adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: Optical depth for the case of α1 = 0, α2 = 45°, λ = −1, and ΔΦ = 0(↑ ↙) with 1012 G (left) and 1014 G (right) magnetic field stars. A wider line indicates a later stage in the evolution. The vertical dashed line highlights the minimum pair-production threshold of 1 MeV while the blue horizontal line is the ﹩{ \mathcal T }=1﹩ line. Note that, in the right-hand panel, ﹩{ \mathcal T }﹩ may be overestimated near ϵ = 1 MeV (see main text for discussion), potentially permitting the escape of marginally higher-energy photons.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: In the first row the high-energy emission skymaps for α1 = 45°, α2 = 90°, ΔΦ = 0, and λ = 1 (↗ →). The two white points, labeled A and B, correspond to two chosen directions for the construction of the respective light curves. In the second row, the normalized light curves from the direction A (left) and B (right) for two rotations of the stars. The dotted vertical lines correspond to the instances of the first row, while the gray line serves as a separation of the two rotations.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: (Left) Evolution of the curvature radiation cutoff energy prior to BNS merger for different typical magnetic field strengths. (Right) A contour plot of the characteristic cutoff energies in the B⋆ − τ log–log plane. Horizontal slices at fixed surface magnetic field values illustrate the evolution of cutoff energies throughout the BNS system’s inspiral.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: Regions of high-energy emission origin for the case with α1 = 0°, α2 = 45°, λ = −1, and ΔΦ = 0° (↑ ↙), similar to the middle row of Figure 5. The two snapshots, taken at τ = −10.11 ms and τ = −8.76 ms, are separated by half an orbital rotation. The color scale represents the strength of the parallel electric field, ﹩{E}_{\left|\right|}﹩.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: Similar to Figure 8 the structure of the magnetosphere, at τ ≃ −7 ms, for the cases with α1 = 0°, α2 = 45°, ΔΦ = 0°, and λ = 1 (↑ ↗) in top row while λ = −1 (↑ ↙) in bottom row. Left are the simulations with the resolution used in the main text while right are the higher-resolution simulations.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: Similar to Figure 26. Snapshots of the evolution of high-energy emission skymaps for the case with α1 = 0°, α2 = 45°, ΔΦ = 0°, and λ = −1 (↑ ↙) in higher resolution.
Paper: Magnetosphere Evolution and Precursor-driven Electromagnetic Signals in Merging Binary Neutron Stars
Authors: Dimitrios Skiathas, Constantinos Kalapotharakos, Zorawar Wadiasingh, Demosthenes Kazanas, Alice K. Harding, Paul T. Kolbeck
Figure caption: The Poynting flux evolution for the cases with α1 = 0°, α2 = 45°, ΔΦ = 0°, and λ = 1 (↑ ↗) in red, and λ = −1 (↑ ↙) is in black with the regular (solid line) and double (dashed line) resolution.
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: Free eccentricities ﹩{ \mathcal Z }﹩ versus period-ratio deviations from resonance Δ for observed systems (blue points), with values normalized to those expected from crossing a first-order MMR adiabatically. The gray curve shows the full evolution after crossing to Δ > 0, with ﹩{ \mathcal Z }/{Z}_{{\rm{Jump}}}=1﹩ denoting the maximum eccentricity reached, and Δ/ΔJump = 1 to the corresponding value of Δ at the moment of maximum eccentricity. Migration then continues rightward toward larger values. In red, we plot the equilibrium value of the eccentricity (normalized to ﹩{{ \mathcal Z }}_{{\rm{Jump}}}﹩). This is the value to which eccentricity damping should drive the observations, and it decreases with distance from the resonance. Most observed planet pairs have eccentricities too high to be consistent with the predictions from strong eccentricity damping.
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: Selection of rotational transitions of ﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩, v = 0 covered by the ReMoCA survey. The LTE synthetic spectrum of ﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩, v = 0 used to derive the upper limit to its column density toward Sgr B2(N1S) is displayed in red and overlaid on the observed spectrum shown in black. The blue synthetic spectrum contains the contributions of all molecules identified in our survey so far. The values written below each panel correspond from left to right to the HPBW, the central frequency in MHz, the width in MHz of each panel in parentheses, and the continuum level in K of the baseline-subtracted spectra in brackets. The y-axis is labeled in brightness temperature units (K). The dotted line indicates the 3σ noise level.
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: Evolution under divergent migration across the 3:2 MMR for different values of the total planetary mass (different colors) before (left panel) and after (right panel) normalization. We plot the free eccentricity (﹩| { \mathcal Z }| ﹩) versus the period-ratio deviation from resonance (Δ), with those quantities in the right panel normalized to analytically calculated values (Equations (A7) and (A8)).
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: Transition of 2-APN used to compute the column density upper limit toward G+0.693 (see text). The black line and gray histogram show the observed spectrum, the red curve is the LTE synthetic model of 2-APN using the column density upper limit derived toward G+0.693, and the blue curve indicates the emission of all the molecules previously identified toward the source.
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: Combined eccentricities ﹩{ \mathcal Z }﹩ versus Δ for planet pairs exhibiting TTVS, extracted by S. Hadden & Y. Lithwick (2017; adopting their high-mass priors).
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: Left panel: histogram of the period ratio deviation Δ for the full KOI catalog of J. J. Lissauer et al. (2024). Right panel: deviation from resonance, normalized by the mass-dependent width of the resonance, see the main text.
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: Same as Figure 5 but for CH3CH(NH2)CN, v = 0.
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: The distribution of period ratios between adjacent planets in the NASA Exoplanet Archive. Dashed–dotted lines at strong MMRs are labeled with their corresponding integer ratio.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: The sSFR distribution for arm and interarm spaxels in inner radius R1 (left column) and outer radius R2 (right column) for galaxies NGC 1097, NGC 1512, and NGC 4254. The median ratios are 1.507 and 2.104 for NGC 1097; 2.898 and 0.706 for NGC 1512; and 1.357 and 0.691 for NGC 4254. The two small median ratios could be the result of small statistics, and their p-values are 0.4 and 0.8, meaning that these differences are not significant.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Similar to 6 but for galaxies NGC 4579, NGC 0628, and NGC 4321. The smallest median ratio is NGC 0628 (R1), 1.073; the largest median ratio is NGC 4579 (R1), 1.639. All median ratios are less than 2 and have p-values >0.06.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: The molecular gas mass Mgas and star formation efficiency (SFE) across six galaxies after correcting for inclinations. Left: the median of Mgas in arm and interarm regions are −0.124 and −0.301, respectively; the median ratio is 1.505. Right: the SFE median in arm and interarm regions are −0.560 and −0.745, corresponding to a median ratio of 1.533, consistent with the gatherer scenario.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: SFR and Mstar distributions for arm and interarm spaxels across six galaxies. Left: normalized SFR, with median log values of −0.636 (arm) and −1.218 (interarm), yielding a median ratio of 3.823. Right: normalized Mstar, with median log values of −0.061 (arm) and –0.424 (interarm), corresponding to a median ratio of 2.304.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Distributions of best-fit values of the sSFR (where the SFR is calculated over the most recent 107 yr) for the six galaxies. The arm spaxels and the interarm spaxels are plotted in blue and orange, respectively. For both galaxies, the sSFR distributions of arm/interarm regions are similar, and their median values are shown as vertical dashed lines.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Similar to Figure 1 but for NGC 4254. In each row, the three panels from left to right are: best-fit values of all spaxels with S/N 3 in SPIRE 250 image, including bulge spaxels; arm spaxels; interarm spaxels, with the bulge excluded.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Similar to Figure 9 but for NGC 4579. In each row, the three panels from left to right are best-fit values of all spaxels with S/N 3 in SPIRE 250 image, including bulge spaxels; arm spaxels; and interarm spaxels, with the bulge excluded.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Similar to Figure 11 but for Mstar.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Similar to Figure 1 but for NGC 1512.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Differences in spectral indices between the α-enhanced ([α/Fe] = +0.4) and solar-scaled SSPs at fixed [Fe/H] = +0.0 as a function of ages. The thick black lines show the differences from the α-enhanced models where both isochrones and stellar spectra are α-enhanced. The blue and red lines show the “spectral effect” and “isochrone effect,” respectively, by adopting α-enhanced models only for stellar spectra and isochrones, respectively. In most cases, we find the opposite effects of isochrones and stellar spectra on spectral indices. α-enhancement in isochrones increases the line strengths by lowering the temperature of stars dominating the SSP fluxes. On the other hand, α-enhancement in stellar spectra makes most indices weaker, except for the indices involving α-elements where the enhanced α-abundances make them stronger.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Age-sensitive indices (Hβ, HγA, HδA, and D4000) as a function of ages (zooming for ﹩\mathrm{log}(\mathrm{age}/\mathrm{yr})=8.5-10.3﹩) for SSPs with [Fe/H] = –1.0 (top) and [Fe/H] = +0.0 (bottom). The same color code is used for different [α/Fe] as in Figure 10. We find that the α-enhanced models at fixed [Fe/H] show weaker Balmer strengths and the SSP ages the most sensitive to [α/Fe] depend on [Fe/H]. Therefore, to accurately derive the ages of stellar populations, a detailed analysis with chemical abundances ([Fe/H],[α/Fe]) is required.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Model comparison of the g − r and V − I color evolution. Blue and orange lines show solar-scaled and α-enhanced models ([α/Fe] = +0.4), respectively. SSPs with [Fe/H] = –0.5, +0.0, +0.2 are shown in each column. The solid lines show the color evolution of our models. The models from P. Coelho et al. (2007) and A. T. Knowles et al. (2023) are shown as dashed and dotted–dashed lines, respectively. In each panel, the top subset panel shows the color difference between the α-enhanced ([α/Fe] = +0.4) and solar-scaled models. The different line types represent different models.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Color differences between the models with α-enhanced ([α/Fe]= + 0.4) and solar-scaled mixtures ([α/Fe] = +0.0) at constant [Z/H]. We find that bluer bands show great sensitivities to the Fe abundances for old stellar populations (>1 Gyr); the models with α-enhanced mixtures show much bluer u − g colors due to lower Fe abundances than with the solar-scaled mixtures.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Model comparison of the Lick indices as a function of SSP ages at fixed [Fe/H]. The α-enhanced ([α/Fe] = +0.4) and solar-scaled models are shown as orange and blue lines, respectively. The solid lines show the indices measured from our models. The models from P. Coelho et al. (2007) and A. T. Knowles et al. (2023) are shown as dashed and dotted–dashed lines, respectively. All models are smoothed to FWHM = 8.4 Å to measure the index strengths, and the Kroupa IMF (P. Kroupa 2001) is assumed for all models.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Comparisons of Lick indices between α-enhanced (red) and solar-scaled (blue) models at constant [Z/H]: [Z/H] = −0.19 (dashed lines) and [Z/H] = +0.31 (solid lines). We find that Ca4227 and Mg b show great sensitivity to α-enhancement. However, all iron (e.g., Fe5015, Fe5270, Fe5335, and Fe5406) and iron-sensitive lines (e.g., Ca4455 and NaD) are weakened in the models with α-enhanced mixtures due to decreased iron abundances.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Stellar parameter coverage of self-consistent α-enhanced models: wavelength ranges (upper panel) and [Fe/H] and ages (bottom panel).
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Flux ratios between models with α-enhanced ([α/Fe] = +0.4) and solar-scaled mixtures ([α/Fe] = +0.0) at constant [Z/H] = +0.31. From top to bottom, we show the flux ratios of SSPs for different ages, from 0.1 Gyr to 10 Gyr.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Model comparison of SSPs for 0.1, 0.5, 1, 4, 10 Gyr with [Fe/H] = –0.5 and [α/Fe] = +0.4 (left) and solar-scaled [Fe/H] and [α/Fe] (right).
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF energy spectra for different regions of the solar flare for source g2 (described in Equation (6)). The left column displays results for n = 3 × 1010 cm−3, while right column shows results for n = 5 × 109 cm−3. The shaded regions represent the estimated uncertainty of each bin, multiplied by 100 for better visualization. The τacc color-coding used in panel (a) is kept the same across every other panel. δnVF represents the spectral indices obtained applying a fit on nVF between 15–25 and 40–90 keV.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: nVF spectra as a function of (a) the electron energy, where the shaded areas represent the estimated uncertainty multiplied by 100 for better visualization, (b) loop position, and (c) pitch-angle cosine. In panel (b) the black dashed line represents the chromosphere boundary and the cyan dashed line is the acceleration region, σ = 3″.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: The two atmospheric models used in the simulations, showing the plasma number density (blue) and temperature distribution (orange). In the coronal region, the continuous blue line represents atmospheric model 1 and dashed blue atmospheric model 2. Outside the corona models 1 and 2 are identical.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: The evolution of the turbulent acceleration time amplitude, g(t), described by Equations (6)–(8).
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Evolution of the volume density profiles, centered on the stellar COM, for the N-body merger remnant model of NGC 6166 after GW recoil kicks of vk/vesc = 0.1 (left) and 0.5 (right), using binned SPH profiles. tk is the time when the N-body simulation is paused for the SMBH merger and the GW recoil kick is given; “An” and “Pn” indicate the nth apocenter and pericenter passages of the kicked SMBH; “Br” indicates that the SMBH has settled into Brownian motion. The inset plots use spherical shells centered on the SMBH. For the the vk/vesc = 0.5 kick, the density changes as the SMBH remnant moves away from and back to the center, and the central density becomes more prominent within a flattened core.
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Volume (top three rows) and surface density (bottom three rows) profiles when the SMBH remnant has settled to Brownian motion for NGC 1600, NGC 6166, and IC 1101. Columns from left to right are for kicks with a vk/vesc of 0.1, 0.3, and 0.5 respectively. Profiles labeled “nucleus” indicate those for particles that were within the influence radius of the SMBH at first apocenter (blue), and all other particles as “remainder” (orange). The combined profiles are labeled “total” (green dotted). The prominent increases in central density in NGC 1600 with vk = 0.3vesc, and for NGC 6166 and IC 1101 with vk = 0.5vesc are seen to be due to the “nucleus” particles.
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Bound mass to the SMBH remnant (here “A” and “P” indicate apocenter and pericenter passages, respectively, followed by the number of passages; “Br” indicates the SMBH remnant has settled into Brownian motion) for galaxy NGC 6166 with vk/vesc = 0.1, 0.3, and 0.5. The bound mass is lower at higher vk/vesc, for comparable phases after the kick. For the slower kicks, the bound mass quickly rises as the SMBH slows and remains high as the motion of the SMBH remnant is rapidly damped. For the vk/vesc = 0.5 kick, the bound mass is lower at each pericenter than the corresponding apocenter, as the SMBH speeds up and slows down.
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Volume density profiles, centered on the stellar COM, at the end of the recoil kick. This is at “Br,” which indicates the time the SMBH has settled into Brownian motion. The galaxy models shown are NGC 1600 (left) and IC 1101 (right), for GW recoil kicks of vk/vesc = 0.5. We use binned SPH profiles for the main profiles, but the inset plots use spherical shells centered on the SMBH. Increases in central density, which we interpret as NSCs, are clearly seen within a flattened core.