adsabs/AstroCLIMB huggingface dataset:
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: Ongoing accretion process of SN ejecta onto the νNS and the NS companion, simulated in Becerra et al. (2019). The νNS is located at the center of the dark-blue spot accumulating material around it. And at the center of the green spot, the NS companion is also accreting SN ejecta. Also, we notice that a portion of the SN ejecta is flowing back toward νNS due to the distortion of SN ejecta caused by the companion NS.
Paper: GRB-SN Association within the Binary-driven Hypernova Model
Authors: Y. Aimuratov, L. M. Becerra, C. L. Bianco, C. Cherubini, M. Della Valle, S. Filippi, Liang Li, 亮 李, R. Moradi, F. Rastegarnia, J. A. Rueda, R. Ruffini, N. Sahakyan, Y. Wang, 瑜 王, S. R. Zhang, 书瑞 张
Figure caption: Luminosity light curve of GRB 180720B and spectra related to the different episodes identified in GRB 180720B. The energetics of the episodes are given in Section 6 and Table 3. See also Rastegarnia et al. (2022) for the analysis of the UPE phase.
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: Composite UV spectrum of Pox 186 from multiple HST COS observations. Each panel plots a portion of the composite spectrum corrected for the systemic velocity of Pox 186 and is color-coded by the PID and filter of the observation. The G130M and G160M spectra are binned in 6 pixels, and the G185M spectrum is binned in 3 pixels. Galactic absorption features are denoted by gray shaded areas and geocoronal Lyα is grayed out. Significant emission/absorption features are shown with dotted lines, fine-structure absorption lines with dashed lines.
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption: Left and center columns: time series in each coordinate for each stellar maser. The lower panel for each shows the coordinate offset from Sgr A* and the weighted LS linear proper motion fit. The upper panel shows the best-fit residual vs. epoch. The shaded region indicates ±4 au. R.A. offsets are true angular offsets (i.e., they are corrected for ﹩\cos (\mathrm{decl}.)﹩). Right column: sky tracks for the masers. The arrows indicate the direction of the 2D proper motion.
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption: Example residual proper motion time series showing the three fitting methods (LS = least-squares; CF = conservative formulation; GB = good-and-bad data). The residual is with respect to the weighted LS fit, and the shaded regions indicate ±4 au. Top: IRS 19NW, showing proper motion solutions for the conservative formulation and good-and-bad methods that differ from the canonical LS fit. Bottom: SiO-6 shows differing proper motion solutions in R.A. for all three methods. For most of the masers, the two less conventional fitting methods do not improve upon or differ significantly from the LS method. R.A. offsets are true angular offsets (i.e., they are corrected for ﹩\cos (\mathrm{decl}.)﹩).
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption: Example differential coordinate offsets of the stellar SiO masers used for the Galactic center astrometric reference frame. This is epoch 1998.410. The vector field includes rotation and a radial component. The amplitude scales linearly with angular distance from Sgr A*. The gray circle marks Sgr A* (not to scale). Projected distances assume a Galactic center distance of 8.2 kpc, and the R.A. offset is corrected for decl.
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption: Three-dimensional velocity of stellar masers vs. projected distance from Sgr A*. Point color indicates the sign of the radial velocities (red is redshifted; blue is blueshifted). The size of the points scales linearly with the transverse velocity, spanning 59–241 km s−1. Velocity error bars are uniformly smaller than the data points. The blue line indicates the upper bound on 3D velocity based on the enclosed stellar and black hole masses (see Section 6 and Equation (3)). Projected distances assume a Galactic center distance of 8.2 kpc.
Paper: An Updated Reference Frame for the Galactic Inner Parsec
Authors: Jeremy Darling, Jennie Paine, Mark J. Reid, Karl M. Menten, Shoko Sakai, Andrea Ghez
Figure caption: Example residual proper motion time series showing the result of EUs that are added in quadrature to the measurement uncertainties (see Appendix C). The residual is with respect to the weighted LS fit, and the shaded regions indicate ±4 au. Top: IRS 19NW shows proper motion solutions that differ from the canonical LS fits but are formally consistent given the uncertainties. The additional uncertainties are 2.0 mas in R.A. and 2.8 mas in decl. Bottom: SiO-6 shows a differing proper motion solution in R.A. but not in decl., which have EUs of 4.0 and 4.3 mas, respectively. R.A. offsets are true angular offsets (i.e., they are corrected for ﹩\cos (\mathrm{decl}.)﹩).
Paper: HST UV Spectroscopy of the Dwarf Starburst Galaxy Pox 186
Authors: Noah S. J. Rogers, Claudia M. Scarlata, Evan D. Skillman, Nathan R. Eggen, Anne E. Jaskot, Vihang Mehta, John M. Cannon
Figure caption: Left: NUV acquisition image of Pox 186. Right: normalized light profile in the cross dispersion direction. Pox 186 is not described by a point source (green) but is slightly extended and well described by a Cauchy distribution (gray).
Paper: Enhanced Size Uniformity for Near-resonant Planets
Authors: Armaan V. Goyal, Fei Dai, Songhu Wang
Figure caption: Additional statistical evidence supporting the notion that enhancement in size uniformity for near-resonant systems is driven primarily by inherent physical differences between the near-resonant and nonresonant populations. Left: we observe from variation in the near-resonant cutoff parameter ﹩{\zeta }_{\mathrm{lim}}﹩ the behavior expected from a physical link between intra-system size uniformity and proximity to resonance, including low significance values for incomplete near-resonance populations (﹩{\zeta }_{\mathrm{lim}}\lt 0.2﹩), followed by an increase and subsequent plateau as more resonant systems are added to this population (﹩0.2\leqslant {\zeta }_{\mathrm{lim}}\lt 0.55﹩), and terminated by a drop in significance as the added near-resonant systems are sufficiently deviant from MMR to no longer exhibit enhanced size uniformity (﹩{\zeta }_{\mathrm{lim}}\geqslant 0.55﹩). Middle: the significance of enhanced size uniformity drops steadily as the near-resonant population is offset progressively from MMR (Δζ exc increases, dashed line), while being maintained at or beyond the 2.4σ level as the boundary between the near-resonant and nonresonant populations is given increasing nonzero width Δζ amb (dotted line). Both of these trends are suggestive of a physical link between the prevalence of enhanced size uniformity and proximity to MMR. Right: significance distributions for 1000 iterations of the null hypothesis test where considerations of resonance are entirely ignored, and the near-resonant population is instead N sys systems drawn randomly (without replacement) from the overall CKS population. We observe that values for all N sys are consistent with null significance and exhibit no apparent trend with sample size, thus suggesting our primary ∼2.4σ result cannot be obtained by random population assignment and that our null hypothesis procedure is itself largely devoid of underlying sample size biases.
Paper: Enhanced Size Uniformity for Near-resonant Planets
Authors: Armaan V. Goyal, Fei Dai, Songhu Wang
Figure caption: Classification of the 446 neighboring planetary pairs within 299 CKS systems into near-resonant and nonresonant populations. Left: aggregate distribution of the resonance parameter ζ 2,1 for the 446 pairs considered in this work partitioned into the 54 near-resonant pairs (hatched black region) selected by ∣ζ 2,1∣ ≤ 0.25 and the remaining 392 nonresonant pairs (pink region). The morphology of our distribution bears a great degree of qualitative similarity to that provided in Fabrycky et al. (2014), and we observe the same spike at −0.2 ≲ ζ 2,1 ≲ − 0.1 that describes an abundance of pairs lying just wide of first-order MMR. Right: direct mapping of our near-resonant and nonresonant classifications onto the period ratio distribution of the 446 CKS pairs. We observe here the effectiveness of our ∣ζ 2,1∣ ≤ 0.25 filter in selecting configurations in close physical proximity to first-order MMR, as well as the natural shrinking of the near-resonant neighborhoods as the relevant MMR period ratios approach unity and become increasingly crowded by nearby higher-order resonances (note that the bin width itself is greater than the entire resonant neighborhood for the 4:3, 5:4, and 6:5 first-order modes). This distribution also provides further confirmation that the 2:1 and 3:2 first-order modes are the dominant resonances for Kepler systems (Fabrycky et al. 2014). We may also see here more directly the aforementioned asymmetries around each of the MMR integer ratios, for which there is a greater number of pairs that lie just wide of first-order resonances than just narrow of them.
Paper: Enhanced Size Uniformity for Near-resonant Planets
Authors: Armaan V. Goyal, Fei Dai, Songhu Wang
Figure caption: The enhanced intra-system size uniformity exhibited by near-resonant systems is driven primarily by the size similarity of near-resonant pairs and chains. Left: near-resonant pairs exhibit enhanced size uniformity when compared to nonresonant pairs in the same system. Across 27 systems with both near-resonant and nonresonant pairs, the total size Gini of nonresonant pairs (black line) falls ∼2.2σ below the distribution of total Gini values for equally sized samples of nonresonant pairs drawn randomly each system (pink histogram). Note that the relative coarseness of the histogram is a result of the probability space of random shufflings being fully encapsulated in 2304 possible combinations, far less than the ≳105 combinations available for our other statistical tests. Center: the nonresonant components of near-resonant systems are statistically indistinguishable from systems that are completely nonresonant. The total Gini index for 23 systems rendered nonresonant via removal of their innermost or outermost planets (black line) lies within ∼1.2σ of the control distribution generated from 105 random draws of 23 nonresonant systems (pink histogram). Right: near-resonant pairs or chains within near-resonant systems exhibit even greater enhancement in their size uniformity than the same systems taken as a whole. The total Gini index of the 48 near-resonant systems in our sample, once removed of all nonresonant pairs (black line), lies ∼3.5σ below the distribution generated from 105 random draws of 48 nonresonant systems (pink historgram).
Paper: Enhanced Size Uniformity for Near-resonant Planets
Authors: Armaan V. Goyal, Fei Dai, Songhu Wang
Figure caption: The 48 near-resonant systems in our sample exhibit enhanced intra-system size uniformity at the level of ∼2.4σ confidence when compared to a distribution of equally sized, randomly drawn mock samples from the nonresonant population. The pink histogram illustrates the control distribution of total size Gini ﹩\sum {{ \mathcal G }}_{R}﹩ values for 105 randomly drawn (without replacement) samples of 48 systems from the 251 in the nonresonant population. The black line denotes the value of ﹩\sum {{ \mathcal G }}_{R}﹩ calculated for the 48 near-resonant systems, which falls well below the bulk of the nonresonant control distribution and thus denotes a stronger overall expression of intra-system size uniformity within the near-resonant population.
Paper: Enhanced Size Uniformity for Near-resonant Planets
Authors: Armaan V. Goyal, Fei Dai, Songhu Wang
Figure caption: Near-resonant systems exhibit a greater preference for high-uniformity architectures and disfavoring of high degrees of diversity in planetary sizes as compared to nonresonant systems. Top: unit-normalized histograms corresponding to ﹩{{ \mathcal G }}_{R}﹩ distributions for the near-resonant (black) and nonresonant (pink) populations. We observe both a relative overrepresentation of near-resonant systems in the high-uniformity (﹩{{ \mathcal G }}_{R}\leqslant 0.2﹩) regime as well as the lack of a high-diversity (﹩{{ \mathcal G }}_{R}\gt 0.3﹩) tail that is present in the nonresonant group. Bottom: corresponding ﹩{{ \mathcal G }}_{R}﹩ cumulative distributions functions (CDFs) for the two populations. The near-resonant systems are 38% and 81% contained by respective low-Gini regimes of ﹩{{ \mathcal G }}_{R}\leqslant 0.1﹩ and ﹩{{ \mathcal G }}_{R}\leqslant 0.2﹩, for which only 28% and 65% of nonresonant systems reside. The 75th and 90th percentile Gini values for the near-resonant population (﹩{{ \mathcal G }}_{R}=0.17﹩, and ﹩{{ \mathcal G }}_{R}=0.24﹩) also lie well below the respective values for the nonresonant population (﹩{{ \mathcal G }}_{R}=0.24﹩, and ﹩{{ \mathcal G }}_{R}=0.34﹩).
Paper: Enhanced Size Uniformity for Near-resonant Planets
Authors: Armaan V. Goyal, Fei Dai, Songhu Wang
Figure caption: The 54 near-resonant planetary pairs in our sample exhibit an increased propensity for uniform planetary sizes as compared to the 392 nonresonant pairs. 10% of the nonresonant pairs lie above the maximum Gini value of the near-resonant population (﹩{{ \mathcal G }}_{R}=0.38﹩). The majority (∼57%) of near-resonant pairs assume extremely high-uniformity configurations (﹩{{ \mathcal G }}_{R}\leqslant 0.1﹩), while only 43% of near-resonant pairs occupy the same regime. Gray lines represent smoothed 10th, 25th, 50th, 75th, and 90th percentile regression curves for the global ﹩{\zeta }_{\mathrm{2,1}}-{{ \mathcal G }}_{R}﹩ sample generated via a constrained B-splines (COBS) smoothing algorithm (Ng & Maechler 2007, 2022). We note a pronounced rise in both the 75th and 90th percentile curves with increasing ∣ζ 2,1∣, demonstrating a tendency for the most nonuniform pairs to exist farther from MMR, regardless of any binary classification scheme.