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 minimum required orbital inclination to produce a self-lensing pulse for a MS–BH binary, a black widow binary and a NS–WD binary. The largest minimum angle required would be for the NS–WD system as the WD source has a far smaller angular size relative to the MS and the degenerate core counterparts.
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 maximum amplifications produced by a neutron star eclipsing a WD companion as a function of inclination angle for a variety of different orbital periods. We assume a neutron star mass of 1.44 M ⊙, a WD mass of 0.4 M ⊙, and a WD radius of 0.02 R ⊙. We can see that high inclination angles are needed for self-lensing to be observable. Also, shorter orbital periods produce smaller flux increases, but they allow for a greater range of inclination angles that can create an observable self-lensing event.
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 light curves for an example binary system of a sunlike star and a 10 M ⊙ black hole with a 3 day orbital period. Doppler boosting is plotted in orange, ellipsoidal variations in blue, self-lensing in red, and the overall light curve in purple. On the left, we have assumed circular orbits. On the right, we see how the shape of each effect and the overall light curve change for an eccentricity of e = 0.3.
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 effect of ellipsoidal variations on a light curve of a binary system containing a sunlike star and a 10 M ⊙ black hole. The orbital period is 3 days, the orbital inclination is i = 90°, β = 1, and the argument of periapsis ω is set to 90°. As the eccentricity of the system increases, the amplitude of the change in flux increases at periapsis, whereas it slightly decreases at apoapsis.
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 maximum amplification as caused by self-lensing, ellipsoidal variations, and Doppler boosting as a function of orbital period in an example binary system. We assume that the binary is composed of a sunlike star and a black hole of 10 M ⊙ in circular orbits.
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: Optical data from Cygnus X-1 with our best-fit model denoted by the orange curve. This model assumes an orbital period of 5.59 days and argument of periapsis of ω = 306.°6, as found by Miller-Jones et al. (2021). Our best-fit parameters are listed in Table 1, along with the best-fit values determined by Miller-Jones et al. (2021).
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: Line intensities, Doppler velocities, and nonthermal velocities for ions with T < 10 MK, for four rasters beginning at 14:02:39 UT, 14:06:13 UT, 14:09:48 UT, and 14:13:22 UT, corresponding approximately to the pre-flare/early impulsive phase, peak impulsive phase, end of impulsive/beginning of the gradual phase, and after the cessation of nonthermal electron injection, respectively. Each column represents a different ion, with formation temperatures increasing left to right across the figure. The provided scales for each parameter are scaled to be consistent between observed ions and observation times. In the case of Ca XVII, there was no significant nonthermal velocity at 14:02:39 UT, and this panel is left blank. RHESSI 25–50 keV CLEAN imaging contours are overlaid in cyan on all images, corresponding to 5%, 30%, and 70% of the image maximum.
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: Line intensities, line core Doppler velocities, and velocity separation of blue-wing components for ions Fe XXIII λ263.78, Fe XXIV λ255.13, and Fe XXIV λ192.02, for four rasters beginning at 14:02:39 UT, 14:06:13 UT, 14:09:48 UT, and 14:13:22 UT. These times correspond approximately to the pre-flare/early impulsive phase, peak impulsive phase, end of impulsive/beginning of the gradual phase, and after the cessation of nonthermal electron injection. Each raster time occupies two rows (intensity and Doppler velocity for each time interval), while each ion occupies two columns (line core and blue wing). The color bar scale is consistent between ion species and observation times. At the earliest times, only Fe XXIV λ192.02 displays emission above the background. RHESSI 25–50 keV CLEAN imaging contours are overlaid in cyan on all images, corresponding to 5%, 30%, and 70% of the image maximum.
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: Top panel: the power in nonthermal electrons from spectral fitting and two estimates for the IRIS time-dependent footpoint area, as discussed in Section 2.3. The time-dependent footpoint areas are shown in pink and correspond to the right-hand axis. Second panel: the flux of nonthermal electrons, obtained by dividing the power shown in the top panel by the time-dependent footpoint area. The conservative estimate given by the 10% footpoint contours is given as solid lines, while the estimate from a compact 50% footpoint area is shown as the dotted lines. Third panel: the electron flux at the reference energy of 50 keV in units of 1034 e − s−1 keV−1. Fourth panel: the power-law slope of the nonthermal electron distribution. Fifth panel: the low-energy electron cutoff in keV. Sixth panel: the reduced χ 2 per fit interval and detector.
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: Spectral fitting parameters from the IRIS raster spanning 14:08:21–14:10:24 UT, superimposed on the co-temporal C II slit-jaw image. Top: the full slit-jaw image, with the FOV of the EIS instrument overlaid in orange and each raster slit position shown in green. The purple box denotes the region of interest shown in each panel below. Each column denotes the line intensity (in photons s−1 Å−1), the Doppler velocity of the line (in km s−1), and the nonthermal width (in km s−1), for C II λ1335.71 (top), Si IV λ1402.81 (middle), and Fe XXI λ1354.07 (bottom). In the case of Fe XXI, where fewer profiles could be fit, the overlaid images are integrated through the duration studied, taking the value with the larger magnitude where multiple values existed. The width of the IRIS slit has been exaggerated by a factor of five. Overlaid contours represent the 25% (blue) and 50% (orange) levels of RHESSI 40–100 keV emission.
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: IRIS spectral fitting results for the C II λ1335.71 line (top row), Si IV λ1402.81 (middle row), and Fe XXI λ1354.07 (bottom row). Left column: intensity for each of the three lines. Middle column: Doppler velocity for each of the three lines. Right column: nonthermal velocity width for each of the three lines. For C II λ1335.71 and Si IV λ1402.81, which are significantly brighter and more easily fit than Fe XXI λ1354.07, the running mean of each parameter is overlaid in orange. Note that the appearance of periodicity in the running mean of C II and Si IV parameters is an artifact induced by the loss of spatial information.
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: Fe XIV λ264.81/λ274.23 calculated electron density. Left: density maps for four EIS rasters spanning the impulsive, peak, and early gradual phases of the flare. Right: selected density slices along the flare ribbon. Each slice is cospatial with an HXR-emitting source during one or more raster. The raster beginning at 14:02:39 UT has three dashed lines overplotted corresponding to the location in the raster of each slice. The lines are omitted for following times, but the endpoints remain as a reference. RHESSI 25–50 keV CLEAN imaging contours are overlaid in cyan on all images, corresponding to 5%, 30%, and 70% of the HXR maximum.
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: The Fe XXIV λ192.02 complex for three times, 14:02:39 UT (top; pre-nonthermal HXR), 14:06:13 UT (middle; peak nonthermal HXR), and 14:09:48 UT (bottom; late nonthermal HXR). Fit profiles for the core of the line are shown along with the fit to the blue-wing enhancement and the fit to the Fe XII λ192.39 line used for reference wavelength determination. The rest position of Fe XXIV is overlaid as the dotted red line, and the dotted brown line denotes the rest position of the Fe XII line. Note the difference in intensity scale between the top and middle panels.
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: Spatially averaged Doppler and nonthermal velocities taken from a region in the center of the HXR footpoint (approximate coordinates are X = −250″, Y = −320″), for each of the four rasters presented in Figure 8. Doppler velocities are shown in blue, while nonthermal velocities are shown in orange. Points obtained from IRIS spectral fitting are denoted by stars, and points corresponding to EIS line core fits are denoted by circles, while fit blue-wing enhancements are denoted by downward-pointing triangles. Each point displays associated error bars. However, the wide span of velocities causes many of the error bars to fall within the area subtended by the data point.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: (a) A schematic diagram of the obscuration scenario. The black circle represents the SMBH, surrounded by the X-ray corona shown in pink. The yellow region represents the accretion disk. The green arrows represent the absorber (e.g., an outflowing disk wind) with a half-opening angle of θ oa and a covering factor of ﹩\cos {\theta }_{{\rm{oa}}}﹩. The system inclination angle is θ inc. The dashed line traces the transmitted (absorbed) radiation through the absorber in the direction of the observer (transmitted component). The dotted curves trace the radiation reflected from the opposite side of the absorber and the radiation scattered to the line of sight through the absorber (reprocessed component). The absorber is clumpy, allowing a fraction (f leak) of the intrinsic continuum to leak through without being absorbed (leaked component). There is probably also a fraction (f scatter) of the intrinsic continuum scattered to the line of sight by a large-scale highly ionized “mirror” (not shown in the cartoon). We treated f leak and f scatter together in this model. (b) An example of the X-ray spectral components for a given set of the absorber parameters. The black solid curve shows the total observed model spectrum, while the gray long-dashed line, yellow dashed–dotted curve, red dotted curve, and blue dashed line represent the intrinsic power law, transmitted component, reprocessed component, and leaked component, respectively.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: X-ray-to-optical power-law slope parameter (α OX) vs. 2500 Å monochromatic luminosity for the three quasars, showing their significant soft X-ray weakness derived using archival Chandra and XMM-Newton observations. For PHL 1811, the α OX values from the 2001 December 5 and December 17 Chandra observations are shown; the α OX measurements from the two XMM-Newton observations not shown here are very close to the 2001 December 5 Chandra value. The solid blue line represents the α OX–L 2500 Å relation from Steffen et al. (2006). The small gray circles and downward-pointing arrows represent the α OX values and upper limits of the Steffen et al. (2006) AGN sample, respectively.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: The 2015 XMM-Newton spectrum for PHL 1811 overlaid with the best-fit (a) simple power-law model and (b) simple power-law plus Compton-reflection model (with a fixed photon index). The spectra are grouped for display purposes only. The bottom panels display the ratios of the data to the best-fit models. Compared to the simple power-law model, there are significant fitting residuals above ≈3 keV, which require an unrealistically large reflection factor (≈23) to explain. The spectrum thus cannot be well described by a simple unabsorbed power-law continuum plus a reasonable amount of Compton reflection.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: SEDs of the three quasars (see Section 3.3 for the IR–UV data). The 2 keV luminosities were derived from the power-law spectral fitting of the Chandra or XMM-Newton spectra (Section 3.1). The 8 and 15 keV luminosities were derived from the NuSTAR photometric results (Section 3.2). For PHL 1811, we show the soft X-ray spectral slopes (with negligible uncertainties) from the two XMM-Newton observations and the hard X-ray spectral slope (with the shaded area representing the uncertainties) constrained from the NuSTAR observation, which differ beyond the 1σ level. The green dashed curve in each panel shows the mean quasar SED from Krawczyk et al. (2013) normalized to the 2500 Å luminosity; the X-ray component is a Γ = 2 power-law continuum that follows the α OX–L 2500 Å relation.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: Similar to Figure 4, displaying the 2015 XMM-Newton and NuSTAR spectra for PHL 1811 overlaid with the best-fit power-law plus Compton-reflection model. The Compton-reflection component was modeled with (a) pexrav and (b) borus02. An unrealistically large reflection factor (≈24) is required in the pexrav model, while the self-consistent borus02 Compton reflection is not sufficient to account for the excess emission in the hard X-rays.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: The Chandra, XMM-Newton, and NuSTAR spectra for the three quasars, overlaid with the best-fit models using the obscuration model described in Section 4.2. The spectra are grouped for display purposes only. The bottom panels display the ratios of the data to the best-fit models. We break the five observations of PHL 1811 into two panels for clarity. For PG 1001, the energy ranges used are 1–8 keV for the Chandra observation and 1–10 keV for the XMM-Newton observation owing to the apparent soft X-ray excess emission at lower energies. The obscuration scenario explains reasonably well the multiepoch broadband X-ray spectra of the three quasars.
Paper: NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario
Authors: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, D. Stern
Figure caption: NuSTAR hard-band (8–24 keV) images of the three quasars, smoothed with a Gaussian kernel with standard deviation of 2.0 pixels. Each image is centered on the corresponding X-ray source position, and the circle indicates the 35″-radius aperture used for source extraction. Due to statistical fluctuations, the smoothed images of these faint sources do not have circular morphologies following the NuSTAR on-axis point-spread function.
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 stellar velocity dispersions (σ ⋆), z-band concentration indices (C), δ 0.5Mpc, and M  h  from Lim et al. (2017) for starbursts, strong-Hδ  A  AGNs, QPSBs, SFMS galaxies, and QGs. Although the first three samples overlap in the plotted parameters, starbursts have similar σ ⋆ and C to SFMS galaxies (some are disk-dominated/less centrally concentrated), while QPSBs and strong-Hδ  A  AGNs have similar structures to QGs (i.e., most are bulge-dominated). Starbursts also have lower M  h  and δ 0.5Mpc than QGs. Their structures correlate weakly (ρ ≈ 0.2) with M  h  and δ 0.5Mpc.
Paper: Merger Effects on the Spin and Shape Alignments of Galaxy Stellar, Cold Gas, Hot Gas, and Dark Matter Components
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Mean values of the cosines of the angles of the galaxy stellar, cold gas, and hot gas spin axes from their DM spin axes (top, middle, and bottom panels, respectively), at z = 0, averaged over each of the four controlled samples classified by the latest merger epochs, a(z  m ). The errorbars are not visible due to their tiny sizes. The earlier the galaxies experience their latest mergers, the weaker the spin alignments between their baryon and DM components become.
Paper: Merger Effects on the Spin and Shape Alignments of Galaxy Stellar, Cold Gas, Hot Gas, and Dark Matter Components
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Mean values of the galaxy total masses averaged over each of the four controlled samples for three different cases of the particle number cuts: n  s , n  d  ≥ 300 (top panel); n  cg , n  d  ≥ 300 (middle panel); n  hg , n  d  ≥ 300 (bottom panel).
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: Simultaneously matching all QPSBs to starbursts, upper-SFMS galaxies, strong-Hδ  A  AGNs, and QGs of similar multiscale (0.5–8 h −1 Mpc) environmental indicators (panels (a) to (f)), M ⋆, σ ⋆, and C (panels (g) to (i), respectively). The figure demonstrates that some starbursts, upper-SFMS galaxies, and AGNs are progenitors of QPSBs, which in turn are progenitors of some QGs.
Paper: Merger Effects on the Spin and Shape Alignments of Galaxy Stellar, Cold Gas, Hot Gas, and Dark Matter Components
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Mean values of the environmental density contrasts averaged over each of the four controlled samples for the three different cases of the particle number cuts.
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 environments of AGNs with those of the other samples. The environments of AGNs have lower densities than those of QGs. The overdensities (nearest neighbor distances) of AGNs with Hδ  A  > 4 Å are significantly lower (longer) than those of SFMS galaxies, while the opposite is true for AGNs with Hδ  A  < 3 Å.
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 stellar mass and concentration index distributions of various samples before matching. The distributions of C of QPSBs and strong-Hδ  A  AGNs are more similar to those of QGs than to those of starbursts and upper-SFMS galaxies, while their M ⋆ are significantly lower than 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: Comparing stellar mass overdensities with luminosity overdensities. The latter are computed by Tempel et al. (2014).
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Noise decorrelation test with DECam data. The upper panels show the zoomed-in region of SN candidate AT 2018fjd (R.A. = 21:12:25.980 decl. = −66:00:56.50) discovered by DECamERON (Mould et al. 2017; Hu et al. 2018). R 0 (S 0) is from individual observations DECam-OBS18a (DECam-OBS04a). R (S) is the stacked reference (science) image. The subtraction between R and S results in the difference image D, and D dc is the decorrelated difference image. The black dashed boxes (41 × 41 pixels) are selected on the background region in the vicinity of AT 2018fjd. The lower panel shows the corresponding covariance matrix measured from the boxes. To probe the local correlation of background pixels, we constructed a multivariate random variable X for the flux of adjacent pixels with fixed positional relationship, where X= (X (0,0), X (1,0), X (−1,0), X (0,1), X (0,−1), X (1,1), X (1,−1), X (−1,1), X (−1,−1), X (2,0), X (−2,0), X (0,2), X (0,−2), X (3,0), X (−3,0), X (0,3), X (0,−3), X (4,0), X (−4,0), X (0,4), X (0,−4), X (5,0), X (−5,0), X (0,5), X (0,−5)). Note the subscripts represent the relative pixel locations with respect to the first element. Only the pixels within the boxes are allowed to be involved in the random vector. The covariance matrix is calculated by exhausting all possible realizations of X.