adsabs/AstroCLIMB huggingface dataset:
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Comparison of the lens mass M  L , distance D  L , transverse velocity v  T,L , proper motion vector (μ  L,E , μ  L,N ), and lens–source relative proper motion direction φ inferred from the various studies of OB110462.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: CDF of normalized residuals for astrometric models and data, as compared to the CDF of a standard normal distribution. The CDF of normalized residuals for the astrometry in R.A. (decl.) is shown in the blue solid (orange dotted) line. The CDF of a standard normal distribution is shown as the black curve.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Comparison of HST photometry derived by Lam et al. (2022a, 2022b), Sahu et al. (2022), and this work. The top (bottom) row compares the differences in the photometry in Sahu et al. (2022) to Lam et al. (2022a, 2022b) (this work); red (blue) points denote data in the F814W (F606W) filter.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Energy dependency of the fractional rms amplitude over the pulsation cycle of ULX-1 calculated from the XMM-Newton PN detector (filled circles) and FPM (open circles) data. For clarity, only the data from FPM-A are shown for NuSTAR.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: X-ray pulse profile (bottom) and its energy dependency (top) obtained from the 0.3–10  keV band of XMM-Newton EPIC-pn (left) and the 3–25  keV of NuSTAR FPM-A (right). For clarity, only FPM-A is presented for the NuSTAR data. The color scales of the top panels represent the fluctuation over the average count rate in percent. The count rates in the bottom panels are the average over respective energy bands; 0.3–3  keV (filled circles), 3–10  keV (open circles), and 10–25  keV (filled triangles). The data points of 10–25  keV are scaled by a factor of 4 for clarity.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Background-subtracted light curves of ULX-1 taken with EPIC-pn (0.3–10.0  keV: black) and FPM-A (3–25  keV: red). The zero-point of the horizontal axis corresponds to the beginning of the NuSTAR observation (MJD 57738.6573). Those in the larger panel have a full length of the observation with 700 s width per bin, whereas that in the other panel is a 200 s fraction of particular interval in the EPIC-pn observation with a 4 s bin width.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Panels (a)–(c) (red error bars) show the evolution of abundance in the logarithmic scale with A(H) = 12 for Mg, Al, and Si during the evolution of AR 12749, AR 12758, and AR 12759. These abundances are measured with respect to the soft X-ray continuum, which is mostly determined by the choice of oxygen abundance, which was considered to be 8.8 dex. The magenta bars represent the average abundances when the ARs are very bright, as bounded by the vertical dashed lines. The y-error bars represent the 1σ uncertainty for each parameter, and the x-error bars represent the duration over which a given spectrum is integrated. The black horizontal dashed lines represent the average abundances for the quiet Sun in the absence of any AR reported by Vadawale et al. (2021b). The XSM light curves for each AR are shown in gray in the background, and the blue XSM light curves represent the time duration excluding the flaring activities. The range of coronal and photospheric abundances from various authors compiled in the CHIANTI database is shown as orange and green bands. The right y-axis shows the FIP bias values for the respective elements with respect to the average photospheric abundances.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Evolution of the temperature (red points in panel (a)) and EM (red points in panel (b)) during the evolution of AR 12749, AR 12758, and AR 12759. When the ARs are very bright, as bounded by the vertical dashed lines, the magenta bars represent the average values of the temperature and EM. The black horizontal dashed lines represent the average temperature and EM for the quiet Sun in the absence of any AR reported by Vadawale et al. (2021b). The XSM light curves of the ARs are shown in gray, and the light curves for the quiescent regions are shown in blue.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Results showing the emerging phase of AR 12758. The black curve in panel (a) shows the evolution of the total unsigned photospheric magnetic flux. Panels (b) and (c) show the evolution of temperature and EM. Panel (d) shows the evolution of the FIP bias for Si. The dashed lines in panels (b)–(d) represent the corresponding parameter for the background solar emission from the rest of the solar disk except the AR. The background gray curves in each panel represent the X-ray light curve observed by XSM, whereas the blue curves represent the selected times excluding the flaring period, representing the quiescent AR.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: The XSM 1–15 keV light curves during the disk passage of AR 12749 (panel (a)), AR 12758 (panel (b)), and AR 12759 (panel (c)). The top row of each panel shows representative full-disk X-ray images (negative intensities) taken with the XRT Be thin filter during the evolution of the ARs. The vertical dashed lines represent the timing of the XRT images.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Soft X-ray spectra measured by XSM for 3 representative days of the AR period are shown. Solid lines represent the best-fit isothermal model, and the residuals are shown in the bottom panel. Gray points correspond to the nonsolar background spectrum. The black dashed curve in the above panel represents the average quiet-Sun spectrum.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Variation of the FIP bias with the FIP of the elements. The red points are the averaged FIP bias for one of the ARs (AR 12749) reported in the present study. The blue points are the FIP bias for the XBPs as reported by Vadawale et al. (2021b). The green points are the measured FIP bias during the solar flare peak as reported by Mondal et al. (2021).
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Evolution of AR 12758 during its emergence phase on the solar disk. The top row shows the evolution of the photospheric magnetograms as observed by HMI, and the bottom row shows the evolution of the X-ray emission as observed by the XRT Be thin filter.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Selection of the quiescent AR periods (orange shaded regions) from the XSM light curves for 1 representative day of AR 12749 (panel (a)), AR 12758 (panel (b)), and AR 12759 (panel (c)).
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: Results from the errors-in-variables hurdle model run on the full sample of Local Group galaxies. In all plots, 90% credible intervals are colored gray. In the plots that show L gcs on a log10 scale, zero values are added with an axis break for visualization purposes. (Upper left) The logistic portion of the luminosity hurdle model. The two logistic parameters given in Table 2, which constitute this curve, give the probability that a galaxy with a given luminosity has GCs. (Lower left) The linear portion of the model. The linear parameters give the expected total luminosity of a galaxy’s GC population, given that it has GCs (i.e., only the nonzero values are fitted). Zero values are grayed out. (Upper right) The expectation value of the Bayesian lognormal hurdle model. The hurdle model is a combination of the logistic and linear portions of the model shown on the left, and gives the overall expectation value for the mass of a galaxy’s cluster system. The linear portion of the model is reproduced on this plot for comparison, and three interesting galaxies are labeled for further discussion. (Lower right) Posterior predictive plot containing data simulated from the model in purple with the Local Group sample plotted in blue. The two separate populations of galaxies—those with and without GCs—are clearly seen in the simulated data.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: Results from the hierarchical hurdle model run on the full sample of Local Group galaxies. The stellar masses plotted are the best-fit values sampled by the model, and the GC system masses are converted from luminosities using an M/L of 1.88. Gray shaded regions indicate 90% credible intervals. In the plots that show M gcs on a log10 scale, zero values are added with an axis break for visualization purposes. (Upper left) The logistic portion of the hurdle model, which models the probability that a galaxy does or does not have clusters. (Lower left) The linear portion of the hurdle model, which shows the expected size of a nonzero cluster population. Zero values are grayed out. (Upper right) The expectation value of the entire hurdle model with the linear fit overplotted as a dotted line for comparison. Galaxies of interest are labeled and discussed individually in Section 6. (Lower right) Posterior predictive plot with data simulated from the hurdle model fit in purple.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: A DAG of the hierarchical model. The model predicts GC system luminosities (the response variable) with a set of model parameters and galaxy luminosities (the predictor variable). The measured galaxy luminosity data are modeled by a normal distribution that depends on the true luminosities and the measurement error. The true luminosities are random variables that are calculated with true stellar masses and an M/L, both of which are sampled for in the model. The M/L s for each galaxy are sampled from a global normal distribution of V-band M/L s that has a prior-set mean and standard deviation that is fit by the model. The model can be collapsed along the true luminosities and M/L s since these are nuisance parameters, the true luminosity values are deterministic, and the normal distributions can be convolved. See Figure 5 for the collapsed version of the model.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: The collapsed portion of the model. The true luminosities and M/L s, which are nuisance parameters, have been removed from the model. This shifts the rest of the model downward and combines the distributions from these levels of the model, which is feasible because the distributions describing these nuisance parameters are all either deterministic or normal distributions. This simplified, collapsed version of the model is the version actually implemented.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: Galaxy luminosities and GC system luminosities of our full Local Group data sample, including galaxy candidates. The shape of points corresponds to the source of their GC luminosity data (galaxies without GCs are shown as vertical bars). Points are colored based on the source of the galaxy luminosity data. Note that a subset of galaxies have multiple references for galaxy data; some of the dwarf galaxies have information from Simon (2019) as well as from another source. These points are colored according to the non-Simon source.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: DAG of the errors-in-variables luminosity hurdle model. Arrows follow down the steps of the model, linking inputs with responses of each distribution and leading to the response variable ﹩\mathrm{log}{L}_{\mathrm{GC},i}﹩ in the bottom row. Priors for the model parameters are blue, data are teal, and model parameters are pink. The distributions that follow down the layers of the DAG are written beside each arrow.
Paper: The HERBAL Model: A Hierarchical Errors-in-variables Bayesian Lognormal Hurdle Model for Galactic Globular Cluster Populations
Authors: Samantha C. Berek, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, William E. Harris
Figure caption: Posterior plot of the global model parameter σ  M/L . The lognormal prior is plotted as a black dashed–dotted line, while the posterior is solid gray. The posterior is constrained between σ  M/L  values of approximately 0.3 and 1, with a mean of 0.59.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison between the two selected magnetic maps of the radial magnetic field B  r  for the minimum (left panel) and maximum (middle panel) of activity. The left panel shows a GONG synoptic map corresponding to 2008 December 15, representative of a minimum of activity (dipolar field with very few active regions). The middle panel shows a GONG-ADAPT map corresponding to 2015 March 20, representative of a maximum of activity (multipolar field with intense active regions). We also show for information the GONG map corresponding to the date chosen for the maximum of activity (right panel). We can thus see that there is a greater difference between the minimum and maximum of activity than between GONG and GONG-ADAPT. The positive polarity of the magnetic field is shown in red, and negative polarity in blue. The color bar has been set symmetric and saturated to better visualize the structures (between −20 and 20 G). Note that the y-axis for the left panel is in sine latitude.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the heliospheric wind background at the minimum (left panel) and maximum (right panel) of activity. The first row illustrates the radial wind speed in kilometers per second, the second row the number density per cubic centimeter normalized to 1 au, and the last row the radial magnetic field in nanotesla. For each row, we show the ecliptic (view from above) and meridional (view from the side crossing Earth) views in the HEEQ frame. Various planets and satellites are also shown in the bottom legend.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the EUHFORIA input boundary condition at 0.1 au for the minimum (left panel) and maximum (right panel) of activity. The first row shows the radial velocity v  r  in kilometers per second, the second row the number density N per cubic centimeter, the third row the temperature T in 106 K, and the fourth row the radial magnetic field B  r  in nanotesla. All these profiles were derived from the magnetic maps displayed in Figure 1 using Wang–Sheeley–Arge and PFSS+SCS empirical relations. X-axis is in Stonyhurst longitude, and the y-axis is in latitude.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the ICME parameters obtained at Earth for the median case at the minimum (left panel) and maximum (right panel) of activity. The first row illustrates the total magnetic amplitude in nanotesla, the second row the total velocity amplitude in kilometers per second, the third row the temperature in 10,000 kelvin, the fourth row the number density for the protons per cubic centimeter, and the last row the β parameter of the plasma. A yellow rectangle highlights the region corresponding to the sheath, and a blue rectangle the region corresponding to the magnetic cloud. The method used to derive these regions is explained in more detail in Appendix A.
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption:  X-CIGALE SED modeling of the Spitzer/IRAC photometry (black triangles) and SDSS and Spitzer/IRS spectrophotometry described in Section 2. Total best-fit SED, UV/optical stellar component, dust stellar component, and smooth-torus model are shown with black, blue, red, and green lines, respectively. For illustration purposes only, overlaid are the HST and MAGNUM high-spatial-resolution photometric data described in Sections 2.4 and 2.5, as well the SDSS and Spitzer/IRS spectra. These points used in the forward-modeling process fit the data with a reduced χ 2 = 2.71.
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption: Left: a compilation of various observations of NGC 4395, listed with corresponding apertures and dates of observation. We include published data from the Lick Observatory (Desroches et al. 2006), the HST/WFC3 NSC photometry from Carson et al. (2015), and UV data from Peterson et al. (2005), in addition to the archival SDSS, Spitzer/IRS, and MAGNUM K-band data used in this study. To yield insight into the intrinsic optical variability of the AGN, the minimum and maximum gri-band photometry from the ZTF have been overplotted as red bars. For reference, Elvis et al. (1994) quasar templates normalized to the Spitzer IRS spectrum at 12 μm have been overplotted. Right: ZTF point-source photometry for NGC 4395 in the g-, r-, and i-bands (blue, green, and red points, respectively). The day-long UV/optical variability is similar in both the g and r bands with ∼0.48 mags (AB).
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption: Nonparametric plot of near-IR (α MIR) and near-IR (α NIR) spectral slopes of the AGN emission in NGC 4395 (filled circle). For comparison, CAT3D-WIND models are shown for 15° and 30° inclination angles (solid lines), varying fractions of the polar wind contribution to the mid-IR emission (f wind = {0.15, 0.30, 0.45, 0.60};  dashed lines), and disk scale heights of 0.1 and 0.2 (red and blue lines, respectively). Panels provide number of dust clumps along the line of sight (N 0 = {5, 7, 10}) and the radial distribution of dust clouds in the wind (A wind = {−0.5, −1.0, −1.5}). All models shown assume a radial power-law slope of a = −2.5, and a half-opening angle and angular width of the wind θ  W  = 45° and σ  θ  = 15°, respectively; see Hönig & Kishimoto (2017) for details of the CAT3D-WIND models.
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption: The χ 2 of the HST/WFC3 photometry to the fitted galaxy model plotted against the fraction of the fitted AGN model at 9.7 μm, shown for different values for four of the most relevant skirtor torus parameters. We seek the minimum χ 2 value to ensure that the best-fit parameters that shape the global model SED in Figure 3 encompass a model galaxy in satisfactory agreement with the NSC photometry. All models exhibit minimum χ 2 values at an AGN fraction of approximately 60%, suggesting that the best-fit parameterization of the torus is in sufficient agreement with the global SDSS+IRS photometry as well as the galactic anchor specified in Section 4.1.
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption: The different X-CIGALE model SED fits with alternating values for opening angle θ and inclination angle i. The SDSS and Spitzer/IRS spectrum as well as the HST/WFC3 NSC photometry have been overplotted for consistency. Note that the models demonstrate a diminishing optical component of the AGN with increasing inclination, presumably due to a line of sight passing through the obscuring torus.
Paper: Modeling the Spectral Energy Distribution of the Active Galactic Nucleus inside NGC 4395
Authors: Hector Afonso G. Cruz, Andy D. Goulding, Jenny E. Greene
Figure caption: SED comparison of the Spitzer/IRAC photometry (black triangles) and Spitzer/IRS spectrophotometry, against the CLUMPY-torus models. The UV/optical stellar component and dust stellar component predicted by X-CIGALE are denoted in blue and red, respectively. In gray are the space of 10 CLUMPY AGN SEDs closest in fit to the IRS spectrum, with the best-fitting SED represented in green. For illustrative purposes, the Spitzer/IRS spectrum is overlaid in orange.