adsabs/AstroCLIMB huggingface dataset:
Paper: Breaking the Mass Inclination Degeneracy of Radial Velocity Measurements via Monitoring von Zeipel–Lidov–Kozai Cycles: Implications in the HD 41004 System
Authors: Zhizhen Qin, 至臻 秦, Shang-Fei Liu, 尚飞 刘, Bo Ma, 波 马, Fabo Feng, 发波 冯
Figure caption: Ratio of vZLK to GR-induced pericenter precession rates (﹩{\dot{\omega }}_{1,\,\rm{vZLK}\,}/{\dot{\omega }}_{1,\,\rm{GR}\,}﹩) and tide-induced pericenter precession rates (﹩{\dot{\omega }}_{1,\,\rm{vZLK}\,}/{\dot{\omega }}_{1,\,\rm{Tide}\,}﹩) for an HD 41004 Ab–like planet as a function of semimajor axis (a1) and eccentricity (e1). The color map illustrates the relative dominance of GR and tidal (green) vs. vZLK-induced (red) precession across the (a1, e1) parameter space. The gray point with error bars marks the nominal location of HD 41004 Ab, with a1 = 1.7 au and e1 = 0.74 ± 0.2. Three gray contours denote the periastron distances typical of warm Jupiters (a1 =  0.5 au; dashed–dotted line), HD 41004 Ab itself (solid line), and cold Jupiters (a1 =  5 au; dashed line). The system resides well within the vZLK-dominated regime, with a precession rate ratio ﹩{\dot{\omega }}_{1,\,\rm{vZLK}\,}/{\dot{\omega }}_{1,\,\rm{GR}\,}﹩ of ∼3.5 × 105 and ﹩{\dot{\omega }}_{1,\,\rm{vZLK}\,}/{\dot{\omega }}_{1,\,\rm{Tide}\,}﹩ of ∼1.8 × 1013 at iinitial = 75°.
Paper: Breaking the Mass Inclination Degeneracy of Radial Velocity Measurements via Monitoring von Zeipel–Lidov–Kozai Cycles: Implications in the HD 41004 System
Authors: Zhizhen Qin, 至臻 秦, Shang-Fei Liu, 尚飞 刘, Bo Ma, 波 马, Fabo Feng, 发波 冯
Figure caption: Dependence of the vZLK timescale on the initial mutual inclination in the HD 41004 system for different binary eccentricities. Filled points indicate the simulated vZLK timescales as functions of iinitial, with horizontal error bars denoting the corresponding inclination oscillation amplitudes (from ﹩{i}_{{\rm{\min }}}﹩ to ﹩{i}_{{\rm{\max }}}﹩). The green dashed–dotted lines mark the theoretical vZLK timescales derived from the test-particle approximation, calculated as 1.02 × 104 yr for e2 = 0 and 7.89 × 103 yr for e2 = 0.4. Both panels reveal a systematic decrease in the vZLK timescale with increasing inclination, highlighting enhanced dynamical interactions at higher iinitial values.
Paper: Breaking the Mass Inclination Degeneracy of Radial Velocity Measurements via Monitoring von Zeipel–Lidov–Kozai Cycles: Implications in the HD 41004 System
Authors: Zhizhen Qin, 至臻 秦, Shang-Fei Liu, 尚飞 刘, Bo Ma, 波 马, Fabo Feng, 发波 冯
Figure caption: Dynamical RV fitting of HD 41004 A for a2 = 30 au and a2 = 40 au. The structure is the same as in Figure 3. Different colors and line styles indicate varying eccentricities. The planetary mass is fixed at ﹩{m}_{1}\sin {I}_{1}=2.54\,{M}_{{\rm{J}}}﹩. rms values of the O − C residuals are listed in the legends.
Paper: Breaking the Mass Inclination Degeneracy of Radial Velocity Measurements via Monitoring von Zeipel–Lidov–Kozai Cycles: Implications in the HD 41004 System
Authors: Zhizhen Qin, 至臻 秦, Shang-Fei Liu, 尚飞 刘, Bo Ma, 波 马, Fabo Feng, 发波 冯
Figure caption: Dynamical RV fitting of HD 41004 A for different planetary masses at a2 = 22 au. The structure is the same as in Figure 3. The top panel represents fits for mpl = 1.8 MJ, while the bottom panel corresponds to mpl = 3.28 MJ.
Paper: An Energy Perspective of Core Erosion in Gas Giant Planets
Authors: J. R. Fuentes, Christopher R. Mankovich, Ankan Sur
Figure caption: Interior models with different radial distributions of heavy elements. The blue and orange curves represent the density, normalized by the central density, and the mass fraction of heavy elements, respectively. Panel (a) shows a model with a narrow fuzzy core, where a sharp compositional gradient is confined to the central region. Panel (b) presents a fuzzy core with a smooth compositional gradient, similar to the structure proposed by F. Debras & G. Chabrier (2019). Panel (c) depicts a broad, dilute core with a sharp compositional gradient, akin to the model in B. Militzer et al. (2022). Panel (d) corresponds to a fully mixed planet. In all models, the total mass of heavy elements within the gradient is fixed at 20 M⊕.
Paper: An Energy Perspective of Core Erosion in Gas Giant Planets
Authors: J. R. Fuentes, Christopher R. Mankovich, Ankan Sur
Figure caption: Evolutionary models for Jupiter (top row) and Saturn (bottom row) computed using the APPLE code (A. Sur et al. 2024). Blue curves denote compact-core models and orange curves denote fuzzy-core models (both with a 20 M⊕ core). Left panels: time evolution of the temperature profiles. Center panels: time evolution of the heavy-element mass fraction Z. Right panels: luminosity vs. time. All models are calibrated to match the observed effective temperatures of Jupiter and Saturn and Jupiter’s atmospheric helium abundance.
Paper: An Energy Perspective of Core Erosion in Gas Giant Planets
Authors: J. R. Fuentes, Christopher R. Mankovich, Ankan Sur
Figure caption: Core mass redistributed into the envelope as a function of time, using γ−1 values between 0.5 and 1 (shaded areas). Results are presented for both Jupiter and Saturn, considering both compact and fuzzy-core configurations.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Optically thin dust modeling of WTP14adbjsh (the closest). Top: assumed underlying flare heating the dust, with Δt = 9.3 yr, L = 5.5 × 1044 erg s−1, nsub = 1.5 × 10−10 cm−3, and γ = 0. The model plateaus when it reaches a luminosity of Lplat = 2 × 1042 erg s−1. We denote the two phases in which we model the spectrum with MRN and graphite dust in green and purple, respectively. We assume that the graphite dust is responding to the last year of the flare to roughly mimic the dust composition evolution we expect in the innermost regions around the SMBH. Bottom: resulting optically thin dust model from the above underlying accretion flare. The MRN dust (green curve) fits the long-wavelength spectrum well but underestimates the short-wavelength spectrum. Larger graphite grains near the SMBH (purple curve) can account for this short-wavelength excess. We stress that this is not a self-consistent model or a direct fit to the data, and other parameter combinations could also produce a similarly good fit. We will fully explore this parameter space in a follow-up work with self-consistent dust physics incorporated.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Line ratios for both the nuclear (purple stars) and annular (blue diamonds) MIRI/MRS spectra for each source in our sample as a proxy for the underlying ionizing spectrum. The strength of accretion-driven ionization increases to the upper right part of the plot (i.e., to higher [Ne V]/[Ne II] and [Ne III]/[Ne II] ratios). For comparison, the green circles show data from recent JWST MIRI/MRS nuclear spectra of nearby AGN (M. Pereira-Santaella et al. 2022; L. Armus et al. 2023; L. Hermosa Muñoz et al. 2024; L. Zhang et al. 2024), and the orange squares show Spitzer IRS high-resolution (R ∼ 600) data of starburst galaxies, excluding those with a known AGN (J. Bernard-Salas et al. 2009). The black horizontal and gray vertical lines show different AGN indicators from H. Inami et al. (2013) and L. M. Feuillet et al. (2025), respectively. The gray hatched region shows the intersection of these two regimes, where the JWST AGN fall. The WISE TDE nuclear spectra show line ratios that are comparable to AGN, confirming their accretion-driven nature. The annular spectra show lower line ratios, suggesting a significant change to the ionization source in the nuclei.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Comparison of TDEs, AGN, and ULIRGs in the MIR band. Left: we show the JWST MIRI/MRS nuclear spectra from our TDE sample in blue. The green and purple spectra are examples of Type 1 and Type 2 AGN, respectively, at similar distances that have also been observed with JWST MIRI/MRS (L. Armus et al. 2023; I. García-Bernete et al. 2024). We also show a representative MIR spectrum of IRAS 08572+3915, a ULIRG observed with the Spitzer Infrared Spectrograph (IRS) with deep silicate absorption in gray (N. A. Levenson et al. 2007) and the mean QSO Spitzer spectrum from H. Netzer et al. (2007) in black. Right: 9.7 μm vs. 18 μm silicate strengths. A positive (negative) silicate strength corresponds to emission (absorption). The blue stars show our measurements of WISE TDEs with JWST. The green squares and purple circles are Type 1 and Type 2 AGN measurements, respectively (E. Hatziminaoglou et al. 2015). The smoothed histograms on the top and left of this plot show a density of 9.7 and 18 μm  strengths for each class. The TDEs show significantly stronger silicate emission features than almost all AGN.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Line profiles for a few of the prominent atomic lines with different IPs. Each panel shows the nuclear spectrum for a different source with lines colored by IP. For each line, we have continuum-subtracted the data, normalized the flux, and shifted to the expected velocity center. We show the [Ne VI] 7.65 μm  (IP = 126.2 eV), [Ne II] 12.81 μm  (IP = 26.1 eV), [Ne V] 14.31 μm  (IP = 97.1 eV), and [Ne III] 15.56 μm  (IP = 41.0 eV) lines, which span over 100 eV change in IP. In most sources, there is no clear change between profile shapes of the high- and low-ionization lines, with the exception of WTP18aampwj (the optical transient), for which the high-IP lines are relatively skewed.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Left: host galaxies of the four TDEs in our sample, adapted from Figure 9 in M. Masterson et al. (2024). Right: multiwavelength light curves of the four TDEs in our sample, adapted from Figure 1 in M. Masterson et al. (2024), including the most recent WISE data up to 2024. The left y-axis denotes the flux density in the IR and optical bands. The right y-axis denotes the resulting luminosity, corresponding to νLν at the central frequency of the W2 band for the IR band, the 0.2–2.3 keV luminosity for eROSITA, and the 0.2–2 keV luminosity for XMM-Slew. Red pentagons and orange diamonds denote the ATLAS c- and o-band data, respectively. The data are binned to 30 days, except for WTP18aampwj (the optical transient), which is binned to a 10-day cadence to highlight the optical transient. Green crosses and yellow hexagons show the X-ray data for WTP17aamzew (the X-ray transient) from eROSITA and XMM-Slew, respectively. The vertical black dashed line denotes the time of the JWST observation of each source.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Optically thin dust model for the late-time MIR spectrum from a TDE-like flare. Each panel shows how the model changes for a different free parameter. The free parameters are the time since the flare (Δt), luminosity of the flare (L), density at the sublimation radius (nsub), and slope of the radial density profile (γ). The black model is a base model that is the same in each panel. The parameters for the model are Δt = 5 yr, L = 5 × 1044 erg s−1, nsub = 10−10 cm−3, and γ = 1. All models assume a single grain size of a = 0.1 μm, an MRN mixture of silicates and graphite dust, and a plateau luminosity of Lplat = 1042 erg s−1.
Paper: JWST’s First View of Tidal Disruption Events: Compact, Accretion-driven Emission Lines and Strong Silicate Emission in an Infrared-selected Sample
Authors: Megan Masterson, Kishalay De, Christos Panagiotou, Erin Kara, Wenbin Lu, Anna-Christina Eilers, Muryel Guolo, Armin Rest, Claudio Ricci, Sjoert van Velzen
Figure caption: Comparison of JWST MIRI/MRS nuclear and annular spectra for WTP14adbjsh (the closest). The blue spectrum is the nuclear spectrum shown in Figure 1, with a conical extraction equal to 1 FWHM of the PSF. The annular spectrum is shown in orange, with the darker orange showing the spectrum binned to 0.01 μm. The wavelengths of key high- and low-IP lines are shown in dark and light green, respectively, where we define the threshold energy between high and low IP at 40 eV. The wavelengths of the molecular H2 transitions are shown in red. Likewise, the locations of key silicate features and PAHs are shown in dark and light purple, respectively. The PAHs, low IP lines, and molecular lines are much stronger in the annular spectrum compared to the nuclear spectrum.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole 4U 1630-472 in Outburst
Authors: Jon M. Miller, Misaki Mizumoto, Megumi Shidatsu, Ralf Ballhausen, Ehud Behar, María Díaz Trigo, Chris Done, Tadayasu Dotani, Javier A. García, Timothy Kallman, Shogo B. Kobayashi, Aya Kubota, Randall Smith, Hiromitsu Takahashi, Makoto Tashiro, Yoshihiro Ueda, Jacco Vink, Shinya Yamada, Shin Watanabe, Ryo Iizuka, Yukikatsu Terada, Chris Baluta, Yoshiaki Kanemaru, Shoji Ogawa, Tessei Yoshida, Katsuhiro Hayashi
Figure caption: (Left) Long-term X-ray light curve of 4U 1630−472 over ∼30 yr, obtained with RXTE/ASM (gray) and MAXI/GSC (2–20 keV; black). The brightening in the shaded region is due to the nearby source MAXI J1630−276. The RXTE/ASM intensity is normalized so that the light-curve profile of the outburst around MJD 55200–55400 fits that of MAXI/GSC. (Right) Enlarged view around the XRISM observation.
Paper: Physics-informed Priors Improve Gravitational-wave Constraints on Neutron-star Matter
Authors: Spencer J. Magnall, Christian Ecker, Luciano Rezzolla, Paul D. Lasky, Simon R. Goode
Figure caption: Priors for the source-frame chirp mass ﹩{ \mathcal M }﹩ and the dimensionless tidal deformability ﹩\tilde{{\rm{\Lambda }}}﹩ in the case of BNS (top panel) or NSBH binaries (bottom panel). In both panels, dashed black curves indicate analytic fits to the 90% contours of the distribution given in Equation (6), while the dashed gray curves are the corresponding fits obtained when imposing the GW170817 constraint on the prior following S. Altiparmak et al. (2022). Horizontal red bands represent the 90% credible intervals for the measured chirp masses of GW170817 (B. P. Abbott et al. 2017), GW190425 (B. P. Abbott et al. 2020), GW200115 (R. Abbott et al. 2021), and GW230529 (A. G. Abac et al. 2024).
Paper: Physics-informed Priors Improve Gravitational-wave Constraints on Neutron-star Matter
Authors: Spencer J. Magnall, Christian Ecker, Luciano Rezzolla, Paul D. Lasky, Simon R. Goode
Figure caption: Posterior distributions of the range of pressures and energy densities for a nuclear-matter EOS (top panel) and of the corresponding masses and radii (bottom panel) in the case of GW170817. In both panels, the shaded regions show the 90% credible intervals of the posterior distributions obtained using the physics-informed priors (red) or the uniform priors (blue), while the dashed curves show the 90% credible intervals of the effective priors of the relationship between chirp mass and tidal deformability for the uniform (blue) and physics-informed (red) priors, when mapped to the spectral parameterization.
Paper: Physics-informed Priors Improve Gravitational-wave Constraints on Neutron-star Matter
Authors: Spencer J. Magnall, Christian Ecker, Luciano Rezzolla, Paul D. Lasky, Simon R. Goode
Figure caption: The same as in Figure 3 but for the GW190425 event. The top panel shows the posterior distributions in pressure–density space, while the bottom panel shows the reconstructed mass–radius curves. The shaded regions show the 90% credible intervals of the posterior distributions obtained from the analysis using the physics-informed BNS prior (red) and the NSBH prior (green). The black dashed curve shows the 90% credible interval of the effective prior of the relationship between chirp mass and tidal deformability for the physics-informed prior, when mapped to the spectral parameterization.
Paper: Physics-informed Priors Improve Gravitational-wave Constraints on Neutron-star Matter
Authors: Spencer J. Magnall, Christian Ecker, Luciano Rezzolla, Paul D. Lasky, Simon R. Goode
Figure caption: Marginalized posterior distributions of the tidal deformability ﹩\tilde{{\rm{\Lambda }}}﹩ for GW170817. The posterior using a physics-informed prior is shown in red, while the posterior using uniform priors from the LVK analysis is shown in blue: we show the (marginalized) prior with the black curve. Note that the posterior from the LVK shows support up to ﹩\tilde{{\rm{\Lambda }}}=2000﹩.
Paper: Physics-informed Priors Improve Gravitational-wave Constraints on Neutron-star Matter
Authors: Spencer J. Magnall, Christian Ecker, Luciano Rezzolla, Paul D. Lasky, Simon R. Goode
Figure caption: The same as in Figure 2 but for the GW190425 event. The posterior using a physics-informed prior for BNS mergers is shown in red, while the posterior for NSBH mergers is shown in green. The posterior using uniform priors and assuming a BNS origin from the LVK is reported in blue.
Paper: A Plasma Torus around a Young Low-mass Star
Authors: Luke G. Bouma, Moira M. Jardine
Figure caption: Time-variable fit to Hα line profiles. Left column: raw spectrum at each epoch fλ minus the time-averaged spectrum f〈t〉 (as in Figure 3(e)). Underplotted sinusoids are not fits; they are meant to guide the eye. Middle columns: model of emission from the inner clump (sum of two Gaussians) and the outer clump (single Gaussian), plotted over the data. Right column: residual of the left column after subtracting the sum of the two middle columns, leaving variability in the line core. Appendix B discusses the use of this model.
Paper: A Plasma Torus around a Young Low-mass Star
Authors: Luke G. Bouma, Moira M. Jardine
Figure caption: TIC 141146667 age diagnostics. (a) Dereddened Gaia DR3 color vs. absolute magnitude for TIC 141146667, USco (8 Myr), IC 2602 (40 Myr), the Pleiades (112 Myr), and stars within 100 pc. The location of TIC 141146667 in this diagram suggests an age of 30–150 Myr. (b) A dearth of photospheric lithium for TIC 141146667 (yellow triangle denotes 2σ upper limit) yields a lower bound on the star’s age of ≳20 Myr. Comparison stars are from the Gaia-ESO survey (R. D. Jeffries et al. 2023); rich clusters in these data include NGC 2264 (4.5 Myr), λ Ori (8.7 Myr), γ2 Vel (16.4 Myr), NGC 2547 (35.0 Myr), IC 2391 (42.0 Myr), and NGC 2451A (50.0 Myr). Measurement uncertainties are large below +50 mÅ; negative equivalent width does not correspond to significant emission.
Paper: A Plasma Torus around a Young Low-mass Star
Authors: Luke G. Bouma, Moira M. Jardine
Figure caption: (a) Orbits fit to mean radial velocities extracted from Hα profile fits in Figure 6. Radial velocities on the vertical axis are in units of the equatorial velocity, veq = 130 km s−1. Each marker denotes the best-fit Gaussian mean at a given epoch. Filled circles were adopted in the fits; transparent crosses were excluded owing to reliability concerns (see text). The inner double-peaked clump is shown in violet and orange; the outer clump is shown in green. Five model draws from each posterior probability distribution are plotted. (b) Idealized emissivity from mean model fits in panel (a), assuming a constant emission amplitude and velocity width σ = 0.25veq and neglecting eclipses.
Paper: A Plasma Torus around a Young Low-mass Star
Authors: Luke G. Bouma, Moira M. Jardine
Figure caption: SED of broadband photometric magnitudes (filled cyan circles) plotted over the best-fit BT-Settl stellar atmosphere model (F. Allard et al. 2012) and the associated photometric predictions (open purple diamonds). This plot was made from an adaptation of astroARIADNE (J. I. Vines & J. S. Jenkins 2022). The photometry extends from the Gaia DR3 blue passband to WISE W3; the W4 passband (22 μm) did not yield a confident detection. This fit yields the star’s temperature and size. The lack of excess infrared flux relative to the photospheric model sets an upper limit on emission from circumstellar dust.
Paper: Little Red Dots as the Very First Activity of Black Hole Growth
Authors: Kohei Inayoshi
Figure caption: Left: the redshift dependence of the AGN comoving number density. Each modeled curve presents the AGN population that undergo nth AGN active episodes, illustrating the distribution of the total elapsed time Tn (1 ≤ n ≤ 8): the first (magenta), second (green), third (cyan), and fourth (orange) episodes, as well as the total population in this model (black). The normalization is set such that the modeled LRD abundance is consistent with the observed ones (red; V. Kokorev et al. 2024a; D. D. Kocevski et al. 2025). The predicted abundance in this model agrees with those of LRD candidates at 1.7 < z < 3.7 photometrically selected by wide-area ground-based telescope surveys (purple; Y. Ma et al. 2025), as well as with X-ray selected AGNs over 0 < z < 5 (gray; Y. Ueda et al. 2014) and 4 < z < 6 (green; E. Pouliasis et al. 2024). Right: the fraction of non-LRDs (black curve; model) and observational constraints on the fraction (95% confidence level) derived from a sample of 62 broad-line AGNs (blue symbol; A. J. Taylor et al. 2025a).
Paper: Little Red Dots as the Very First Activity of Black Hole Growth
Authors: Kohei Inayoshi
Figure caption: Left: the occurrence rate of LRDs as a function of cosmic time (bottom x-axis) and redshift (top x-axis). The histogram, based on the data from D. D. Kocevski et al. (2025), shows 341 photometrically selected LRDs (blue), including 39 with spectroscopically confirmed redshifts (green). The colored bars indicate the redshift range where the 4000 Å break falls within the bandpass of each wide-band filter. The photometric selection of z > 9 LRDs becomes incomplete (gray shaded region). The magenta curve represents the best-fit function with a log-normal distribution, while the gray curve shows the case with constant abundance in unit comoving volume for reference. Right: the cumulative number distribution of the observed LRD number (blue) with error bars computed via binomial statistics. The best-fit result obtained using a log-normal distribution is shown (p = 0.873), along with a Gaussian distribution yielding a worse fit (p = 1.17 × 10−4).