adsabs/AstroCLIMB huggingface dataset:
Paper: Protostellar Disk Formation Regimes: Angular Momentum Conservation versus Magnetic Braking
Authors: Hsi-Wei Yen, Yueh-Ning Lee
Figure caption: (a) Observed disk radius and protostar+disk mass distribution in our sample (data points; the same as Figure 3) in comparison with the theoretical predictions. Blue and red shaded areas represent the theoretically predicted relationship between disk radius and protostar+disk mass from the hydrodynamic (Equation (1)) and nonideal MHD models (Equations (2) and (3)), respectively. The nonideal MHD solutions in principle extend toward the left-hand side, as delineated with red dashed lines. However, those solutions imply more angular momentum than that available in initial dense cores, so they are physically irrelevant. (b) Probability distribution of disk radii and protostar+disk masses of our sample sources (gray shaded area and contours) overlaid with the observed data points. From outer to inner contours, they enclose 99%, 92%, 87%, 60%, and 27% of the total number of the sample sources, respectively. (c) is the same as (b) but for the comparison of the probability distributions between our observed and synthetic (red contours) samples. The synthetic sample is generated with the observed protostar+disk mass distribution and theoretical disk radii from hydrodynamics and nonideal MHD. (d) Cumulative distributions of the disk radii of our observed (black) and synthetic (red) samples. Gray shaded area and red dashed lines delineate the corresponding uncertainties. Similar to Figure 2, the cumulative distributions and their uncertainties are inferred from 1000 iterations of varying data points within their uncertainties. The K-S test on the two distributions results in a p-value of 0.5.
Paper: Protostellar Disk Formation Regimes: Angular Momentum Conservation versus Magnetic Braking
Authors: Hsi-Wei Yen, Yueh-Ning Lee
Figure caption: (a) Radial profiles of specific angular momentum in dense cores inferred from observations. Shaded areas in different patterns and colors represent the results from different literature as labeled in the panel. The horizontal and vertical extents of the shaded areas denote the spatial ranges probed by those observations and the uncertainties in their measurements, respectively. A dashed line demonstrates the slope of the specific angular momentum profile of a dense core in rigid-body rotation. (b) Radial profiles of the ratio of rotational to gravitational energy in dense cores. Blue shaded area represents the profile derived from the averaged specific angular momentum profile of four observational results shown in panel (a), and its vertical extents represent the uncertainty. Black shaded area represents the ranges of the sizes and ratios of rotational to gravitational energy in dense cores observed by A. A. Goodman et al. (1993) for comparison. A horizontal dashed line denotes a constant ratio of 0.02. The corresponding enclosed mass for a given radius is labeled at the top of the panel.
Paper: Protostellar Disk Formation Regimes: Angular Momentum Conservation versus Magnetic Braking
Authors: Hsi-Wei Yen, Yueh-Ning Lee
Figure caption: Cumulative distributions of the disk radii in our sample (black) and in Orion measured with the ALMA observations (red; J. J. Tobin et al. 2020a). The gray shaded area and﻿ red dashed lines represent the uncertainties of the disk radius﻿ distributions. In the Orion sample, only disks without companions within 2000 au are included, the same as our sample. Eighteen out of 227 Orion disks included here are unresolved, and the minimum observed disk radius is 11 au, so its cumulative distribution starts at 11 au with a fraction of 0.08. The K-S test of these two distributions results in a p-value of 0.5.
Paper: Protostellar Disk Formation Regimes: Angular Momentum Conservation versus Magnetic Braking
Authors: Hsi-Wei Yen, Yueh-Ning Lee
Figure caption: Observed disk radius and protostar+disk mass distribution in our sample. The solid line represents the single power-law fitting to the data points, which results in a power-law index of 0.7 ± 0.1. The dashed line represents the double power-law fitting, where the power-law indices are 1.1 and 0.6 at masses lower and higher than 0.5 M ☉, respectively. Statistically, the fitted single power-law function better represents the data.
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: (Top) The 2D, master-background-subtracted, NIRSpec Prism spectrum of SN 2023adta and its host galaxy in MJy sr–1. As shown in Figure 1, our observations capture both the SN and part of its host galaxy. The central rows for the extraction of SN 2023adta and its host galaxy are noted by the dashed blue and pink horizontal lines, respectively. (Middle) The resulting 1D extractions of SN 2023adta (blue) and its host galaxy (pink) in flux converted to f  λ . The spectrum of SN 2023adta was scaled to its photometry at the same epoch, and the spectrum of the host galaxy was scaled to the 2022 photometry at the position of the SN with an identical 0.″1 aperture. Notable narrow emission lines from the host galaxy are marked with the dashed vertical lines. (Bottom) The difference between the flux-calibrated SN and host galaxy spectra from the middle panel. Assuming the host galaxy emission underlying the SN is similar to the galaxy emission at our extracted location, this spectrum should be mostly isolated SN flux. However, the presence of narrow emission lines could indicate that this subtraction is imperfect.
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: False-color images of SN 2023adta and its host galaxy taken in 2022 (left) and 2023 (right). The white rectangles show the orientation of the MSA three-shutter slitlet on the sky. Two additional nodded exposures were acquired north and south of this central location. The SN (indicated by the red arrow) is located near the southern edge of the central slit.
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: Rest-frame NIRSpec Prism spectrum of SN 2023adta (black curves) compared with spectra of a variety of other SN types at similar phases (colored curves). We mask negative values that result from imperfect host galaxy subtraction. The dotted gray curves show clipped host galaxy emission lines. The color of each curve corresponds to the SN type. From top to bottom, we show five SNe Ic-BL (blue), one SN Ic (light blue), two SNe Ib (green), one SN Ia (yellow), one Ca-rich SN (orange), and one SN IIb (dark red). An asterisk next to the phase of a comparison spectrum indicates that it was a matched spectrum using the SN classification code NGSF (Goldwasser et al. 2022).
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: (Left) The multiband light curve of SN 2023adta (colored points), plotted with the offsets shown for visual clarity, and its best-matched SN Ib/c light curve (dashed curves). The epoch of our NIRSpec Prism spectrum is marked with the dashed vertical line and indicates an approximate phase of +11 days relative to peak brightness in F150W . (Middle) Similar to the left panel but showing the best-fit SN II. (Right) Similar to the other panels but showing the best-fit SN Ia SALT3-NIR model (Pierel et al. 2022) with shape and color parameters of x 1 = −0.29 and c = 0.63, respectively.
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: A comparison of the host galaxy properties of SN 2023adta to the mass–metallicity relationship observed in SDSS field galaxies (gray contours, z ∼ 0; Eisenstein et al. 2011), core-collapse SN host galaxies from Kelly & Kirshner (2012) and additional SN Ic/Ic-BL host galaxies from Modjaz et al. (2020; colored points), and high-z galaxies observed with JWST (pink–yellow hexagons; Morishita et al. 2024). The dashed yellow line is the empirical, z = 3.3, mass–metallicity relationship derived in Sanders et al. (2021).
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: Comparison of the light-curve peak brightness (M  R,r ) and shape (Δm 15,R,r ) characteristics of SN 2023adta to other SESNe from Drout et al. (2011) and SNe Ic-BL from Taddia et al. (2019). Measurements were derived from R- and r-band photometry, respectively.
Paper: Discovery of a Relativistic Stripped-envelope Type Ic-BL Supernova at z = 2.83 with JWST
Authors: M. R. Siebert, C. DeCoursey, D. A. Coulter, M. Engesser, J. D. R. Pierel, A. Rest, E. Egami, M. Shahbandeh, W. Chen, O. D. Fox, Y. Zenati, T. J. Moriya, A. J. Bunker, P. A. Cargile, M. Curti, D. J. Eisenstein, S. Gezari, S. Gomez, M. Guolo, B. D. Johnson, B. A. Joshi, M. Karmen, R. Maiolino, R. M. Quimby, B. Robertson, L. G. Strolger, F. Sun, Q. Wang, T. Wevers
Figure caption: Similar to Figure 5 but zoomed in on the O I and Ca II NIR triplet region of each SN Ic-BL. The velocity width of the primary absorption feature suggests ejecta moving at >20,000 km s−1. The velocity we measure from the absorption minimum is 29,000 ± 2000 km s−1.
Paper: Neutron Star Kicks plus Rockets as a Mechanism for Forming Wide Low-eccentricity Neutron Star Binaries
Authors: Ryosuke Hirai, 遼介 平井, Philipp Podsiadlowski, Alexander Heger, Hiroki Nagakura, 洋樹 長倉
Figure caption: Period–eccentricity distributions of post-SN binaries with different forms of NS kicks. Gray dashed curves indicate fixed periastron distances, and the black solid curve is where it equals the pre-SN separation. Histograms at the top and right are the marginalized probability distributions of period and eccentricity, respectively. Black pluses (+) mark the locations of observed NS systems discovered with Gaia (K. El-Badry et al. 2024b), whereas green crosses (×) mark the location of symbiotic X-ray binaries with eccentricity measurements (D. K. Galloway et al. 2002; K. H. Hinkle et al. 2006, 2024; P. Nagarajan et al. 2024). Gaia NS1 is highlighted with an open plus.
Paper: Neutron Star Kicks plus Rockets as a Mechanism for Forming Wide Low-eccentricity Neutron Star Binaries
Authors: Ryosuke Hirai, 遼介 平井, Philipp Podsiadlowski, Alexander Heger, Hiroki Nagakura, 洋樹 長倉
Figure caption: Example evolution of orbital vector components. The horizontal axis is the accumulated rocket velocity normalized by the average orbital velocity, which can be regarded as a measure of time (see Equation (20)). Results from direct numerical integration of Equations (2)–(3) are shown as thin solid curves, and the analytical predictions are presented as thick dashed curves. The numerical model was evolved with an acceleration magnitude of ∣ a  roc∣ = ∣ F   g /μ∣/50.
Paper: Neutron Star Kicks plus Rockets as a Mechanism for Forming Wide Low-eccentricity Neutron Star Binaries
Authors: Ryosuke Hirai, 遼介 平井, Philipp Podsiadlowski, Alexander Heger, Hiroki Nagakura, 洋樹 長倉
Figure caption: Evolution of the orbital eccentricity as a function of the accumulated rocket velocity. Solid curves show results from direct numerical integration with various acceleration timescales τ acc. The black dashed curve is our analytical solution. Orbital parameters are the same as in Figure 1.
Paper: Neutron Star Kicks plus Rockets as a Mechanism for Forming Wide Low-eccentricity Neutron Star Binaries
Authors: Ryosuke Hirai, 遼介 平井, Philipp Podsiadlowski, Alexander Heger, Hiroki Nagakura, 洋樹 長倉
Figure caption: Trajectory of the orbital state vectors projected on the xy-plane. Circles indicate the initial values, and the arrows point the direction of evolution. Parameters for the orbit are the same as in Figure 1.
Paper: Relation between the keV–MeV and TeV Emission of GRB 221009A and Its Implications
Authors: Yan-Qiu Zhang, Haoxiang Lin, Shao-Lin Xiong, Zhuo Li, Ming-Yu Ge, Chen-Wei Wang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang, Li-Ming Song, Chao Zheng, Wang-Chen Xue, Jia-Cong Liu, Wen-Jun Tan, Yue Wang, Wen-Long Zhang
Figure caption: Results of fitting the TeV light curve using the cumulative curve of the keV–MeV emission. The fitted time period is T ref + (235.0, 245.5) s (i.e., time interval C), as shown in panel (a). In panel (a), the blue data points are the TeV light curve with LHAASO, and the red dashed line is the fitting result of TeV light curve presented in Z. Cao et al. (2023). The cyan dashed line is the result of fitting the TeV light curve using the keV–MeV cumulative curve, and the corner plots of this fitting are shown on the right. The residuals for these fittings are shown in panel (b). The keV–MeV flux light curve measured with GECAM-C (Z.-H. An et al. 2023) is displayed in panel (c).
Paper: Relation between the keV–MeV and TeV Emission of GRB 221009A and Its Implications
Authors: Yan-Qiu Zhang, Haoxiang Lin, Shao-Lin Xiong, Zhuo Li, Ming-Yu Ge, Chen-Wei Wang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang, Li-Ming Song, Chao Zheng, Wang-Chen Xue, Jia-Cong Liu, Wen-Jun Tan, Yue Wang, Wen-Long Zhang
Figure caption: Evolution of delay time induced by kinetic energy propagation for ISM (left) and wind (right) models. The shaded square corresponds to T  C  = T ref + (235, 245.5) s and ﹩{\rm{\Delta }}{T}_{C}={4.45}_{-0.26}^{+0.26}\,{\rm{s}}﹩, the fitted time period and time translation between keV–MeV and TeV emission in Figure 2. Throughout all the models, we have chosen T 0 = T ref + 0 s (solid lines) and T 0 = T ref + 225 s (dashed lines) and the fiducial parameters as η  γ  = A 0 = A 34 = 1.
Paper: Relation between the keV–MeV and TeV Emission of GRB 221009A and Its Implications
Authors: Yan-Qiu Zhang, Haoxiang Lin, Shao-Lin Xiong, Zhuo Li, Ming-Yu Ge, Chen-Wei Wang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang, Li-Ming Song, Chao Zheng, Wang-Chen Xue, Jia-Cong Liu, Wen-Jun Tan, Yue Wang, Wen-Long Zhang
Figure caption: The best-fit SSC/(SSC+EIC) emission and ISM/wind medium solutions (red lines) to the LHAASO TeV light curves (blue) in the upper panel for each subplot. The data residuals (blue) for the SSC component are shown together with the EIC component (red dotted) in the lower panels. The GECAM-C fluxes (orange) with arbitrary normalization are shown in the background for the time reference. The model fittings were performed over T ref + (230, 300) s.
Paper: Relation between the keV–MeV and TeV Emission of GRB 221009A and Its Implications
Authors: Yan-Qiu Zhang, Haoxiang Lin, Shao-Lin Xiong, Zhuo Li, Ming-Yu Ge, Chen-Wei Wang, Shu-Xu Yi, Zhen Zhang, Shuang-Nan Zhang, Li-Ming Song, Chao Zheng, Wang-Chen Xue, Jia-Cong Liu, Wen-Jun Tan, Yue Wang, Wen-Long Zhang
Figure caption: Light curves of GRB 221009A in the keV–MeV band measured with GECAM-C (orange; Z.-H. An et al. 2023) and TeV band measured by the WCDA of LHAASO (blue; Z. Cao et al. 2023). The orange color represents the keV–MeV flux light curve of the bolometric emission in the energy range of 1–10,000 keV/(1+z). The cyan dashed line is the cumulative curve of the keV–MeV emission (orange). The cumulative curve is scaled down by 10−4 for comparison with the TeV light curve.
Paper: Ancient Nova Shells of RX Pup Indicate Evolution of Mass Transfer Rate
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Michael M. Shara, Jacqueline K. Faherty, Simone Scaringi
Figure caption: Top two panels: Hα and [O III] images of extended emission regions around RX Pup. Slit trails are marked with blue lines and named A–D with positional angles of 179°, 50°, 86°, and 93.°5. All slits were centered at the position of RX Pup. The identified extended emission regions along slit positions are marked with red rectangles. Bottom four panels: observed fluxes along slit positions (A–D) as a function of distance from RX Pup that were smoothed with a five-pixel-wide tophat filter. The direction on the sky from RX Pup is marked with black letters. The observed fluxes were at Hα (black line) and [O III] 5007 (red line) wavelengths. For each slit position the identified extended emission regions are marked with a gray area. The extended emission regions are then numbered. The final assigned slit position name and the extended region number are marked with blue symbols.
Paper: Ancient Nova Shells of RX Pup Indicate Evolution of Mass Transfer Rate
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Michael M. Shara, Jacqueline K. Faherty, Simone Scaringi
Figure caption: False-color image of RX Pup with [O III] represented in blue, R in green, and Hα in red color. North is up, east is left. RX Pup is in the center of the image, indicated with turquoise ticks. The entirety of the image west of RX Pup is dominated by Hα emission of an unrelated nearby H II region. The ∼1300 yr old nova shell is seen as a bright [O III] and Hα emission 43″ east of RX Pup. A possible ∼7000 yr old shell is seen as a Hα bright shell centered on RX Pup and with a radius of 240″.
Paper: Ancient Nova Shells of RX Pup Indicate Evolution of Mass Transfer Rate
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Michael M. Shara, Jacqueline K. Faherty, Simone Scaringi
Figure caption: Diagnostic diagrams based on emission line ratios designed to distinguish between H II regions, PNe, and SNRs (Sabin et al. 2013). The measured line ratios for the nova shell around RX Pup are marked with colored markers. Region A1 has emission line ratios consistent with a SNR, suggesting a shock between the nova ejecta and the interstellar medium. The other regions' emission line ratios are consistent with low-density PNe, as expected for an old nova remnant.
Paper: Ancient Nova Shells of RX Pup Indicate Evolution of Mass Transfer Rate
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Michael M. Shara, Jacqueline K. Faherty, Simone Scaringi
Figure caption: SuperCOSMOS (left) and Swope (right) images of the irregular arc east of RX Pup revealing expansion of the nova shell. The red contour shows position of the nova shell in the SuperCOSMOS image (1998), and the blue contour shows its position on the Swope image (2016). The SuperCOSMOS image has been smoothed with a four-pixel-wide Gaussian filter.
Paper: Ancient Nova Shells of RX Pup Indicate Evolution of Mass Transfer Rate
Authors: Krystian Iłkiewicz, Joanna Mikołajewska, Michael M. Shara, Jacqueline K. Faherty, Simone Scaringi
Figure caption: Spectra of different nova shell regions in the Hα and [O III] regions with names of regions given with a red text (see Figure 2). The flux was normalized to the Hα maximum flux.
Paper: Neutron Star Kicks plus Rockets as a Mechanism for Forming Wide Low-eccentricity Neutron Star Binaries
Authors: Ryosuke Hirai, 遼介 平井, Philipp Podsiadlowski, Alexander Heger, Hiroki Nagakura, 洋樹 長倉
Figure caption: Fractions of systems that become wide (P orb ≥ 100 days) and low-eccentricity (e ≤ 0.3) binaries. Different colors assume different average rocket velocities σ roc. The dashed curve shows the total survival fraction, and the dotted curve shows the fraction of wide binaries regardless of the eccentricity.
Paper: Neutron Star Kicks plus Rockets as a Mechanism for Forming Wide Low-eccentricity Neutron Star Binaries
Authors: Ryosuke Hirai, 遼介 平井, Philipp Podsiadlowski, Alexander Heger, Hiroki Nagakura, 洋樹 長倉
Figure caption: Schematic diagram of our formation channel for wide low-eccentricity systems like Gaia NS1. Each box (1–4) shows a specific phase of evolution and is placed in the period–eccentricity plane based on how it qualitatively evolves.
Paper: Analysis of the Stellar Occultations during the Unprecedented Long-duration Flare
Authors: K. Bicz, R. Falewicz, P. Heinzel, M. Pietras, P. Preś
Figure caption: (a) Part of the light curve of CD-36 3202 corrected to the variability caused by the stellar spots. The red curve and red interval mark the modulated flare model with the occultations models and the fit error, respectively. The green curve shows the recreated course of the stellar flare without the effects of foreshortening or stellar rotation from Paper I. The solid line arrows mark the occultations that were modeled in this Letter. The dashed line arrows mark the parts of the light curve that are possible next dimmings. (b) Fragments of the light curve from (a) phased with the rotational period of the star for each of the occultations. First, second, and third occultations are marked with blue, green, and red dots, respectively. The black lines present the numerical models for each dimming.
Paper: Analysis of the Stellar Occultations during the Unprecedented Long-duration Flare
Authors: K. Bicz, R. Falewicz, P. Heinzel, M. Pietras, P. Preś
Figure caption: Each of the three panels presents the value of the temperature of the flare region and the relationship between the temperature of the arcade, the thickness of the arcade loops, and the electron density for the first (left panel), second (middle panel), and third eclipse (right panel). The values of electron density are color-coded. Black isolines on each panel represent lines of constant electron density. The surface marked by black oblique lines represents the area where the range of loop thicknesses is the same for each eclipse. The shaded area within these surfaces represents the common range of arcade temperature and thickness.