adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Shock-cooling model (Piro et al. 2021) fits to multiband data.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: The slope of the IMF in the intermediate- to high-mass end plotted as a function of the stellar surface density, σ *. The green triangles correspond to the sample of young Galactic clusters of Lim et al. (2015a). The black circle corresponds to the Arches cluster. The red point corresponds to the massive Galactic star-forming region W43. The full black line is a power-law fit to the Lim et al. (2015a) data alone whereas the green dashed line is a power-law fit to the entire data set (see the main text for details).
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: Ratio of the infall timescale to the coalescence timescale of cores for a CMF with fixed values of γ = 0.6 and M ch = 1.2 M ⊙, for various values of Γ, and for the fiducial values of the core parameters. The upper panel displays the case of a 104 M ⊙ protocluster clump and the lower panel corresponds to a protocluster clump whose mass is 105 M ⊙. In both cases, the CFE is equal to 0.2, leading to a total mass in the cores of 2 × 103 M ⊙ and 2 × 104 M ⊙, respectively. The parameters of the mass–radius scaling relation are β = 2.5 and A cl = 4000.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: The value of the slope of the postcoalescence IMF at the high-mass end (mass range [1–40] M ⊙) in the models as a function of the stellar surface density. The size of the symbols reflects the mass of the protocluster clump, starting from 5 × 103 M ⊙ for the smallest symbol size up to 4 × 104 M ⊙ increasing by steps of 5 × 103 M ⊙. The value of the coalescence efficiency parameter is fixed to η = 0.01 in all models and the core-to-star efficiency parameter is ϵ * = 0.4. The purple line is a fit to the observations (Equation (1)). The dashed–dotted line is the initial value of the slope for the ICMF in all models.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: The value of the slope of the postcoalescence IMF at the high-mass end (mass range [1–40] M ⊙) in the models as a function of the stellar surface density. The size of the symbols reflects the mass of the protocluster clump, starting from 5 × 103 M ⊙ for the smallest symbol size up to 4 × 104 M ⊙ increasing in steps of 5 × 103 M ⊙. The value of the coalescence efficiency parameter is fixed to η = 0.025 in all models and the core-to-star efficiency parameter is ϵ * = 0.4. The purple line is a fit to the observations (Equation (1)). The dashed–dotted line is the initial value of the slope for the ICMF in all models.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: Coalescence probability of cores in a CMF with fixed values of γ = 0.6 and M ch = 1.2 M ⊙, and for various values of Γ. The upper panel displays the case of a 104 M ⊙ protocluster clump and the lower subpanel corresponds to a protocluster clump whose mass is 105 M ⊙. In both cases, the CFE is equal to 0.2, leading to a total mass in the cores of 2 × 103 M ⊙ and 2 × 104 M ⊙, respectively. The parameters of the mass–radius scaling relation are β = 2.5 and A cl = 4000.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: Distributions of the high-mass slopes for the sample of young Galactic clusters measured by Lim et al. (2015a) and of clusters in M31 constructed using data from Weisz et al. (2015). In Lim et al. (2015a) and Weisz et al. (2015), the values of Γ have been measured using stars that are more massive than 1 M ⊙ and 2 M ⊙, respectively. The black arrow marks the position of the Salpeter value of Γ = 1.35 for the present-day stellar mass function of the Milky Way and the red arrow marks the value of Γ ≈ 0.9 found by Mor et al. (2019) for the time-averaged galaxy-integrated initial stellar mass function of the Milky Way.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: Final postcoalescence IMF for clumps with masses M cl = 104 and 2 × 104 M ⊙ and a CFE of 0.05, 0.1, and 0.2. The parameters of the mass–radius scaling relation of the clump are β = 2.5 and A cl = 4000. The coalescence parameter is η = 0.025. In all models, the ICMF is generated with the fiducial values of the parameters, namely Γ = 1.3, M ch = 1.2 M ⊙, and γ = 0.6.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: Time evolution of the protostellar CMF (left) and initial stellar mass function (right) in a 2 × 104 M ⊙ mass clump and with a CFE = 0.2. The parameters of the mass–radius scaling relation of the clump are β = 2.5 and A cl = 4000. The coalescence parameter is η = 0.025. The ICMF is generated with the fiducial values of the parameters, namely Γ = 1.3, M ch = 1.2 M ⊙, and γ = 0.6.
Paper: Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations
Authors: Sami Dib
Figure caption: Examples of the ICMF for fixed values of γ = 0.6 and M ch = 1.2 M ⊙ and for various values of Γ. The upper subpanel displays the case of a 104 M ⊙ protocluster clump and the lower subpanel a protocluster clump whose mass is 105 M ⊙. In both cases, the CFE is equal to 0.2 leading to a total mass in cores of 2 × 103 M ⊙ and 2 × 104 M ⊙, respectively.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: Left: Three-color mosaic of the northern part of the N 105 star-forming region combining the Hα image from the MCELS2 survey with the MOSAIC II camera on the Blanco 4 m Telescope at CTIO (red; a pixel size of 0.″27 × 0.″27, PI You-Hua Chu), the CS (5–4) image of the ALMA field N 105–1 from Sewiło et al. (2022, green; an angular resolution of ∼0.″5), and the ATCA 4.8 GHz/6 cm image (blue; ∼2″, Indebetouw et al. 2004). The white box indicates the area shown in the image in the right panel. Right: Three-color mosaic of N 105–1 A combining the H36β recombination line (red, this paper), the CS (5–4) (green; the same as in the left panel), and SO 3Σ 66–55 (blue) images from Sewiło et al. (2022). All the images have the same angular resolution of ∼0.″5 (∼0.12 pc). Green/blue contours correspond to the CS/SO emission with contour levels of (20, 50, 90)% of the CS/SO integrated intensity peak of 230.8/262.8 mJy beam−1 km s−1. White contours correspond to the 1.2 mm continuum emission with contour levels of (3, 10, 100) times the image rms noise level of 6.9 × 10−5 Jy beam−1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The 1.2 mm (left) and 3 mm (right) continuum images of N 105–1 A. In the left/right panel, white contours correspond to (3, 10, 30, 250)/(3, 20, 100) times 6.9 × 10−5/2.5 × 10−4 Jy beam−1, the 1.2/3 mm continuum image rms noise (σ). Red contours in the right panel are the same as white contours in the left panel. The size of the ALMA synthesized beam is indicated in the bottom left corner in each image: 0.″51 × 0.″47 for 1.2 mm and 2.″49 × 1.″83 for the 3 mm continuum image.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: A comparison between the predicted and observed peak intensity ratios of hydrogen mm-RLs (the peak intensity of a given mm-RL with respect to the peak intensity of the H36β transition) detected in Band 6 toward N 105–1 A (see Section 4.1 for details). The uncertainties of the observed peak intensity ratios shown in the plot were calculated by error propagation using the 1σ uncertainties of the mm-RL peak intensities provided in Table 1.
Paper: Deep Symbolic Regression for Physics Guided by Units Constraints: Toward the Automated Discovery of Physical Laws
Authors: Wassim Tenachi, Rodrigo Ibata, Foivos I. Diakogiannis
Figure caption: Example of the generalization capability of SR. Here we show randomly drawn data points (black dots) from the damped harmonic oscillator model given in Equation (12) (black line). The data are well fitted by an MLP (green line), which however fails in regions beyond the range of the training data (vertical-dotted lines). In contrast, our SR algorithm Φ-SO (red-dashed line) manages to provide much more reliable extrapolation.
Paper: Deep Symbolic Regression for Physics Guided by Units Constraints: Toward the Automated Discovery of Physical Laws
Authors: Wassim Tenachi, Rodrigo Ibata, Foivos I. Diakogiannis
Figure caption: SR results when applying the Φ-SO algorithm (allowing two free parameters) to the Hubble diagram of SNe Ia from the Pantheon sample. Φ-SO rediscovers the ΛCDM relation (in red) as well as another relation (in blue), which has a slightly better fit than ΛCDM when solely considering Pantheon's observational constraints due to the overabundance of low-z SNe.
Paper: A Comparison of Particle-in-cell and Hybrid Simulations of the Heliospheric Termination Shock
Authors: M. Swisdak, J. Giacalone, J. F. Drake, M. Opher, G. P. Zank, B. Zieger
Figure caption: Comparison of hybrid (black) and PIC (red) simulations in a portion of the domain centered near the shock front and averaged over the y-direction. The PIC results have been shifted in x to align the curves. Panels (a)–(d) show E  x , ∣ B ∣, the proton velocity along the shock normal direction, and the total (thermal + pickup) proton density, respectively.
Paper: A Comparison of Particle-in-cell and Hybrid Simulations of the Heliospheric Termination Shock
Authors: M. Swisdak, J. Giacalone, J. F. Drake, M. Opher, G. P. Zank, B. Zieger
Figure caption: Position–velocity (x  −  v  x ) phase-space density, on a logarithmic scale, in the PIC simulation for protons at ﹩t=40{{\rm{\Omega }}}_{p}^{-1}﹩ taken over a narrow range in y (≈1d  p ). Panel (a) The distribution of protons that were part of the thermal component at t = 0. Panel (b) The distribution of protons that were in the pickup component at t = 0. Velocities are in the simulation frame with the dashed horizontal line showing the shock velocity. The vertical dashed line shows the position of the density maximum seen in Figure 1.
Paper: A Comparison of Particle-in-cell and Hybrid Simulations of the Heliospheric Termination Shock
Authors: M. Swisdak, J. Giacalone, J. F. Drake, M. Opher, G. P. Zank, B. Zieger
Figure caption: Omnidirectional differential intensity (flux) vs. kinetic energy of protons in the shock rest frame for the hybrid (black) and PIC (red) simulations. The energy unit, ﹩{m}_{i}{U}_{1}^{2}/2﹩, corresponds to the ram speed of the incoming flow. Panel (a) Upstream distributions showing thermal solar wind protons (dashed lines) and freshly ionized pickup protons (solid lines). Panel (b) Downstream distributions at ﹩t=40{{\rm{\Omega }}}_{p}^{-1}﹩. Panel (c) Development in time of the distributions in the PIC simulation. The blue, green, and red curves are from t = 15, t = 30, and ﹩t=40{{\rm{\Omega }}}_{p}^{-1}﹩, respectively. The red curves are the same as in panel (b).
Paper: A Comparison of Particle-in-cell and Hybrid Simulations of the Heliospheric Termination Shock
Authors: M. Swisdak, J. Giacalone, J. F. Drake, M. Opher, G. P. Zank, B. Zieger
Figure caption: 2D images of the total proton density, normalized to the upstream value, at ﹩t=30{{\rm{\Omega }}}_{p}^{-1}﹩ (top) and ﹩t=40{{\rm{\Omega }}}_{p}^{-1}﹩, and overplotted with magnetic field lines (white). The x-axis has been shifted to match Figure 1.
Paper: A Comparison of Particle-in-cell and Hybrid Simulations of the Heliospheric Termination Shock
Authors: M. Swisdak, J. Giacalone, J. F. Drake, M. Opher, G. P. Zank, B. Zieger
Figure caption: The proton density, averaged over y, in the simulation frame. Each cut is separated from the previous by ﹩2{{\rm{\Omega }}}_{p}^{-1}﹩ and offset upwards. The x-axis has been shifted to match Figure 1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The CH3OH 50,5–40,4 A integrated intensity (upper panel) and velocity (lower panel) images of N 105–1. The CH3OH emission was integrated over the velocity range 233.9–244.2 km s−1. The 1.2 mm continuum contours are overlaid with contour levels the same as in Figure 1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The 12CO (3–2) integrated intensity (left) and velocity (right) images of N 105–1. The emission was integrated between 219 and 251 km s−1. Pixels with the signal-to-noise value less than 5 in the 12CO (3–2) integrated intensity image are masked in both images. The ALMA beam size is indicated in red in the lower left corner in each image. The 1.2 mm continuum contours are overlaid on both images with contour levels of (3, 30)σ.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The HCO+ (4–3) integrated intensity (top) and velocity (bottom) images of N 105–1. The emission was integrated between 232 and 244 km s−1. Pixels with the signal-to-noise value less than 3 in the HCO+ (4–3) integrated intensity image are masked in both images. The ALMA beam size is shown in the lower left corner in each image. The 1.2 mm continuum contours are overlaid on both images with contour levels of (3, 30)σ.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The SO 3Σ 66–55 integrated intensity (top panel), velocity (center panel), and line-width (bottom panel) images of N 105–1. The SO emission was integrated over the velocity range 233.2–244.6 km s−1. The 1.2 mm continuum contours are overlaid with contour levels the same as in Figure 1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The CS (5–4) integrated intensity (top panel), velocity (center panel), and line-width (bottom panel) images of N 105–1. The CS emission was integrated over the velocity range 232.7–244.7 km s−1. The 1.2 mm continuum contours are overlaid with contour levels the same as in Figure 1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The 12CO (3–2) channel maps. The 1.2 mm continuum contours are overlaid on all channel maps for reference; the contour levels are (3, 30)σ.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The HCO+ (4–3) channel maps. The 1.2 mm continuum contours are overlaid on all channel maps for reference; the contour levels are (3, 30)σ.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The CS (5–4) channel maps. The 1.2 mm continuum contours are overlaid on selected channel maps with contour levels of (5, 20)σ. The brightest CS emission is associated with the continuum source 1 B with the peak CS intensity of 0.12 Jy beam−1.
Paper: The Detection of Higher-order Millimeter Hydrogen Recombination Lines in the Large Magellanic Cloud
Authors: Marta Sewiło, Kazuki Tokuda, Stan E. Kurtz, Steven B. Charnley, Thomas Möller, Jennifer Wiseman, C.-H. Rosie Chen, Remy Indebetouw, Álvaro Sánchez-Monge, Kei E. I. Tanaka, Peter Schilke, Toshikazu Onishi, Naoto Harada
Figure caption: The SO 3Σ 66–55 channel maps. The 1.2 mm continuum contours are overlaid on selected channel maps with contour levels of (5, 20)σ.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Velocity-resolved time delays (top) across the broad Hβ emission-line profile (bottom).
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: The final calibrated and binned V-band light curve for NGC 3227. For comparison with the AGN variations and uncertainties, the bottom panel shows the scatter in residuals for a non-varying field star of similar brightness.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Light curves (left) for the continuum and the broad emission lines throughout the course of the monitoring program. Cross-correlation functions (right) are for each light curve relative to the V-band continuum, and in the case of the V band, we show the autocorrelation function.
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: Mean (top) and rms (bottom) spectra of NGC 3227 based on the observed-frame spectra obtained throughout the monitoring program. The strong broad emission lines are labeled for ease of identification. The spectra traced in black (gray) have the narrow lines subtracted (included).
Paper: Velocity-resolved Reverberation Mapping of NGC 3227
Authors: Misty C. Bentz, Madison Markham, Sara Rosborough, Christopher A. Onken, Rachel Street, Monica Valluri, Tommaso Treu
Figure caption: The inner ﹩10^{\prime} \times 10^{\prime} ﹩ region of the reference image, centered on the nucleus of NGC 3227 and oriented with north up and east to the left.
Paper: X-PSI Parameter Recovery for Temperature Map Configurations Inspired by PSR J0030+0451
Authors: Serena Vinciguerra, Tuomo Salmi, Anna L. Watts, Devarshi Choudhury, Yves Kini, Thomas E. Riley
Figure caption: Posterior distributions (smoothed by GetDist KDEs) from 18 runs, for radius, compactness, and mass. Results are obtained using data sets produced with two different noise realizations, labeled as one (left panel) and two (right panel). The two data sets were generated and analyzed with the ST-U model. Each of the two plots shows posteriors from nine inference runs, which use different MULTINEST settings, as reported in the legend (for definitions, see Section 2.4). On top of the 1D posteriors, we report the 68% credible intervals (representing the area within the 16% and 84% quantiles in the 1D marginal posterior mass) starting from the median of the distributions. These values, as well as the colored areas, refer to the two runs enabling the mode-separation modality (dashed black lines). The lines in the 2D plots represent the 68% credible areas of the 2D marginalized posterior, while the shadow refers to the whole distribution of the inferences enabling the mode-separation modality. The thin solid black lines represent the injected values. Overall, the various settings seem to recover consistent marginalized posteriors, while the different noise realizations adopted to build the two analyzed data sets have a significant impact on the shapes of these distributions. The outlier within the runs in the left panel has MULTINEST settings: SE 0.8, ET 0.1, LP 103, MM off (2). The outlier within the runs in the right panel has MULTINEST settings: SE 0.3, ET 0.1, LP 103, MM off (2).