adsabs/AstroCLIMB huggingface dataset:
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Distributions of different properties in our sample. The dashed line denotes the median. (a) Distribution of the redshift of the sample objects. (b) Distribution of the black hole mass. (c) Distribution of the Eddington ratio. (d) Distribution of the GTI of each observation. (e) Distribution of the 0.3–10 keV net photon counts. (f) Distribution of the 0.3–10 keV luminosity.
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Distribution of the photon index, black hole mass, and Eddington ratio of each source in different time-averaged spectral subgroups. The vertical dashed lines represent the average values.
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Connection of the rms spectrum and the time-averaged spectrum. Left panel: distribution of the time-averaged spectral classification in different LF rms subsamples. Middle panel: distribution of the time-averaged spectral classification in different HF rms subsamples. Right panel: distribution of the LF rms classification in different HF rms subsamples.
Paper: A Systematic Study of the Short-term X-Ray Variability of Seyfert Galaxies. I. Diversity of the X-Ray rms Spectra
Authors: Jingwei Hu, Chichuan Jin, Huaqing Cheng, Weimin Yuan
Figure caption: Distribution of the photon index, black hole mass, and Eddington ratio of each source in different rms spectral subgroups. The vertical dashed lines represent the average values. The LF rms subgroups are shown in black lines, and the HF rms subgroups are shown in red lines.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: The correlations between the stellar mass overdensity δ 0.5Mpc and halo mass M  h  (Lim et al. 2017) as a function of M ⋆ and ΔSSFR. The ρ value in each panel is the Spearman correlation coefficient for the indicated M ⋆ range and ΔSSFR class. For guidance, the dashed lines mark the median values of δ 0.5Mpc and M  h  for starbursts; they are same for all the panels in a given M ⋆ range. The orange point denotes the median values of δ 0.5Mpc and M  h  for a given panel. Generally, δ 0.5Mpc shows a moderate (ρ ≈ 0.4–0.7) correlation with M  h . The strength of the correlation decreases as M ⋆ increases or as ΔSSFR increases, from QGs to starbursts. The contours represent the number density of the galaxies. The plumes of points in the upper right corners of the panels are mainly satellites. Centrals occupy the horizontal contours at low M  h . Their distribution shifts leftward and downward as M ⋆ decreases, as expected from the M ⋆–M  h  relation.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: Similar to Figure 4, but here the cumulative distributions of the tidal parameter of the five nearest neighbors (Q 5) and the projected distance to the nearest neighbor (r  p,1) are shown. The Q 5 and r  p,1 of starbursts are slightly lower than those of SFMS galaxies, and are much lower than those of green-valley galaxies and QGs. Note that ∼10%–15% of the starbursts have Q 5 > −2 or nearby neighbors within r  p,1 < 0.1–0.2 Mpc, with only ∼2%–3% enhancement compared to SFMS galaxies. About 55%–60% of Q 5 is contributed by the nearest neighbor.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: Comparing the cumulative distributions of the mass densities δ 0.5Mpc and δ 1Mpc of QPSBs to those of starbursts, SFMS galaxies, and QGs. Depending on M ⋆, the 0.5–1 h −1 Mpc scale environments of QPSBs are similar to or slightly lower than those of starbursts, but they are quite different from the environments of QGs. As shown in panel (a), QPSBs and starbursts do not necessarily have similar δ 0.5Mpc distributions. This can be understood if only a subset of starbursts become QPSBs; the number of starbursts is much higher than QPSBs. The environments of AGNs with Hδ  A  > 4 Å are similar to upper-SFMS galaxies.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: The cumulative distributions of the halo mass (M  h ) estimates from (Lim et al. 2017; panels (a) and (b)) and (Tinker 2021; panels (c) and (d)) for galaxies grouped by M ⋆ and ΔSSFR. Both M  h  estimates indicate that ∼90% of starbursts have M  h  < 1013 h −1 M ⊙, which is a significantly higher percentage than that for QGs below this halo mass. However, the two estimates disagree on the trends of M  h , with ΔSSFR below M  h  ≲ 3 × 1012 h −1 M ⊙.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: The ECDFs of the fifth-nearest neighbor overdensity (δ 5) and tidal parameter (Q 5) of QPSBs and AGNs with Hδ  A  > 4 Å are compared with starbursts, other SFGs, and QGs. The distributions of δ 5 and Q 5 of QPSBs and AGNs with Hδ  A  > 4 Å are more similar to those of SFGs than to those of QGs.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: The correlations between the stellar mass overdensity δ 0.5Mpc and halo mass M  h  for satellites and centrals. Panel (a) uses the Lim et al. (2017) measurements of M  h  and central/satellite classification, whereas panel (b) uses the Tinker (2021) measurements. The ρ values are the Spearman correlation coefficients.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: Similar to Figure 2, but here the cumulative distributions of the normalized fifth-nearest neighbor number densities (δ 5) are shown. The δ 5 of the starbursts are slightly lower than those of normal SFGs, but they are much lower than those of green-valley galaxies and QGs.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: Comparing the mean percentages of the starbursts that are isolated, in pairs, in groups with m = 3 − 6 members, in rich groups (m > 6 and σ < 400  km s−1), and in clusters (m > 6 and σ > 400 km s−1) with their counterparts in SFMS galaxies and QGs. The error bars denote the 95% multinomial confidence intervals.
Paper: Quenching in the Right Place at the Right Time: Tracing the Shared History of Starbursts, Active Galactic Nuclei, and Poststarburst Galaxies Using Their Structures and Multiscale Environments
Authors: Hassen M. Yesuf
Figure caption: Similar to Figure 9, but here the fractions of QPSBs and Hδ  A  > 4 Å AGNs that are isolated, in pairs, in groups, or in clusters are shown to be similar to the corresponding fractions of starbursts.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: The mass distribution of the cool phase in the metallicity (Z) and vertical velocity (v  z ) plane (first and third columns) and the ICM mass fraction ﹩{f}_{\mathrm{ICM}}^{}﹩ and vertical velocity (v  z ) plane (second and fourth columns) over z = 1–2 kpc. We consider two epochs at early times t = 260–280 Myr (left two columns) and late times t = 360–380 Myr (right two columns). From top to bottom, we show the models in ascending order of the ICM pressure, ICM-P1, ICM-P3h, ICM-P7h, and ICM-P14. As a reference, we show the mass distribution of the noICM model in the the first and third columns as contours. In the second and fourth columns, we plot a linear relation between ﹩{v}_{z}^{\mathrm{cool}}﹩ and ﹩{f}_{\mathrm{ICM}}^{\mathrm{cool}}﹩ (Equation (7)). This can be translated into a linear relation between ﹩{v}_{z}^{\mathrm{cool}}﹩ and Z using Equation (6) (assuming ﹩{f}_{\mathrm{SN}}^{}=0﹩) as shown in the first and third columns.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Outward fluxes of each phase through z = 3 kpc for the strong ICM models (top: ICM-P7h; bottom: ICM-P14) normalized by injected fluxes (by ICM and SNe). Colors of lines and symbols denote different thermal phases: blue for cool, orange for intermediate, and red for hot. The points denote the center of the time bin over which the time-averaged outward flux (selecting only gas with v  z  > 0) is calculated using Equation (18), with Equation (11) for mass flux, Equation (12) for momentum flux, and Equation (13) for energy flux (neglecting the Poynting flux term). The injected ICM fluxes are similarly calculated at z = −3 kpc for the gas with v  z  > 0. In the ICM-P7h model (top), the outflow rates are more or less constant over time, with significant mass carried out by the cool phase, while the hot phase dominates energy flux. In contrast, the ICM-P14 model shows a gradual decrease of the outgoing fluxes of the cool phase as the hot phase continuously shreds and entrains the cool phase in the hot outflows.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Left: time evolution of (a) SFR surface density ΣSFR (Equation (19)) and (c) dense gas surface density Σdense ≡ Σgas(n H > 10 cm−3). The colored solid lines correspond to the models with the different ICM pressure, while the black dashed line is the noICM model. Right: box-and-whisker plots of (b) ΣSFR and (d) Σdense for early (t < 330 Myr) and late (t > 330 Myr) periods. Boxes include 25th to 75th percentile with median (white dashed horizontal line) and mean (red circle). Whiskers represent 5th to 95th percentile, with outliers shown as diamonds.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Soft X-ray surface brightness, ﹩{{ \mathcal S }}_{X,0.3-2\,\mathrm{keV}}﹩, as a function of SFR surface density in the past 40 Myr, ΣSFR,40. The ICM models presented in this paper are shown as colored points, while the TIGRESS suite results (C.-G. Kim et al. 2022, in preparation) are shown as gray points, with their mean values as black circles for reference. The two diagonal dashed lines denote the SN to soft X-ray efficiencies of ﹩{\epsilon }_{\mathrm{SN}\to {\rm{X}}}=1﹩% and 0.1%. The horizontal dotted lines are for the ICM to soft X-ray conversion efficiency ϵ ICM→X of 0.05% for the given ICM total energy flux.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Term-by-term decomposition of energy change rate (see Equation (17)) for the ICM-P7h model. We show the decomposition of (a) the net energy change rates per unit area into (b) the time-dependent term, (c) flux term (Equation (13)), (d) source term (only in the hot phase), (e) sink term by cooling, and (f) sink term by gravity. Noisy, checkerboard-like patterns below the ICM−ISM interface depict the nonconservative errors of the analysis, mainly due to significantly time-varying fluxes. The majority of the energy flux transferred from hot to intermediate and cool phases is lost through cooling.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Top: vertical position at which new star clusters are born. The size of each symbol represents the mass of the star cluster. Bottom: metallicity of new star clusters colored by the star formation position. Star clusters with significantly low metallicity are marked by black dotted circles in both panels.
Paper: Nature and Scalings of Density Fluctuations of Compressible Magnetohydrodynamic Turbulence with Applications to the Solar Wind
Authors: Xiangrong Fu, Hui Li, 晖 李, Zhaoming Gan, Senbei Du, John Steinberg
Figure caption: Run 1: β 0 = 1.0, (a) time evolution of the magnetic field, velocity field, and density fluctuations. The fluctuation level saturates after about t = 50 when the system enters into a quasi-steady state; (b) time evolution of cross helicity σ  c , and Alfvén ratio r  A . Run 4: β = 0.2, (c–d) Similar to panels (a–b) but for Run 4 with β 0 = 0.2.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Outflow metallicity measured at z = 3 kpc for the (a) weak and (b) strong ICM models. Colors of lines and symbols denote different thermal phases: blue for cool, orange for intermediate, and red for hot. The same noICM points are repeated in both panels.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Morphological classifier in sparse-flavor SFFT demonstrated by an arbitrary DECam image of Legacy Survey (Blum et al. 2016). The classifier is based on the photometric results of the image using SEXTRACTOR. The data points show the relationship between instrumental magnitude (SEXTRACTOR catalog value MAG_AUTO) and flux radius (SEXTRACTOR catalog value FLUX_RADIUS) for the detected objects with SEXTRACTOR catalog value FLAG being zero. We also group the data by the morphological types in the Tractor catalog of Legacy Survey (Blum et al. 2016) shown with different markers in the figure. The dashed black line is detected by Hough transformation as the strongest straight line feature with vertical orientation. Two dotted lines are parallel to the dashed line with fixed separation being 0.2 (SFFT parameter BeltHW), the region between that is referred to as the point-source belt.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Analysis of flux residuals of the ZTF test. The second row and third row show thumbnail images of the selected five samples from the SFFT difference and ZOGY difference, respectively. From left to right, thumbnail images are sorted by the sample labels shown in Figure 3. For each thumbnail image, the flux integral along the y-axis can produce a flux curve as a function of the index of the x-axis. These functions are shown in the first row, denoted by red solid curves for ZOGY and black solid curves for SFFT. In each panel of the first row, the two flux curves have been rescaled with the same factor for the clarity of the display clarity. The green dashed line denoted the flux level of constant zero.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Performance of the image subtraction of the DECam test on the selected sources. The panels are arranged as in Figure 7 but show the subtraction results on the set of preselected individual sources. Each panel shows a synthetic image that combines thumbnail cutouts of 64 sources from the original images. The presented samples are drawn from the brightest end of the complete selection, and the thumbnails in the four panels are placed in order of decreasing brightness.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Image subtraction performance of the DECam test from the DECamERON survey. The upper panel shows the input reference image DECam-SREFand science image DECam-OBS02f. The lower panel shows the resulting difference image by SFFT (left) and HOTPANTS (right). The full field of view of DECam is too large for display, so here we only present them in a narrow view of a 3′ width.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Image subtraction performance of the ZTF test around the galaxy center of M31. The panel descriptions are the same as those in Figure 2, however, in a close-up view of the region enclosed by the red square in Figure 2. In each panel, the solid black squares mark five field stars to be checked in detail as shown in Figure 4.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Image subtraction performance of the AST3-II test with observations of the LMC center. The figure, from left to right, shows the input reference image AST-REF, science image AST-SCI, and the resulting difference image by SFFT. The red dashed square at the center of the image indicates a known RRAB variable TY Dor (R.A. = 05:24:06.35 decl. = −69:25:11.0) from the VSX catalog (Watson et al. 2006). The vertical strip illustrates the detection readout sections with slightly different gain values.
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Image subtraction performance of the ZTF test with observations covering M31. The upper panel, from left to right, shows the input reference image ZTF-REF and science image ZTF-SCI. The lower panel presents the resulting difference image from SFFT (left) and ZOGY (right), where the ZOGY difference is directly downloaded from ZTF Data Release 3. The red dashed square marks the core region of M31.