adsabs/AstroCLIMB huggingface dataset:
Paper: Can Repeating and Nonrepeating Fast Radio Bursts Be Drawn from the Same Population?
Authors: Paz Beniamini, Pawan Kumar
Figure caption: Key results for the distributions of detectable sources. In all panels solid lines depict PL-distributed variable rates, ﹩P(\geqslant {{ \mathcal R }}_{{\rm{c}}})={({{ \mathcal R }}_{* }/{{ \mathcal R }}_{0,* })}^{-a}﹩, and dashed lines a constant source rate. Top left: number of sources above a given fluence with ≥k repeats. For k > kγ and a(γ − 1) < 3/2, the distribution above Φall,k is dominated by gradually rarer and more active sources. Top right: distance distribution of sources observed ≥k times above a fluence Φ. Bottom left: number of sources observed k times as a function of k. For Φ < Φall,1, the distribution peaks at k such that Φall,k = Φ (﹩k\approx {({{\rm{\Phi }}}_{{\rm{all}},{\rm{1}}}/{\rm{\Phi }})}^{\gamma -1}﹩; dotted line), while at larger k the number declines as described in the text. Bottom right: distances and typical observed activity rate in the parameter space of a (describing the activity rate distribution) and k (number of observed repetitions per source). We also list the dependence of N≥k( > Φ) on k and Φ at the limit of large k and for ﹩{{\rm{\Phi }}}_{{\rm{all}},{\rm{1}}}({{ \mathcal R }}_{{\rm{0}},{\rm{c}}}.)\lt {\rm{\Phi }}\lt {{\rm{\Phi }}}_{{\rm{c}}}﹩. A shaded region marks the range of a favored by the analysis in Section 4.
Paper: The Epoch of Reionization 21 cm Bispectrum at z = 8.2 from MWA Data. I. Foregrounds and Preliminary Upper Limits
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj, Khandakar Md Asif Elahi, Shiv K. Sethi, Akash Kumar Patwa
Figure caption: ∣Δ3(k1, μ, t)∣ for triangles of all possible sizes (k1) and shapes (μ, t) available from this data. Each panel, which shows ∣Δ3(k1)∣ as a function of k1, corresponds to a different shape (μ, t), as indicated by the inset figure in the lower-left corner and detailed in S. Bharadwaj et al. (2019). The top-left and top-right panels, respectively, correspond to the equilateral (μ = 0.55, t = 0.95) and squeezed (μ = 0.95, t = 0.95) triangles for which the results have been shown in Figure 6. The results shown in black solid lines do not incorporate any foreground avoidance (A0+A1+A2+A3). The black dashed lines, k1 = 0.025 Mpc−1 (vertical) and ∣Δ3∣ = 1014 mK3 (horizontal), are shown for reference. The purple dashed lines show Ntri(k1, μ, t), the number of (k1, k2, k3) triangles in each (k1, μ, t) bin.
Paper: Neutron Star–Main Sequence Collisions Robustly Form Dynamically Stable Thorne–Żytkow Objects
Authors: Lauryn E. Williams, Philip Chang, Emily M. Levesque, Thomas R. Quinn
Figure caption: Separation between the center of the MS star and the NS, r (in units of R⊙), over simulation time is plotted in the left column, with ρc of our dTŻOs plotted in the right column. Each line is colored by the progenitor mass, ranging from 5 to 15 M⊙, and each row corresponds to a different type of encounter: direct collision (rp = 0 R⋆, top), envelope disturbance (rp = 0.5 R⋆, middle), and grazing encounter (rp = 1 R⋆, bottom).
Paper: Neutron Star–Main Sequence Collisions Robustly Form Dynamically Stable Thorne–Żytkow Objects
Authors: Lauryn E. Williams, Philip Chang, Emily M. Levesque, Thomas R. Quinn
Figure caption: Frames from our 7 M⊙ MS star merging with the NS: the highest density point, representing the core of the MS star, is indicated by the pentagon, and the NS is indicated by the cross. The color bar denotes the density of the gas. The NS successfully merges with the MS star at t = 3 days (frame e).
Paper: The Epoch of Reionization 21 cm Bispectrum at z = 8.2 from MWA Data. I. Foregrounds and Preliminary Upper Limits
Authors: Sukhdeep Singh Gill, Somnath Bharadwaj, Khandakar Md Asif Elahi, Shiv K. Sethi, Akash Kumar Patwa
Figure caption: Shows how the normalization factor—relating the MABS to the three visibility correlations—varies with ΔU. The solid black curve uses the Gaussian beam approximation (Equation (A2)), while the green markers correspond to normalization computed using the sinc2 beam profile (Equation (A3)).
Paper: Neutron Star–Main Sequence Collisions Robustly Form Dynamically Stable Thorne–Żytkow Objects
Authors: Lauryn E. Williams, Philip Chang, Emily M. Levesque, Thomas R. Quinn
Figure caption: Radial temperature and entropy profiles of our dTŻOs. The top row shows the temperature profiles, and the bottom row shows the entropy profiles, extending from the center of the dTŻO to approximately 20 R⊙, limited by resolution. The flat entropy profile indicates that the dTŻO is fully mixed or has a convective core. The three columns correspond to one of the three encounter types that we modeled: direct collision, envelope disturbance, and grazing encounter(rp = 0, 0.5, 1 R⋆).
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Top: reproduction of Figure 3 of S. Blouin & S. Xu (2022), which shows the accretion rates as a function of cooling age for hydrogen dominated white dwarfs, with the accretion rate for LSPM J0207+3331 added (red star). All stars with only a Ca abundance are represented in black. The typical error bar is represented in the upper-right corner. Bottom: total mass of metals in the convection zone of the DAZ sample in S. Blouin & S. Xu (2022) and LSPM J0207+3331 estimated from the Ca mass and assuming that Ca represents 1.6% of the total mass. The horizontal lines indicate the mass corresponding to a spherical asteroid with radius of 10, 50, 100, and 200 km assuming a density of 2.1 g cm−3. Stars with detailed spectroscopic analysis are colored in blue (GJ 1042, NZ = 4; B. Zuckerman et al. 2003) and yellow (NLTT 43806 = WD 1653+385, NZ = 9; B. Zuckerman et al. 2011).
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Log abundance ratios relative to Si (top) and Fe (bottom) and normalized to solar (K. Lodders et al. 2025) for LSPM J0207+3331 assuming BU and SS. The gray shaded region around solar shows the 95% range of the abundance ratios of main sequence FG stars from N. R. Hinkel et al. (2014). Relative abundances for the bulk Earth, including uncertainties shown by the green shaded region (H. S. Wang et al. 2018), are also plotted for comparison.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Best-fit model spectrum (orange) overlaid on the smoothed (five-point average window) HIRES spectrum (black) of LSPM J0207+3331. The feature at 3630 Å is a detector artifact. For this panel, all the unlabeled lines are Fe. The last panel shows the unsmoothed MagE data with our best-fit model.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Temperature (left) and pressure (right) structure as a function of the optical depth for a hydrogen-rich white dwarf model with Teff = 5000 K and ﹩\mathrm{log}g﹩ = 8.0. Cases explored include no metals and metal abundances between log(Ca/H) = −6 and −10.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Deviations between fitted and the model’s true Teff (top) and ﹩\mathrm{log}g﹩ (bottom) when models with heavy elements are fit using a pure-hydrogen grid, shown as a function of the white dwarf’s true Teff for metal abundances from ﹩\mathrm{log}({\rm{Ca}}/{\rm{H}})=-9.0﹩ to −6.0 for ﹩\mathrm{log}g﹩ = 8.0. The experiment is done using Pan-STARRS grizy and 2MASS JHKs bandpasses.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Spectral energy distribution for a model white dwarf with Teff = 4000 K and ﹩\mathrm{log}g﹩ = 8.0 for various metallicities. The 2MASS JHKs spectral bands are indicated by dashed lines.
Paper: Tracing Planetary Accretion in a 3 Gyr old Hydrogen-rich White Dwarf: The Extremely Polluted Atmosphere of LSPM J0207+3331
Authors: Érika Le Bourdais, Patrick Dufour, Carl Melis, Beth L. Klein, Laura K. Rogers, Antoine Bédard, John Debes, Ashley Messier, Alycia J. Weinberger, Siyi Xu, 偲艺 许
Figure caption: Models covering Hα with He abundances of ﹩\mathrm{log}({\rm{He}}/{\rm{H}})=-2,-1,﹩ and 0 overplotted on the MagE spectrum.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(α) (top) and P(α) (bottom) for λ = 0.8 μm for our HS and SE scenarios with either clear atmospheres (solid lines) or atmospheres containing a band of optically thick water ice clouds around the equator (dashed lines). The peaks in P around α = 40° are due to modeling our water ice cloud particles using Mie theory.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(λ) (top) and P(λ) (bottom) for α = 40° (left) or α = 90° (right) for our modern Earth scenario, centered on the Amazon, with three different views of the clouds rotating throughout one day. The distributions of the clouds for each view can be seen in the inlaid globe plots, where View 1 corresponds to the original Amazon cloud distribution of Figure 2.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(λ) (top) and P(λ) (bottom) for α = 40° (left) or α = 90° (right) for our HS scenario with various distributions of water ice clouds. The P curves show clearer separation than the πFn curves, especially at α = 40°.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(α) (top) and P(α) (bottom) for λ = 0.8 μm for our modern Earth scenario, centered on the Amazon, with three different views of the clouds rotating throughout one day. Small variations between the different views can be seen in both the flux and polarized phase curves.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(λ) (top) and P(λ) (bottom) for α = 40° (left) or α = 90° (right) for our HS and SE scenarios with either clear atmospheres (solid lines) or atmospheres containing a band of optically thick water ice clouds around the equator (dashed lines). Reflection and scattering by the clouds increase both the reflectivity and polarization of the planets at α = 40°, while at α = 90° the clouds increase πFn but decrease P.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(λ) (top) and P(λ) (bottom) for α = 40° (left) or α = 90° (right) for our modern Earth scenario, centered on the Amazon, with surface and cloud distributions taken from MODIS data observed in May (solid green lines) or November (dashed blue lines).
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(α) (top) and P(α) (bottom) for λ = 0.8 μm for our HS scenario with various distributions of water ice clouds. While the flux curves overlap in all cases, the polarized curves show clear differences between the varying distributions.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: Surface (left) and aerosol (right) distributions for our early Mars simulation. The surface was comprised of bare soil (brown), open water (blue), and sea/lake ice and snow (white) based on ROCKE-3D calculations. The properties of the water ice clouds on early Mars were computed for three distinct latitudinal regions (see Section 3.3.3): a North Polar (NP) region (gray), an Equatorial (EQ) region (white), and a South Polar (SP) region (blue).
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: πFn(λ) (top) and P(λ) (bottom) for α = 40° (solid red lines) or 90° (dashed black lines) for our early Mars scenario. Note the strong absorption bands of the atmospheric gases.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: HST/COS CN spectrum showing the C IVλ 1548 line (CIViL⋆) and C IIIλ 977 (COS-Halos) absorption features of the QSO-galaxy pairs and the set in the rest frame of each individual galaxy. The red line in each spectrum represents the continuum flux error. We note that the absorption features for C III are particularly saturated and result in high column density measurements. Specifically for J0950+4831_177_27, this results in a log10NCIII value of 17.59 (as published in J. K. Werk et al. 2013). We include this value in Table 2 but exclude it from Figure 5, as it is the consequence of the Voigt profile having difficulty taking into account the incredibly high saturation. Similar to Figure 1, we see good correspondence over the velocity ranges of absorption; however, just like J. K. Werk et al. (2016), we see that some lines of sight have strong-ion absorption, but no low-ion absorption.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Left panel: HST/COS continuum-normalized (CN) spectrum showing the C IVλ 1548 line (CIViL⋆) and O VIλ 1031 (COS-Halos) absorption features of the QSO-galaxy pairs and the set in the rest frame of each individual galaxy. Right panel: HST/COS continuum spectrum showing the C IVλ 1548 line (CIViL⋆) and Si IIIλ 1206 (COS-Halos) absorption features of the QSO-galaxy pairs and the set in the rest frame of each individual galaxy. QSO-galaxy pair J1619+3342, 113_40 did not have any Si III detection, so we compare C IV to Si IV instead. The red line in each spectrum represents the continuum flux error. Despite overall correspondence between the velocity ranges, the absorption features are detected; we see differences between the component structure of C IV; in some lines of sight, there are impressive alignments in the component structure, while others have some misalignment.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: (a) πFn(λ) (top row) and P(λ) (bottom row) for five cases of our early SE and HS and modern Earth (ME) scenarios as well as our early Mars scenario, with their atmospheres and surfaces containing various heterogeneities. The spectra are plotted at either α = 40° (left column) or α = 90° (right column). (b) Unpolarized (top row) and polarized (bottom row) contrast ratios for the six models of panel (a). These contrast ratios assume the planets are in circular edge-on orbits at 1 au from the star. Also marked are contrast ratio limits of 1 × 10−10, 1 × 10−11, and 1 × 10−12 (dashed gray lines), as well as the preliminary HWO lower limit of 2.5 × 10−11 (dashed black lines). The breaks in some of the Fpol/Fs curves at α = 90° are due to the polarized light changing directions.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Normalized histograms of CIViL⋆ column density (N), Doppler parameter (bD), and Δvsys (the difference between the galaxy systemic redshift and the component velocity centroid) for Si III (green) and C III (pink) in the upper panels and C IV (purple) and O VI (orange) in the lower panels. We note that for the column densities (left panels), 72% of the observations are saturated and are thus lower limits. We also note that the highly saturated C III component observation (noted in Figure 2 and listed in Table 2) is not included in the upper left panel.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: HST/COS CN spectrum showing the C IVλ 1548 line (CIViL⋆), O VIλ 1031 (COS-Halos), and N Vλ 1238 absorption features of QSO-galaxy pair J1016+4706_359_16 et in the rest frame of the galaxy. The red line in each spectrum represents the continuum flux error. For our sample, this is the only line of sight that has a detection feature for these three ions.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: The difference between the galaxy systemic redshift (the assumed “rest” frame) and the velocity centroids as a function of virial halo mass (M200c) for C IV (circles), O VI (diamonds), Si III (squares), C III (hexagons), and H I (x’s) for each Voigt profile fitted component. The various curved lines show the mass-dependent escape velocities at Rproj = 50, 100, and 150 kpc. We find that most of the component ion velocities do not exceed the escape velocities of the galaxies. Therefore, we conclude that most of the ions, but especially C IV and O VI, are bound to the dark matter halos of their host galaxies.
Paper: Polarized Signatures of Variable Worlds: Modeling Heterogeneous Habitable Earth- and Early Mars-like (Exo)planets
Authors: Kenneth E. Goodis Gordon, Theodora Karalidi, Kimberly M. Bott, Connor J. Vancil, Maxwell A. Millar-Blanchaer, Nicholas F. Wogan, Eric T. Wolf
Figure caption: Ps(α) for our early Mars model at λ = 0.5 μm compared to archival observations of the polarization of modern Mars with a clear (at λ = 0.51 μm; blue diamonds) or dusty (at λ = 0.52 μm; black squares) atmosphere. Between α = 20°−25°, the polarization switches from being parallel (for smaller α) to perpendicular (for larger α) to the scattering plane.
Paper: Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos
Authors: Samantha L. Garza, Yakov Faerman, Trystyn A. M. Berg, Jessica K. Werk, Benjamin D. Oppenheimer, Rongmon Bordoloi, Sara Ellison
Figure caption: Visual representation of the number of components for each ion per sight line. The number of components is colored as follows: nondetections are in gray, a singular component is colored red, two components are shown in orange, three components are colored light green, and four components are colored in dark green. We find that for 70% of the sample, C IV has the same number of components as O VI. For 40% of the sample, C IV has the same number of components as Si III and C III.
Paper: The Relation between the Optical Variability Timescale, Magnetic Field of Jets, and Black Hole Spin in Active Galactic Nuclei
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Dingrong Xiong, 定荣 熊, Xiaoling Yu, 效龄 俞, Xiaotong Guo, 晓通 郭, Nan Ding, 楠 丁, Ting-Feng Yi, 庭丰 易
Figure caption: Relations between the amplitude of variability and physical parameters for our sample. (a) Relation between amplitude of variability and jet magnetic field. (b) Relation between amplitude of variability and black hole spin. (c) Relation between the amplitude of variability and jet power. (d) Relation between amplitude of variability and black hole mass. (e) Relation between amplitude of variability and Eddington ratio. Shaded gray colored areas correspond to 1σ confidence bands. The black line is the best fit.
Paper: The Relation between the Optical Variability Timescale, Magnetic Field of Jets, and Black Hole Spin in Active Galactic Nuclei
Authors: Yongyun Chen, 永云 陈, Qiusheng Gu, 秋生 顾, Junhui Fan, 军辉 樊, Dingrong Xiong, 定荣 熊, Xiaoling Yu, 效龄 俞, Xiaotong Guo, 晓通 郭, Nan Ding, 楠 丁, Ting-Feng Yi, 庭丰 易
Figure caption: Relations between damping timescale in the rest frame (τDRW) and black hole mass for our sample. Shaded gray colored areas correspond to 1σ confidence bands. The black line is the best fit.
Paper: FOGGIE. X. Characterizing the Small-scale Structure of the Circumgalactic Medium and Its Imprint on Observables
Authors: Ramona Augustin, Jason Tumlinson, Molly S. Peeples, Brian W. O'Shea, Britton D. Smith, Cassandra Lochhaas, Anna C. Wright, Ayan Acharyya, Jessica K. Werk, Nicolas Lehner, Lauren Corlies, Raymond C. Simons, J. Christopher Howk, John M. O'Meara
Figure caption: Physical properties of an individual clump entrained in an outflow. We find that the overdense structures show up prominently in the temperature and metallicity plots as low-temperature, low-metallicity objects. In the radial velocity plot we find that while both the clump and its surroundings are outflowing, the clump itself is moving against its environment, causing the distinct head–tail structure. The H I is well contained within the clump whereas high-ionization ions like O VI are more spatially extended and most prominent at the edge of the clump.