adsabs/AstroCLIMB huggingface dataset:
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Pulse profiles of PSR B1237+25 observed at RCP (panels (a) and (b)), dynamic spectra of diffractive scintillation at RCP (panels (c) and (d)), and rate of change of the visibility phases as a function of pulsar longitude for both senses of polarization (panels (e) and (f), each averaged over six scans. The left and right panel columns are for our two observing epochs, 2017 December 22 and 2018 February 26, respectively. Pulse profiles in (a) and (b) are computed as the visibility magnitude obtained by the correlator at zero baseline for ART with the off-pulse levels subtracted. The vertical dashed lines indicate the nine on-pulse sub-windows, w0–w8, used as gates for the correlation and for our analysis. Dynamic spectra in (c) and (d) denote the averages for ART over the full on-pulse windows and are shown in normalized linear gray scale. The black and white regions represent the maxima and minima of the power density, respectively. Phase rates, in panels (e) and (f), are the derivatives of the ART-GBT VLBI visibility phases from strong pulses with respect to delay, ﹩\tfrac{d({\varphi }_{k}-{\varphi }_{4})}{d\tau }﹩ for the nine pulse windows with 0 ≤ k ≤ 8. Uncertainties are standard errors. They were derived from the 1σ uncertainty from the least-squares fit of the phase rates in the approximately ±125 ns central delay region for each of the six scans and then divided by ﹩\sqrt{6}﹩.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: For each galaxy in the training set of the Astrid suite, we have considered four properties: (1) stellar mass, M *; (2) gas mass; M  g , (3) maximum circular velocity, ﹩{V}_{\max }﹩; and (4) stellar metallicity, M *. The different panels show the 2D distributions of these properties with hexagons. The color of a hexagon indicates the number of galaxies in that region of parameter space (see the color bar). We then test our model, trained on Astrid galaxies, on IllustrisTNG galaxies. For each of those galaxies, we compute their ﹩{\chi }_{i}^{2}﹩ values and select the 10 galaxies with the highest values. The ﹩{\chi }_{i}^{2}﹩ of these galaxies ranges from 40 to 144. We then project these galaxies into the different 2D properties. The colors of the points are used to match the galaxies across panels, and their sizes indicate the χ 2 values: larger points represent higher values. As can be seen, these galaxies tend to reside in regions in parameter space with very low density in one or several dimensions. This indicates that these outliers tend to correspond to galaxies whose properties are on the tails (or outside) of the Astrid distribution.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: The dynamic spectra in longitude windows w0 (top) and w8 (bottom) observed at ART in LCP on 2017 December 22 (scan 1). The left panels show the dynamic spectra before correction. A shift of about 1 MHz toward lower frequencies from w0 to w8 can be seen. The right panels show the corresponding spectra after correction as described in Section 4. The spectrum in w0 is copied from the left side for better comparison. The spectrum in w8 shows that the frequency shift has largely disappeared. For the difference between the time-averaged spectra and a discussion, see Section 4.1.
Paper: Technical Constraints on Interstellar Interferometry and Spatially Resolving the Pulsar Magnetosphere
Authors: M. V. Popov, N. Bartel, A. S. Andrianov, M. S. Burgin, E. N. Fadeev, A. G. Rudnitskiy, T. V. Smirnova, V. A. Soglasnov, V. A. Zuga
Figure caption: Upper panel: average ART-GBT visibility magnitude as a function of interferometer delay for PSR B1237+25 obtained in sub-window w1 for one scan (10:00) on 2017 December 22. The solid line shows a Lorentzian, fit to the data. It has an HWHM of 65 ns. Lower panel: corresponding average differences of the visibility phases between the leading (w0) and trailing (w8) sub-windows relative to the phases for sub-window, w4. The phases were corrected for 2π ambiguities. Only RCP pulses with the highest S/N were used. The tilted lines denote least-squares fits to the aligned phases in the central region of the visibility magnitude curve. Uncertainties are smaller or approximately equal to the symbol sizes. Phases outside the central region have much larger errors.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: The same as Figure 8, but testing the model on Magneticum galaxies. The ﹩{\chi }_{i}^{2}﹩ of these galaxies ranges from 111 to 180.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: The same as Figure 4, but training on SIMBA and Astrid galaxies (left column), Astrid and IllustrisTNG galaxies (middle column), and IllustrisTNG and SIMBA galaxies (right column). As can be seen, training on galaxies from two suites does not make the model robust.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: The same as Figure 8, but testing the model on SIMBA galaxies. The ﹩{\chi }_{i}^{2}﹩ of these galaxies range from 252 to 531.
Paper: Cosmology with One Galaxy? The ASTRID Model and Robustness
Authors: Nicolas Echeverri-Rojas, Francisco Villaescusa-Navarro, Chaitanya Chawak, Yueying Ni, ChangHoon Hahn, Elena Hernández-Martínez, Romain Teyssier, Daniel Anglés-Alcázar, Klaus Dolag, Tiago Castro
Figure caption: The same as Figure 8, but testing the model on Astrid galaxies. The ﹩{\chi }_{i}^{2}﹩ of these galaxies ranges from 24 to 49.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The time evolution of planetesimal eccentricities e (left panels) and apsidal angles Δϖ (right panels, relative to the planet) at five different semimajor axes, extracted from the nominal N-ring simulation of Model A (Table B1) shown in Figure 4. The values of the probed semimajor axes are indicated on the right side of the figure, and the time t is also indicated in the upper x-axis relative to τ ≈ 332 Myr. The envelope of the eccentricity oscillations shown in black curves are obtained using Equation (C7) (see also Section 4.1.3). Note that at the secular resonance (﹩a={a}_{\mathrm{res}}\approx 75﹩ au), Δϖ(t) ≈ − π/2 at all times (panel b; note the different scale). It is also evident that the eccentricities at the resonance grow following a quadratic curve, which is perfectly reproduced by Equation (20) as shown by the dashed yellow curve in panel (b). This figure can be compared to Figure A1, which portrays the corresponding results of the same planet–disk model in the simplified, ‘Paper I’–like, N-ring simulations. See the text (Sections 4.1.2 and 4.1.3) for more details.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The apsidal precession rate of the planetary orbit in each N-ring simulation, scaled relative to the theoretical free precession rate (Equation (8,PI)), i.e., ﹩{\dot{\varpi }}_{p}/{A}_{d,p}﹩, as a function of planetary semimajor axis a  p . Results are shown for all planet–disk models listed in Table B1, each evolved within two sets of simulations: nominal (shown in blue circles) and simplified (i.e., Paper I–like, shown in red circles). Note that results for systems with the same a  p  but different combinations of m  p , M  d , and e  p (0) (Table B1) overlap with each other almost perfectly. The solid black line represents the analytical prediction based on Equation (21), which accounts for both axisymmetric and nonaxisymmetric perturbations of the disk on the planet (as in the nominal simulations) under two simplifying assumptions about the disk: that its eccentricity is proportional to 1/a, and its precession is dominated by the planet’s gravity within the entire disk (Appendix D). The dashed black line represents a one-to-one correlation between ﹩{\dot{\varpi }}_{p}﹩ and A  d,p , as is expected in the simplified simulations. See the text (Section 5.1) for more details.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The disk-to-planet mass ratio M  d /m  p  required, as a function of planetary semimajor axis a  p /a in, to place a secular resonance within the disk at ﹩{a}_{\mathrm{res}}﹩. Calculations are done for the fiducial disk model (i.e., p = 1, a in = 30 au, and a out = 150 au) by solving the resonance condition given by Equation (28) under two assumptions: once within the context of simplified simulations (i.e., A(a) = A  d,p ; red curves), and once within the context of nominal simulations (i.e., ﹩A(a)={\dot{\varpi }}_{p};﹩ blue curves). The results obtained for three different values of ﹩{a}_{\mathrm{res}}﹩ are shown by different line types, as indicated in the legend. One can see that for planets orbiting close to the disk, M  d /m  p  is larger in the setting of nominal simulations compared to the simplified ones. Note also that the scaling of M  d /m  p  with a  p /a in in the nominal case is well captured by the black curve representing Equation (19, PI), or (25), even in the limit of a  p  → a in. See the text (Section 5.3) for more details.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The location of the secular resonance ﹩{a}_{\mathrm{res}}﹩ in each N-ring simulation, plotted as a function of the planetary semimajor axis a  p . Simulations are done for 67 different planet–disk models (Table B1), each within two sets: nominal (blue circles) and simplified (i.e., Paper I–like; red circles). Note the overlapping values of ﹩{a}_{\mathrm{res}}﹩ for systems sharing the same a  p , but differing in m  p , M  d , and e  p (0) (Table B1). One can see that results of simplified simulations lie along the dashed black line: this represents the resonance location expected from Paper I, ﹩{a}_{\mathrm{res}}=70\,\mathrm{au}﹩. It is also evident that results of nominal simulations follow closely the solid black curve: this represents the theoretical expectation based on Equation (28) that accounts for the reduced planetary precession rate due to the disk’s nonaxisymmetric torque (Equation (21)). Clearly, the disk’s nonaxisymmetric torque on the planet shifts the location of ﹩{a}_{\mathrm{res}}﹩ outward when compared to Paper I. See the text (Section 5.3) for more details.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The exponential decay rates of planetary eccentricity per unit mass of the planet D/m  p  as a function of its semimajor axis a  p , measured from the nominal N-ring simulations of 67 different planet–disk models (Table B1; blue filled circles). Note that results for systems sharing the same a  p  but different m  p , M  d , and e  p (0) (Table B1) coincide with each other almost perfectly. The solid black line represents the theoretical expectation based on Equation (22), evaluated at the system parameters of interest. The dashed black line shows the scaling of D/m  p  with a  p  (Equation (24)). The gray dashed lines mark the planetary semimajor axes, for which, based on Paper I, the expected resonance widths are w = 3, 5, and 10 au (Equation (22, PI)). See the text (Section 5.2) for more details.
Paper: Formation of Gaps in Self-gravitating Debris Disks by Secular Resonance in a Single-planet System. II. Toward a Self-consistent Model
Authors: Antranik A. Sefilian, Roman R. Rafikov, Mark C. Wyatt
Figure caption: The secular evolution of the complex eccentricity, ﹩\zeta =e\,\exp (i{\rm{\Delta }}\varpi )﹩, of planetesimals orbiting at semimajor axes of a = 50 au (panel A) and a = 110 au (panel B) in the nominal N-ring simulation of Model A (Table B1). In each panel, the blue and red open circles represent the initial and final values of forced eccentricities about which the free eccentricity vector of planetesimals precesses; see also Equations (C4) and (C5). Note that the forced eccentricities lie nearly along the x-axis but not exactly; their phase angles are φ 0 ≈ 0.°18 and φ 0 ≈ 179.°16 in panels (A) and (B), respectively—see Equation (C6). The black crosses mark the initial planetesimal eccentricities. Note that the precession is counterclockwise for the planetesimal at a = 50 au, and clockwise for the one orbiting at a = 110 au. The time t is represented by the color bar, which runs from t = 0 to t = τ ≈ 332 Myr. The data is plotted at every ≈0.025 Myr. See the text (Section 4.1.3) for further details.
Paper: SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission
Authors: Rishabh Singh Teja, Avinash Singh, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Tatsuya Nakaoka, Koji S Kawabata, Masayuki Yamanaka, Ali Takey, Miho Kawabata
Figure caption: Variations in 13 M ⊙ ZAMS model using different parameters to achieve a shorter plateau length. Zoomed out, a plot in the bottom left shows the variation in explosion energy for different model light curves around the plateau transition. The second plot in the right inset shows the corresponding Fe 5169 velocities obtained using models. The thicker line represents the model where the expansion velocity could be matched with the observed velocities.
Paper: SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission
Authors: Rishabh Singh Teja, Avinash Singh, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Tatsuya Nakaoka, Koji S Kawabata, Masayuki Yamanaka, Ali Takey, Miho Kawabata
Figure caption: Variations in 19 M ⊙ ZAMS model using different parameters to achieve a shorter plateau length. Zoomed out, a plot in the bottom left shows the variation in explosion energy for different model light curves around the plateau transition. The second plot in the right inset shows the corresponding Fe 5169 velocities obtained using models. All the 19 M ⊙ models underestimate the velocity evolution.
Paper: SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission
Authors: Rishabh Singh Teja, Avinash Singh, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Tatsuya Nakaoka, Koji S Kawabata, Masayuki Yamanaka, Ali Takey, Miho Kawabata
Figure caption: The effect of adding CSM around the progenitor is prominently seen in the early stage and can explain the initial excess in the individual light curves in redder bands. The thicker dashed lines represent the light curves obtained using 120 frequency bins.
Paper: SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission
Authors: Rishabh Singh Teja, Avinash Singh, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Tatsuya Nakaoka, Koji S Kawabata, Masayuki Yamanaka, Ali Takey, Miho Kawabata
Figure caption: Optical bolometric luminosities obtained using MESA+STELLA are plotted along with the optical bolometric light curve of SN 2018gj. The initial rise is not fitting well in the optical regime.
Paper: SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission
Authors: Rishabh Singh Teja, Avinash Singh, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Tatsuya Nakaoka, Koji S Kawabata, Masayuki Yamanaka, Ali Takey, Miho Kawabata
Figure caption: Scaling relations (Goldberg et al. 2019) in the context of Type IIP SNe as applicable to SN 2018gj.
Paper: SN 2018gj: A Short Plateau Type II Supernova with Persistent Blueshifted Ha Emission
Authors: Rishabh Singh Teja, Avinash Singh, D. K. Sahu, G. C. Anupama, Brajesh Kumar, Tatsuya Nakaoka, Koji S Kawabata, Masayuki Yamanaka, Ali Takey, Miho Kawabata
Figure caption: EPM distance estimates for various filter sets and different dilution factors from Hamuy et al. (2001), Dessart & Hillier (2005), and Vogl et al. (2019).
Paper: Structure, Kinematics, and Observability of the Large Magellanic Cloud’s Dynamical Friction Wake in Cold versus Fuzzy Dark Matter
Authors: Hayden R. Foote, Gurtina Besla, Philip Mocz, Nicolás Garavito-Camargo, Lachlan Lancaster, Martin Sparre, Emily C. Cunningham, Mark Vogelsberger, Facundo A. Gómez, Chervin F. P. Laporte
Figure caption: DM overdensity of simulations from the Fiducial case after t = 0.7 Gyr of integration. Each panel shows the projected overdensity (Equation (19)) in a 120 kpc-thick slice of the box centered on the LMC potential (i.e., we select particles with z ∈ [−60, 60]) for different DM models. A white cross in each panel denotes the center of the LMC potential. In each panel, the wake manifests as a net overdensity trailing the LMC. The left panel shows the CDM wake without self-gravity, while the central panel shows the CDM wake with self-gravity. To compare the strength and extent of the wake across the panels, the contour in each panel encloses the region with an overdensity greater than the half-max of the CDM wake with self-gravity, which is 0.38. Comparing the two CDM simulations, the addition of self-gravity increases the size and strength (see also Figure 4) of the wake. Specifically, while the wake without self-gravity decays to δ ρ < 0.38 ∼ 130 kpc behind the LMC, the wake with self-gravity takes ∼200 kpc to do the same. This indicates self-gravity has a significant effect on the wake structure, keeping the wake coherent over larger distances. The right panel shows the FDM wake. The signature “granular” structure of the FDM is apparent both in the background and in the wake. Some granules within the wake reach much higher overdensities than either CDM wake achieves, though the FDM wake is still qualitatively similar to the CDM wake with self-gravity.
Paper: Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae
Authors: Noah E. Wolfe, Carla Fröhlich, Jonah M. Miller, Alejandro Torres-Forné, Pablo Cerdá-Durán
Figure caption: The f-mode frequency at each time against the hot PNS surface gravity M PNS/R PNS 2 at the same times from the suite of exploding models considered in this work (colored points). We overplot fits of the dominant frequency of GW emission as a function of M PNS/R PNS 2 from the erratum (Torres-Forné et al. 2021) to Torres-Forné et al. (2019a, solid black line fit, with a shaded region for the 2σ confidence interval), and a similar fit only considering the “CoCoNuT” general-relativistic models used in this same work (dashed yellow line fit, also with a shaded confidence interval). This fit takes the same form as the fit to all of the models (see Table 1 of Torres-Forné et al. 2019a), with a = 0 Hz, b = 5.88 × 105 Hz M ⊙ −1 km2, c = − 86.2 × 106 Hz M ⊙ −2 km4, and d = 4.67 × 109 Hz M ⊙ −3 km6. We also include a similar fit from Sotani et al. (2021) in the form of their Equation 5 (dotted black line), and the fit from Table 5 of Mori et al. (2023) labeled as “0.2–20” that extends to 20 s post-bounce (dashed–dotted black line). As we expect the f-mode after the avoided crossing at ∼0.4 s to correspond to the dominant mode of emission, points from times after the avoided crossing are comparable to the displayed fits from the literature. Points prior to the avoided crossing at ∼0.4 s post-bounce are partly transparent and included for completeness.
Paper: Structure, Kinematics, and Observability of the Large Magellanic Cloud’s Dynamical Friction Wake in Cold versus Fuzzy Dark Matter
Authors: Hayden R. Foote, Gurtina Besla, Philip Mocz, Nicolás Garavito-Camargo, Lachlan Lancaster, Martin Sparre, Emily C. Cunningham, Mark Vogelsberger, Facundo A. Gómez, Chervin F. P. Laporte
Figure caption: Time-averaged density profile plots for the simulations in Figure 2, showing how the overdensity varies across the wake in the x-direction for each DM model over the past 100 Myr. The procedure for making these plots is explained in Figure 3 and in the text. The upper panel shows the overdensity as a function of x, while the lower panel shows the residuals of the upper panel with respect to CDM with self-gravity. The CDM simulation without self-gravity is shown as the orange dashed line, the CDM simulation with self-gravity is the red solid line, and the FDM simulation is the blue dotted line. The peak overdensity of the CDM wake without self-gravity is ∼10% lower than in the CDM simulation with self-gravity included, demonstrating the addition of self-gravity increases the peak wake density. The density across the FDM wake oscillates about that of the CDM wake with self-gravity included, with an amplitude of δ ρ ∼ 0.05.
Paper: Gravitational Wave Eigenfrequencies from Neutrino-driven Core-collapse Supernovae
Authors: Noah E. Wolfe, Carla Fröhlich, Jonah M. Miller, Alejandro Torres-Forné, Pablo Cerdá-Durán
Figure caption: Top: histograms of the characteristic frequency f 1 for each EOS, identified at the characteristic time t 1 as noted in each panel. Each histogram is plotted with a bin width of 10 Hz and normalized to have an area of one. While t 1 ≲ 0.4 s post-bounce, prior to the avoided crossing between the f- and g 1-modes, these results reflect those of the left panel of Figure 6, showing a dependence of f 1 on the choice of nuclear EOS. Bottom: we plot remnant surface gravity of each model vs. characteristic frequency f 2 as identified at the time t 2 noted in each subplot. For t 2 ≳ 0.4 s post-bounce, these results reflect those of the right panel of Figure 6, showing a linear correlation between the surface gravity of the cold neutron star and f 2 independent of the EOS.