adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray Investigation of Possible Super-Eddington Accretion in a Radio-loud Quasar at z = 6.13
Authors: Luca Ighina, Alessandro Caccianiga, Thomas Connor, Alberto Moretti, Fabio Pacucci, Cormac Reynolds, José Afonso, Bruno Arsioli, Silvia Belladitta, Jess W. Broderick, Daniele Dallacasa, Roberto Della Ceca, Francesco Haardt, Erini Lambrides, James K. Leung, Alessandro Lupi, Israel Matute, Fabio Rigamonti, Paola Severgnini, Nick Seymour, Fabrizio Tavecchio, Cristian Vignali
Figure caption: Light curve at 888 MHz, observed frame, of RACS J0320−35 based on the data from the VAST survey. Measurements span a range of ∼2 yr in the observed frame, from 2023 July to 2025 April. The dashed line is the weighted average, while the shaded area represents the 1σ standard deviation (=0.5 mJy beam−1), comparable to the median uncertainty of the measurements (=0.4 mJy beam−1).
Paper: X-Ray Investigation of Possible Super-Eddington Accretion in a Radio-loud Quasar at z = 6.13
Authors: Luca Ighina, Alessandro Caccianiga, Thomas Connor, Alberto Moretti, Fabio Pacucci, Cormac Reynolds, José Afonso, Bruno Arsioli, Silvia Belladitta, Jess W. Broderick, Daniele Dallacasa, Roberto Della Ceca, Francesco Haardt, Erini Lambrides, James K. Leung, Alessandro Lupi, Israel Matute, Fabio Rigamonti, Paola Severgnini, Nick Seymour, Fabrizio Tavecchio, Cristian Vignali
Figure caption: Left: Chandra images (20″ × 20″) of RACS J0320−35 in the energy band 0.5–7 keV. The red cross indicates the optical position of the quasar, consistent with the X-ray source detected in the Chandra image. Right: contour levels of the photon index and normalization parameter derived from the fit of the Chandra observations. Different colors indicate different observation segments, with the filled ellipses showing the contours from all the observations combined. Dashed (solid) lines indicate the 90% (68%) confidence regions.
Paper: X-Ray Investigation of Possible Super-Eddington Accretion in a Radio-loud Quasar at z = 6.13
Authors: Luca Ighina, Alessandro Caccianiga, Thomas Connor, Alberto Moretti, Fabio Pacucci, Cormac Reynolds, José Afonso, Bruno Arsioli, Silvia Belladitta, Jess W. Broderick, Daniele Dallacasa, Roberto Della Ceca, Francesco Haardt, Erini Lambrides, James K. Leung, Alessandro Lupi, Israel Matute, Fabio Rigamonti, Paola Severgnini, Nick Seymour, Fabrizio Tavecchio, Cristian Vignali
Figure caption: LBA-VLBI images of RACS J0320−35 centered at 2.3 (left) and 8.4 (right) GHz. The white cross shows the optical position of RACS J0320−35 from the DES catalog. Contours start at ±3× rms and increase by factors of ﹩\sqrt{2}﹩.
Paper: Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems
Authors: Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg
Figure caption: Trends observed between the cold water vapor reservoir in the inner disk (traced by the 1500/6000 K line flux ratio) and the dust disk radius (left) or inner disk gap location (right). The data are color coded to illustrate the gap depth (darker color indicates a deeper gap), and the symbol size indicates the number of gaps detected in the disk, including at larger radii. Five disks without detected gaps at the current spatial resolution are also included for comparison in gray.
Paper: The Impact of Organic Hazes and Graphite on the Observation of CO2-rich Sub-Neptune Atmospheres
Authors: Haixin Li, Chao He, Sai Wang, Zhengbo Yang, Yu Liu, Yingjian Wang, Xiao'ou Luo, Sarah E. Moran, Cara Pesciotta, Sarah M. Hörst, Julianne I. Moses, Véronique Vuitton
Figure caption: Thermochemical equilibrium of carbon species. The calculations from the CEA code (S. Gordon & B. J. McBride 1994) at 5 mbar and solar C/O ratio, ∼0.577 (K. Lodders et al. 2009), show the dominant carbon-bearing gas (CH4, CO, or CO2) as a function of temperature and metallicity. The shaded region indicates where solid graphite is thermodynamically favored. Red and blue stars mark the experimental conditions for the 500 and 300 K haze samples, both at 2000× solar metallicity. Pie charts illustrate the corresponding initial gas mixtures, composed of CO2 (orange), CH4 (red), N2 (green), H2O (blue), He (gray), and H2 (purple), calculated from CEA without graphite in the list of species. The mean molecular mass of the 500 and 300 K cases are 27.4 and 28.2 g mol−1, respectively.
Paper: The Impact of Organic Hazes and Graphite on the Observation of CO2-rich Sub-Neptune Atmospheres
Authors: Haixin Li, Chao He, Sai Wang, Zhengbo Yang, Yu Liu, Yingjian Wang, Xiao'ou Luo, Sarah E. Moran, Cara Pesciotta, Sarah M. Hörst, Julianne I. Moses, Véronique Vuitton
Figure caption: (a) Transmittance spectra of haze analogs produced at 300 (blue) and 500 K (red), exhibiting rich vibrational absorption bands (e.g., N–H, C–H, C≡N, C=O). Both samples have ∼0.3% concentration of organic haze and share similar spectral features, with subtle differences in band intensity reflecting temperature-dependent composition. (b) Transmittance spectra of graphite pellets at three concentrations (0.008%, 0.016%, 0.03%), showing smooth, broadband absorption with consistent spectral shapes. (Note that graphite pellets were prepared at much lower concentrations due to the higher absorbance of graphite, and higher concentrations would result in saturated spectra.) Small features near 2.9, 5.8, and 6.1 μm may come from absorbed water in graphite structure and/or the byproducts during the commercial production process of graphite (B. L. Mojet et al. 2010; M. Bera et al. 2018), which likely arises from O–H stretching (2.9 μm), C=O stretching (5.8 μm), C=C stretching, or H–O–H bending (6.1 μm) vibrations.
Paper: The Impact of Organic Hazes and Graphite on the Observation of CO2-rich Sub-Neptune Atmospheres
Authors: Haixin Li, Chao He, Sai Wang, Zhengbo Yang, Yu Liu, Yingjian Wang, Xiao'ou Luo, Sarah E. Moran, Cara Pesciotta, Sarah M. Hörst, Julianne I. Moses, Véronique Vuitton
Figure caption: Modeled transit spectra of GJ 1214b including haze and graphite scenarios. Planet mass 8.17 M⊕, radius 2.742 R⊕, and equilibrium temperature ∼596 K are adopted from R. Cloutier et al. (2021). The stellar radius, 0.2162 R⊙, is adopted from A. S. Mahajan et al. (2024). Simulations include a cloud-free atmosphere (cyan), haze analogs produced at 300 (blue) and 500 K (red), graphite-based aerosols (dark gray), and the graphite-based aerosols using 10% of the number density (5 cm−3 volumetric; light gray) overlaid with observational data from L. Kreidberg et al. (2014), E. M. R. Kempton et al. (2023), and E. Schlawin et al. (2024). The upper panel shows the full wavelength range (0.5–15 μm), while the lower panel provides a magnified view of the visible to near-infrared region (0.5–7 μm), emphasizing haze-induced modulations and absorption features. Hazy scenarios suppress molecular absorption bands and introduce new spectral signatures (e.g., at 3.0, 4.5, 4.7, and 6.0 μm). Graphite shows extreme flattening due to its broadband opacity.
Paper: The Impact of Organic Hazes and Graphite on the Observation of CO2-rich Sub-Neptune Atmospheres
Authors: Haixin Li, Chao He, Sai Wang, Zhengbo Yang, Yu Liu, Yingjian Wang, Xiao'ou Luo, Sarah E. Moran, Cara Pesciotta, Sarah M. Hörst, Julianne I. Moses, Véronique Vuitton
Figure caption: Complex refractive indices (n and k) of graphite compared with previous studies. (a) Extinction coefficient k(λ) derived using two approaches: multiconcentration fitting (black) and single-pellet averaging (gray). Prior data sets from A. B. Djurišić et al. (2000, D & L 2000, brown), R. J. Papoular & R. Papoular (2014, P & P 2014, turquoise), and B. T. Draine (2016, D 2016, indigo) are overlaid for comparison, illustrating the wide variation in reported graphite optical constants. (b) Real part of the refractive index n(λ) retrieved via the SKK method. The fit-based result (black) shows better alignment with R. J. Papoular & R. Papoular (2014), while the averaged result (gray) displays a steeper rise. The discrepancies among all data sets reflect differences in material preparation, spectral methods, and analytical assumptions, underscoring the difficulty in constraining graphite’s complex optical properties.
Paper: The Impact of Organic Hazes and Graphite on the Observation of CO2-rich Sub-Neptune Atmospheres
Authors: Haixin Li, Chao He, Sai Wang, Zhengbo Yang, Yu Liu, Yingjian Wang, Xiao'ou Luo, Sarah E. Moran, Cara Pesciotta, Sarah M. Hörst, Julianne I. Moses, Véronique Vuitton
Figure caption: Complex refractive indices (n and k) of haze analogs synthesized at 300 and 500 K. (a) Extinction coefficient k(λ) retrieved from transmittance data using the Beer–Lambert relation. Both samples exhibit multiple absorption peaks associated with vibrational modes of organic functional groups. A dominant peak near 6.2 μm is present in both spectra, with k values diverging beyond 7 μm. (b) Real part of the refractive index n(λ) derived via the SKK method. A pronounced dip near 6 μm corresponds to the k peak, while small but consistent differences between the 300 and 500 K samples appear across the spectrum.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Left panel: V-band surface brightness profile at 12 Gyr. Only stellar objects with masses above 0.559 M⊙ are included, corresponding to B-band instrumental magnitudes brighter than −10, consistent with the quality cuts applied in R. P. van der Marel & J. Anderson (2010). Their data are shown as green diamonds. Round symbols in black are a compilation of ground-based observations from S. C. Trager et al. (1995). An extinction factor of Av = 0.372 is applied to our data (W. E. Harris 1996). The dashed lines are models that were evolved with a time-varying tidal tensor representative of ω Cen’s orbit for the last Gyr. Middle panel: proper motion velocity dispersion profile at 12 Gyr shown as points. Lightly shaded lines correspond to profiles between 11.9 and 12.1 Gyr. Only stellar objects with 13.9 < mF625W < 24 are included, consistent with the magnitude cuts in M. Häberle et al. (2024a). The errors are computed as ﹩\sqrt{{\sigma }^{2}/(2N)}.﹩ Right panel: we further limit the stellar population to stars with mF625W < 19, and follow a similar binning procedure as detailed in L. L. Watkins et al. (2015), with the caveat that we exclude stars in the inner arcsecond.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Left: comparison of tidal disruption rates per crossing time for our Monte Carlo simulations (black), previous Monte Carlo results of S. Umbreit et al. (2012, blue), and direct N-body model of H. Baumgardt et al. (2004, purple). Our models show the average and standard deviation across five realizations of the model, while the previous Monte Carlo work was averaged over nine models. The disruption rates and errors of the N-body results are time averages and standard deviations, respectively. Right: example number density profile for one of the single-mass component models. A density cusp with a power-law slope of γ = 1.75 forms after 300 Myr, in agreement with theoretical predictions (J. N. Bahcall & R. A. Wolf 1976).
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Main-sequence stars with projected 2D speeds greater than 62 km s−1. The initial sample (shown as black circles) is filtered to include only stars with 13.9 < mF625W < 24  (shown as colored circles), consistent with the observed stellar population in M. Häberle et al. (2024a, shown as purple stars). The empty circles indicate stars that are remnants of a binary disruption. The shaded gray region shows the 1″ uncertainty in the cluster center.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Top panel: distribution of BH masses formed from stellar collapse (dashed) and masses of inspiraling BHs (shaded). Bottom panel: BH capture rate as a function of time.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Top panel: distribution of stellar masses involved in TDEs for two time intervals, shown at 0.5 ± 0.5 Gyr (dashed lines) and 12 ± 0.5 Gyr (shaded). Bottom panel: TDE rate as a function of time. Tidal disruptions of both components of a binary are counted as separate events.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Distribution of penetration parameters (β) for TDEs. Here, we consider only TDE events involving single stars where the disruption occurred outside of the Schwarzschild radius. In a dashed line we show the theoretical prediction from the full loss cone (e.g., A. P. Lightman & S. L. Shapiro (1977) ; N. C. Stone & B. D. Metzger 2016).
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: The time evolution of the mass density power-law indices for the stellar (top panel) and BH (bottom panel) populations, fitted in the range [0.001–1] pc.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Example RW trajectories from our loss-cone treatment, shown in dimensionless specific energy vs. dimensionless specific angular momentum (where Jc is the specific angular momentum of an orbit at a given energy). Red dots indicate TDEs.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Upper panel: the mass of the BH seed as a function of time. Lower panel: the cumulative mass accreted from TDEs (inspirals) in dashed (solid) lines.
Paper: Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems
Authors: Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg
Figure caption: Compilation of pebble mass flux vs. time evolutions. Solid lines show models developed in this study for various gap positions (see Section 3.1), which can be compared to mass fluxes required in pebble accretion simulations to form diverse inner planetary systems (dashed area; see M. Lambrechts et al. 2019) and the pebble mass flux inferred for the inner solar system using models capable of matching the non-carbonaceous (NC) and carbonaceous (CC) chondrite isotopic dichotomy (red dashed; see T. Lichtenberg et al. 2021). Symbols show ages and cold water masses of all 21 objects in our sample computed from JWST/MIRI line ratios (Table 1) in combination with Equation (4) (see Appendix A), and the left and right y-axes are related through Equation (3). Symbol color corresponds to inner gap position as obtained from high-spatial-resolution ALMA observations (see Section 2), and error bars reflect uncertainties in measured line ratios.
Paper: Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems
Authors: Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg
Figure caption: Inspired by the model series in A. Banzatti et al. (2025; shown in blue and red for different values of the hot water emitting radius RH and temperature power-law index α) and additional multicomponent slab models presented in Appendix A (gray points), we employ an empirical relation (Equation (4), shown in green) to convert cold water masses (bottom x-axis) to 1500/6000 K line ratios. Gold stars show ﹩{M}_{{{\rm{H}}}_{2}{\rm{O}}}^{{\mathrm{cold}}}﹩ for seven objects as obtained by C. E. Romero-Mirza et al. (2024) through fitting the entire rotational part of the water spectrum against line ratios for the same objects as reported in A. Banzatti et al. (2025).
Paper: Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems
Authors: Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg
Figure caption: Similar to Figure 3 but for alternative scenarios (see Table 2) in which: drift is more rapid (top row), gaps are leakier (second row), gaps appear later (third row), or gaps are indiscriminate, i.e., the reduction in snowline pebble flux does not depend on the gap’s location (bottom row).
Paper: Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems
Authors: Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg
Figure caption: Results for our fiducial model series described in Section 3.3. (A) Collection of pebble drift models in disks with gaps appearing at different times and positions (see Section 3.3). For every model, a single time between 0.5 < tage/Myr < 2 is selected at random (shown by the small dots). (B) H2O 1500/6000 K diagnostic ratio for every model in panel (A) at their respective tage, calculated from the pebble mass flux using Equations (3) and (4). Gold stars show data from Table 1.
Paper: Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems
Authors: Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg
Figure caption: Left: same as the right panel in Figure 1 but including target names for reference. Right: using the radial location of the deepest gap in each disk rather than the innermost gap.
Paper: Growing the Intermediate-mass Black Hole in Omega Centauri
Authors: Elena González Prieto, Carl L. Rodriguez, Tomás Cabrera
Figure caption: Proper motion velocity dispersion (left) and V-band surface brightness (right) profiles at 12 Gyr. The Elson profile corresponds to the model presented in the main text with a BH seed of 5000 M⊙, while the King model has identical initial conditions but uses a King profile with concentration parameter w0 = 8. Observational data are the same as those shown in Figure 1.
Paper: Solar Disk Gamma-Ray Emission via Synthetic Magnetic Field from Photosphere to Low Corona
Authors: Eleonora Puzzoni, Federico Fraschetti, József Kóta, Joe Giacalone
Figure caption: Top panel: average angle 〈θ〉⊥ (in degrees) as a function of the altitude z with σ2 = 10. Bottom panels: magnetic field lines (in black) and magnitude (color bar) in the xz-plane (lowest y = 0.0003 R⊙ plane in the grid, left panel) and xy-plane (lowest z = 0.0003 R⊙ plane in the grid, right panel) with σ2 = 10.
Paper: Solar Disk Gamma-Ray Emission via Synthetic Magnetic Field from Photosphere to Low Corona
Authors: Eleonora Puzzoni, Federico Fraschetti, József Kóta, Joe Giacalone
Figure caption: Left panel: ratio Nint/Ninj (Nesc/Ninj) for the interacting (escaping) GCRs marked by the solid (dashed) lines as a function of σ2 for injection at z = zup and z = zdown for 100 GeV (red and magenta lines, respectively) and 10 TeV (blue and black lines, respectively) GCRs. Right panel: same as Figure 2, lower left panel, with color scale showing the gyroradius of 10 TeV GCRs with magnetic field lines (in white).
Paper: Solar Disk Gamma-Ray Emission via Synthetic Magnetic Field from Photosphere to Low Corona
Authors: Eleonora Puzzoni, Federico Fraschetti, József Kóta, Joe Giacalone
Figure caption: Magnetic field magnitude in the 3D domain (with logarithmic color scale in Gauss) together with the decomposition of the particle velocity vector defined by the angles θ and ϕ. The xy-plane is tangent to the solar surface, and the z-axis is parallel to the local radial direction.
Paper: The Effect of Stellar Magnetic Activity on Measurements of Morning and Evening Asymmetry of Planetary Terminator
Authors: N. Kostogryz, A. I. Shapiro, L. Carone, L. Gizon, Ch. Helling, S. Kiefer, S. Mercier, S. Seager, S. K. Solanki, Y. Unruh, J. de Wit, V. Witzke
Figure caption: Asymmetry of the transit light curve caused by the asymmetric spatial distribution of stellar magnetic activity. Panel (a) shows asymmetric light curves (flux normalized to unity outside of the transit as a function of time in arbitrary units) for a planet transiting a star, combined from half-disks with different magnetic activity. The different magnetic activity distributions are represented by lines of different colors: red, blue, and magenta correspond to a quiet eastern half-disk (represented by SSD) and 100, 200, and 300 G magnetization of the western half-disk, respectively. The green line corresponds to 200 G magnetization of the western half-disk and 100 G magnetization of the eastern half-disk. Panel (b) illustrates the difference between the symmetric and asymmetric light curves. The light curve is simulated with a planet-to-star radius ratio of 0.1 and an impact parameter of 0.0 at a wavelength of 0.6 μm. The dashed vertical line in panel (b) indicates the ingress transit depth, while the dotted line indicates the egress transit depth. The figure demonstrates that stellar surface magnetic fields have a pronounced effect on the shape of the transit ingress and egress. An asymmetric distribution of the magnetic field on the stellar disk causes asymmetry in the transit light curves.
Paper: Solar Disk Gamma-Ray Emission via Synthetic Magnetic Field from Photosphere to Low Corona
Authors: Eleonora Puzzoni, Federico Fraschetti, József Kóta, Joe Giacalone
Figure caption: Solar disk average gamma-ray spectrum observed by Fermi-LAT with (purple points) and without (black points) solar flares, from T. Linden et al. (2022), by HAWC (blue line, from A. Albert et al. 2023), and obtained from our simulations, with σ2 = 10 (orange diamonds), σ2 = 1 (in brown), and σ2 = 0.1 (in green). The orange stars represent simulations with σ2 = 10 but with a total magnetic field strength 10 times higher (B0 = 50 G leading to low-photosphere Bmax ∼ 1 kG). A detailed comparison is shown in the zoomed-in inset at the top right. The solid black line represents the estimated (see text for further details) gamma-ray flux considering a 100% efficiency of conversion from GCRs to gamma rays.