adsabs/AstroCLIMB huggingface dataset:
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: Planetesimal free precession rate A = A  d  + A  p  due to both planet and disk gravity (red curve) as a function of semimajor axis. Calculations are done using the softened N-ring model (Section 3), assuming the parameters of the fiducial planet–disk model (Model A; Table B1) with N = 5000 and H = 0.1. The dotted and dashed black curves represent A  p (a) and A  d (a), respectively. The solid and dashed blue lines represent the rate of the free and total planetary precession due to the disk, A  d,p  and ﹩{\dot{\varpi }}_{p}﹩, respectively. Note that the former is calculated using A  jj  of Equation (7) with j = 0 (Section 3.2.1), whereas the latter is measured from the simulation of Model A presented in Section 4. This figure is to be interpreted as the softened analog of Figure 1 of Paper I: for reference, the curve representing the unsoftened version of A  d (a) is shown with the dashed gray line and labeled as ﹩{A}_{d}^{{\rm{H}}=0}(a)﹩. Note that A(a) = A  d,p  at 70 au and ﹩A(a)={\dot{\varpi }}_{p}﹩ at ≈75 au. See the text (Section 3.2.1) for further 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: A sketch of the initial setup of the model system considered in this and our previous work (Sefilian et al. 2021). A central star of mass M  c  is orbited by a planet of mass m  p  and an external debris disk of mass M  d  (M  d , m  p  ≪ M  c ). The entire star–planet–disk system is coplanar. The planetary orbit (dashed green line), characterized by its semimajor axis a  p , is slightly eccentric such that it does not cross the disk along its orbit (typically, e  p  ≤ 0.1). The disk, extending from a in to a out ≫ a in, is axisymmetric characterized by a truncated surface density profile given by Equation (1). The disk is modeled as a series of N ≫ 1 massive rings with fixed semimajor axes, each characterized by a small radial and vertical half-thickness ﹩{\mathfrak{h}}﹩, such that the aspect ratio H of the disk is constant (Equation (3)). See the text (Section 2) for further 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: Contour plot of the disk mass M  d  for damping the planetary eccentricity due to resonant friction with a half-life time of τ  D  = 200 Myr, plotted in the space of planetary semimajor axis a  p  and mass m  p . Calculations are done using the approximate equation for τ  D , i.e., Equation (27), assuming the parameters of the fiducial disk model (i.e., p = 1, δ = 5) around a solar-mass star of age t age = τ  D . For a given combination of a  p  and m  p , increasing (decreasing) M  d  leads to a shorter (longer) e  p -damping timescale than that stipulated (Equation (27)). Note that for a fixed value of M  d , the planet’s mass scales approximately linearly with its semimajor axis, namely, ﹩{m}_{p}\propto {a}_{p}^{17/16};﹩ see Equation (27). See the text (Sections 5.2 and 6.2) 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 timescale τ for planetesimal eccentricity excitation at the secular resonance as a function of planetary semimajor axis a  p , as measured from N-ring simulations. Results correspond to 67 different planet–disk models, each evolved within two sets of simulations (Table B1): simplified (shown as red circles and denoted by τ axi), and nominal (shown using various black symbols that are explained in the legend; denoted by τ n-axi). Note that the timescales are scaled by the planet’s mass m  p  and initial eccentricity e  p (0). One can see that results of simplified simulations lie along the dashed black line, which represents the expectation from Paper I (Equation (16, PI)). It is also evident that results of nominal simulations follow closely the solid curves of different colors (see the legend), which represent the theoretical expectations as a function of e  p (0) upon accounting for the damping of the planetary eccentricity due to resonant friction (Equation (29)). Clearly, the disk’s nonaxisymmetric torque on the planet causes the timescales to be longer than those expected in Paper I, i.e., τ n-axi ≳ τ axi, with some dependence on e  p (0). See the text (Section 5.4) 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: Test of the N-ring model of Section 3: a comparison of the planetesimal orbital evolution in the softened N-ring numerical simulation (blue curves) vs. the unsoftened analytical results of Paper I (Equations (11) and (12) therein; red curves). Each row displays the time evolution of the planetesimal eccentricity e (left panels) and apsidal angle Δϖ (right panels, measured relative to that of the precessing planet) at a given semimajor axis a, as indicated on the right side of the figure. The planetesimals were initiated on circular orbits (e(0) = 10−5) in the fiducial planet–disk model (Model A, Table B1). The N-ring simulation assumed N = 5 × 103 disk rings, each with a softening parameter of H = 0.1, while leaving the planet’s potential unsoftened. One can see very good agreement between the numerical results of the N-ring model and the theoretical results of Paper I at all semimajor axes. See the text (Appendix A.2) for more details.
Paper: A New Galaxy Cluster Merger Capable of Probing Dark Matter: A56
Authors: David Wittman, Rodrigo Stancioli, Kyle Finner, Faik Bouhrik, Reinout van Weeren, Andrea Botteon
Figure caption: Surface mass density contours from weak lensing (white) overlaid on a Pan-STARRS multiband image and red XMM-Newton surface brightness contours. The small closed contour between the subclusters is a trough. Green GMRT 650 MHz contours (Section 6) start at 70 μJy beam−1 with increments of 680 μJy beam−1 and a 4″ beam.
Paper: A New Galaxy Cluster Merger Capable of Probing Dark Matter: A56
Authors: David Wittman, Rodrigo Stancioli, Kyle Finner, Faik Bouhrik, Reinout van Weeren, Andrea Botteon
Figure caption: A56: 0.4–1.25 keV XMM-Newton contours over SDSS multiband (left) and HST/ACS F814W (right) images.
Paper: A New Galaxy Cluster Merger Capable of Probing Dark Matter: A56
Authors: David Wittman, Rodrigo Stancioli, Kyle Finner, Faik Bouhrik, Reinout van Weeren, Andrea Botteon
Figure caption: Corner plot showing distribution of subcluster members in R.A., decl., and velocity space relative to the overall mean. Members of the north (south) subcluster are shown in blue (red).
Paper: A New Galaxy Cluster Merger Capable of Probing Dark Matter: A56
Authors: David Wittman, Rodrigo Stancioli, Kyle Finner, Faik Bouhrik, Reinout van Weeren, Andrea Botteon
Figure caption: Redshift map. A56 galaxies are coded with a continuous color map, while galaxies in the putative background cluster at z = 0.37 (0.46) are shown as open (closed) green circles. XMM-Newton contours are shown in red.
Paper: A New Galaxy Cluster Merger Capable of Probing Dark Matter: A56
Authors: David Wittman, Rodrigo Stancioli, Kyle Finner, Faik Bouhrik, Reinout van Weeren, Andrea Botteon
Figure caption: Redshift histogram, with inset showing the redshift interval around A56.
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: Semianalytical model fitting for SN 2018gj using two-component model as described in Nagy & Vinkó (2016). The contributions from the shell and the core are also shown independently. In the inset, best-fitting parameters are listed for reference. The evolution of the light curve without γ − ray leakage is shown by the cyan dashed line.
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: Spectral time series for SN 2018gj containing 31 epochs spanning 295 days post-explosion. All spectra have been calibrated with photometry for absolute flux and corrected for host redshift. Some of the prominent spectral lines have been marked for clarity.(The data used to create this figure are available.)
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: Photometric data for SN 2018gj spanning ∼300 days post-discovery. Corresponding spectral epochs are marked along the abscissa. [Violet pentagon markers overplotted on V and B bands are from Swift UVV and UVB bands, respectively.]
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:  V-band light-curve evolution of SN 2018gj along with other Type II SNe. Continuous light blue lines are representative of a larger Type II sample from Anderson et al. (2014a), Faran et al. (2014a). Estimated light-curve parameters for V-band, viz., Optically thick phase duration (OPTd), Plateau duration (Pd), and light-curve slopes ( s1, s2, and s3), are also shown. SNe data used in this plot are mentioned in Table 7.
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: Mean color evolution of Type II SNe along with the color evolution of SN 2018gj for different bands is shown. The shaded region color with a solid line represents the mean colors from a larger Type IIP sample with 1σ scatter from the mean value. Sources of data have been referenced in Table 7.
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: Location of SN 2018gj in the host NGC 6217. The dashed violet line marks the separation between the host center and SN. The image is a red, green, and blue color composite utilizing Bessell’s V, R, and I filters.
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: Posterior plot for nickel mass and characteristic time estimates for SN 2018gj using Equation (2).
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: Pseudobolometric and bolometric light curves for SN 2018gj obtained using multiband photometry are shown. The second plot at the bottom shows the temperature and radius evolution obtained using blackbody fits from the SEDs.
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: Top: 1D representation of mass fractions for 13 M ⊙ ZAMS model with final mass 7.3 M ⊙. The elements are part of the nuclear reaction rates network used in the model’s evolution. The abscissa is shown until 4 M ⊙ as the trend followed beyond it is the same for the outer hydrogen envelope. Bottom: the effect of mixing with the implementation of Duffell RTI on the ejecta structure just before the breakout is shown for some of the prominent elements for the same model as in the top panel.
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: Temporal evolution of pseudo-equivalent width (pEW) for Fe II  5169 Å line obtained using optical spectra. Other markers represent the pEWs obtained from models given in Dessart et al. (2013). The solid blue line and the shaded region around it represent the mean pEW and the corresponding 1σ scatter about the mean for a larger sample of Type II SNe given in Gutiérrez et al. (2017).
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: Late phase (+295 days) spectrum of SN 2018gj compared with the model spectra around similar phase to estimate the initial mass of the progenitor. The model spectra are obtained from Jerkstrand (2017b).
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: Temporal velocity evolution of various lines identified in the spectra using the absorption minimum is shown here. The velocities have been compared with the sample from Gutiérrez et al. (2017) where the solid lines are the mean values from the sample, and the shaded area around it in similar color represents the 1σ scatter from the mean 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: SN 2018gj spectrum during maximum light. Spectra of other Type II SNe around the maximum is shown for comparison. The comparison sample is drawn from Table 7.
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: Spectrum of SN 2018gj during plateau phase is shown in comparison with other Type II SNe. The comparison sample is drawn from Table 7.
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: Focused view of spectral time series for Hα line in SN 2018gj. The black line marked is the rest wavelength for Hα. The spectra are corrected for host redshift, and it is evident that the peak of emission features never reaches the rest wavelength.
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: Velocity evolution of blueshifted Hα emission peak. Velocity evolution for emission features obtained using other ions has also been plotted.
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: Spectral comparison of SN 2018gj with other Type II SNe around similar epochs during the nebular phase.
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: Projected overdensity (similar to Figures 2 and 5) of stars in the Fiducial simulations after t = 0.7 Gyr of integration. As in Figures 2 and 5, a white contour in each panel traces the region with a density greater than the half-max of the CDM simulation with self-gravity (center). The CDM simulation without self-gravity (left) shows the stellar wake that is present due to only the passage of the LMC, i.e., we would expect this wake to form in the stellar halo regardless of the behavior (or existence) of the DM wake. When compared to the stellar wake with CDM self-gravity (center), we see that the entire wake is not enclosed by the contour in the absence of self-gravity (left), i.e., there is a region in the center of the wake without CDM self-gravity that drops below δ ρ * = 0.48. This demonstrates that adding the gravity of the DM wake enhances the density of the stellar wake, which we quantify in Figure 14. Additionally, the contoured region extends ∼50 kpc farther behind the LMC when the DM wake’s gravity is included. Comparing the CDM simulation with self-gravity to the FDM simulation (right), the stellar wake’s density looks similar in both of these DM models.
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: Divergence of the projected x–y velocity field for the Fiducial case. See Section 3.2 for how this is calculated. Regions of converging flows (blue, negative ∇ ·  v ) clearly identify the wake boundaries and velocity structure in each simulation. The self-gravity-off CDM simulation in the left panel shows only the effect of the LMC on the particle velocities: particles that pass close to the center of the LMC potential are deflected most strongly, producing a region of highly converging flow directly behind the LMC. After they are deflected, particles continue on relatively straight paths in the absence of wake self-gravity, producing a region of diverging flow at the center of the wake. Meanwhile, strongly deflected particles continue to move toward the box edges, passing near particles that have been deflected less strongly, creating a converging flow at the wake boundary. Turning on wake self-gravity (center panel) means that strongly deflected particles continue to feel a force toward the wake after they pass the LMC. This eliminates the diverging region behind the LMC that is seen in the no-self-gravity case, and keeps the wake boundaries narrower. The net result is the effect seen in Figures 2 and 7: a denser, more coherent wake. The FDM simulation on the right shows a similar overall structure to the self-gravity-on CDM case; however, the granularity of the FDM results in a less smooth signature in the velocity divergence. The wake boundaries are less smooth, and some regions of converging flow can be seen inside the wake. Together with Figure 7, it is clear that the FDM velocity field is not as coherently affected by the LMC as the CDM velocity field.
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: Same as Figure 2, but showing the z (into/out of the page) component of the velocity dispersion for the Fiducial case. The wake shows up as an enhancement of the velocity dispersion behind the LMC as DM particles converge. The dispersion is computed in a similar fashion to the overdensity: the simulated dispersion is divided by the mean dispersion, then subtract 1 (see Equation (20)). The effect of self-gravity in the CDM simulations is evident, as the region enclosed by the contour is larger (∼20 kpc wider and ∼40 kpc longer) with self-gravity. The FDM granularity is apparent in the velocity dispersion signature as well. Overall, the granularity results in a weaker dispersion signature in FDM compared to CDM: while the contour in the FDM simulation reaches the same length as in the CDM simulations with self-gravity, it is ∼40 kpc thinner and tapers more quickly than CDM without self-gravity. We discuss this effect further in Figure 8 and in the text.
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: The profile of the z-velocity dispersion computed across the wakes in the Fiducial simulations, shown in the same fashion as the overdensity (Figures 4 and 6). Results are averaged over five snapshots spanning t = 0.6−0.7 Gyr of evolution. The addition of self-gravity to the CDM simulations raises the peak of the dispersion by δ σ  z  ∼ 0.03. The FDM dispersion profile across the wake is consistently weaker than either CDM case, though the FDM peak is very close to the peak in CDM without self-gravity. Overall, the FDM wake is colder than the CDM wake.
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: Overdensity of the Infall orbit case simulations after t = 2 Gyr of evolution (similar to as Figure 2). Comparing the CDM simulations in the left and central panels reveals that the effect of the wake’s self-gravity is almost negligible at this speed. The CDM with self-gravity half-max contour is placed at δ ρ = 0.87, and extends to ∼130 kpc behind the LMC in both CDM simulations. The FDM wake (right panel) is once again more granular than the CDM wakes, though overall it remains qualitatively similar to CDM. At this slower wind speed, the wakes reach higher overdensities and are wider when compared to the Fiducial case (i.e., the max. width of the contour is ∼80 kpc wide in the Fiducial case, compared to ∼100 kpc in the Infall case here).