adsabs/AstroCLIMB huggingface dataset:
Paper: Metallicity Dependence of Molecular Cloud Hierarchical Structure at Early Evolutionary Stages
Authors: Masato I. N. Kobayashi, Kazunari Iwasaki, Kengo Tomida, Tsuyoshi Inoue, Kazuyuki Omukai, Kazuki Tokuda
Figure caption: The size and mass functions of CNM clumps. The gray filled histogram shows 1.0 Z ⊙, and the other step histograms show 0.5 Z ⊙ (red) and 0.2 Z ⊙ (blue). The mass function shows a reference power-law distribution of ﹩{dn}/{dm}\propto {m}^{-1.7}﹩ (black dashed line).
Paper: Metallicity Dependence of Molecular Cloud Hierarchical Structure at Early Evolutionary Stages
Authors: Masato I. N. Kobayashi, Kazunari Iwasaki, Kengo Tomida, Tsuyoshi Inoue, Kazuyuki Omukai, Kazuki Tokuda
Figure caption: The square root of the second-order velocity structure function S(r) as a function of the distance r between CNM cells at 3 t cool. The black shaded region shows the maximum and minimum of S(r) among the 27 sampled subvolumes. The red solid curve shows the volume-weighted average of all of the subvolumes. The black solid (dashed) line shows the Larson (Kolmogorov) power-law relation as ﹩\sqrt{S(r)}\propto {r}^{1/2}﹩ (﹩\sqrt{S(r)}\propto {r}^{1/3}﹩). The vertical gray dotted line at k/2π = 0.4 pc−1 indicates one-tenth of the Nyquist frequency (i.e., the typical spatial scale below which the turbulent power is affected by the numerical diffusion).
Paper: Metallicity Dependence of Molecular Cloud Hierarchical Structure at Early Evolutionary Stages
Authors: Masato I. N. Kobayashi, Kazunari Iwasaki, Kengo Tomida, Tsuyoshi Inoue, Kazuyuki Omukai, Kazuki Tokuda
Figure caption: A schematic figure showing the relationship between the density structures and their thermal states in the metallicity range of 1.0–0.2 Z ⊙. The WNM/UNM turbulence on the entire cloud scale powers the relative velocity between CNM clumps with 3–5 km s−1, while the internal velocity dispersion within individual CNM clumps remains ≲1 km s−1. The velocity two-point correlation of the CNM volume follows Larson’s law as ﹩\sqrt{S(r)}\propto {r}^{1/2}﹩.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Continuum-normalized premaximum spectra of the studied Type W (on the bottom with purple–bluish colors) and Type 15bn SLSNe-I (on the top with orange–greenish colors) shifted vertically from each other and corrected for redshift and Milky Way extinction. The wavelength range of the W-shaped O II feature is highlighted with a semitransparent red rectangle to emphasize the difference between these two subtypes.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Continuum-normalized pseudo-nebular spectra of the studied SLSNe-I plotted with the same methodology and color coding as in Figure 2. The places of the commonly present nebular lines are presented using black vertical lines.
Paper: Metallicity Dependence of Molecular Cloud Hierarchical Structure at Early Evolutionary Stages
Authors: Masato I. N. Kobayashi, Kazunari Iwasaki, Kengo Tomida, Tsuyoshi Inoue, Kazuyuki Omukai, Kazuki Tokuda
Figure caption: The t cool-normalized time evolution of the turbulence mode fraction. The upper (lower) three lines correspond to the solenoidal (compressive, respectively) mode.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Top left: spectrum modeling of the “early postmaximum” (+7 days phase) spectrum of PTF12dam, a Type W SLSN-I. The corrected and continuum-normalized observed spectrum is plotted with black, while the red color denotes the best-fit model obtained in SYN++. Single-ion contributions to the overall model spectrum are shown with purple lines shifted vertically from each other. Top right: spectrum modeling of the “later postmaximum” (+14 days phase) spectrum of PTF12dam with the same color coding as the top left panel. Middle left: spectrum modeling of the “early postmaximum” (+7 days phase) spectrum of SN 2015bn, a Type 15bn SLSN-I (black line). The best-fit SYN++ model (green line) and the identified ions (orange lines) are plotted similarly to the top left panel. Middle right: spectrum modeling of the “later postmaximum” (+20 days phase) spectrum of SN 2015bn. Bottom: pseudo-nebular spectrum of SN 2015bn taken at +30 days phase (black line) plotted together with the fitting with Gaussians (green line) added to a constant continuum of 1.3; the identifications of nebular emission features and absorption lines remained there from the photospheric phase.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Left panel: photospheric velocity evolution of the SLSNe-I in the sample. Premaximum v phot values were adopted from Könyves-Tóth & Vinkó (2021), while “later postmaximum” photospheric velocities were estimated via cross-correlation. Type W SLSNe-I are coded with red colors, while Type 15bn objects are shown in blue. For clarity, the epoch of the maximum light (black vertical line) and v phot = 12,000 km s−1 (black horizontal line) are displayed as well. Right panel: photospheric temperature evolution of the studied objects, using the same color coding as in the left panel. Here, the black horizontal line codes the T phot = 12,000 K value. It can be seen that despite the premaximum bimodality, Type W and Type 15bn SLSNe-I show similar v phot and T phot values by the “later postmaximum” phases.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Left panel: pEW calculations of the “W-place” feature for all available spectra of SN 2015bn (green) and PTF12dam (orange). Right panel: evolution of the pEWs of all studied SLSNe-I in the “early postmaximum,” the” later postmaximum,” and the pseudo-nebular phases. Type W SLSNe-I are coded with red, while blue colors denote the Type 15bn objects. The vertical black lines show the supposed maximum place of the pEW of the W-place feature for Type W SLSNe-I (∼+13 days phase) and Type 15bn SLSNe-I (∼+80 days phase).
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: The time interval of the transition from the photospheric to the nebular phase in the case of each studied object (orange rectangles). The left sides of these rectangles show the phase of the latest available postmaximum spectrum, while the right ends of the rectangles denote the epoch when the spectra have already reached the pseudo-nebular phase. Type W SLSNe-I are plotted above the blue horizontal line, while Type 15bn SLSNe-I can be seen below the blue line.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Photometric phase vs. spectroscopic phase of the examined SLSNe-I. Type W objects are coded with red colors, while blue colors denote Type 15bn SLSNe-I. The left panel of the figure shows the overall evolution from the premaximum phases to the pseudo-nebular phases, while the right panel zooms in on the region between −30 and +40 rest-frame days with respect to the moment of maximum light to make the premaximum bimodality between Type W and Type 15bn SLSNe-I more visible.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: The +17 days phase spectrum of SN 2018hti. The three regions used for the pEW calculations are shaded with different colors: the wavelength range between 4166 and 5266 Å, where the W-shaped O II blend before the maximum is supposedly present in the case of Type W objects, is marked with blue; the basin-shaped feature present in all examined SLSNe-I in the postmaximum phases between 5290 and 6390 Å is plotted with purple; while the red color denotes the place of the commonly present O I line between 7295 and 7797 Å.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Photospheric velocity vs. photospheric temperature of the studied Type W (red) and Type 15bn (blue) SLSNe-I in the “later postmaximum” phase. 10,000 K and 10,000 km s−1 are marked with the black horizontal and vertical lines, respectively. It is seen that the T phot and v phot of most objects decrease below 10,000 K and 10,000 km−1, with the exception of SN 2010kd and SN 2010gx (both of them are Type W SLSNe-I).
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Left panel: pEW evolution of the “basin” feature for all studied SLSNe-I. Right panel: pEW evolution of the O I λ7775 line for all studied objects. The color coding is the same as in Figure 11.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: The corrected and normalized “later postmaximum”–phase spectra of the examined objects (black lines) plotted together with their best-fit template spectra (orange lines) used in the cross-correlation process.
Paper: Type W and Type 15bn Subgroups of Hydrogen-poor Superluminous Supernovae: Premaximum Diversity, Postmaximum Homogeneity?
Authors: Réka Könyves-Tóth, Bálint Seli
Figure caption: Top left: star formation rate vs. stellar mass of the host galaxies of the studied SLSNe-I. Top right: star formation rate vs. brightness of the galaxy of the SLSNe-I with available data. Bottom: absolute brightness of the SN at the moment of the maximum (﹩{M}_{\mathrm{SN}}﹩ max) vs. the stellar mass of the host galaxy. Type W SLSNe-I are plotted with red, while Type 15bn SLSNe-I are shown with blue dots.
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: Left: the MAXI light curve in the 2–20 keV band of the 2022–2023 outburst of XTE J2012+381 (top). The following five panels show the evolution of the measured Galactic column density N H, the inner disk temperature and normalization of the diskbb component, the power-law index Γ, and the normalization of the powerlaw component, obtained when fitting the NICER spectra of the source with the model TBabs*(diskbb+powerlaw). The seventh panel shows the exposure of the NICER observations analyzed, and the eighth panel shows the reduced χ 2 returned by the fits to the NICER spectra. The colors of the points represent time evolution. The vertical cyan lines show the dates of the two NuSTAR observations of XTE J2012+381 analyzed in this paper. The observations between the dashed vertical magenta lines were combined to produce the spectrum shown in Figure 5. Right: the evolution of the measured disk temperature of the source (top) and of the 1–10 keV flux (bottom) vs. the hardness defined as the ratio of the 5–10 keV flux to the 2–5 keV flux. In the top panel, we omitted the measurements that had an uncertainty larger than 0.5 keV. The colors of the points are the same as in the left panels and represent the time evolution of the source.
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: Panels (a) show the unfolded spectra of XTE J2012+381. The blue points represent the NICER spectra, and the different shades of red indicate the spectra from the NuSTAR FPMA and FPMB detectors. The solid lines represent the total best-fit models, while the dashed and dotted lines show the contributions to the model by the diskbb and relxill/relxillD components, respectively. Panels (b) show the residuals in terms of σ for the TBabs*(diskbb+powerlaw) model. The residuals show a clear indication of relativistic reflection for both observations. Panels (c) show the residuals of the best-fit models, TBabs*(diskbb+relxill) or TBabs*(diskbb+relxillD), respectively, for each observation, together with the statistic produced by the models. Panels (d) show the ratio of data to model for the best-fit models. The left panels show the spectra and residuals when fitting NICER and NuSTAR observations jointly, while the right panels show the results obtained when fitting the NuSTAR observations alone. The top set of panels indicate the first epoch (2022 December 29), while the bottom set of panels show the second epoch (2023 January 18 and 21 for NuSTAR and NICER, respectively).
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: The left panels shows the posterior distributions resulting from the MCMC analysis of XTE J2012+381 for spin, while the right panels shows the posterior distributions for the inclination of the inner accretion disk in the model. The width of the lines is proportional to the ratio of the reflected flux to the total flux in the 3–79 keV band, which were used as weighting when combining the posterior distributions. The top panels indicate the results obtained from joint NICER and NuSTAR fits, while the bottom panels represent the results obtained from NuSTAR-only fits. The blue and red lines represent the posteriors obtained when fitting the two sets of observations analyzed, and the black curves represent the combined inferred distributions, derived as highlighted by Draghis et al. (2023b). The green lines represent the combined distributions obtained as highlighted in this paper, which better account for systematic variations between the results obtained from the independent observations. The solid vertical black and green lines represent the modes of the combined distributions, and the dashed vertical black and green lines represent the 1σ credible intervals of the respective measurements. The inset in the bottom left panel shows the complete posterior distribution for the spin obtained when fitting the second NuSTAR observation alone with the TBabs*(diskbb+relxillD) model, which obtains two solutions similar in terms of statistic produced but with very different spin constraints. Nevertheless, as the first observation (blue) weights significantly more in the combining algorithm owing to stronger reflection, the combined distribution still significantly favors a high spin, but with a broader lower limit on the credible interval.
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: Two-dimensional histograms of the a–θ (middle left panel) and of the a–χ 2 (bottom left panel) parameter space based on the posterior samples in the MCMC analysis. The dashed, dashed–dotted, and dotted contours in these panels represent the 1σ, 2σ, and 3σ confidence intervals, respectively. The top left, middle right, and bottom right panels show the one-dimensional histograms of the posterior distributions in the MCMC analysis for spin, inclination, and reduced χ 2, respectively. The width of the contours is proportional to the strength of reflection in the observation, which was used as weighting when combining the posterior distributions into a single measurement. The solid lines represent the modes of the distributions, and the dashed lines represent the ±1σ credible regions. Throughout the entire figure, the blue lines represent the results from the first epoch, and the red lines represent the results from the second epoch. In the middle left panel, the black and green points show the values obtained by combining the posterior distributions through the two different methods highlighted in this paper.
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: Residuals in terms of σ in the 6–8 keV band produced when fitting the spectrum obtained by combining 52 NICER observations from the soft state of XTE J2012+381 using the best-fit reflection model obtained by fitting the second NuSTAR observation. The NICER observations used to obtain this combined spectrum are indicated by the two vertical dashed magenta lines in Figure 1. The vertical red line in this plot indicates the rest energy of the H-like Fe XXVI at 6.97 keV.
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: The complete corner plot of the MCMC analysis. The lower left half of the plot shows the corner plot of the analysis of the observations from the first epoch, with the dark-blue contours representing the joint NICER and NuSTAR fits and the light-blue ones representing the NuSTAR fits alone. The upper right half of the plot shows the corner plot of the analysis of the observations from the second epoch, with the yellow contours showing the results from the joint NICER and NuSTAR fits and the red ones showing the individual NuSTAR results. The panels on the diagonal of the plot represent the one-dimensional histograms of the marginalized posterior distributions for each parameter in the MCMC analysis. The vertical lines in the diagonal subplots represent the values around which Gaussian proposal distributions were generated and used to initialize the walkers in the MCMC run.
Paper: An Extreme Black Hole in the Recurrent X-Ray Transient XTE J2012+381
Authors: Paul A. Draghis, Jon M. Miller, McKinley C. Brumback, Andrew C. Fabian, John A. Tomsick, Abderahmen Zoghbi
Figure caption: Histograms of the posterior distributions in the MCMC analysis for spin and inclination. The two columns of panels on the left show the distributions grouped by observation analyzed, when using different models, with the first and third rows indicating fits to the NuSTAR observations alone and the second and fourth rows indicating joint NuSTAR and NICER fits. The two columns of panels on the right show the distributions grouped by the model used to fit the observations.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: CHIMERA r (red) and g (blue) 10 s cadence photometry reveals deep eclipses. Upper three panels: Entire observation on each occasion. The gaps are due to large error bars in the data where cloud cover or highly variable seeing prevented a good extraction of the data. Bottom panel: The data from 2023 January 23 and February 17 are folded over the 55.08 minute orbital period.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Left: False-color X-ray image of SRGeJ0453 in the 0.3–2.3 keV energy band from combined data of four all-sky surveys of SRG/eROSITA. The image was smoothed with a 15″ Gaussian kernel. The white box shows the field of view of the optical image on the right. Right: Optical image around SRGeJ0453 based on RTT-150 data with a white filter. The red circle with a radius of 5.″6 (98% localization error, R98) is centered at the X-ray position of SRGeJ0453.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: The SED of SRGeJ0453 is well fit by a T eff = 16,570 K blackbody (solid, black line) or a T eff = 12,210 K pure-helium WD model atmosphere (blue squares) at UV/optical wavelengths. There is an IR contribution from the donor and/or accretion disk.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: Phase-folded light curve of RTT-150 data. Blue circles correspond to the 2023 January 19 data, and red circles correspond to the 2023 January 20 data. The light curve shows low-amplitude (≈01–03 m ) flickering. Only the upper part of the light curve is shown out of eclipses.
Paper: SRGeJ045359.9+622444: A 55 Minute Period Eclipsing AM Canum Venaticorum Star Discovered from a Joint SRG/eROSITA + ZTF Search
Authors: Antonio C. Rodriguez, Ilkham Galiullin, Marat Gilfanov, Shrinivas R. Kulkarni, Irek Khamitov, Ilfan Bikmaev, Jan van Roestel, Lev Yungelson, Kareem El-Badry, Rashid Sunayev, Thomas A. Prince, Mikhail Buntov, Ilaria Caiazzo, Andrew Drake, Mark Gorbachev, Matthew J. Graham, Rustam Gumerov, Eldar Irtuganov, Russ R. Laher, Frank J. Masci, Pavel Medvedev, Josiah Purdum, Nail Sakhibullin, Alexander Sklyanov, Roger Smith, Paula Szkody, Zachary P. Vanderbosch
Figure caption: LRIS phase-averaged spectrum of SRGeJ0453. The characteristic features of an AM CVn are clear: helium emission lines imposed over a blue continuum. Metals such as Mg, Ca, N, and Na are present. Gray lines are locations where there are telluric features from the Keck Telluric Line List.