adsabs/AstroCLIMB huggingface dataset:
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Mass-loss rate surface density maps for carbon-rich (C-type), oxygen-rich (M-type), and combined (M+C-type) stars in galaxies NGC 147 and NGC 185. White arrows indicate the approximate direction toward M31, and the black arrow in the NGC 147 panel shows the approximate direction of the tidal stream, following J. Preston et al. (2025).
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: DHO PSDs (left column) and their corresponding simulated light curves (right column) of the three representative points A, B, and C shown in Figure 5. Left: in each panel, the black solid curves show the model DHO PSDs multiplied by 3, the blue and orange dashed curves show the best-fit Lorentzian components, and the red solid curves show the sum of the two Lorentzian components. The PSD of A can be well fitted by a sum of one narrow Lorentzian component and one broad Lorentzian component. The peak frequency of the narrow component matches the DHO’s natural oscillation frequency (ω0), and peak frequency of the broad component coincides with 1/τdecay. The PSD of B is not well fitted by the two-Lorentzian model, while 1/τperturb coincides with the frequency where the PSD changes slope from low to high frequencies. The PSD of C can be well fitted by a sum of two broad Lorentzian components. The low-frequency component peaks at 1/τdecay, the high-frequency component peaks at 1/τrise, and the dip between the two peaks coincides with 1/τperturb. Right: the simulated light curve of A shows quasiperiodic variability, and appears smooth on short timescales. The simulated light curve of B also appears smooth on short timescales; however, it lacks a regular quasiperiodic pattern in comparison to the light curve of A. The simulated light curve of C exhibits excess variability at short timescales in comparison to the light curves of A and B. The black points overplotted on the simulated light curves represent observed light curves of selected clean sample quasars whose best-fit DHO parameters closely match those of A, B, and C, all of which also have similar values of the long-term variability amplitude (σDHO).
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: Top: the rest-frame distribution of g-band DHO fits in the clean sample. The left panel shows the DHO space of ξ and ω0 (LHS of Equation (3)), and the right panel shows the DHO space of σϵ and τperturb (RHS of Equation (3)), where the color gives the SF slope of each best-fit DHO, as defined by Equation (6). The vertical dashed–dotted line in the left panel divides the parameter space into underdamped and overdamped regions. Underdamped DHOs have an SF slope steeper than that of a DRW (i.e., 0.5); overdamped DHOs with log(ξ) ≲ 0.5 have an SF slope steeper than 0.5, while overdamped DHOs with log(ξ) ≳ 0.5 have an SF slope flatter than 0.5. The median error bars of best-fit DHO parameters are plotted at the bottom right corner of the left panel and the bottom left corner of the right panel. The purple contour shows the distribution of DHO fits in the final overdamped sample of Y22. Bottom: the DHO model SF (blue solid line), the comparison best-fit DRW SF (red dashed line), and the empirical ensemble SF (black point) for three representative points marked as A, B, and C in the top panels. All SFs are normalized to a maximum value of 1 mag. The gray region indicates the noise floor for the input light curve. The DHO SFs follow the empirical SFs better than the DRW SFs.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: χ2 per degree of freedom (﹩{\chi }_{\mathrm{dof}}^{2}﹩) distribution for standard star light curves compiled from the SDSS-I Legacy Survey, the SDSS-II Supernova Survey, PS1, and ZTF (Zubercal). The dashed lines show the median of the χ2 distribution computed using the pipeline photometric errors, as a function of the star’s mean magnitude. The solid lines and the shaded regions show the χ2 distribution computed using the recalibrated photometric errors. Recalibration is not performed for SDSS-I photometry.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: The distributions of initial sample, clean sample, and core sample quasars in L3000, FWHMMg II, and log(1 + z). The clean sample and core sample quasars are centered at slightly lower L3000 than those in the initial sample, but their FWHMMg II distributions appear comparable. The modest shift in L3000 for the clean sample and core sample can be attributed to the τdecay-based cut, which preferentially excludes high-redshift quasars (and thus higher-luminosity sources) due to the redshift-dependent contraction of the rest-frame baseline. This effect is also illustrated in the ﹩{\mathrm{log}}\,(1+z)﹩ distributions.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: A comparison between the DHO parameters inferred from the full light curves with a 22 yr baseline (x-axis) and those inferred from light curves with shortened baselines (y-axis). The blue, green, and red contours show the distributions (80 percentile) of DHO parameters inferred from light curves with 5, 10, and 15 yr baselines, respectively. The inferred σDHO and τdecay decrease systematically with a decreasing baseline, while σϵ and τperturb do not show systematic shifts with a decreasing baseline.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: Three examples of combined SDSS-PS1-ZTF light curves. The ID shown at the bottom left corner of each panel gives the identifier of each corresponding quasar’s SDSS spectrum, in the format of PLATE-MJD-FIBERID.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: Simulated class-C DHO PSDs as a function of λRF, L/LEdd, and MBH. The input DHO parameters are computed using Equation (9), with coefficients provided in Tables 3 and 4. Top: DHO PSDs at log(λRF/Å) = 3.1–3.7 in steps of 0.1 dex, given log(L/LEdd) = −1.0 and log(MBH/M⊙) = 8.0. The variability power decreases as λRF increases, at all frequencies shown. Middle: DHO PSDs at log(L/LEdd) = −2.0–0.0 in steps of 0.4 dex, given log(λRF/Å) = 3.4 and log(MBH/M⊙) = 8, and each PSD is normalized relative to its power at a frequency ≃ 0. The relative short-term variability power decreases significantly with an increasing log(L/LEdd). Bottom: DHO PSDs at log(MBH/M⊙) = 7.5–9.5 in steps of 0.4 dex, given log(λRF/Å) = 3.4 and log(L/LEdd) = −1.0, and each PSD is normalized relative to its power at a frequency ≃ 0. Similar to the middle panel, the relative short-term variability power decreases with log(MBH). The peak frequency of the HF component increases with log(MBH), but we note that our light-curve cadence is not sufficient to robustly constrain this variability feature, so the trend shown could be an artifact.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: A schematic diagram showing the accretion flow geometry (top) and the suggested contributions of different accretion flow components to the PSD of the quasar UV/optical variability captured by class-C DHOs (bottom). Top: a side cross section of the accretion disk, the inner hot accretion flow, and the central SMBH are shown. The blue arrow at the top shows the direction of the inwardly propagating accretion rate fluctuations. The solid arrows coming out of the accretion disk represent the intrinsic disk emission. The dashed arrows hitting and coming out of the accretion disk represent coronal emission reprocessed by the disk. Bottom: in the PSD, the low-frequency bump (red) owes to intrinsic variability from the accretion disk, while the high-frequency bump (blue) owes to variability from the inner hot flow. In UV/optical wavelengths, one observes both the intrinsic disk variability (solid arrows in the top panel) and the reprocessed X-ray variability (dashed arrows in the top panel) associated with the inner hot flow.
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: The temporal evolution of the density (left panel) and temperature (right panel) of CDS. The gray-shaded area in the left panel represents the region in which ﹩{\tau }_{{\rm{coll}}}\gt {\tau }_{{\rm{\exp }}}﹩, suggesting that dust formation is suppressed under these conditions. The red-shaded region in the right panel indicates the area where ﹩T\leqslant {T}_{{\rm{d}},{\rm{\max }}}﹩, representing conditions under which dust formation is possible. After sweeping through the confined CSM, the CDS undergoes rapid adiabatic cooling, causing its temperature to drop sharply from ∼104 K, which can be seen from the right panel. The adopted parameters are finj = 0.3 and tinj = 10 yr (see Figure 3).
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: The wavelength dependence of best-fit parameters of class-C DHOs. The best-fit DHO parameters (y-axis) have been redshifted to the rest frame of their quasars, as well as normalized to log(L3000/[erg s−1]) = 45 and log(FWHMMg II/[km s−1]) = 3.6 using the coefficients reported in Table 3. The green and red contours in each panel give the distribution of the g-band and r-band best-fit DHO parameters in the core sample, respectively. σDHO, τperturb, σϵ, and τperturb exhibit nearly monotonic correlations with λRF. The black points in each panel show the binned average with their error bars estimated through bootstrapping.
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: The expected dust mass formed in the CDS (left panel) and the condensation time of dust τcond (right panel) as a function of tinj for each value of finj.
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: The temporal evolution of the shock velocity, ejecta velocity, shocked mass, and CDS mass. The time at which the shock reaches the transition radius and the outer edge of the CSM is marked by the vertical lines r* and rout, respectively. The subscript rev (for) denotes the mass of the shocked region/CDS on the shocked ejecta (CSM) side. The adopted parameters are tinj = 10 yr and finj = 0.5.
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: Schematic illustration of the interaction between the homologously expanding SN ejecta and the CSM (not scaled). This leads to the instantaneous formation of the CDS (blue-shaded region within the magnified view), where the new dust is expected to form.
Paper: Examining Active Galactic Nucleus UV/Optical Variability beyond the Simple Damped Random Walk. II. Insights from 22 yr Observations of SDSS, PS1, and ZTF
Authors: Weixiang Yu, 伟翔 于, Gordon T. Richards, John J. Ruan, Michael S. Vogeley, Franz E. Bauer, Matthew J. Graham
Figure caption: Trends of clean sample DHO parameters with L3000 and FWHMMg II. We have redshifted the best-fit DHO parameters to the rest frame of their quasars as well as normalized them to log(λRF/Å) = 3.4 (∼2500 Å) using the coefficients listed in Table 3. σDHO, σϵ, and τperturb show clear correlations with both L3000 and FWHMMg II. τdecay shows a weak correlation with FWHMMg II and no correlation with L3000.
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: The expected light curves of dust assuming Td = Tgas for tinj = 3,  4,   ⋯, 15 yr. The dashed line indicates the dust luminosity, which is proportional to ﹩{\mathrm{log}}\,{L}_{{\rm{d}}}\propto -1/{T}_{{\rm{d}}}﹩. The adopted value for finj is 0.3.
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: Example integrations of the inner planet’s eccentricity e1 for two values of the outer planet’s semimajor axis a2, with all other system parameters identical. In each panel, the pink curve shows the solution without GR, and the green curve includes GR. The top panel corresponds to a2 = 0.05 au and the bottom to a2 = 0.25 au. The outer planet mass is set at a value of 20 M⊕. The eccentricity oscillations are larger for the closer outer planet, and in both cases the inclusion of GR suppresses their amplitude.
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: Comparison of the dust light curve with the i,  j, and h band light curves of AT 2017gfo, scaled with the peak luminosity Lpeak. The rising phase, approximated by Equation (28), is indicated by dashed lines. The adopted parameter is finj = 0.3. The light curves of AT 2017gfo are taken from D. Kasen et al. (2017).
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: Comparison of the dust IR luminosity with our model. We assume Td = Tgas when we calculate the upper limit, while Td = 0.5 Tgas for lower limit. Left: blackbody luminosity. Right: IR luminosity integrated over 1.5–4.8 μm. The data were taken from M. Pozzo et al. (2004).
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: Example integrations of the inner planet’s eccentricity e1 for two values of the outer planet’s mass m2 (top panel: m2 = 5 M⊕; bottom panel: m2 = 150 M⊕), with all other system parameters identical and the outer planet semimajor axis set at a value of 0.15 au. Larger outer planet masses lead to higher-frequency eccentricity oscillations. In both cases, the inclusion of GR strongly suppresses the oscillation amplitude, more strongly for smaller masses of the outer planet.
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: Parameter space showing the effect of GR on eccentricity oscillations due to an exterior planetary companion for a variety of combinations of the mass ratio m2/m1 and semimajor axis ratio a2/a1. The interior planet was assumed to be a 1 M⊕ planet at 0.01 au. When ξ < 1 (bottom left, red), GR amplifies eccentricity oscillations; when ξ > 1 (top right, black), GR suppresses them. The dashed line marks the transition as derived in F. C. Adams & G. Laughlin (2006).
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: The plot shows the precession rate for an inner planet a1 perturbed by an exterior companion planet with mass m2 = 10M⊕ at an orbital distance of a2 = 0.1 au. The red curve represents the precession rate due to GR, while the dashed black curve represents the precession rate due to perturbations from the exterior companion. The shaded green region highlights the range corresponding to the CHZ identified in E. Agol (2011).
Paper: Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae
Authors: Yuki Takei, Kunihito Ioka, Masaru Shibata
Figure caption: SEDs of the thermal emission from newly formed dust at several epochs t = 218, 442, 891 days, which correspond to Td = 2000, 1000, 500 K, respectively. The adopted parameters are finj = 0.5 and tinj = 5 yr.
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: Parameter sweep over outer planet mass (m2) and semimajor axis (a2), testing whether a 1 M⊕ inner planet at a1 = 0.01 au orbiting a 0.5 M⊙ white dwarf undergoes a tidal-driven runaway greenhouse, if the runaway greenhouse will onset at the level of tidal heating caused by an orbital eccentricity of e ≈ 10−4. Left panel: a parameter sweep that includes GR apsidal precession. Right panel: an identical parameter sweep but without GR. GR enlarges the stable region (where the inner potentially habitable planet avoids the runaway greenhouse) by suppressing secularly forced eccentricity, whereas without GR nearly all configurations with a2 ≲ 0.18 au trigger a runaway greenhouse. All runs assume e2 = 0.05 and are integrated for 3 × 105 yr.
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: Comparison of REBOUNDx and celmech simulations, showing their agreement for integrations run both with and without GR. The initial conditions for both the celmech and REBOUND integrations were identical: an Earth-like inner planet at 0.01 au with an outer planet of mass 55.36 M⊕, eccentricity 0.05, and semimajor axis 0.1043 au.
Paper: General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs
Authors: Eva Stafne, Juliette Becker
Figure caption: Maximum eccentricities of an inner planet with varying outer planet parameters. The contour shows a runaway greenhouse effect cutoff of e = 10–4.
Paper: The Parallel Ionizing Emissivity Survey (PIE). I. Survey Design and Selection of Candidate Lyman Continuum Leakers at 3.1 < z < 3.5
Authors: Alexander Beckett, Marc Rafelski, Claudia Scarlata, Wanjia Hu, Keunho Kim, Ilias Goovaerts, Matthew A. Malkan, Wayne Webb, Harry Teplitz, Matthew Hayes, Vihang Mehta, Anahita Alavi, Andrew J. Bunker, Annalisa Citro, Nimish Hathi, Alaina Henry, Alexandra Le Reste, Alessia Moretti, Michael J. Rutkowski, Maxime Trebitsch, Anita Zanella
Figure caption: Expected transmission of the IGM at z = 3.1 and z = 3.5, using the method from R. Bassett et al. (2021). Left panel: median IGM transmission as a function of observed wavelength (solid line). The dashed lines outlining the shaded regions show the 10th and 90th percentiles, and the F336W filter throughput is also shown in black. Vertical dashed lines also indicate the Lyman limit and the wavelength of Lyα for both redshifts. Top-right panel: histogram of average IGM transmission through the F336W filter for each of the 10,000 simulated sight lines, showing the fraction of mock sight lines in each bin of TIGM. Bottom-right panel: cumulative histogram of TIGM, showing the fraction of sight lines more transparent than the given value.
Paper: The Parallel Ionizing Emissivity Survey (PIE). I. Survey Design and Selection of Candidate Lyman Continuum Leakers at 3.1 < z < 3.5
Authors: Alexander Beckett, Marc Rafelski, Claudia Scarlata, Wanjia Hu, Keunho Kim, Ilias Goovaerts, Matthew A. Malkan, Wayne Webb, Harry Teplitz, Matthew Hayes, Vihang Mehta, Anahita Alavi, Andrew J. Bunker, Annalisa Citro, Nimish Hathi, Alaina Henry, Alexandra Le Reste, Alessia Moretti, Michael J. Rutkowski, Maxime Trebitsch, Anita Zanella
Figure caption: Color and magnitude offsets between the mock input catalog and the SEXTRACTOR measurements on the mock images, with sources curated as described in Section 5.2. Field 51 (medium-depth) is shown, but results are similar for the other mock fields. Left panel: magnitude offsets in the three PIE filters. Middle panel: color offsets in the two colors used for our primary selection of high-redshift galaxies. Right panel: F625W − F814W color offsets using sources above different signal-to-noise thresholds. The median of each distribution is shown by a vertical line. The median and spread of the distribution are given in Table 3.
Paper: The Parallel Ionizing Emissivity Survey (PIE). I. Survey Design and Selection of Candidate Lyman Continuum Leakers at 3.1 < z < 3.5
Authors: Alexander Beckett, Marc Rafelski, Claudia Scarlata, Wanjia Hu, Keunho Kim, Ilias Goovaerts, Matthew A. Malkan, Wayne Webb, Harry Teplitz, Matthew Hayes, Vihang Mehta, Anahita Alavi, Andrew J. Bunker, Annalisa Citro, Nimish Hathi, Alaina Henry, Alexandra Le Reste, Alessia Moretti, Michael J. Rutkowski, Maxime Trebitsch, Anita Zanella
Figure caption: The locations of the PIE fields on the sky. Fields are divided into shallow (<2 hr), medium (2–4 hr), and deep (>4 hr), based on the usable F336W exposure time. Fields for which the PIE+ program contributed F475W observations are also circled in black. Regions within 10∘ of the galactic plane are shaded, as the extinction is generally too high in these regions for our UV observations to be useful.
Paper: The Parallel Ionizing Emissivity Survey (PIE). I. Survey Design and Selection of Candidate Lyman Continuum Leakers at 3.1 < z < 3.5
Authors: Alexander Beckett, Marc Rafelski, Claudia Scarlata, Wanjia Hu, Keunho Kim, Ilias Goovaerts, Matthew A. Malkan, Wayne Webb, Harry Teplitz, Matthew Hayes, Vihang Mehta, Anahita Alavi, Andrew J. Bunker, Annalisa Citro, Nimish Hathi, Alaina Henry, Alexandra Le Reste, Alessia Moretti, Michael J. Rutkowski, Maxime Trebitsch, Anita Zanella
Figure caption: Average density of galaxies in the PIE fields. We show only fields observed in F814W and F625W with the PIE program (as PIE+ data is usually at a different orientation, affecting the overlapping area), split into fields with half-orbit and full-orbit depth in F625W. Also included are the densities of F606W sources from the UVUDF galaxy catalog presented in M. Rafelski et al. (2015) and the fit to several galaxy surveys given by S. Koushan et al. (2021). For comparison, the vertical dashed lines show the typical 5σ depth of half-orbit and full-orbit F625W exposures, as presented in Table 1.