adsabs/AstroCLIMB huggingface dataset:
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Parameter recovery in the static accretion disk case. Top panel: varying e drawn from e ∈ [0.01, 0.1, 0.3, 0.5], for a fixed semimajor axis of a = 100Rg, M• = 105 M⊙, and MBH spin χ• = 0.5. Middle panel: varying semimajor axes drawn from a ∈ [100, 200, 400] Rg, for a fixed eccentricity of e = 0.1, M• = 105 M⊙, and MBH spin χ• = 0.5. Bottom panel: varying MBH mass drawn from ﹩{\mathrm{log}}\,{M}_{\bullet }\in [5,6]\,{M}_{\odot }﹩, for a fixed semimajor axis of a = 100 Rg, eccentricity of e = 0.1, and MBH spin χ• = 0.5.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Evolution of the distance between the secondary object and the accretion disk, and the corresponding timing of flares. The top panel shows the distance between the secondary and the disk as a function of time, with flare events indicated by red and blue stars when the distance crosses zero. The bottom panel shows the extracted flare timings, where each vertical line marks the time of a disk crossing and the color distinguishes successive crossings coming from above and below the disk. The flares shown in the bottom panel do not have flux units; their heights are purely schematic. Only the timing of the flares conveys quantitative information in this plot. Distance and time are in geometric units with Rg = GM•/c2 and tg = GM•/c3. The semimajor axis is 100 Rg, eccentricity is 0.3, i = 40°, χ• = 0.4, θdisk = 30° and Tdisk = 1000tg.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: The blue dashed ellipse represents the orbit of the secondary body, inclined relative to the accretion disk (gray plane). The vectors ﹩\widehat{E}﹩, ﹩{\widehat{a}}_{\bullet }﹩, and ﹩\hat{d}﹩ denote the orbit normal, black hole spin axis, and disk normal, respectively. The angles i and θdisk describe the tilts of the orbital and disk planes relative to the black hole spin axis. Note that generic Kerr orbits do not lie in a single plane but rather occupy a toroidal region. The inclination angle i depicted here is a conserved quantity derived from the constants of motion, rather than a geometric angle between a fixed orbital plane and the black hole spin axis. The figure is schematic and not meant to represent the full 3D structure of the orbit. The red circle and red cross mark the two points where the orbit intersects the disk: the circle denotes the intersection from below, and the cross denotes the intersection from above. The origin of the coordinate system is at the MBH.
Paper: Prospects for EMRI/MBH Parameter Estimation Using Quasiperiodic Eruption Timings: Short-timescale Analysis
Authors: Joheen Chakraborty, Lisa V. Drummond, Matteo Bonetti, Alessia Franchini, Shubham Kejriwal, Giovanni Miniutti, Riccardo Arcodia, Scott A. Hughes, Francisco Duque, Erin Kara, Alberto Sesana, Margherita Giustini, Amedeo Motta, Kevin Burdge
Figure caption: Corner plot for a static accretion disk aligned with the MBH spin axis. The posterior distributions are produced using QPE-FIT, and the blue lines indicate the true injected values used to generate the synthetic QPE timing data. Two-dimensional posteriors are smoothed by a 2σ Gaussian kernel for visual clarity.
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: Initial parameter space (the green area) for producing eclipsing MSPs in the log﹩{P}_{{\rm{orb}}}^{{\rm{i}}}-{M}_{2}^{{\rm{i}}}﹩ plane. The solid circles in the green area represent the binaries that could evolve into eclipsing MSPs. The color bar represents the duration of the first mass-transfer phase. We also show the final evolutionary outcomes of the companions, i.e., CO WD, ONe WD, and NS. The blue area indicates the NS binaries that RLOF begins when the He star is at the zero-age main sequence stage. The yellow area denotes the NS binaries that can form UCXBs. The purple area represents other NS binaries that cannot form the eclipsing MSPs. The square and triangle symbols denote the representative systems Case BA and Case BB, respectively. The cross marks the system that best reproduces the properties of PSR J1928+1815.
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: Evolutionary tracks for the binaries within the initial parameter space shown in Figure 4. The green and red regions represent the eclipsing MSPs formed via Case BA and Case BB RLOF, respectively. Circles and squares denote pulsar binaries containing CO/ONe WD and NS companions, respectively, with orbital period <4 days and spin period ≲30 ms. BW and RB samples are also included in the diagram. Observational data are taken from the ATNF Pulsar Catalog, http://www.atnf.csiro.au/research/pulsar/psrcat (version 2.5.1, 2024 September; R. N. Manchester et al. 2005).
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: Similar to Figure 4, but with the color bar indicating the number of eclipsing MSPs formed under the assumption of αCEλ = 1.0. The cross indicates the initial system that provides the best match to the observed properties of PSR J1928+1815.
Paper: Eclipsing Millisecond Pulsars with He Star Companions
Authors: Yunlang Guo, Bo Wang, Xiangdong Li, Dongdong Liu, Wenshi Tang
Figure caption: Evolution of the Galactic rates of eclipsing MSPs with He star companions as a function of time, assuming a constant Population I SFR of 5 M⊙ yr−1.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: CPD before and after applying the CC method. In the right panel, two stars show periods between 20 and 25 days; these are based on single-sector TESS observations and should therefore be treated with caution, although their consistency with gyrochronology adds confidence.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Comparison between the recovered rotation periods from simulated blends and the original periods reported by D. Gruner et al. (2023a) for both components in WBs. Red dashed lines mark the 2:1, 1:1, and 0.5:1 period ratios. The shaded region, bounded by dashed lines at 12 days, highlights the TESS Reliable Zone. In this period range, TESS is most sensitive and reliable for detecting rotation signals due to its 27 days observing window per sector. Within this region, our method correctly recovers 88% of the original periods, demonstrating strong performance where TESS is most effective.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Contamination ratio (Rcont) from the TIC as a function of the magnitude difference (ΔGmag) between the two components. Rcont is a crowding metric based on the summed flux from all sources within 10 TESS pixels, weighted by the target’s point-spread function K. G. Stassun et al. (2018), not a direct flux ratio between binary members. As a result of this weighting, even the fainter component can have Rcont < 1.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Distribution of Galactic space velocities (U, V, W) in km s−1 for the initially agreeing and reconciled pairs.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Recovery rate as a function of ΔGmag. Bins with recovery = 0 still contain systems, highlighting that correct period assignment fails for high ΔGmag ranges.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: HR diagram of our 360 MS+MS WB pairs sample. Gray lines connect components of each pair.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Histogram of rotation periods per component of the recovered and inconclusive pairs.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Occurrences of combinations.
Paper: Evaluating the Limits of Rotation Period Recovery Through Gyrochronology Criteria
Authors: Mariel Lares-Martiz, Terry D. Oswalt, Derek L. Buzasi, Kylie R. Boyer, Luca Guida, Ryan J. Reynolds
Figure caption: Histogram of Rcont per component of the recovered and inconclusive pairs.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Initial (⨂) and final (○) equilibrium configurations of stellar tracer populations in the numerical experiments with an adiabatically evolving dark matter halo. Shown are half-light radii rh and average velocity dispersions ﹩{\langle {\sigma }^{2}\rangle }^{1/2}﹩ of four stellar tracers with mono-energetic initial conditions, embedded in a cuspy (γ = 1 in Equation (1), left panel) and a cored (γ = 0, right panel) dark matter halo. Stellar tracers with initial half-light radii rh0/rmx0 = 1, 1/4, 1/16, and 1/64 are shown in dark blue, light blue, orange, and red, respectively. All initial conditions lie along the thick gray curve labeled M/M0 = 1. In each simulation, the mass sourcing the underlying dark matter potential is lowered slowly by −0.2 dex, −0.4 dex, …, −2 dex. Solid gray curves are computed from Equation (30), assuming mono-energetic distribution functions with isotropic kinematics. All equilibrium configurations fall along lines of ﹩{r}_{{\rm{h}}}{\langle {\sigma }^{2}\rangle }^{1/2}=\,\rm{const}\,﹩.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Equilibrium energy distributions of the four stellar profiles embedded in the cuspy halo shown in the right-hand panel of Figure 5. Energies are expressed in units of the initial potential minimum, ﹩{{ \mathcal E }}^{({\rm{IC}})}=1-E/{{\rm{\Phi }}}_{0}^{({\rm{IC}})}﹩. The top panel shows the initial conditions (IC), while the three subsequent panels correspond to snapshots where the mass M sourcing the potential has been slowly lowered by −0.2, −0.4, and −1.0, dex with respect to the initial value M0. The value of the evolved potential minimum Φ0 is shown in each panel, and the inaccessible region of energies below Φ0 is shaded in gray. Bottom panel: energy distribution for the model with ﹩{\mathrm{log}}_{10}M/{M}_{0}=-1.0﹩, with energies expressed in units of the evolved potential minimum ﹩{ \mathcal E }=1-E/{{\rm{\Phi }}}_{0}﹩. The slight broadening of the energy distribution is caused by the difference in response of radial and circular orbits to the adiabatic perturbation. Dashed and dotted vertical lines are computed from the conservation of radial action (Equation (35)) and angular momentum (Equation (27)), respectively, and accurately delimit the energy distributions measured in the N-body snapshots. The same systematics are observed in the case of the cored halo (not shown).
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Top panel: 3D exponential number density ν⋆(r), Equation (5), of a stellar tracer with N⋆ stars and scale radius r⋆ ≈ rh/2.67 (black solid curve), as well as an approximation to this profile consisting of the sum of five mono-energetic stellar distributions. Red curves show the individual mono-energetic profiles, Equation (13), and a dashed curve shows their sum, with each component weighted by ﹩d{N}_{\star }/d{ \mathcal E }{| }_{{ \mathcal E }={{ \mathcal E }}_{\star }}﹩. Bottom panel: differential energy distribution ﹩d{N}_{\star }/d{ \mathcal E }﹩, Equation (10), of an exponential stellar profile embedded deeply in the density cusp of a Hernquist dark matter halo, Equation (4). Energies are expressed in units of the energy ﹩{\hat{{ \mathcal E }}}_{\star }﹩ where ﹩d{N}_{\star }/d{ \mathcal E }﹩ peaks, and the energy distribution is normalized here so that ﹩{\int }_{0}^{1}(d{N}_{\star }/d{ \mathcal E })d{ \mathcal E }=1﹩. The five δ-functions corresponding to the mono-energetic profiles shown in the top panel are depicted as arrows.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Number density profiles ν⋆(r) of stellar tracers with (initial) delta function energy distributions, embedded in a cuspy dark matter halo. Profiles are shown for the initial conditions (M/M0 = 1), as well as for snapshots where the mass sourcing the potential as been adiabatically lowered to M/M0 = 1/10 and 1/100, respectively. The profiles are normalized by the initial central number density ν⋆0(0). Left panel: stellar tracer with initial half-light radius rh0/rmx0 = 1/64, deeply embedded within the density cusp of the surrounding halo. The density profile remains well approximated by Equation (17) throughout the entire adiabatic evolution, consistent with the energy distribution remaining narrow and the kinematics remaining approximately isotropic. Right panel: stellar tracer with rh0/rmx0 = 1/4. As the stellar tracer expands into a region of steeper power-law slope of the density profile of the underlying halo (see bottom panel of Figure 2), the inner regions retain isotropic kinematics, whereas at larger radii, the stellar velocity distribution becomes tangentially biased. The same systematics are observed in the case of the cored halo (not shown).
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Top panel: relation between stellar binding energy ﹩{{ \mathcal E }}_{\star }﹩ and half-light radius rh for mono-energetic stellar tracers embedded in a cuspy (black solid curve) and a cored (gray solid curve) potential. The values corresponding to the models of Figure 3 are shown as filled circles. The dashed curves show the truncation radii rt beyond which there is no stellar density (Equations (18) and (23)). The energetic spacing of stellar populations with matching half-light radii differs between models embedded deeply in a cuspy and cored halo. Bottom panel: crossing time ﹩{T}_{{\rm{cross}}}={r}_{{\rm{h}}}{\langle {\sigma }^{2}\rangle }^{1/2}﹩ as a function of energy ﹩{{ \mathcal E }}_{\star }﹩. Stellar populations that are deeply embedded in the density core all have virtually identical crossing times, regardless of their binding energy.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Top panel: cuspy (black, Equation (1) with γ = 1) and cored (gray, γ = 0) dark matter halo density profiles considered in this study. The half-light radii of four mono-energetic stellar tracers with rh/rmx = 1, 1/4, 1/16, and 1/64 are indicated by filled circles in dark blue, light blue, orange, and red, respectively (see Table 1 for the corresponding energies). Bottom panel: 3D logarithmic slope of the dark matter density profiles shown above.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Top panel: average velocity dispersion ﹩{\langle {\sigma }^{2}\rangle }^{1/2}﹩ as a function of half-light radius rh, relative to their respective initial values. The same simulation snapshots are shown as in Figure 5, each point corresponding to an equilibrium configuration reached after an adiabatic change to the underlying potential. By plotting the relative evolution of structural parameters, the systematics of Figure 5 can be collapsed onto a single curve. Bottom panel: the same as above, but showing the remnant (dark matter) mass Mh ≡ M(<rh) enclosed within the current half-light radius.
Paper: Impulsive Mixing of Stellar Populations in Dwarf Spheroidal Galaxies
Authors: Raphaël Errani, Matthew G. Walker, Simon Rozier, Jorge Peñarrubia, Julio F. Navarro
Figure caption: Mono-energetic stellar number density profiles ν⋆(r) (Equation (13)) with energies as listed in Table 1, with half-light radii of rh/rmx = 1, 1/4, 1/16, and 1/64. Stellar profiles embedded in a cuspy (Equation (17)) and a cored (Equation (22)) dark matter halo are shown using solid and dashed lines, respectively. Filled circles indicate the locations of the respective half-light radii. The profiles are sharply truncated at a radius rt. Note that for these mono-energetic energy distributions, the relative density and velocity dispersion profiles coincide.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The Euler angles for the transformation between JCRS and the Jupiter-fixed coordinate system (Y. Yang et al. 2017). Precession angle(ϕ): the angle at which Jupiter rotates around the Z-axis of the fixed coordinate system; nutation angle (θ): the angle at which Jupiter rotates around the X-axis obtained after the first rotation (the intersection line of Jupiter’s celestial coordinate system and the equatorial plane of the fixed coordinate system); spin angle(ψ): the angle at which the rigid body rotates around the Z-axis obtained after the second rotation.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The integration starts at the J2000 epoch. By reproducing the dynamical model from the current ephemeris, we calculate and compare the orbital differences with the position of Callisto from the NOE-5-2023 ephemeris. The ordinate shows positional differences (in kilometers), and the abscissa represents the integration duration (in years).
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The integration commences at the J2000 epoch. The reproduced dynamical model is subjected to data fitting using position and velocity data of Callisto from the NOE-5-2023 ephemeris. The ordinate depicts positional differences (in kilometers), while the abscissa represents the integration duration (in years).
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: After fitting the reproduced model of Callisto to the NOE-5-2023 ephemeris, the differences in the x-, y-, and z-directions between the calculated results and the positions of Callisto in the NOE-5-2023 ephemeris.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The influence of the gravitational fields of the three Galilean satellites (Io, Europa, and Ganymede) on Callisto’s orbit. The ordinate ΔP represents the difference between the orbit that includes the perturbations of the Galilean satellites and the calculated orbit that does not, with the unit being meters; the abscissa represents the integration duration starting from the J2000 epoch.
Paper: A High-precision Dynamical Model of Callisto: Incorporating Rotation Effects within Multilayer Internal Structure Models
Authors: Kai Huang, Yongzhang Yang, Yuhao Chen, Yining Zhang, Yuqiang Li
Figure caption: The established rotation model of Callisto is integrated, and the temporal variations of the three Euler angles are presented.
Paper: Central Massive Black Holes Are Not Ubiquitous in Local Low-mass Galaxies
Authors: Fan Zou, Elena Gallo, Anil C. Seth, Edmund Hodges-Kluck, David Ohlson, Tommaso Treu, Vivienne F. Baldassare, W. N. Brandt, Jenny E. Greene, Piero Madau, Dieu D. Nguyen, Richard M. Plotkin, Amy E. Reines, Alberto Sesana, Jong-Hak Woo, Jianfeng Wu
Figure caption: The probability distribution, p(λ), of the SARDF for galaxies with M⋆ = 1010 M⊙ is shown as a function of ﹩{\mathrm{log}}\,\lambda ﹩ (top axis) and ﹩{\mathrm{log}}\,{\lambda }_{{\rm{Edd}}}=\mathrm{log}\lambda -34﹩ (bottom axis). Here, λ is converted to λEdd by assuming kbol = 25 and MBH = 0.002 M⋆ (see Section 4.4 for a more in-depth discussion). The gray shaded regions bracket the range of allowed p(λ) as inferred directly from the data (see Section 4.2), based on a subsample of 457 nearby objects with M⋆ > 1010 M⊙. The red curve represents our inferred parametric p(λ), which is formally valid between ﹩27\lesssim \mathrm{log}\lambda \lesssim 31﹩ (shown as a solid line). The probability distributions derived by J. Aird et al. (2018) and F. Zou et al. (2024b) for AGNs are shown as dashed curves for comparison. The probability distributions obtained by L. C. Ho (2009) and B25 based on different samples of nearby galaxies are shown as dotted lines.