adsabs/AstroCLIMB huggingface dataset:
Paper: SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields
Authors: Robert Jarolim, Benoit Tremblay, Andrés Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, Anna Jungbluth, Miraflor Santos, Angelos Vourlidas, James P. Mason, Sairam Sundaresan, Cooper Downs, Ronald M. Caplan
Figure caption: Qualitative evaluation of the SuNeRF reconstruction of simulation data. We compare the ground-truth image (first row) with our SuNeRF reconstructions (second row) at different latitudes. The pixelwise difference shows where our reconstruction deviates from the ground-truth reference (third row). The uncertainty maps are computed from an ensemble of five different runs (fourth row). The SuNeRF reconstructions appear indistinguishable at larger scales. The primary errors occur close to off-limb and due to pixelwise shifts, while large-scale structures are consistent. The uncertainty maps align with regions of increased error, which enables a performance estimate in the absence of a reference image.
Paper: SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields
Authors: Robert Jarolim, Benoit Tremblay, Andrés Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, Anna Jungbluth, Miraflor Santos, Angelos Vourlidas, James P. Mason, Sairam Sundaresan, Cooper Downs, Ronald M. Caplan
Figure caption: Correlation between SuNeRF reconstruction and ground-truth reference. Left: 2D histogram of simulation data (ground truth) and our SuNeRF reconstructions. Right: 2D histogram of MAE and model uncertainty. The color bars give the total number of pixels per bin.
Paper: Starburst-induced Gas–Star Kinematic Misalignment
Authors: Elia Cenci, Robert Feldmann, Jindra Gensior, James S. Bullock, Jorge Moreno, Luigi Bassini, Mauro Bernardini
Figure caption: Left panels: temporal evolution of the average circularity parameter for the gas (top panel) and stars (bottom panel) in H22, computed with respect to the average angular momentum of the stellar component, within different apertures (0.1 R vir, 10 kpc, and 5 kpc). The gray bands, at z = 0.45–0.4 and z = 0.4–0.35, highlight approximately the time period during which the gas–star kinematic misalignment (KM) event occurs. Right panels: temporal evolution of the star formation rate (SFR; averaged over 100 Myr; top panel) and total gas mass (M gas;  bottom panel) in H22, within different apertures (0.1 R vir, 10 kpc, and 5 kpc). The gas disk is corotating with the stellar component at redshift z = 0.5 and experiences KM at z ∼ 0.45–0.35 that coincides with a large reduction of both the SFR and total gas mass.
Paper: Starburst-induced Gas–Star Kinematic Misalignment
Authors: Elia Cenci, Robert Feldmann, Jindra Gensior, James S. Bullock, Jorge Moreno, Luigi Bassini, Mauro Bernardini
Figure caption: Evolution of the baryons forming the preexisting gas disk in H22 at z = 0.45 (i.e., the preexisting baryons). Left panel: evolution of the fraction of preexisting baryons that formed stars (circles), which is still within the initial aperture of 10 kpc (triangles) and which has a circularity parameter ε > 0 (i.e., on corotating orbits with respect to the stellar component of the galaxy). Middle panel: mass-weighted probability density function (PDF) of the galactocentric radii of the preexisting baryons. Right panel: mass-weighted PDF of the circularity parameter of preexisting baryons with respect to stars, within 10 kpc. The color code refers to redshift. About 70% of the preexisting baryons is still within the galaxy by z = 0.3 and is concentrated within 2–5 kpc. About 95% of the preexisting baryons is converted into stars already by z ∼ 0.35. About 80% of the preexisting baryons retain a circularity parameter ε > 0.
Paper: Starburst-induced Gas–Star Kinematic Misalignment
Authors: Elia Cenci, Robert Feldmann, Jindra Gensior, James S. Bullock, Jorge Moreno, Luigi Bassini, Mauro Bernardini
Figure caption: Face-on and edge-on projections (upper and lower panels, respectively) of H22 in four snapshots around the period of KM and at z = 0. The gas is color-coded according to whether it is within (purple) or outside (blue) the 10 kpc from the center of the galaxy at z = 0.45, when the preexisting gas disk is still in place. The projections are rotated in the ﹩\left(x,y\right)﹩-plane such that the x-axis is aligned with the principal inertia axis associated with the largest moment. The preexisting gas is depleted by z ∼ 0.35, and the counterrotating gas accreted from the merging satellite settles into a misaligned disk by z ∼ 0.3. Stars formed out of the preexisting gas (orange points) remain within the galaxy. At z = 0, the stars formed from the preexisting baryons are still found in the central regions of H22.
Paper: From Feast to Famine: A Systematic Study of Accretion onto Oblique Pulsars with 3D GRMHD Simulations
Authors: Ariadna Murguia-Berthier, Kyle Parfrey, Alexander Tchekhovskoy, Jonatan Jacquemin-Ide
Figure caption: Several quantities averaged in time, as a function of obliquity angle. The quantities are the same as in Figure 2. The gray horizontal lines represent Ψopen = Ψopen,0, L = L 0, N tot = − ∣N 0∣, and r mag = r co. We averaged at times when the quantities are in the steady state (t > 10,000 r g/c); the error corresponds to the standard deviation over that time period. We show lines that connect the values for simulations with μ = 20 (green) and μ = 5 (blue) for both parallel (solid line) and antiparallel (dashed line) configurations. The data behind this figure is available in the tar.gz package. The package contains numerous numpy files with the data shown and a Juypter notebook to read and display the figure.(The data used to create this figure are available.)
Paper: From Feast to Famine: A Systematic Study of Accretion onto Oblique Pulsars with 3D GRMHD Simulations
Authors: Ariadna Murguia-Berthier, Kyle Parfrey, Alexander Tchekhovskoy, Jonatan Jacquemin-Ide
Figure caption: Different quantities as a function of time for μ = 20. The dashed lines correspond to simulations in which the magnetic field of the torus and the NS are antiparallel, and the solid line represents simulations in which they are parallel. The magenta line represents the perpendicular simulation. From top to bottom, the quantities are (a) mass accretion rate at the NS surface; (b) open magnetic flux at r = R LC normalized to an isolated pulsar; (c) jet power at r = R LC, similarly normalized; (d) total torque, similarly normalized; and (e) magnetospheric radius. See Section 3 for a detailed explanation of the quantities and how they were calculated. The horizontal lines represent Ψopen = Ψopen,0, L = L 0, N tot = − ∣N 0∣, and r mag = r co. The data behind this figure is available in the tar.gz package. The package contains numerous numpy files with the data shown and a Juypter notebook to read and display the figure.(The data used to create this figure are available.)
Paper: From Feast to Famine: A Systematic Study of Accretion onto Oblique Pulsars with 3D GRMHD Simulations
Authors: Ariadna Murguia-Berthier, Kyle Parfrey, Alexander Tchekhovskoy, Jonatan Jacquemin-Ide
Figure caption: Density slices through the μ–Ω (top row) and equatorial (bottom row) planes of our simulations with a magnetic moment of μ = 20 reveal that the increase in magnetic obliquity brings the system closer to the propeller state. We show the system at t = 14,200 r g/c ≈ 113 P *, for both parallel and antiparallel configurations. Left and middle left panels: at low obliquity, χ = 10°, the gas reaches the NS. Right and middle right panels: however, at high obliquity, χ = 60°, the magnetosphere pushes most of the gas outside of the corotation radius, shown with the dashed lines. As a result, the system enters the propeller regime, and the gas struggles to reach the NS. Directed pink lines trace out the magnetic field in the image plane. The solid cyan lines indicate the light cylinder.
Paper: From Feast to Famine: A Systematic Study of Accretion onto Oblique Pulsars with 3D GRMHD Simulations
Authors: Ariadna Murguia-Berthier, Kyle Parfrey, Alexander Tchekhovskoy, Jonatan Jacquemin-Ide
Figure caption: Density snapshots of a simulation with a magnetic moment of μ = 10 at different times, where the star's magnetic moment is perpendicular to its rotation axis. Top panels show different planes, from left to right: (a) the plane perpendicular to μ–Ω, (b) the μ–Ω plane, and (c) a plane between those two. The bottom panels are the equatorial plane. The pink lines represent the magnetic field of the in-plane component. The solid cyan line is placed at the light cylinder, and the dashed cyan line is the corotation radius.
Paper: From Feast to Famine: A Systematic Study of Accretion onto Oblique Pulsars with 3D GRMHD Simulations
Authors: Ariadna Murguia-Berthier, Kyle Parfrey, Alexander Tchekhovskoy, Jonatan Jacquemin-Ide
Figure caption: Density snapshots of the μ–Ω plane (top panel) and the equatorial plane (bottom panel) for simulations with χ = 60°, in an antiparallel configuration. We show different magnetic moments at time t = 14,200 r g/c, or around 113 NS spin periods. The pink lines represent the in-plane magnetic field component. The solid cyan line is placed at the light cylinder, and the dashed cyan line is the corotation radius.
Paper: TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068
Authors: Damiano F. G. Fiorillo, Maria Petropoulou, Luca Comisso, Enrico Peretti, Lorenzo Sironi
Figure caption: Spectral energy distribution of photons (thick solid yellow line) and all-flavor neutrinos (thick solid orange line) from the reconnection region. Single-flavor neutrino spectra, not including mixing (i.e., flavor oscillations), are also shown (dashed and dotted orange lines). For comparison, we show the estimated peak neutrino luminosity in Equation (C10) (orange circle). The nonthermal cascade spectrum is overplotted with a dotted black line. Other lines indicate emission from different processes (see inset legend) before accounting for γ γ pair production. Gamma-ray data by Fermi-LAT (Abdollahi et al. 2020) and upper limits by MAGIC (Acciari et al. 2019) are also included (light and dark green markers, respectively). Solid and dashed black lines show the best-fit all-flavor IceCube neutrino spectrum with a 68% confidence interval, adopted from Abbasi et al. (2022).
Paper: TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068
Authors: Damiano F. G. Fiorillo, Maria Petropoulou, Luca Comisso, Enrico Peretti, Lorenzo Sironi
Figure caption: Regions of the L − L X,[2,10] keV parameter space leading to a neutrino signal from NGC 1068 consistent with IceCube observations. The axis at the top shows the bolometric intrinsic X-ray luminosity L X, which we use in our equations. We show in red the requirements on the cooling break (Equation (12)) and in blue the constraints on the peak neutrino luminosity (Equation (17)). We show in green the region where the pairs injected by the attenuation of hadronically produced MeV photons have a number density from 5% to 100% of the pair density inferred from the Compton opacity. We use benchmark values M 7 = 0.67, η  p  = 0.05, and E  p,br = 25 TeV.
Paper: On the Source Contribution to the Galactic Diffuse Gamma Rays above 398 TeV Detected by the Tibet ASγ Experiment
Authors: S. Kato, D. Chen, J. Huang, T. Kawashima, K. Kawata, A. Mizuno, M. Ohnishi, T. Sako, T. K. Sako, M. Takita, Y. Yokoe
Figure caption: Incoming directions of the Galactic diffuse gamma-ray events above 398 TeV observed by the Tibet ASγ experiment (red points) and the positions and extensions of the sub-PeV LHAASO sources: the gamma-ray sources detected by LHAASO above 100 TeV (blue circles; Cao et al. 2023) in the Galactic coordinates. The extensions of the sub-PeV LHAASO sources have 95% containment radii assuming a two-dimensional Gaussian morphology. For point-like sources, the 95% upper limits on the extensions are shown. The green dashed circle with a 6° radius encloses the Cygnus region centered at (l, b) = (79.°62, 0.°96), the position of HAWC J2030 + 409 (Abeysekara et al. 2021). Note that some of the sub-PeV LHAASO sources have ∣b∣ > 10° and thus are not shown in the plot.
Paper: TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068
Authors: Damiano F. G. Fiorillo, Maria Petropoulou, Luca Comisso, Enrico Peretti, Lorenzo Sironi
Figure caption: Proton (thick blue line) and all-flavor neutrino (thick orange line) energy density spectra normalized to the magnetic energy density. The steady-state proton distribution has η  p  = 0.05. The spectrum of protons “injected” into the radiative region with ﹩{\eta }_{p}^{* }=0.1﹩ (i.e., the reconnection downstream) is overplotted with a light blue solid line. Vertical lines indicate characteristic proton energies discussed in the text. Protons with energies E  p  ≳ E  p,cool cool due to photomeson interactions with the X-ray coronal photons. Cyan and yellow markers indicate the analytical expression for the steady-state proton and neutrino energy distribution, which agrees well with the numerical solution.
Paper: TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068
Authors: Damiano F. G. Fiorillo, Maria Petropoulou, Luca Comisso, Enrico Peretti, Lorenzo Sironi
Figure caption: Timescales for proton acceleration, escape, and cooling in the reconnection region. We include synchrotron cooling, p γ interactions with X-ray photons, and BH losses due to X-rays and OUV photons. We choose benchmark parameters L = 5 r  g , L X,43 = 5, and M 7 = 0.67. Vertical lines indicate three characteristic proton energy scales discussed in the text.
Paper: TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068
Authors: Damiano F. G. Fiorillo, Maria Petropoulou, Luca Comisso, Enrico Peretti, Lorenzo Sironi
Figure caption: Same as Figure 2, accounting for the corrections arising in the fast-cooling regime. We choose ﹩{\eta }_{p}^{* }=0.067﹩ to match the value of η  p  = 0.05 used in the marginally fast-cooling regime of Figure 2. Below the thin black dashed line, protons are fast-cooling (E  p,cool < E  p,br).
Paper: TeV Neutrinos and Hard X-Rays from Relativistic Reconnection in the Corona of NGC 1068
Authors: Damiano F. G. Fiorillo, Maria Petropoulou, Luca Comisso, Enrico Peretti, Lorenzo Sironi
Figure caption: Same as Figure 2 but for spherical geometry. We show the regions in the parameter space R − L X,[2–10] keV, where R is now the size of the spherical region.
Paper: Empirically Constraining the Spectra of Stellar Surface Features Using Time-resolved Spectroscopy
Authors: David Berardo, Julien de Wit, Benjamin V. Rackham
Figure caption: On the use of loose (nonbiasing) physical constraints. Left: example of constraining the out-of-feature portion of a spectrum (gray bands) to be consistent with a blackbody envelope. Right: all spectra from a blind retrieval for a spot shown in blue, with the subset consistent with a blackbody envelope shown in orange. All spectra have been multiplied by the projected surface area of the spot feature to illustrate scatter due only to model uncertainty. Using this simple physics-based constraint, precision in the retrieved spectra is increased by ∼15×, which leads to an increase in the precision on the spot size and position by ∼5–8×. The true spot size and latitude for this example are 0.2 and 0.7 radians, respectively, illustrating that the posterior constraints provide a more accurate and precise retrieval.
Paper: Empirically Constraining the Spectra of Stellar Surface Features Using Time-resolved Spectroscopy
Authors: David Berardo, Julien de Wit, Benjamin V. Rackham
Figure caption: Long stare vs. series of snapshots, highlighting the effectiveness of different observing strategies for stars with rotation periods of 3, 10, and 30 days. Heat maps show the median residual on the photosphere spectrum when observing in snapshots (relative to the OOT uncertainty) for three different rotation periods. The percentage in each cell represents the total observation time relative to the rotation period of the star. The snapshot duration is relative to a 2 hr duration that would be typically observed OOT for a transit of planets around TRAPPIST-1.
Paper: Empirically Constraining the Spectra of Stellar Surface Features Using Time-resolved Spectroscopy
Authors: David Berardo, Julien de Wit, Benjamin V. Rackham
Figure caption: An example retrieval when fitting for the position, size, and spectral contribution of a spot feature. The upper plot shows the posterior distribution for the position and size of the spot feature, with the true value indicated in blue. The bottom panel shows the retrieved spectrum of both the photosphere and the spot itself, similar to Figure 2.
Paper: Empirically Constraining the Spectra of Stellar Surface Features Using Time-resolved Spectroscopy
Authors: David Berardo, Julien de Wit, Benjamin V. Rackham
Figure caption: Minimum phase coverage of observations to leverage time-resolved spectroscopy. The Y-axis represents the median error on the photosphere during a continuous observation of a star with three spot features. The x-axis shows the starting phase of an observation, while different colors correspond to different durations of a continuous observation (relative to the full rotation period). The dashed line shows the targeted precision, chosen as the out-of-transit spectrum of a previous NIRISS observation of the TRAPPIST-1 system (“OOT uncertainty”).
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Violin plots showing (from left to right) the inferred black hole mass, disrupted star mass, TDE penetration factor β ≡ r p/r t, and the time since optical peak when the envelope has fully contracted to the circularization radius (R  v  = R c) and the SMBH accretion rate peaks. The bottom panels show event-averaged distributions for each parameter (in blue) alongside the expectations of TDE loss-cone analysis (black lines; see text for details). The orange ticks in the third panel show the maximum penetration factor ﹩{\beta }_{\max }({M}_{\star },{M}_{\mathrm{BH}})﹩ imposed by the Hills limit given the most probable SMBH and star mass for each event. For comparison, we also show in the final panel the observed timescales relative to the optical peak of delayed radio transients, nominally associated in the cooling envelope with when the SMBH accretion rate peaks. References: iPTF 16fnl (Horesh et al. 2021a); AT 2018hyz (Cendes et al. 2022); ASASSN-15oi (Horesh et al. 2021b); IGR J12580 + 0134 (Perlman et al. 2022).
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Evolution of ν L  ν  light curve at ν = 6 × 1014 Hz and the effective temperature, photospheric radius, and proxy X-ray light curves ﹩{L}_{{\rm{X}}}\equiv {10}^{-2}\dot{M}{c}^{2}﹩ (where ﹩\dot{M}﹩ is the SMBH accretion rate) of the postcircularization cooling envelope emission phase for different parameter choices. The black curves correspond to a fiducial model with SMBH mass M BH = 2 × 106 M ⊙, stellar mass M ⋆ = 1 M ⊙, penetration factor β = 1, disk viscosity α = 0.01, and SMBH feedback efficiency parameter η = 10−4. Solid curves show the effect of changing various parameters as marked while keeping the other parameters fixed at the fiducial model values. Dashed curves correspond to β = 5, with the rest of the parameters the same as the corresponding solid curve. The sudden decrease in the photosphere radius and concomitant increase (decrease) in the emission luminosity (temperature) corresponds to the final contraction of the envelope to the circularization radius. While this signals the end of the envelope phase, thermal and nonthermal emission from the accretion disk and/or its jet can fully commence after this transition.
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Proxy X-ray light curves ﹩{L}_{{\rm{X}}}\equiv {10}^{-2}{\dot{M}}_{\mathrm{BH}}{c}^{2}﹩ of the best-fit models for all TDEs in our sample, where ﹩{\dot{M}}_{\mathrm{BH}}(t)﹩ is the SMBH accretion rate. Insofar as X-ray emission from the inner accretion disk may only be visible through the initially narrow polar funnel of the envelope, these luminosities may reflect those observed for a fraction of viewing angles.
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Light curves for a subset of TDEs from our sample. The green and red markers indicate the ztfg and ztfr band for different TDEs, while the band represents the 90% credible interval from our fit. The vertical gray band indicates the 90% credible interval for χ t fb, i.e., where the fit transitions from the Gaussian rise to the cooling envelope.
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Inferred black hole masses from the application of our model vs. the observed galaxy bulge velocity dispersion σ gal. The red shaded band shows the 3σ contour M BH–σ gal relation from Kormendy & Ho (2013).
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Photospheric radius and temperature evolution for time since envelope circularization for the best-fit model for all TDEs in our sample.
Paper: Tidal Disruption Events through the Lens of the Cooling Envelope Model
Authors: Nikhil Sarin, Brian D. Metzger
Figure caption: Example corner plot showing a subset of the parameters from our analysis of AT 2020mot.
Paper: The Hidden Companion in J1527: A 0.69 Solar-mass White Dwarf?
Authors: Zhi-Xiang Zhang, Hao-Bin Liu, Tuan Yi, Mouyuan Sun, Wei-Min Gu
Figure caption: The CFHT spectrum and the best-fitting templates. The green spectrum represents the observed data. The blue curves are the rebinned spectrum with 10 times of the sampling interval. The red spectrum corresponds to the best-fitting template. The black spectrum is the broadened template using a rotational kernel of ﹩v\sin i=94\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩ (Lin et al. 2023). The residuals between the rebinned spectrum and the templates are shown in the lower panels. Gray vertical dotted lines indicate strong stellar absorption lines.
Paper: The First Polarimetric View on Quasiperiodic Oscillations in a Black Hole X-Ray Binary
Authors: Qing-Chang Zhao, Lian Tao, Han-Cheng Li, Shuang-Nan Zhang, Hua Feng, Ming-Yu Ge, Long Ji, Ya-Nan Wang, Yue Huang, Xiang Ma, Liang Zhang, Jin-Lu Qu, Yan-Jun Xu, Shu Zhang, Qian-Qing Yin, Qing-Cang Shui, Rui-Can Ma, Shu-Jie Zhao, Pan-Ping Li, Zi-Xu Yang, He-Xin Liu, Wei Yu
Figure caption: Panel (a): the phase-folded light curve on QPO period of Swift J1727.8–1613. The flux is normalized by averaged flux. Panel (b): the PD as a function of the QPO phase. The PD is estimated from the model Const∗Polconst∗Powerlaw. The horizontal dashed line represents the constant fit, while the solid line represents the sine function fit of PD. Panel (c): same as panel (b), but for PA. Panel (d): Γ as a function of the QPO phase. Panel (e): the two-dimensional QPO evolution with time.
Paper: The First Polarimetric View on Quasiperiodic Oscillations in a Black Hole X-Ray Binary
Authors: Qing-Chang Zhao, Lian Tao, Han-Cheng Li, Shuang-Nan Zhang, Hua Feng, Ming-Yu Ge, Long Ji, Ya-Nan Wang, Yue Huang, Xiang Ma, Liang Zhang, Jin-Lu Qu, Yan-Jun Xu, Shu Zhang, Qian-Qing Yin, Qing-Cang Shui, Rui-Can Ma, Shu-Jie Zhao, Pan-Ping Li, Zi-Xu Yang, He-Xin Liu, Wei Yu
Figure caption: Left panel: representative example of a 100 s light curve of Swift J1727.8–1613 and the corresponding IMFs (C1–C5). Right panel: the PDS of the original light curve and the 1st to 5th IMFs.