hernández, E. Macías, M. Reynolds, P.-G. Yan
Figure caption: Schematics showing that the inner and outer disks are coplanar (left) and misaligned (right). If the inner disk has nodal precession along the vertical direction, it changes from the left to right panel after half the precession cycle.
Paper: Evidence for Dust Depletion in a Misaligned Protoplanetary Disk with JWST
Authors: C. C. Espaillat, T. Thanathibodee, Z. Zhu, I. Rabago, J. Wendeborn, N. Calvet, L. Zamudio-Ruvalcaba, M. Volz, C. Pittman, M. McClure, J. F. Babb, R. Franco-Hernández, E. Macías, M. Reynolds, P.-G. Yan
Figure caption: Hα profiles (blue) of UX Tau A and the average accretion flow model fit (black line) along with the top 100 best-fitting models (gray lines). The horizontal and vertical dotted lines correspond to the continuum and line center, respectively.
Paper: Evidence for Dust Depletion in a Misaligned Protoplanetary Disk with JWST
Authors: C. C. Espaillat, T. Thanathibodee, Z. Zhu, I. Rabago, J. Wendeborn, N. Calvet, L. Zamudio-Ruvalcaba, M. Volz, C. Pittman, M. McClure, J. F. Babb, R. Franco-Hernández, E. Macías, M. Reynolds, P.-G. Yan
Figure caption: MIR light curve of UX Tau A from WISE/NEOWISE. The W1 and W2 data points are shown as light magenta and teal circles. The diamonds are the median flux taken over 2–3 days, and the error bars are the standard deviation. The vertical dotted line notes the time of the JWST observation.
Paper: Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Gianna Cauzzi, Kevin Reardon
Figure caption: Magnetic field topology and mean twist evolution derived from the data-driven simulation. Left and middle panels: top and side views of the magnetic field lines, highlighted by different colors; background image shows the HMI B LOS at 20:54 UT. Black arrow indicates a possible location of the magnetic null point. Right panel: the temporal evolution of the mean twist in the R1 region of the photosphere consisting of pores A and B. Yellow shaded area and dashed line refer to the GOES flare duration and flare peak time, respectively.
Paper: A Consistency Test of the Cosmological Model at the Epoch of Recombination Using DESI Baryonic Acoustic Oscillation and Planck Measurements
Authors: Levon Pogosian, Gong-Bo Zhao, Karsten Jedamzik
Figure caption: Left panel: constraints on H 0, r d, r d h, and Ωm derived from the DESI Y1 BAO data, from DESI Y1 BAO combined with a prior on Ωm h 2, from DESI Y1 BAO combined with the CMB acoustic scale β ⋆ and a prior on Ωm h 2, and the best-fit Planck ΛCDM. Right panel: same analysis as in the right panel using the pre-DESI BAO data.
Paper: A Consistency Test of the Cosmological Model at the Epoch of Recombination Using DESI Baryonic Acoustic Oscillation and Planck Measurements
Authors: Levon Pogosian, Gong-Bo Zhao, Karsten Jedamzik
Figure caption: Marginalized 68% and 95% confidence level (CL) contours for H 0 and r d from the SDSS+ and DESI Y1 BAO data, and the two BAO data sets combined with the CMB acoustic scale β ⋆ and a prior on Ωm h 2. Shown also are the contours for the best-fit Planck ΛCDM model.
Paper: On the Kinematic Nature of Apparent Disks at High Redshifts: Local Counterparts are Not Dominated by Ordered Rotation but by Tangentially Anisotropic Random Motion
Authors: Bitao Wang, Yingjie Peng, Michele Cappellari, Hua Gao, Houjun Mo
Figure caption: The stellar spin ﹩{\lambda }_{{R}_{{\rm{e}}}}﹩ vs. flattening ε, indicating the overall warm/hot stellar kinematics of low-mass galaxies in the local Universe. The large black square and error bars denote the median and 16th–84th percentiles of the low-mass sample, respectively, each galaxy of which is shown by a small black square. The most actively star-forming ones (0.5 dex above the SFMS) are circled in orange, and among local low-mass galaxies they can be better analogs of high-z low-mass systems for further similarity in star formation and gas properties. For comparison, Milky Way analogs in the local Universe, as representatives of real dynamically cold thin disks, are shown by the large blue square, and the area occupied by dynamically hot slow rotators is illustrated by the shaded trapezoid. The green and magenta solid curves are loci, respectively, for isotropic and anisotropic edge-on axisymmetric galaxies, predicted by tensor virial theorem, with anisotropy in the stellar random motion as given by the relations δ = 0 and ﹩\delta =0.7{\varepsilon }_{\mathrm{intr}}﹩. The relations for nearly face-on (at an inclination angle of 30°) rotators are shown by the green and magenta dashed curves. We note that roughly half of low-mass galaxies distribute below the magenta solid curve, suggesting that they are significantly more anisotropic than galaxies of higher stellar masses that lie mostly above the magenta solid curve. The suggested high anisotropy of low-mass galaxies explains their flattened shapes at low levels of rotation.
Paper: On the Kinematic Nature of Apparent Disks at High Redshifts: Local Counterparts are Not Dominated by Ordered Rotation but by Tangentially Anisotropic Random Motion
Authors: Bitao Wang, Yingjie Peng, Michele Cappellari, Hua Gao, Houjun Mo
Figure caption: The misalignment (PAkine − PAphot) between the kinematic and photometric major axis as a function of ellipticity ε for MaNGA low-mass galaxies at z = 0, color coded by stellar spin ﹩{\lambda }_{{R}_{{\rm{e}}}}﹩ (slightly smoothed using the locally weighted regression method LOESS by W. S. Cleveland & S. J. Devlin 1988, as implemented by M. Cappellari et al. 2013a; the Python package LOESS is available at https://pypi.org/project/loess/). The measurements of the position angles of the two axes are detailed in the text. The gray contour lines show the Gaussian kernel-estimated density of galaxies, and to avoid edge effects and account for the periodicity of angles, we have utilized two more duplicates of the data points shifted by ±180°. Taking measurement uncertainty into account, the distribution is consistent with the case of oblate rotators that have aligned kinematic and photometric major axes.
Paper: On the Kinematic Nature of Apparent Disks at High Redshifts: Local Counterparts are Not Dominated by Ordered Rotation but by Tangentially Anisotropic Random Motion
Authors: Bitao Wang, Yingjie Peng, Michele Cappellari, Hua Gao, Houjun Mo
Figure caption: The probability density distributions of the ellipticity ε of galaxy-projected shapes for low-mass galaxies (black solid line) and Milky Way analogs (blue dashed line) observed at z = 0 and for galaxies in the early Universe z = 3−8 (﹩9\lt \mathrm{lg}({{ \mathcal M }}_{\star }/{{ \mathcal M }}_{\odot })\lt 9.5﹩ in JWST CEERS studied by V. Pandya et al. 2024b; the purple shaded area). The density distributions are derived via kernel density estimation with Gaussian kernels of widths determined based on Scott’s rule. For local low-mass galaxies, we estimate the uncertainty of the distribution using 1000 bootstrap samples shown by the thin black lines. Suggesting the intrinsic shapes to first order, we have also shown the predicted distributions of oblate (﹩c\lt b=a,c/a\sim { \mathcal N }(\mu =0.3,\sigma =0.1);﹩ the thick gray line) and prolate (﹩c=b\lt a,c/a\sim { \mathcal N }(\mu =0.3,\sigma =0.1);﹩ the orange shaded area) ellipsoids randomly projected on the sky plane.
Paper: On the Kinematic Nature of Apparent Disks at High Redshifts: Local Counterparts are Not Dominated by Ordered Rotation but by Tangentially Anisotropic Random Motion
Authors: Bitao Wang, Yingjie Peng, Michele Cappellari, Hua Gao, Houjun Mo
Figure caption: The concentration of rest-frame optical surface brightness profiles, as quantified by Sérsic indices, vs. the ellipticity ε (i.e., flattening or fractional axial difference 1 − b/a) of optical isophotes. The red and blue symbols mark the medians and 16th–84th percentiles of JWST visually identified spheroids and disks, respectively, from K23 and F23, while the black symbol is for low-mass galaxies in the local Universe observed in the MaNGA survey. The stellar masses of these low-mass galaxies at z = 0 are typical in the JWST samples.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). II. A Second Giant Planet in the 17 Myr System HIP 67522
Authors: Madyson G. Barber, Pa Chia Thao, Andrew W. Mann, Andrew Vanderburg, Mayuko Mori, John H. Livingston, Akihiko Fukui, Norio Narita, Adam L. Kraus, Benjamin M. Tofflemire, Elisabeth R. Newton, Joshua N. Winn, Jon M. Jenkins, Sara Seager, Karen A. Collins, Joseph D. Twicken
Figure caption: Ground-based follow-up transits of HIP 67522c from MuSCAT4 (left) and Sinistro (top right), with 5 minute bins shown for clarity. The MuSCAT4 transits were taken simultaneously, with each filter fitted separately. The three simultaneous Sinistro ﹩r^{\prime} ﹩ transits were stacked and fit together. Each filter was fit with a BATMAN model, two Gaussian spot models, and a second-order polynomial to account for stellar variability. The opaque pink lines are the best-fit model, and the translucent lines are 100 models pulled from the fit posterior. The residuals for each transit are also shown. Bottom right: transit depth, measured by ﹩{({R}_{p}/{R}_{* })}^{2}﹩, posterior from each of the transit fits. The data sets used to create this figure are available for download from the online journal.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). II. A Second Giant Planet in the 17 Myr System HIP 67522
Authors: Madyson G. Barber, Pa Chia Thao, Andrew W. Mann, Andrew Vanderburg, Mayuko Mori, John H. Livingston, Akihiko Fukui, Norio Narita, Adam L. Kraus, Benjamin M. Tofflemire, Elisabeth R. Newton, Joshua N. Winn, Jon M. Jenkins, Sara Seager, Karen A. Collins, Joseph D. Twicken
Figure caption: Representative section of the TESS light curve (gray points) with the best-fit GP model (red line). The locations of transits of HIP 67522b and c and the location of the removed flare are shown as the highlighted regions. The data set used to create this figure is available for download from the online journal.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: The evolution of the stripped mass δ M with ever-decreasing R  p /R  t  during the RPD process, calculated from Equations (1), (2), and (7). The black, red, and blue lines are for different initial WD masses. Note that we start the process for all initially at R  p /R  t  = 1.8 and later keep R  p  fixed. As the RPD proceeds, M * decreases due to mass stripping; thus, R  t  increases.
Paper: TESS Investigation—Demographics of Young Exoplanets (TI-DYE). II. A Second Giant Planet in the 17 Myr System HIP 67522
Authors: Madyson G. Barber, Pa Chia Thao, Andrew W. Mann, Andrew Vanderburg, Mayuko Mori, John H. Livingston, Akihiko Fukui, Norio Narita, Adam L. Kraus, Benjamin M. Tofflemire, Elisabeth R. Newton, Joshua N. Winn, Jon M. Jenkins, Sara Seager, Karen A. Collins, Joseph D. Twicken
Figure caption: Individual transits of HIP 67522c and the GP model. Data in Sector 64 (20 s cadence) are binned to 2 minute intervals for easier comparison with Sector 11 and 38 (2 minute cadence). The transits show high levels of in-transit variation (potentially due to spot crossings). Bottom right: phase-folded light curve of HIP 67522 taken with TESS (gray points) and individual transits binned to 10 minute intervals (colored points) after the GP model of stellar variability has been removed. The best-fit model transit of HIP 67522c is shown as the red line. The data set used to create this figure is available for download from Figure 1 in the online journal.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: The evolution of the stripped mass with time (in units of orbital period P) for a WD with the initial mass of 1.3 M ⊙, as calculated by Equations (1), (2), and (7). The zero time here is chosen to be when the stripped mass first reaches a GRB-jet-generating threshold, which is set to be δ M ≃ 0.1 M ⊙. The first episode lasts very long (∼104 orbits; see J.-H. Chen et al. 2023), and the second episode produces GRB and shows QPM, while the third episode has no or weak QPM, and the RPD process ends at this episode.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: The periodic analysis results of the light curve of GRB 230307A in the QPM phase in the 500–2000 keV band. Panels (a), (b), (c), and (d) show the results of WWZ, PDS, LSP, and epoch folding, respectively. The dashed red line indicates the period corresponding to the extreme peak power, and the green, blue, and purple dashed lines represent the 95%, 99%, and FAP = 0.01% confidence levels, respectively.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: The left panel presents the light curve of GRB 230307A in the 30–2000 keV energy range, where the light yellow region indicates the QPM episode. The right panel shows an enlarged view of the QPM episode, in three energy bands. The blue dashed lines indicate the cycles of the QPM.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: The evolution of the stripped masses of the WDs during the QPM episode, in the RPD scenario for GRBs 060614 and 211211A, respectively. The zero time here is chosen to be when the stripped mass first reaches 0.1 M ⊙.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: Same as in Figure 3 but for GRB 060614 (15–350 keV).
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: Same as in Figure A2 but for GRB 060614 (15–350 keV); note that the orange dashed line indicates the 99.7% confidence level.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: Same as in Figure A2 but for GRB 230307A (100–300 keV).
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: Same as in Figure 3 but for GRB 211211A (15–5000 keV).