adsabs/AstroCLIMB huggingface dataset:
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: Radial variations of the average stellar mass of parent galaxies. The cyan-edged and magenta-edged squares represent the galaxy masses estimated from the dispersions of GCLFs in the g and z bands, respectively (see Section 4.1 for details). The solid or dashed curves represent the weighted average for five TNG50 subhalos that match the basic properties of NGC 3115. The blue-shaded region represents the 68% confidence interval for the subhalo plotted as solid curve (see Section 4.2 for details).
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Left: F275W, F275W − F336W CMD of the internal field zoomed around the WD cooling sequence region. Stars marked as teal asterisk-shaped stars are the objects excluded from this study. Pink and purple triangles mark selected WDs divided into magnitude bins (see text for more details). The dashed horizontal lines indicate the lower bounds of the magnitude bins, and the solid black line is a BaSTI CO-core/H-envelope WD cooling model for a mass of 0.54 M⊙. Right: same zoomed-in CMD for the external field. Light and dark blue triangles mark selected WDs in the two magnitude bins.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Left: the black solid and dashed lines indicate the completeness curves for WDs observed in the F275W filter for the internal and the external field, respectively. The dashed–dotted horizontal line indicates a completeness level of 50%. Right: same, but for the completeness of the other evolutionary phases, such as MSTO, RGB, and HB.
Paper: Mass Stratification in the Globular Cluster System Revealing the Assembly History of the Nearest S0 Galaxy NGC 3115
Authors: Haoran Dou, 浩然 窦, Hao Li, 昊 李, Hong-Xin Zhang, 红欣 张, Heng Yu, 恒 余, Huiyuan Wang, 慧元 王
Figure caption: The assembly histories of the TNG50 subhalos that most closely (top panels) and least closely (bottom panels) match the radial profiles of the average parent galaxy mass of NGC 3115 shown in Figure 13. The first column presents the evolution of the stellar mass surface density profiles for stars formed in situ. The second, third, and fourth columns show the profiles for stars accreted through major mergers (secondary-to-primary stellar mass ratio μ > 1/4), minor mergers (1/10 < μ < 1/4), and mini mergers (μ < 1/10), respectively. See Section 4.2 for more details.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Stars from the HST HUGS catalog for NGC 2808 are plotted in the R.A. and decl. plane as black dots (“internal field”), while red dots indicate stars detected and measured from the HST program GO-15857 (“external field”). The corners of the internal field are cut since only the region covered by photometry in all WFC3-UVIS near-UV filters is represented.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Left: zoom-in around the HB region of NGC 2808 F275W vs. F275W − F336W CMD of the internal field. The HB is divided into four groups: the red horizontal branch (RHB, purple) and three extended blue tails, namely, EBT1 (cyan), EBT2 (magenta), and EBT3 (green). Right: same but for the external field. We refer the reader to V. Castellani et al. (2006) for the method of division of HB into four parts.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Left: F275W, F275W − F336W CMD for the internal field with 145,610 objects whose error is <​​​​​​1 mag in F275W and F336W. Right: same plot as the left for the external field with 10,897 objects.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: Density, asymptotic Lorentz factor, and pressure plots at various times throughout our RHD simulation. The right and left columns, showing density and pressure, respectively, illustrate the structure of both the relativistic jet and the mildly relativistic cocoon. In contrast, the asymptotic Lorentz factor in the middle column specifically highlights the relativistic jet. As the jet is injected and breaks out of the surrounding material, it develops and maintains a structured outflow, which is clearly visible in every panel. In panel (a), the solid blue lines delineate a half-opening angle of θj = 5°. The solid red lines in each Γ∞ profile mark off a half-opening angle of ﹩\theta =2\mathop{.}\limits^{^\circ }5﹩. In panel (k), we see that a prominent shock has developed at the front of the jet. This shock is a numerical artifact, as we show in Figures 2 and 3.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: Bolometric lightcurves obtained from mock observations conducted at viewing angles ranging from θv = 1° to θv = 10°. Note that jet injection lasts for 2 s, with the first 1 s carried out in L21 and the final 1 s carried out in this work. Each panel shows a lightcurve comprising all photons selected during the mock observation (red line) alongside another lightcurve with photons from the thin shock (e.g., Figure 1(k)) removed (blue dashed line). The lightcurves shown in red maintain high peak luminosities at steep observing angles. The blue lightcurves, which remove the effects of an unphysical shock, exhibit the expected behavior of the peak luminosity steadily decreasing with observing angle. All lightcurves were obtained by binning photon arrival times into 600 ms bins to be consistent with S. Poolakkil et al. (2021).
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: The energy required to form an external shock at radius R = 9.78 × 1012 cm (black line), corresponding to t  = 326 s, is equal to the energy in the jet for mildly relativistic (blue dashed line) and highly relativistic (red dashed–dotted line) material as a function of angle from the jet axis. When the energy in the jet falls below the shock energy, the shock dominates over the jet. The angle at which the shock begins to compare to and/or dominate the jet depends on the fluid velocity and ranges from 5° to 15°.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: Pseudocolor plots of (a) density and (b) temperature at the same time as the bottom row of Figure 1, scaled spatially to highlight the radial structure of the jet. In panel (a), we see the jet propagating through the interstellar medium, which is characterized by a density of ρISM = 10−14 g cm−3. Far away from the jet axis, there is a thin region just ahead of the jet that is much more dense than the surrounding medium, indicated by a red arrow in both panels. This corresponds to a region in panel (b) that has a much higher temperature than anything outside of the jet.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Plot is the same as the bottom-right CMD of Figure 4. The evolutionary track of mass 0.6 M⊙ (in gray) and 0.7 M⊙ (in red) has been plotted with Y = 0.400 and Y = 0.300, respectively. The gray and red triangles mark the point on the evolutionary track closest to the limit of the magnitude bin.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Histogram of star counts of internal field and external and from C. I. Johnson et al. (2023). Error bars have been plotted assuming a Poissonian distribution.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Cutouts for 20 of the WDs identified in NGC 2808 based on a color image created from WFC3 drizzled images in the F275W, F336W, and F438W filters. Star F275W magnitude and coordinates are labeled on the image. The yellow solid arrow points at the WD.
Paper: An Excess of Luminous White Dwarfs in the Peculiar Galactic Globular Cluster NGC 2808
Authors: Laksh Gupta, Samyaday Choudhury, Annalisa Calamida, Christian I. Johnson, Domenico Nardiello
Figure caption: Differential reddening corrections.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Top: each black point represents the intersection between the cumulative number density predicted by abundance matching (P. S. Behroozi et al. 2013a) for MWA progenitors and the stellar mass corresponding to that number density given by the SMF at that redshift interval. The starting point is a number density of 0.0011 Mpc−3 at z = 0, corresponding to M⋆ = 1010.7M⊙. The solid SMFs are from D. J. McLeod et al. (2021), while the dashed SMFs are from A. Grazian et al. (2015). Bottom left: median stellar mass vs. redshift for MWA progenitors, plotted in black points. The shaded gray region is the 1σ deviation (16th to 84th percentiles) of our sample, which comes from the 1σ range in number density from the abundance matching code. We compare our median stellar mass to the median stellar mass from TNG50 (D. Sotillo-Ramos et al. 2022; A. Pillepich et al. 2024), represented by the blue dashed line. The blue shaded region is the TNG50 sample’s 10th to 90th percentiles. Previous observation-based studies (S. G. Patel et al. 2013; P. G. van Dokkum et al. 2013; C. Papovich et al. 2015; V. Y. Y. Tan et al. 2024) are also plotted in gray with white points. Bottom right: comparison of this sample’s stellar mass evolution for MW progenitors vs. predictions from various simulations, such as TNG50, again in blue: Auriga (R. J. J. Grand et al. 2017), ERIS (J. Guedes et al. 2011), EMERGE (B. P. Moster et al. 2018), FIRE-2 (S. Garrison-Kimmel et al. 2018), and NIHAO-UHD (T. Buck et al. 2020).
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Top: integrated stellar masses (obtained with Dense Basis) vs. photometric redshifts of MWA progenitors in the CANUCS fields selected by abundance matching and SMFs. The solid black line is the rolling median of the stellar mass for each redshift range, and corresponds to the solid black line in Figure 1, while the shaded red region represents the 1σ scatter, the same as the shaded gray region in Figure 1. Some of the stellar masses are scattered below the 1σ region, due to lensing magnification corrections. The large colored points are galaxies that have S/N > 30, and their color represents the sSFR. The small gray points have too low S/N for resolved photometry and are excluded from our final sample. Bottom: catalog log SFR vs. redshift, with the same selection criteria as above. The shaded red region represents the 1σ scatter of the SFR. The color of each point indicates the sSFR. Note that at higher redshifts, galaxies with S/N > 30 skew toward the higher-mass and higher-SFR end of the full distribution of possible MWAs in that redshift range. Note that quiescent galaxies are not used for the main analysis.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: (a) The radiative efficiency η = Eiso/Ekin of MCRaT photon spectra, where Eiso is obtained from mock observations and Ek is the kinetic energy of the jet, integrated over the line of sight. Each point is obtained from a mock observation at the given observing angle. When integrating Ek over the entire line of sight (blue diamonds), the radiative efficiency decreases by an order of magnitude from θobs = 1° to 10°. If we only integrate over relativistic material (green circles), the radiative efficiency can still vary dramatically but increases at high viewing angles. (b) T90 computed by integrating over lightcurves in Figure 4, corresponding to the same observing angles in panel (a) of this figure. Note that the jet injection lasts for 2 s. While most mock observations satisfy the condition T90 ≤ 2 s for short-duration bursts, there are some instances where T90 > 2 s, indicating a possibility for BNS mergers to produce low-luminosity bursts that will not be strictly categorized as SGRBs.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: The Amati correlation. Red squares denote data points obtained from MCRaT simulations, while gray circles and green diamonds denote observational data obtained from S. Poolakkil et al. (2021). Epk and Eiso were obtained by fitting the Band function (Equation (8)) to each spectrum. Green diamonds denote SGRB observations with a T90 < 2 s cutoff, while gray circles denote LGRBs with a T90 ≥ 2 cutoff. Blue plus signs show MCRaT observations with photons from the leading shock removed. Open blue plus signs denote observations with β ≥ −2.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: Time-integrated spectra corresponding to the lightcurves in Figure 4. As with Figure 4, the red markers show spectra that include all photons, including those in the leading shock, while the blue markers show spectra with photons in the shock removed. The Band function is fit to the red points for each spectrum, obtained using the Markov Chain Monte Carlo algorithm implemented in D. Foreman-Mackey et al. (2013). Peak energy is on the order of 1 MeV for observations near the jet axis and decreases in tandem with the jet structure seen in Figure 1. The low-energy slope parameter α is distinctly nonthermal in most spectra.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Color images (top), resolved stellar mass maps (middle), and resolved SFR maps (bottom) of a randomly selected subsample of 120 MWA progenitors. The plots are inset into a total stellar mass vs. redshift plot, to demonstrate the evolutionary trend of the progenitors. Each image has the same physical scale in kiloparsecs, displayed in the bottom left corner. Certain galaxy images are offset by no more than ±0.25z or ±0.25 log M⊙, to lessen overlap. Note that at higher redshifts, the morphologies shown are not fully representative of the progenitor population.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: The distribution of UVJ colors for the MWA progenitors. Since the quiescent fraction of MWAs is small (∼0.03%), the UVJ boundaries are defined with a bimodal distribution of 9615 galaxies in CANUCS at 0 < z < 5, with a 25% quiescent fraction (see Appendix A). The color calibration is adapted from J. Antwi-Danso et al. (2023). The colors of the points represent the sSFR of the MWA progenitor sample.
Paper: The Photospheric Emission of a Short-duration Gamma-Ray Burst Emerging from a Realistic Binary Neutron Star Merger
Authors: Nathan Walker, Davide Lazzati, Tyler Parsotan, Rosalba Perna
Figure caption: Jet density at simulation time t = 12 s, overlaid with photon positions (blue dots). Photons propagate with the jet, within a region of ≲3 × 1010 cm in length, and within the first 5° of the jet axis. Between 5° and 10°, photons begin to diffuse radially across a much larger area. For θ > 10°, photons diffuse even more, which affects the statistics of producing lightcurves and spectra.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Top: median stellar mass growth (left), median SFR (center), and median sSFR (right) as a function of redshift. The red and blue show the change in stellar mass, SFR, or sSFR in the inner (R < 2 kpc) and outer (R > 2 kpc) regions of the galaxies, respectively. The empty points represent redshifts affected by the completeness of the sample. MW values are from J. Bland-Hawthorn & O. Gerhard (2016) for stellar mass and from T. C. Licquia & J. A. Newman (2015) for SFR. Bottom: median stellar mass and SFR densities (left and center) as a function of redshift. The right panel shows the difference in sSFR between inner/outer regions and the overall median sSFR. The error bars in all plots are the standard error. The MW mass density and SFR density values are from X. Cheng et al. (2024) and D. Elia et al. (2025), respectively.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: The observed stellar mass evolution over time of the full unresolved sample (solid black circles) and the stellar mass added by integrating the observed unresolved sample’s SFR of the previous epoch (blue open diamonds). The error bars are the upper and lower limits derived from the 1σ scatter of the SFR at each epoch. The mass added by both the observed SFR and the estimated accretion rate (from V. Rodriguez-Gomez et al. 2016, integrated over the time span of each epoch) improve the agreement when more mergers are included (the red line is the merger mass ratio ≥0.0001, the green line is the mass ratio ≥0.1, and the purple line is the mass ratio ≥0.25). The shaded purple region is the possible time frame at which the GSE merger occurred for the MW (V. Belokurov et al. 2018; A. Helmi et al. 2018).
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Top: from left to right, the median Smerger, ACAS, and Arms for each redshift bin. In each top panel, the solid lines with filled squares represent the median of the distribution as measured from the original resolution of the stellar mass maps, and the dashed lines with unfilled squares represent the median from the resolution-matched stellar mass maps. Bottom: the left panel is the merger fraction, as determined by the number of galaxies per redshift that have Smerger > 0. The center and right panels are the “disturbed” fractions, determined by galaxies with ACAS > 0.3 or Arms > 0.3, respectively. In all cases, resolution matching decreases the fraction of disturbed galaxies but increases the merger fraction at the highest-redshift bins. The integrated halo disruption rate from P. S. Behroozi et al. (2013b) is plotted in dark blue for major mergers (θ ≥ 0.25) and major and minor mergers (θ ≥ 0.1), for comparison.
Paper: Resolved Mass Assembly and Star Formation in Milky Way Progenitors since z = 5 from JWST/CANUCS: From Clumps and Mergers to Well-ordered Disks
Authors: Vivian Yun Yan Tan, Adam Muzzin, Ghassan T. E. Sarrouh, Jacqueline Antwi-Danso, Visal Sok, Naadiyah Jagga, Gregor Rihtaršič, Westley Brown, Roberto Abraham, Yoshihisa Asada, Guillaume Desprez, Kartheik Iyer, Nicholas S. Martis, Rosa M. Mérida, Lamiya A. Mowla, Gaël Noirot, Kiyoaki Christopher Omori, Marcin Sawicki, Roberta Tripodi, Chris J. Willott
Figure caption: Left: stacked and normalized stellar mass profiles for each redshift epoch. The profiles are truncated at the boundary where the noise dominates. The gray region indicates the maximum extent of the central regions affected by the PSF. Right: stacked and normalized sSFR profiles for each redshift epoch. Each sSFR profile is obtained by dividing each normalized SFR profile by the normalized mass profile of the same redshift (see Appendix B). The truncation in radial profile is the same as in the left panel.