adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: Comparison of the periastron flare properties of DQ Tau (colored points) with those of large X-ray flares from young stellar members of the Orion Nebula Cluster, known as COUP flares (Getman et al. 2008), and of numerous other star-forming regions, referred to as MYStIX/SFiNCs flares (Getman & Feigelson 2021). The DQ Tau X-ray flares are color-coded as follows: red for the 2010 flare (Getman et al. 2011), blue for the 2021 flare (Getman et al. 2022a), and green for the 2022 flare (current study). Panels (a) and (b) display the flare rise/decay timescales and peak X-ray luminosities for COUP flares (black) and DQ Tau flares (colored points). Panels (c) and (d) show the flare duration, peak X-ray luminosity, and flare energy for MYStIX/SFiNCs flares (black and gray) and DQ Tau flares (colored points). The lower limits for the “incomplete” (partially captured) MYStIX/SFiNCs flares are shown in gray.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: Fitting of the Chandra spectra. The underlying Chandra data cover the 1.1–1.9 orbital phase range. (a) The “flare” spectrum at the orbital phase 1.6 obtained from the single snapshot ObsID 26471. (b) This spectrum is merged from the data of the remaining 11 Chandra snapshots that include the characteristic (eight observations; Figure 3) and postflare (three observations) X-ray emission states. The best-fit optically thin thermal plasma models are shown with the black solid lines. The lower subpanels of each panel show the residuals between the data and the model.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: ∣P mag/P 0∣ as a function of days since DQ Tau’s apastron, over one-half orbit. Refer to Figure 5 in Adams et al. (2011) for a similar analysis in the case of the V773 Tau A binary system.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: Fitting of the optical SEDs using the blackbody model. The fitted data are represented in red, while the 3σ error bars are displayed in gray. The best-fit blackbody models are illustrated in blue. Legends in the upper left corner of each panel show the sequential numbers listed in column (1) of Table 2.
Paper: X-Ray, Near-ultraviolet, and Optical Flares Produced by Colliding Magnetospheres in the Young High-eccentricity Binary DQ Tau
Authors: Konstantin V. Getman, Ágnes Kóspál, Nicole Arulanantham, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, Sierk E. van Terwisga
Figure caption: Fitting of the NUV SEDs using the blackbody model. The fitted data are represented in red, while the 3σ error bars are displayed in gray. The best-fit blackbody models are illustrated in blue. Legends in the upper left corner of each panel show the sequential numbers listed in column (1) of Table 3.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: SFR as a function of stellar mass. In both panels, GLSBGs are represented by the big blue open circles with error bars. For comparisons, the H I-rich LSBGs from Du et al. (2015; small green circles), the dwarf LSBGs from McGaugh et al. (2017; magenta open diamonds), massive spiral galaxies from Di Teodoro et al. (2021; cyan open squares), the Milky Way with M * = 6.08 × 1010 M ⊙ and SFR = 1.65 M ⊙ yr−1 from Licquia & Newman (2015; red filled star), and the GLSBG UGC 1382 from Hagen et al. (2016; the gray filled triangle with error bars) are displayed as well. For a direct comparison, UGC 1382 with our measurements in this work is highlighted by the filled blue circle. The black solid line shows the MS trajectory defined for the local SDSS SFGs (0.04 < z < 0.1, 5 × 108 < M * < 5 × 1011 M ⊙) by Elbaz et al. (2007), with the extended black, dashed lines representing its linear extrapolation to both the lower-mass and higher-mass ends (E07 MS), and the two black dotted lines show the 68% confidence level of the E07 MS. The red dashed curve is the star formation MS trajectory defined for local SDSS galaxies (0.01 < z < 0.05, 108 < M * < 1012 M ⊙) by Saintonge et al. (2016; S16 MS). The gray solid and dashed lines represent constant sSFR values of 0.1 and 0.001 Gyr−1, respectively. The length of the black downward arrow on some points does not refer to the actual lower error of the point, and it only means that the original lower error bar below the data point is so large that it stretches far below the figure boundary. In the left panel, the SFRs are estimated from FUV fluxes without correction for internal dust extinction, while in the right panel, the SFRs are from dust-corrected FUV fluxes; however, the correction is quite uncertain for this population of LSBGs, which should be very low in dust so it definitely introduces very large errors. The Chabrier IMF is assumed.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: Images of the 17 GLSBGs definitely meeting the “diffuseness index” criterion. For each galaxy, we show its optical and UV images in individual frames of the same physical side size labeled at the top right of the optical frame. The optical images are g, r, and z composite image from DECaLs, except for NGC 5533 and NGC 5905, which have no z-band images from DECaLs, and the UV images are FUV and NUV composite images from GALEX.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: Images of the other 10 GLSBGs from Schombert (1998). The illustration for this figure is the same as Figure 1. UGC 3968 and UGC 4219 have no z-band images from DECaLs so their optical images are a composite of only g- and r-band images from DECaLs.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: Relation between H I mass and stellar mass of the GLSBGs (blue open circles). For comparisons, the H I-selected LSBGs from Du et al. (2015; green crosses), LSBGs from McGaugh et al. (2017; magenta open diamonds), and the M *-selected sample of galaxies binned with a width of log M * = 0.5 (brown filled squares with error bars) from Parkash et al. (2018), and the Milky Way (red filled star) with M H I = 8.2 × 109 M ⊙ from Misiriotis et al. (2006) are displayed as well. The black solid line represents the relation followed by the H I-selected sample of galaxies with a 1σ scatter of 0.5 dex, and the gray dashed line shows the relation followed by the spiral galaxies out of the M *-selected sample with a 1σ scatter of 0.4 dex from Parkash et al. (2018).
Paper: Exploring the Origin of Stars on Bound and Unbound Orbits Causing Tidal Disruption Events
Authors: Shiyan Zhong, Kimitake Hayasaki, Shuo Li, Peter Berczik, Rainer Spurzem
Figure caption: Dependence of the number density of the bound stars on the penetration factor (β). The figure formats are the same as Figure 4, but for β.
Paper: Simultaneous Estimates of Star-cluster Age, Metallicity, Mass, and Extinction (SESAMME). I. Presenting an MCMC Approach to Spectral Stellar Population Fitting
Authors: Logan H. Jones, Svea Hernandez, Linda J. Smith, Bethan L. James, Alessandra Aloisi, Søren Larsen
Figure caption: Fractional residual difference of the ages (top), reddening (middle), and masses (bottom) inferred for the eight synthetic FUV spectra with (“nominal”) and without (“no-neb”) a nebular continuum component in the modeling. All points are colored according to the input age for that mock cluster spectrum (blue for 3 Myr, gold for 30 Myr). Squares denote low-metallicity clusters (spectra 1–4) and circles denote solar metallicity clusters (spectra 5–8).
Paper: Exploring the Origin of Stars on Bound and Unbound Orbits Causing Tidal Disruption Events
Authors: Shiyan Zhong, Kimitake Hayasaki, Shuo Li, Peter Berczik, Rainer Spurzem
Figure caption: The same format as Figure 4, but for the unbound stars. Equation (15) is used to evaluate the theoretical number density quantitatively.
Paper: Exploring the Origin of Stars on Bound and Unbound Orbits Causing Tidal Disruption Events
Authors: Shiyan Zhong, Kimitake Hayasaki, Shuo Li, Peter Berczik, Rainer Spurzem
Figure caption: The same format as Figure 5, but for the unbound stars. Equation (14) is used to evaluate the theoretical number density quantitatively.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Post-impact circumplanetary disk mass (M  d ) for collisions between nonrotating bodies. The disk mass is shown as a function of the pre-impact angular momentum budget (J 0). Each panel presents a distinct impactor-to-target mass ratio (γ). The red dashed horizontal line is the absolute minimum disk mass (M  d  ≥ M ☾) needed to form the Moon assuming perfect accretion from the protolunar disk. The green-shaded region constrains the range of disk masses suggested by post-impact N-body simulations of accretion in the circumplanetary disk.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Pre-impact initial conditions for collisions with nonrotating targets and impactors. The pre-impact trajectory is defined by specifying the initial total angular momentum budget (J 0) and the asymptotic relative velocity (v ∞). The asymptotic impact parameter (b ∞) is then computed according to Equation (4). Each line tracks a constant J 0, where the numbers at the top of each line specify the value of J 0.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Post-impact iron fraction of the protolunar disk (F Fe  d ) for disks with at least one lunar mass, shown as a function of the asymptotic relative velocity (v ∞). The iron fraction of the Moon has been constrained at no more than 2% by mass, indicated by the red dashed horizontal line. This line represents the maximum iron fraction if we assume that iron is accreted from the circumplanetary disk into the Moon at the same rate as silicates. This constraint can be relaxed if we assume that iron is accreted into the growing Moon less efficiently than silicates.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Distribution of compositional variations between the post-impact Earth and protolunar disk, where δ pd is determined according to Equation (1). A value of zero indicates that the planet and disk are composed of the same fraction of impactor material. A value greater than zero indicates that the disk is enriched in impactor material relative to the planet and vice versa. The numbers on the left are the impactor-to-target mass ratio (γ). Note that as γ decreases, the disk tends to be composed predominantly of impactor material.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Pearson correlation coefficients for a selection of pre-impact and post-impact properties. The blue squares indicate a positive correlation between properties, with stronger correlations marked by darker shades of blue. The red squares indicate a negative correlation, with darker shades of red indicating a stronger correlation.
Paper: A Systematic Survey of Moon-forming Giant Impacts. I. Nonrotating Bodies
Authors: Miles Timpe, Christian Reinhardt, Thomas Meier, Joachim Stadel, Ben Moore
Figure caption: Post-impact equatorial radius of the central body (R  p ) relative to the HSSL radius (R  HSSL ). A value at or near one indicates that the post-impact central body is rotating at its maximum rate and may still be actively exchanging material with the circumplanetary disk or ejecta.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Left panel: the mass accretion rate through the inner boundary of the simulation domain in units of L Edd/c 2, smoothed using moving averages over five consecutive dumps (≈460t  G  in time). The shaded regions show the 1σ standard deviations, and the black dashed line shows the target mass accretion rate of ﹩\dot{m}=3﹩ that applies for all the S3E simulations. Middle panel: the total luminosity escaping through a cone of 15° opening angle at r = 150r  G  in units of L Edd, using the same smoothing as in the left panel. Right panel: the instantaneous radiative efficiency, ﹩\eta =L/\dot{M}{c}^{2}﹩.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Spectra for each simulation accounting for the radiation escaping through a cone of 15° opening angle about the z-axis at r = 150r  G , time-averaged over the final 1000t  G  of each simulation, plus a model spectrum from Shimura & Takahara (1995) for T = 3 × 106 K and a spectral hardening factor of f = 2.2. To give some idea of the variability of our spectra, the shaded regions show the minimum and maximum values of the spectra in each bin over the averaging interval.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Pseudocolor plots of 〈ρ〉 t,ϕ , with a white contour showing the effective photosphere for the S3Ea0_gray (left) and S3Ea0 (right) simulations, averaged over azimuth and time for all dumps after t = 6000t  G . Note that 1r  G  on the vertical axis is stretched compared to 1r  G  on the horizontal axis. Thus, the image is distorted, which is necessary in order to be able to adequately see the vertical disk structure.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Time-averaged radial profiles of the disk scale height, H/R (left); the ratio of heating rate, Q +, to cooling rate, Q − (middle); and the mass accretion rate, ﹩\dot{m}﹩ (right), for simulations S3Ea0_gray and S3Ea0. The time averaging is performed over the window 10,000tG –15,000t  G . The shaded regions show the 1σ standard deviations, and the dashed black SS  i  curves show the initial scale height profile and target ﹩\dot{m}﹩ used for both disks.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Left panel: light curves for multiple energy bins for the S3Ea9 simulation, accounting for the radiation escaping through a cone of 15° opening angle about the z-axis at r = 150r  G . Right panel: power spectra for the 3 and 90 keV light curves over the period from 6000tG  to 10,000t  G .
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Pseudocolor plot showing the local luminosity, integrated over all frequency bins, averaged over azimuth and time for the interval t = 2500tG −5000t  G  for simulation S3Ea9. The color scale is chosen such that any radiation moving radially toward the black hole shows up as blue, while outgoing radiation appears red. The solid black line provides the location of the effective photosphere of the disk. Note that at later simulation times, the radiation in most energy bins is outflowing.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Isosurface plots from simulation S3Ea9 at t = 7900t  G  showing roughly where each spectral component dominates the photon energy density. The 3 keV emission (blue) is mostly found along the photosphere of the disk, 9 keV emission (green) is concentrated near the inner edge of the disk, 30 keV emission (yellow) is found in a corona sandwiching the inner part of the disk, and 90 keV emission (orange) occupies the hottest regions of the corona surrounding the black hole. For reference, the blue disk in this plot has a radius of ≈60r  G , i.e., this is not the whole disk or simulation domain.
Paper: Multifrequency General Relativistic Radiation Magnetohydrodynamic Simulations of Thin Disks
Authors: P. Chris Fragile, Peter Anninos, Nathaniel Roth, Bhupendra Mishra
Figure caption: Time evolution of the toroidal component of the magnetic field, B  ϕ , at R = 10r  G  for the S3Ea0_gray (left) and S3Ea0 (right) simulations. The enhanced toroidal field in the gray case provides sufficient vertical support to stabilize the disk, unlike in S3Ea0.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: The colors of NUV − r and g − r of the inner (red triangle) and outer parts (blue square) for each GLSBG. Chilingarian & Zolotukhin (2012) identify the loci of blue clouds (blue dashed) and the red sequence (red dashed) based on SDSS galaxies, and also define the relation between NUV − r and g − r for SDSS galaxies with r-band absolute magnitudes −23 < M  r  < − 21 mag (black solid curve). The right and top bars show the NUV − r and g − r histogram distributions of the inner (red) and outer parts (blue) of the GLSBGs.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: Gas mass fraction vs. stellar mass. The open circles represent GLSBGs and the filled circles represent the mean values of five bins in M * of S16 MS galaxies (Saintonge et al. 2016). The blue and orange colors represent H I gas mass fractions (f H I = M H I/M *) and H2 gas mass fractions (f H2 = M H2/M *), respectively. The molecular-to-atomic ratio (R mol = M H2/M H I) for GLSBGs is assumed as 0.01 in the left panel and 0.1 in the right panel. The red filled star represents the Milky Way (﹩{M}_{{{\rm{H}}}_{2}}﹩ = 1.3 × 109 M ⊙ and M H I = 8.2 × 109 M ⊙) from Misiriotis et al. (2006).
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: SFR against stellar mass (M *) for the inner and outer regions of the 27 GLSBGs. For each galaxy, the inner, the outer, and the entire galaxy are shown as an open red triangle, an open blue square, and an open black circle, respectively. The filled red triangle, blue square, and black circle, respectively, represent the mean values for the inner, outer, and entire galaxy. The black solid line represents the E07 MS (Elbaz et al. 2007). The red dashed curve represents the S16 MS (Saintonge et al. 2016). The Chabrier IMF is assumed. Note that the three isolated markers in the bottom left region in this figure are the inner, outer, and entirety of UGC 9024, which is not a traditional giant galaxy in terms of stellar mass, but is identified as a GLSBG by the “diffuseness index” criterion from Sprayberry et al. (1995).
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: SFR against stellar mass (M *) for the inner (red triangle) and outer (blue square) parts of each GLSBG. The black circle represents the entire GLSBG. The black solid line represents the E07 MS (Elbaz et al. 2007). The red dashed curve represents the S16 MS (Saintonge et al. 2016). The Chabrier IMF is assumed.
Paper: Star-forming Main Sequence of Giant Low Surface Brightness Galaxies
Authors: Wei Du, Cheng Cheng, Pengliang Du, Lin Du, Hong Wu
Figure caption: Continuation of Figure 7.
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: X-ray phase space of extragalactic transients, including GRBs, SBOs, SNe, TDEs, AGNs, and FBOTs, with all other classes of transients from this work underplotted in gray. Peak luminosity vs. duration is shown as points for modeled SBOs (Nakar 2012), with input progenitor radius and breakout energy indicated in the legend by R and E, respectively. We underplot Eddington luminosities (as horizontal dashed lines) for some potentially relevant BH progenitor masses for both FBOTs and TDEs/AGNs (Ramsden et al. 2022; Yao et al. 2023). The FBOT X-ray counterparts occupy a luminosity range that is intermediate between normal SNe (shades of red) and GRBs (shades of green). At right in the TDE/AGN panel, we show preflare AGN luminosities for all included AGNs. Included events are listed in Tables A1–A5.
Paper: The Luminosity Phase Space of Galactic and Extragalactic X-Ray Transients Out to Intermediate Redshifts
Authors: Ava Polzin, Raffaella Margutti, Deanne L. Coppejans, Katie Auchettl, Kim L. Page, Georgios Vasilopoulos, Joe S. Bright, Paolo Esposito, Peter K. G. Williams, Koji Mukai, Edo Berger
Figure caption: X-ray phase space of Galactic (CVs, magnetar flares/outbursts, and cool stellar flares) and Galactic/extragalactic (XRBs, ULXs, and FRBs) transients and variables, including those classes of event with some signals that have been observed to originate within the Galaxy, such as CVs (novae and dwarf novae), magnetar flares and outbursts, FRBs (specifically the Galactic FRB 200428), cool stellar flares, XRBs, and ULXs. We underplot the Eddington luminosity for a 1.4 M ⊙ progenitor for additional context in the XRBs/ULX panel. With the exception of the CV panel, at right, we show quiescent luminosities for each class of object. Included events are listed in Tables A6−A9.