adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling Long-term Variability in Stellar-compact Object Binary Systems for Mass Determinations
Authors: Nicholas M. Sorabella, Sayantan Bhattacharya, Silas G. T. Laycock, Dimitris M. Christodoulou, Alessandro Massarotti
Figure caption: The self-lensing pulses of stellar sources with various limb-darkening coefficients. For the compact object, the model assumes a black hole of 10 M ⊙ and an orbital period of 10 days. The stellar companion has a mass of 2 M ⊙ and a radius of 1 R ⊙. The system is viewed edge on (ψ = 0°). Note that an increase in Γ results in an increase in amplification and a more rounded pulse.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage: Evidence for Kinematics Evolution of Broad-line Region
Authors: Sha-Sha Li, Hai-Cheng Feng, H. T. Liu, J. M. Bai, Rui Li, Kai-Xing Lu, Jian-Guo Wang, Ying-Ke Huang, Zhi-Xiang Zhang
Figure caption: The Hα (left) and Hβ (right) results. The left panels are photometric and show each binned light curve, where the photometry is the g (ZTF) merged with B (Lijiang) results. The right panels display the ACF of photometry, the cross-correlation results between each bin and photometry, including the ICCFs (black) and CCCDs (green).
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage: Evidence for Kinematics Evolution of Broad-line Region
Authors: Sha-Sha Li, Hai-Cheng Feng, H. T. Liu, J. M. Bai, Rui Li, Kai-Xing Lu, Jian-Guo Wang, Ying-Ke Huang, Zhi-Xiang Zhang
Figure caption: Same as Figure 7 but for the Hγ (left) and He I (right) results.
Paper: Velocity-resolved Reverberation Mapping of Changing-look Active Galactic Nucleus NGC 4151 during Outburst Stage: Evidence for Kinematics Evolution of Broad-line Region
Authors: Sha-Sha Li, Hai-Cheng Feng, H. T. Liu, J. M. Bai, Rui Li, Kai-Xing Lu, Jian-Guo Wang, Ying-Ke Huang, Zhi-Xiang Zhang
Figure caption: Same as Figure 7 but for the He II results.
Paper: Dependence of the Radio Emission on the Eddington Ratio of Radio-quiet Quasars
Authors: Abdulla Alhosani, Joseph D. Gelfand, Ingyin Zaw, Ari Laor, Ehud Behar, Sina Chen, Ramon Wrzosek
Figure caption: Left: compactness of the detected 1.4 GHz nuclear emission of these RQQs. This is calculated using the 1.4 GHz flux densities provided in Table 5 and defined in Equation (2). As r Edd increases, we find that the nuclear emission becomes less compact, i.e., more diffuse. Middle: spectral index of the “compact” nuclear emission α compact, defined to be emission from regions small enough to be detected in our 4.8 GHz VLBA observation as described in Section 3.2, whose values are provided in Table 5. The low Eddington RQQs have flat spectra, while both high Eddington RQQs have steep-spectrum components. In both the left and middle panels, the vertical line set at r Edd = 0.3 separates low and high Eddington RQQs. Right: spectral index of the compact nuclear emission α compact vs. the 1.4 GHz compactness for the sources detected in our VLBA images. The color bar indicates the Eddington ratio r Edd of the PQ RQQs, with the same color scale used for all three plots. For PG 0050+124, we indicate the properties of the individual components, C1 and C2, observed in this RQQ (Figure 2). We find that the radio properties of the observed RQQs are strongly dependent on their Eddington ratio: as the Eddington ratio of an RQQ increases, its radio nuclear emission becomes increasingly diffuse and has a steeper radio spectrum (Figure 4). These results suggest that radio emission from the accretion disk (compact and flat spectrum) is responsible for a higher fraction of the nuclear radio emission in low Eddington ratio RQQs than in high Eddington ratio RQQs.
Paper: Dependence of the Radio Emission on the Eddington Ratio of Radio-quiet Quasars
Authors: Abdulla Alhosani, Joseph D. Gelfand, Ingyin Zaw, Ari Laor, Ehud Behar, Sina Chen, Ramon Wrzosek
Figure caption: Ratio of the VLBA and VLA 4.8 GHz integrated flux densities ﹩[\tfrac{{S}_{\mathrm{VLBA}}}{{S}_{\mathrm{VLA}}}]﹩ of the surveyed PG RQQs as a function of their Eddington ratio r Edd. The VLA 4.8 GHz flux density came from archival work, listed in Table 1, the upper limits of the VLBA 4.8 GHz flux density of the nondetections are 5 × the image σ given in Table 2, and the VLBA 4.8 GHz flux density of detected sources is given in Table 5. The vertical dashed line indicates an Eddington ratio r Edd = 0.3—AGN with lower values are considered to have low Eddington ratios. A nondetection by the VLBA suggests that ≲10% of the AGN’s total radio emission comes from regions ≲100 pc. Furthermore, for VLBA detections, the fraction of the total 4.8 GHz flux density coming from such small regions decreases as r Edd increases.
Paper: Call and Response: A Time-resolved Study of Chromospheric Evaporation in a Large Solar Flare
Authors: Sean G. Sellers, Ryan O. Milligan, R. T. James McAteer
Figure caption: Left: full-disk solar filtergrams on 2014 October 22 from AIA 1600 Å (top) and 171 Å (bottom) bands. Middle: image of NOAA AR 12192 during the X1.6 flare with RHESSI 40–100 keV 20%, 40%, and 60% contours (multiple colors), IRIS slit-jaw imager and slit FOV (cyan), and EIS raster (white). Right: detail of NOAA AR 12192 to highlight correlation between AIA intensity enhancements and RHESSI HXR footpoints.
Paper: Call and Response: A Time-resolved Study of Chromospheric Evaporation in a Large Solar Flare
Authors: Sean G. Sellers, Ryan O. Milligan, R. T. James McAteer
Figure caption: Example spectral fits from the EIS and IRIS instruments. The top two rows show fits from the EIS instrument, while the bottom two rows show fits from the IRIS instrument. For each instrument, the top row shows fits from a time early in the flare, while the bottom row shows fits from approximately the time of peak HXR emission. For the EIS instrument, spectral windows containing He II λ256.35, Fe XII λ195.12, Fe XVI λ262.98, Fe XXIV λ192.02, and Fe XII λ192.39 are shown left to right. The faint blend with Fe XII λ195.12 is not shown, as the major line dominates the window. For the IRIS instrument, spectral windows containing the C II λλ1334.54, 1335.71 doublet, the Si IV λ1402.81 line, and the Fe XXI λ1354.07 line are shown left to right. In each panel, the vertical line(s) denotes the calculated rest wavelength, while the pink dashed profile shows the profile of a line with the same peak and offset but only thermal and instrumental width, without nonthermal broadening (Equation (1)).
Paper: Call and Response: A Time-resolved Study of Chromospheric Evaporation in a Large Solar Flare
Authors: Sean G. Sellers, Ryan O. Milligan, R. T. James McAteer
Figure caption: Thermal parameters from RHESSI spectral fitting. Top panel: the reference DEM calculated at T = 2 keV (≈23.2 MK) over all fitted intervals and detectors. Second panel: the maximum temperature of the plasma in MK for all fit intervals and detectors. Third panel: the power-law index used to calculate the DEM for all fit intervals and detectors. Fourth panel: the reduced χ 2 per fit interval and detector. The black dashed lines denote the range shown in Figure 7, where nonthermal emission was found.
Paper: Call and Response: A Time-resolved Study of Chromospheric Evaporation in a Large Solar Flare
Authors: Sean G. Sellers, Ryan O. Milligan, R. T. James McAteer
Figure caption: Light curves for GOES (purple line) and RHESSI (blue, orange, and green lines), with EIS raster times overlaid (translucent green blocks), as well as the interval in which RHESSI fits are performed (solid black line) and the interval in which IRIS fits are performed (solid pink line).
Paper: Call and Response: A Time-resolved Study of Chromospheric Evaporation in a Large Solar Flare
Authors: Sean G. Sellers, Ryan O. Milligan, R. T. James McAteer
Figure caption: For Fe XIV λ264.81/λ274.23 the theoretical curve describing the relationship between the intensity ratio of each line, and the electron density Fe XIV. The theoretical curve is formed from the CHIANTI 10.0 atomic database (Dere et al. 1997, 2019).
Paper: Call and Response: A Time-resolved Study of Chromospheric Evaporation in a Large Solar Flare
Authors: Sean G. Sellers, Ryan O. Milligan, R. T. James McAteer
Figure caption: Example spectral fits from detector 6. Top: the 16 s interval with the highest integrated count level within the data set, from 14:06:24 to 14:06:40 UT. The thick black dashed line denotes the energy range fit. Bottom: a sample 16 s interval after the cessation of nonthermal electron injection from 14:17:36 to 14:17:52 UT.
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: Two examples of the PSD results. The best-fitted broken power laws are shown in red solid lines. The other horizontal lines mark the Poisson noise calculated from various method. The cyan solid lines represent the common formula, ﹩{\mathrm{PN}}_{\mathrm{lev}}=2(\bar{x}+\bar{b})/{\bar{x}}^{2}﹩, where ﹩\bar{b}﹩ is the average count rate of the background, and ﹩\bar{x}﹩ is the average count rate of the background-subtracted light curve. The green dotted–dotted–dotted–dashed lines represent the correction of this formula, ﹩{\mathrm{PN}}_{\mathrm{lev}\_\mathrm{cor}}=2{((\bar{x}/\bar{f})+\bar{b})/(\bar{x}/\bar{f})}^{2}﹩, where ﹩\bar{f}﹩ is the mean PSF correction factor. The blue dashed lines represent the arithmetic average of the power over the PSD frequency range of above 2 × 10−3 Hz.
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: Example of the change in the rms spectral over time for the case of NGC 4051. The top panel shows the fractional count rate variability of 0.3–2 keV and 2–10 keV, shown as orange lines and light blue lines, respectively. The middle panel shows the fractional rms in different frequency ranges. The LF (<10−4 Hz) and the HF (10−4–10−3 Hz) are shown in red dotted lines and blue dashed lines, respectively. The bottom panel shows the time-averaged spectrum (black crosses) and absolute rms spectra in the case of LF (red filled dots) and HF (blue filled triangle).
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 0.5–4 h −1 Mpc mass overdensities of starbursts with those of SFMS galaxies and QGs at different M ⋆ ranges. The names of the samples indicate the starting points of the ﹩\mathrm{log}{M}_{\star }﹩ ranges, which span 0.5 dex. For example, M11 denotes ﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=11\mbox{--}11.5﹩. The boxes mark 15%, 50%, and 85% of the mass overdensity distribution at a given scale, and the error bar extends to show the rest of the distribution, ignoring outliers. The dashed line shows the median overdensity for M105: ﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=10.5\mbox{--}11﹩ at a given scale. The small-scale mass overdensities strongly depend on M ⋆. At all M ⋆ ranges, the mass overdensity distributions of starbursts are different from those of SFMS galaxies and QGs at ∼0.5–2 h −1 Mpc scales. At 4 h −1 Mpc scale, they are more similar to distributions of SFMS galaxies than they are 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 cumulative distributions of the normalized environmental mass densities within 0.5 h −1 Mpc (δ 0.5Mpc) and 8 h −1 Mpc (δ 8Mpc) for galaxies grouped into two M ⋆ ranges and ΔSSFR. The δ 0.5Mpc distributions of starbursts are different from those of normal SFGs, and they are narrower and peak at lower densities compared to those of QGs. In contrast, the δ 8Mpc distributions of 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: Visualizing the various environmental indicators. Panel (a): the SDSS galaxy distribution at z = 0.075–0.08. Panel (b): the fifth-nearest neighbor overdensity. Panel (c): the mass overdensity within 1 h −1 Mpc. Panel (d): the mass overdensity within 4 h −1 Mpc. Panel (e): the tidal parameters of the five nearest neighbors. Panel (f): the nearest neighbor distance. The color bars are truncated outside the 5%–95% range of the data.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Horizontally averaged ICM mass fraction in the hot phase (left) and vertical momentum density (=upward mass flux; right) as a function of time for all ICM models. The symmetric plane of the external gravity (z = 0) is indicated by the horizontal dotted lines. The orange dashed line denotes the ICM−ISM interface as defined by ﹩\overline{{f}_{\mathrm{ICM}}^{\mathrm{hot}}}=0.5﹩. Two left- and right-pointing triangles demark the beginning of the early and active stripping stages as defined by the earliest time at which the ICM−ISM interface reaches z = − 500 and 500 pc, respectively.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Net mass change rates per unit area for each phase due to phase transition. The spacetime bin is separated by Δt = 10 Myr and Δz = 400 pc. Mass sink (source) by star formation (SN ejecta) is calculated in each spacetime bin and added (subtracted) to the cool (hot) phase to isolate the gain and loss solely due to phase transition. The dashed lines in each panel show the ICM−ISM interface as defined in Figure 2. The phase transition driven by the ICM shows a general trend (clearer with stronger ICM pressure) described by the gain (loss) of the hot (cool) phase near the ICM−ISM interface followed by the loss (gain) of the cool (hot) phase in the extraplanar region.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Spacetime diagrams of horizontally averaged (a) hydrogen number density n H, (b) outgoing mass flux ﹩\rho {v}_{z}\mathrm{sgn}(z)﹩, (c) turbulent pressure ﹩\rho {v}_{z}^{2}﹩, (d) thermal pressure P, and (e) magnetic pressure P  B  ≡ B 2/(8π) for the noICM model. We only show the evolution during a self-regulated state over t ∼ 250–500 Myr as a reference that can be directly compared with the models with the ICM. The horizontal dotted line demarks the midplane (z = 0).
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 vertical momentum change rates (see Equation (17)) for the ICM-P7h model. We show (a) net momentum change rates per unit area, which is identical to Figure 7(d). There is no explicit source term, while we show (b) the time-dependent term and (f) sink term due to gravity. The flux term is further decomposed into the (c) kinetic, ﹩\rho {v}_{z}^{2}﹩; (d) thermal, P; and (e) magnetic, ﹩{P}_{\mathrm{mag}}-{B}_{z}^{2}/4\pi ﹩, flux terms. The momentum transferred from hot to cool phase is mostly used to provide appropriate support against the increased weight. At later times (active stripping stage), the cool phase gains kinetic 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: Net vertical momentum change rates per unit area for each phase due to phase transition. The spacetime bin is separated by Δt = 10 Myr and Δz = 400 pc. The weight of gas of each phase (only significant in the cool phase) is included as a sink. The dashed lines in each panel show the ICM−ISM interface as defined in Figure 2. Noisy, checkerboard-like patterns below the ICM−ISM interface depict the nonconservative errors of the analysis, mainly due to significant time-varying fluxes. The hot ICM’s momentum flux is transferred to the cool ISM.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Same as Figure 4, but at t = 340 Myr.
Paper: Ram Pressure Stripping of the Multiphase ISM: A Detailed View from TIGRESS Simulations
Authors: Woorak Choi, Chang-Goo Kim, Aeree Chung
Figure caption: Time evolution of (a) total (ICM+ISM) gas surface density, (b) stellar surface density of newly formed stars, and (c) surface density of outflowing gas. Panels (b) and (c) are cumulatively calculated by counting all new stars’ mass and integrating mass fluxes at both upper and lower boundaries from the restart of the simulations. The colored solid lines correspond to the models with different ICM pressure, while the black dashed line is for the noICM model.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: Best-fit Bagpipes galaxy SEDs (dark red) based on the broadband photometric data (red diamonds) with 1σ uncertainties. The x-axis error bars indicate the filter bandwidth. We note that we enforce 5σ cuts on the HST J 125 and H 160 fluxes. The large J-band fluxes, relative to the J 125 fluxes, in EGS 515 and EGS 29337 correspond to shallower ground-based CFHT data (Bielby et al. 2012). The z ph are fixed based on the best EAZY estimates. The nondetections are indicated with 2σ upper limits. We plot the best-fit quasar template SEDs (light blue). Quasars and starbursts are nearly degenerate at the predicted z ph. We can see that a galaxy model is most appropriate for EGS 29337, as expected from Roberts-Borsani et al. (2016) and Stark et al. (2017). We also plot the best-fit dwarf star templates in dark gray, which also show nearly degenerate fits. The inset plots show the EAZY z ph probability distribution in blue. The resulting p(z ph) distribution across 6.5 ≲ z ≲ 8.5 is broad since Y 105 data are not included.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: (Top) Comparison of Bouwens et al. (2021) galaxy vs. point-source fraction. Point sources dominate a larger fraction of the bright end starting at ∼−22 mag. We compare this with the Harikane et al. (2022) galaxy fraction in gray. (Bottom) We compare the best-fit z ∼ 7–8 luminosity functions for the combined, freely fit point sources and galaxies in purple curves against the galaxy-only models by Bowler et al. (2020) and Bouwens et al. (2021) in black and gray: Schechter in solid lines, DPL in dashed lines. The purple squares indicate the combined effective number density. EGS 29337 has been removed from the point-source number density to avoid duplicate counting. Open symbols indicate observed data, and filled symbols indicate upper limits. The curves are shown with 1σ uncertainties.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: Color–color diagram for the target selections from 3D-HST. The targets fall into the area marked by the dashed lines that define the Bouwens et al. (2015) color selection. Our final point sources from Table 1 are shown as red stars. Point sources that do not meet the photometric redshift selection are shown as dark red stars. Spectroscopically confirmed dwarf stars are shown as gray diamonds. We also compare with dwarf star template colors (Burgasser 2014) in gray dots, predicted quasar colors from a composite Sloan Digital Sky Survey (SDSS) quasar spectrum (Pâris et al. 2018) in blue, and simple power-law spectra at β = −1, −2, −3 in green. The strong overlap of known dwarf star colors and our Lyman-dropout sources indicates the need for further follow-up to disentangle the degeneracy.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: HST ACS and WFC3 3 arcsec2 postage-stamp images of the point-source targets shown at 95th percentile fluxes. Spitzer/IRAC images are shown in 6 arcsec2 boxes with 3 arcsec2 box inserts in black. Filter images with no observations are indicated as “No Data.” Since the IRAC CH3 and CH4 fluxes are dominated by noise, they are not included in the analysis.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: The M UV- and redshift-dependent selection probability distribution as determined from our completeness simulation. The plot shows the ratio of color-selected point sources recovered to all input sources as a function of redshift and M UV. The color bar to the right indicates this recovery fraction. At brighter M UV ≲ −21 mag, at least 50% of the simulated color-selected point sources are recovered (blue contour line). At fainter magnitudes, the recovery fraction decreases due to the combined effect of color selection and source detection (gray contour lines at 40% and 75% detection). We also indicate the observed point-source candidates at their respective z ph and M UV (red stars).
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: Contour plots of the best-fit luminosity function parameters. (Left) Combined point-source + galaxy Schechter fits with free parameters. (Right) Combined point-source + galaxy DPL fits with free parameters. The best-fit parameters are indicated in Table 7. One-dimensional histograms of the fit parameters are shown with the 16th, 50th, and 84th percentile values indicated.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: The observed 3D-HST grism spectra in black with the best-fit SpeX templates in red.