adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers
Authors: Carolyn A. Raithel, Elias R. Most
Figure caption: Peak frequency of the postmerger GW spectrum as a function of the neutron star radius at various masses. The color coding is the same as in Figure 1. Diamonds represent results from the new simulations performed in this work, while circles correspond to results from Most & Raithel (2021). We note that the results from the four microphysical EoS tables are included in all four panels but are only labeled in the bottom-right panel for clarity. Solid-filled symbols indicate a binary mass ratio of q = 0.85, while the hatched symbols are for q = 1. The dotted gray lines correspond to the best-fit, quasi-universal relations reported in Vretinaris et al. (2020), with mean and maximum residuals from that work shown in the dark and light gray bands, respectively. Finally, the blue and red lines correspond to our best-fit, two-parameter quasi-universal relations (Equation (1b)), with varying values of R 1.4/R 1.8, while the purple line corresponds to the best-fit, single-parameter relation for f 2(R 2.0). We find that models with R 1.4/R 1.8 < 1 (blue points) systematically violate the existing quasi-universal relations for stars of intermediate mass (top row) and instead follow a separate relation between f 2 and R  x .
Paper: Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers
Authors: Carolyn A. Raithel, Elias R. Most
Figure caption: Mass–radius relations for the EoSs simulated in this work. The solid lines correspond to our parametric models, while the dashed lines represent four commonly used finite-temperature EoS tables included in this work (in order of increasing radius, these are SLy4, BHBΛϕ, TMA for the red curves, and LS375 in blue). We color-code the curves according to R 1.4/R 1.8, where R  x  represents the radius of a star with mass M = xM ⊙. The parametric EoS sample (solid lines) is specifically constructed to sample a wide range of slopes in the mass–radius relations.
Paper: Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers
Authors: Carolyn A. Raithel, Elias R. Most
Figure caption: Mass–radius relation for the same set of EoSs shown in Figure 1 but now color-coded according to the instantaneous slope. The models have been divided into three panels for visual clarity. Masses above 2 M ⊙ have been grayed out because the mass–radius curves of all EoSs turn-over near the maximum mass, and so the changing slope in this mass range is not especially interesting. Focusing instead then on the mass range of 1–2 M ⊙, it is clear that the majority of these curves can be well defined by a single slope parameter; however, for a subset of cases (grouped in the rightmost panel), the slope is sensitive to the mass at which it is defined.
Paper: Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers
Authors: Carolyn A. Raithel, Elias R. Most
Figure caption: Binary Love relations for the symmetric ﹩{\bar{\lambda }}_{s}﹩ and antisymmetric, ﹩{\bar{\lambda }}_{a}﹩ tidal deformabilities of the coalescing binary with mass ratio q = 0.85 considered in this work. Different curves correspond to the various equation of state models used, with color indicating the slope of the mass–radius curve in terms of the ratio R 1.4/R 1.8, where R  x  denotes the radius of a neutron star with mass M = x M ⊙.
Paper: Characterizing the Breakdown of Quasi-universality in Postmerger Gravitational Waves from Binary Neutron Star Mergers
Authors: Carolyn A. Raithel, Elias R. Most
Figure caption: Pressure as a function of density for the three piecewise polytropic EoSs newly constructed in this work. The density, ρ, is plotted with respect to the nuclear saturation density, ρ sat = 2.7 × 1014 g/cm−3. The labels are arbitrarily assigned, for reference in Table 2.
Paper: A Look at Outbursts of Comet C/2014 UN271 (Bernardinelli–Bernstein) near 20 au
Authors: Michael S. P. Kelley, Rosita Kokotanekova, Carrie E. Holt, Silvia Protopapa, Dennis Bodewits, Matthew M. Knight, Tim Lister, Helen Usher, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tony Angel, Ben Wooding
Figure caption: Ad hoc model lightcurves (absolute magnitude, H(1, 1, 0) versus time) based on illustrative functional forms for the outbursts and quiescent activity of comet C/2014 UN271 (Bernardinelli–Bernstein). LOOK Project photometry of the comet is shown as gray circles (g has been scaled to r as in Figure 4). Outbursts follow an exponential decay in dust cross section, with the same decay timescale, τ, for all events within a panel. Quiescent activity models are scaled to match the PS1 photometry from 2019 August 28. Top: quiescent activity model based on model CO-ice sublimation rates, Z, parameterized as ﹩Z\propto {r}_{{\rm{h}}}^{-2.2}﹩. Bottom: quiescent activity model based on constant activity since 2019 and a linearly increasing enhancement starting at 2021.76 (2021 October 5). Together, the models indicate that the lightcurve is outburst dominated but transitions to quiescent activity dominated by 2021 December.
Paper: A Look at Outbursts of Comet C/2014 UN271 (Bernardinelli–Bernstein) near 20 au
Authors: Michael S. P. Kelley, Rosita Kokotanekova, Carrie E. Holt, Silvia Protopapa, Dennis Bodewits, Matthew M. Knight, Tim Lister, Helen Usher, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tony Angel, Ben Wooding
Figure caption: Surface brightness (S  ν ) profiles as a function of distance to the nucleus (ρ) for the images presented in Figure 4. The profile of the comet is initially steep but flattens with time. A nominal coma profile, ρ −1, is shown for reference. The mean seeing of these images is 1.″8. Also shown are the monthly mean profiles from 2021 October to 2022 February, offset by +1 mag for clarity (mean seeing 2.″3).
Paper: Detection of an Extremely Large Impact Flash on Jupiter by High-cadence Multiwavelength Observations
Authors: Ko Arimatsu, Kohji Tsumura, Fumihiko Usui, Jun-ichi Watanabe
Figure caption: Time-resolved SEDs and model-fitting results. Each panel shows the observed SEDs of the impact flash in each 0.5 s bin and the best-fit spectrum of single-temperature blackbody radiation. The points with error bars represent observed fluxes in the three PONCOTS bands after cloud-reflection correction. The best-fit spectrum of single-temperature blackbody radiation for each time bin is shown as a gray line. Open circles represent model spectra integrated over the spectral response of each photometric band. The best-fit χ 2 value from the fit (with one degree of freedom) is also shown in each panel.
Paper: The Streaming Instability Cannot Form Planetesimals from Millimeter-size Grains in Pressure Bumps
Authors: Daniel Carrera, Jacob B. Simon
Figure caption: Four snapshots of the low-res,A = 0.6 simulation starting at the time when the particle density is about to reach the Roche density. The top-left panel shows the gas density profile, and vertical dashed lines that mark the −2 ≤ x/H ≤ −0.5 zoom-in region of the snapshots; ρ 0 is the initial midplane gas density. The top-right panel shows the maximum particle density over time, with the times of the snapshots marked. The simulation only begins to develop nonaxisymmetric structure after it crosses the Roche density—a telltale sign of gravitational instability.
Paper: H I Narrow-line Self-absorptions toward the High-mass Star-forming Region G176.51+00.20
Authors: Yingjie Li, Ye Xu, Jin-Long Xu, Dejian Liu, Jingjing Li, Zehao Lin, Peng Jiang, Shuaibo Bian, Chaojie Hao, Xiuhui Chen
Figure caption: Integrated intensity map of WCER (left) and SCER (right). Left: the background map is the integrated intensity map of 12CO in the range of [−5, −1] km s−1. Peaks 1–3 label the peaks in the WCER (i.e., corresponding to the intensity peaks in the 12CO map), and the red circles and numbers present the positions and indices of the central seven beams of FAST. Right: the background is an integrated intensity map of C18O in the range of [−30, −10] km s−1, where the blue and red contours show the integrated intensity map of 12CO and 13CO in the same velocity range as the C18O map, respectively. Their levels are 0.3, 0.4, 0.5, 0.6, 0.7, and 0.8 times the corresponding peak intensity. The color bars in the left and right panels are in units of ﹩{({\rm{K}}\ \mathrm{km}\ {{\rm{s}}}^{-1})}^{1/2}﹩.
Paper: H I Narrow-line Self-absorptions toward the High-mass Star-forming Region G176.51+00.20
Authors: Yingjie Li, Ye Xu, Jin-Long Xu, Dejian Liu, Jingjing Li, Zehao Lin, Peng Jiang, Shuaibo Bian, Chaojie Hao, Xiuhui Chen
Figure caption: Left: comparison of ﹩{N}_{{{\rm{H}}}_{2}}^{12\mathrm{CO}}﹩ and ﹩{N}_{{{\rm{H}}}_{2}}^{13\mathrm{CO}}﹩ in the SCER, where 13CO is not detected in Beam 3. Right: comparison of the column density of HINSA, N HI, and of the total gas, N H. The red points represent the results corresponding to the SCER (except for Beam 3), where the column density of the molecular clouds is traced by 13CO. The blue points present the results corresponding to the WCER, where the column density of the molecular clouds is traced by 12CO. The green points indicate the result corresponding to Beam 3 in the SCER (which may be more suitably classified as a WCER component), where the column density of the molecular clouds is traced by 12CO.
Paper: H I Narrow-line Self-absorptions toward the High-mass Star-forming Region G176.51+00.20
Authors: Yingjie Li, Ye Xu, Jin-Long Xu, Dejian Liu, Jingjing Li, Zehao Lin, Peng Jiang, Shuaibo Bian, Chaojie Hao, Xiuhui Chen
Figure caption: HINSA features in Beams 1–7 and the molecular-line spectra of the corresponding regions. The red, green, blue, black, and yellow lines show the spectra of 12CO, 13CO, C18O, HCO+, and CS, respectively, and the purple lines represent the HINSA features. We fitted the profiles of both 12CO and 13CO with a Gaussian profile for each component, except for spectra that showed strong self-absorption or were contaminated by other components. For Beam 6, only the line emission of C18O was fitted because there was strong self-absorption in the spectra of 12CO and 13CO.
Paper: H I Narrow-line Self-absorptions toward the High-mass Star-forming Region G176.51+00.20
Authors: Yingjie Li, Ye Xu, Jin-Long Xu, Dejian Liu, Jingjing Li, Zehao Lin, Peng Jiang, Shuaibo Bian, Chaojie Hao, Xiuhui Chen
Figure caption:  n HI and X HI as a function of time. The H I density in the cloud core drops to its steady-state value of ∼2 cm−3 with a time of ∼4 × 105 yr.
Paper: H I Narrow-line Self-absorptions toward the High-mass Star-forming Region G176.51+00.20
Authors: Yingjie Li, Ye Xu, Jin-Long Xu, Dejian Liu, Jingjing Li, Zehao Lin, Peng Jiang, Shuaibo Bian, Chaojie Hao, Xiuhui Chen
Figure caption: HINSA features of Beams 1–7, where the green lines (marked as T r) show the observed spectrum, the red lines (marked as T HI) the recovered spectrum of H I, and the blue lines (marked as T ab) the fitted spectrum of the HINSA features.
Paper: Beginning a Journey Across the Universe: The Discovery of Extragalactic Neutrino Factories
Authors: Sara Buson, Andrea Tramacere, Leonard Pfeiffer, Lenz Oswald, Raniere de Menezes, Alessandra Azzollini, Marco Ajello
Figure caption: All-sky map in equatorial coordinates (J2000) of the IceCube neutrino local p-value logarithms denoted as L. Locations of PeVatron blazars associated with neutrino hotspots are pointed out by black squares. For visualization clarity, the label of 5BZCat objects is limited to reporting the unique numerical coordinate part. Unassociated hotspots are highlighted by green squares. The location of TXS 0506+056 is shown for reference (green circle). Squares are not to scale and serve the only purpose of highlighting the blazars’ locations. The Galactic plane and Galactic center are shown for reference as a green line and star, respectively.
Paper: Beginning a Journey Across the Universe: The Discovery of Extragalactic Neutrino Factories
Authors: Sara Buson, Andrea Tramacere, Leonard Pfeiffer, Lenz Oswald, Raniere de Menezes, Alessandra Azzollini, Marco Ajello
Figure caption: Pretrial p-value for the blazar/neutrino correlation as a function of the association radii r assoc, for neutrino data set with L min = [3.5, 4.0, 4.5]. The y-axis displays values on a logarithmic scale. The minimum chance probability of 3 × 10−7 is achieved with the set of parameters L min = 4.0 and r assoc = 0.°55. The estimated posttrial chance probability is 6 × 10−7.
Paper: Beginning a Journey Across the Universe: The Discovery of Extragalactic Neutrino Factories
Authors: Sara Buson, Andrea Tramacere, Leonard Pfeiffer, Lenz Oswald, Raniere de Menezes, Alessandra Azzollini, Marco Ajello
Figure caption: Same as Figure 1 but obtained by randomizing the neutrino spot positions in R.A. (see Appendix A.1). Pretrial p-value for the blazar/neutrino correlation as a function of the association radii r assoc for the neutrino data set with L min = [3.5,4.0,4.5]. The y-axis displays values on a logarithmic scale. The minimum chance probability of 1.7 × 10−6 is achieved with the set of parameters L min = 4.0 and r assoc = 0.55°. The estimated posttrial chance probability is 1.8 × 10−6.
Paper: A Look at Outbursts of Comet C/2014 UN271 (Bernardinelli–Bernstein) near 20 au
Authors: Michael S. P. Kelley, Rosita Kokotanekova, Carrie E. Holt, Silvia Protopapa, Dennis Bodewits, Matthew M. Knight, Tim Lister, Helen Usher, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tony Angel, Ben Wooding
Figure caption: Top: LCO images of comet C/2014 UN271 (Bernardinelli–Bernstein). Dates (2021) are as indicated. Except for the image on June 22, which is a single night w-band average, images are median-combined ﹩g^{\prime} ﹩ and ﹩r^{\prime} ﹩ data taken over a range of dates: 2021 July 11–18, August 2–9, and September 3–8. All images are displayed with the same photometric color scale and show an area of 880,000 km × 880,000 km (60″ on 2021 June 22). Bottom: The same images, but normalized by the previous image in the sequence and smoothed with a σ = 1 pixel Gaussian filter. The expanding morphology of the comet is apparent throughout this period.
Paper: A Look at Outbursts of Comet C/2014 UN271 (Bernardinelli–Bernstein) near 20 au
Authors: Michael S. P. Kelley, Rosita Kokotanekova, Carrie E. Holt, Silvia Protopapa, Dennis Bodewits, Matthew M. Knight, Tim Lister, Helen Usher, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tony Angel, Ben Wooding
Figure caption:  V − R color as a function of heliocentric distance, r h, comparing the color of the coma of comet C/2014 UN271 (Bernardinelli–Bernstein) as measured in this work (square symbol) and that of other active LPCs from Jewitt (2015) and Solontoi et al. (2012). The gray rectangle defines the 3σ limits around the average V − R color of active LPCs (0.47 ± 0.01 mag), and the horizontal dashed line is the color of the Sun. Color-wise, comet Bernardinelli–Bernstein is a typical active LPC. The color of the nucleus (Bernardinelli et al. 2021) is also shown for comparison (diamond).
Paper: A Look at Outbursts of Comet C/2014 UN271 (Bernardinelli–Bernstein) near 20 au
Authors: Michael S. P. Kelley, Rosita Kokotanekova, Carrie E. Holt, Silvia Protopapa, Dennis Bodewits, Matthew M. Knight, Tim Lister, Helen Usher, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tony Angel, Ben Wooding
Figure caption: Select LCO images of comet C/2014 UN271 (Bernardinelli–Bernstein). Dates are as indicated, all images are through an ﹩r^{\prime} ﹩ filter, except on 2021 June 22, which is through w. All images are displayed with the same color scale and are 1,320,000 km × 1,320,000 km in size (90″ on 2021 June 22). Celestial north is up, east to the left. Over this time period, the heliocentric distance decreased from 21.78 to 19.28 au, the projected comet–Sun vector increased from position angle 46° to 292°, and the projected velocity vector increased from 144° to 153°.
Paper: A Look at Outbursts of Comet C/2014 UN271 (Bernardinelli–Bernstein) near 20 au
Authors: Michael S. P. Kelley, Rosita Kokotanekova, Carrie E. Holt, Silvia Protopapa, Dennis Bodewits, Matthew M. Knight, Tim Lister, Helen Usher, Joseph Chatelain, Edward Gomez, Sarah Greenstreet, Tony Angel, Ben Wooding
Figure caption: Absolute magnitude, H  r  (1, 1, 0), of comet C/2014 UN271 (Bernardinelli–Bernstein) measured within 6″ radius apertures from LOOK Project photometry (g band as circles, r band as squares) versus time. Data calibrated to the g-band have been scaled with the measured coma colors to make an effective r-band data set. The brightness of the coma from PanSTARRS 1 (PS1) data measured on 2019.66 UTC, using the same aperture size, is marked with a dotted line, and the absolute magnitude of the nucleus is given as a dashed line (Bernardinelli et al. 2021).
Paper: On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath
Authors: Ore Gottlieb, Serena Moseley, Teresita Ramirez-Aguilar, Ariadna Murguia-Berthier, Matthew Liska, Alexander Tchekhovskoy
Figure caption: Panels (a)–(c): Profiles of the different models when the jet head is at 4.5 × 1010 cm. Panel (a): Angular profiles of the isotropic equivalent energy of the material outside the ejecta when the jet head reaches 4.5 × 1010 cm hint at a universal structure with a flat core followed by a power law. The ejecta is important only when the jet fails to break through it. Panel (b): The energy distribution per logarithmic asymptotic proper velocity of the material that broke out from the ejecta. A uniform distribution is shown in the cocoon between ﹩{u}_{\infty }\approx \,{v}_{\max }﹩ and u ∞ ∼ 3. The low level of mixing allows the jet to retain its energy such that the energy rises in ultrarelativistic velocities. Both angular and radial distributions are consistent with those of hydrodynamic jets (Gottlieb et al. 2021). Panel (c): The cumulative energy in gas with magnetization larger than σ out of the total energy of the gas outside the ejecta. When a relativistic jet is present, most of the plasma maintains σ > 0.1, which is expected to be even higher when a realistic σ 0 > 100 is used. Panels (d) and (e): The total jet power postbreakout (integrated over a shell of radius 2 ×1010 cm). It shows a highly variable ∼0.5 s long signal whose energetic varies from model to model (with a total energy spanning the range of 1048–1052 erg).
Paper: On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath
Authors: Ore Gottlieb, Serena Moseley, Teresita Ramirez-Aguilar, Ariadna Murguia-Berthier, Matthew Liska, Alexander Tchekhovskoy
Figure caption: Radial profiles of radial energy flux weighted averages, excluding the rest -mass energy flux and considering only matter with u ∞ > 1. Panel (a): Efficient conversion of magnetic energy into kinetic during the early jet launching in model α3d5, before the jet power becomes too weak to retain its initial energy (inner ∼2 × 1010 cm). Shown are two different times: when the jet head reaches 4.5 × 1010 cm 1.7 s after the merger (solid thick lines) and 0.9 s after the merger (dashed thin line). Panel (b): Similar magnetization profiles in models α3d5, α1d5, and α3d5Bs when the jet head is at r = 4.5 × 1010 cm, implying that the magnetization profile is almost independent of the specific properties of the system as long as the jet successfully breaks out from the ejecta. Panel (c): Magnetization profiles of models with different jet power or polar densities when the jet head is at r = 4.5 × 1010 cm demonstrate that low η 0 results in stronger dissipation. The highest average magnetization is obtained without initial ejecta (model V); stronger dissipation is observed when ejecta is falling toward the launching point (α3d1Mb), or when the jet power is low (α3d5Bw).
Paper: On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath
Authors: Ore Gottlieb, Serena Moseley, Teresita Ramirez-Aguilar, Ariadna Murguia-Berthier, Matthew Liska, Alexander Tchekhovskoy
Figure caption: 3D rendering of the outflows in different models. Panel (a): Logarithm of the asymptotic proper velocity u ∞ shows the jet (white blue) and cocoon (green) during the interaction with the dense winds (yellow) from the accretion disk (red) at ﹩r\lt \,{v}_{\min }{t}_{d}﹩, 0.05 s after the collapse to a BH in model α3d5. Owing to weak mixing between the jet and the winds, the jet retains its high asymptotic proper velocity u ∞. The qualitative behavior in all models (apart from α3d1Mb in which the jet fails to form) is similar at this stage. Panels (b) and (c): Logarithm of the magnetization at the time of jet breakout from the ejecta (b) and when the jet head is at 4.5 × 1010 cm (c) in model α3d5. The weak interaction between the jet and the dynamical ejecta does not disrupt the jet which remains intact and highly magnetized. Panel (d): Logarithm of the magnetization in the MB model α3d5Bw when the jet head is at 4.5 × 1010 cm. The strong mixing chokes the relativistic gas inside the ejecta, allowing just the weakly magnetized cocoon to break out. Panels (c) and (d) also portray the unmagnetized ejecta (which is added to this visualization for completeness) from which the outflows broke out (see movie at http://www.oregottlieb.com/NSM_GRMHD.html).
Paper: Detection of an Extremely Large Impact Flash on Jupiter by High-cadence Multiwavelength Observations
Authors: Ko Arimatsu, Kohji Tsumura, Fumihiko Usui, Jun-ichi Watanabe
Figure caption: Time-resolved SEDs and model-fitting results for the impact flash. (a) Examples of SEDs and best-fit models of the 0.5 s bins. The left, middle, and right panels show SEDs obtained during the rise, peak, and decay phases, respectively. Crosses and points with error bars represent observed fluxes and those after cloud-reflection correction, respectively. The best-fit spectrum of single-temperature blackbody radiation for each time bin is shown as the gray line. Open circles correspond to the model spectrum integrated over the spectral response of PONCOTS photometric bands. (b) Best-fit optical energy (upper panel) and temperature (lower panel) for each 0.5 s bin. The horizontal line in the lower panel represents the weighted-average value of the best-fit temperature (8300 K).
Paper: Detection of an Extremely Large Impact Flash on Jupiter by High-cadence Multiwavelength Observations
Authors: Ko Arimatsu, Kohji Tsumura, Fumihiko Usui, Jun-ichi Watanabe
Figure caption: Impact rates on Jupiter and Earth. Our estimated range of Mt-class impact rates is indicated by the red region, with the red horizontal line in this region representing the best-estimate value (1.3 impacts per year). The solid black rectangle indicates the rate based on five detections during 2010–2017 (Hueso et al. 2018). The dashed black rectangle indicates estimated impact rates on Jupiter based on the Shoemaker–Levy 9 impact of 1994 and impact features observed in 2009 (Sánchez-Lavega et al. 2010). The orange and blue solid lines indicate the expected Jovian impact rates from dynamical models of comets (Levison et al. 2000) and the cratering record of Galilean moons (Zahnle et al. 2003), respectively. The dashed green line indicates the estimated impact rate on Earth (Brown et al. 2002).
Paper: Detection of an Extremely Large Impact Flash on Jupiter by High-cadence Multiwavelength Observations
Authors: Ko Arimatsu, Kohji Tsumura, Fumihiko Usui, Jun-ichi Watanabe
Figure caption: Light curves of the 2021 October impact flash obtained with the PONCOTS observation system. Calibrated light curves for the V, Gh, and CH4 bands are presented in panels (a), (b), and (c), respectively. Fluxes for individual frames and combinations of 0.5 s bins are shown as gray dots and points with 1σ error bars, respectively. The background fluctuation noise is expected to dominate the error of photometry, so the 1σ errors were estimated by examining oscillations of the light curve with no flash in the image.(The data used to create this figure are available.)