adsabs/AstroCLIMB huggingface dataset:
Paper: The Propagation of Coherent Waves Across Multiple Solar Magnetic Pores
Authors: S. D. T. Grant, D. B. Jess, M. Stangalini, S. Jafarzadeh, V. Fedun, G. Verth, P. H. Keys, S. P. Rajaguru, H. Uitenbroek, C. D. MacBride, W. Bate, C. A. Gilchrist-Millar
Figure caption: Wavelet power spectrum of the cross-sectional area time series of P3 from the 4170 Å ROSA continuum filter. The contoured region are those regions calculated to be above the 95% confidence of containing coherent oscillatory power. The hatched region to the bottom of the figure represents the cone of influence.
Paper: GW170817 4.5 Yr After Merger: Dynamical Ejecta Afterglow Constraints
Authors: Arvind Balasubramanian, Alessandra Corsi, Kunal P. Mooley, Kenta Hotokezaka, David L. Kaplan, Dale A. Frail, Gregg Hallinan, Davide Lazzati, Eric J. Murphy
Figure caption: Late-time observations of the GW170817 field at 3 GHz from Makhathini et al. (2021) (black dots), Balasubramanian et al. (2021) (red star), and from this work (red downward pointing triangle for our 3σ upper limit). Chandra 1 keV observations scaled to 3 GHz with a power-law index of β = −0.584 (including the latest measurement by O’Connor & Troja 2022) are shown as purple squares (see, e.g., Haggard et al. 2017; Margutti et al. 2017; Troja et al. 2017, 2022; Hajela et al. 2022, and references therein). We extrapolate all X-ray data to 3 GHz using β = −0.584 because there is only marginal evidence for a potential spectral flattening around 3.5 yr since the merger (Balasubramanian et al. 2021; Hajela et al. 2022), which, however, has not been confirmed in the later observations by O’Connor & Troja (2022). We compare these observations with predicted kilonova afterglow light curves. Left: the solid lines in various shades of blue are the predicted kilonova afterglow light curves as a function of α (see Equation (3)) with the assumption that the minimum speed of the ejecta is β 0 = 0.3, for the parameters E = 1051  erg, p = 2.1, ϵ  e  = 7.8 × 10−3, ϵ B = 9.9 × 10−4, n = 9.8 × 10−3cm−3, and d = 40  Mpc (as in Makhathini et al. 2021) and α  M  = 5, 6, 7, 10, and 20 (the subscript M indicates the parameters from Makhathini et al. 2021). For comparison, the green and red dashed lines show the case of E = 1051  erg, ϵ  e  = 10−1, ϵ B = 10−3, n = 10−2cm−3, p = 2.2, and d = 40  Mpc (as in Kathirgamaraju et al. 2019), with α  K  = 20, ∞ (the subscript K indicates the parameters from Kathirgamaraju et al. 2019; see Section 3); Right: predicted radio light curves of binary NS ejecta for different EoS and mass ratios reproduced from Nedora et al. (2021) (see their Figure 4 and Table 2). See Section 3 for discussion.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Agreement of mock spectra created during forward modeling analysis (see Section 3.5 for more detail) with observed constraints from three X-ray observations of IC 860. The x-axes are the intrinsic 2–10 keV luminosity of the AGN, while the y-axes are the local obscuration column density. Each row shows the comparison to a different data set, labeled on the right. Left: the likelihood that each model (defined by an intrinsic luminosity and its obscuration) could create the number of observed 0.5–8 keV (Chandra) or 3–24 keV (NuSTAR) photons, effectively acting as a constraint on normalization of the model. Middle: the fraction of the 1000 spectra generated for each model that had a hardness ratio consistent with the range determined with BEHR based on the observation, effectively acting as a constraint on the spectral shape of the model. Right: the combined constraint to determine the models most likely to have both the normalization and spectral shape of the AGN needed to reproduce the sparse observed data. While the three data sets do not tell a completely consistent story, they firmly rule out bright AGN with intrinsic luminosity above 1042 erg  s−1.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Fitted kinematic position angles (black solid lines, with black dotted lines representing uncertainties) overplotted on the corresponding velocity fields (centered on the galaxy systemic velocity). The axes are in spatial units (1 kpc indicated by a bar), and the colorbars are in kilometers per second. The gray lines are logarithmically spaced contours from 30% to 95% of the integrated IFS flux peak. North is up in all plots, and the small ellipse in the CO velocity panel shows the beam. The position angles indicate that the stars and molecular gas are kinematically misaligned.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Left: images from HST WFC3 filters F275W (NUV band), F336W (U band), F160W (H band). Middle top: a three-color image of IC 860 constructed from HST WFC3 filters F814W, F606W, F438W, as R, G, and B channels, respectively. This image clearly reveals that IC 860 is a barred spiral galaxy. Middle bottom: F606W (V-band) image after applying an unsharp mask to increase the contrast of the weak features. We can clearly see the dust cones (wide opening angle outlined by the red lines) suggesting a galaxy-wide outflow. The overlaid contours represent the 113 GHz radio continuum source from CARMA (Section 2.4), with the beam size indicated at the upper right. The contour levels are 30%, 50%, 70%, and 90% of the maximum flux. Right: color difference images of IC 860's central regions (marked by the red box on the three-color image). All images follow the convention that north is up and east is left.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Left: the [N II]/Hα vs. [O III]/Hβ diagnostic diagram. The dashed and solid lines are demarcation lines for SF and AGN ionization, from Kauffmann et al. (2003) and Kewley et al. (2001), respectively. The [O III] line is not robustly detected (>3σ) in many bins, so we use the 3σ value as the upper limit for the [O III] line flux (gray squares with downward arrows). Bins where all four lines are robustly detected are shown as red stars. The green lines show the shock ionization boundaries from Alatalo et al. (2016b). Middle: the WHAN diagnostic diagram with classifications shown in different colors. The star-forming category, which is not shown because no spaxels meet this classification, lies to the upper left of the plotted region. Right: the WHAN classification map on top of the HST V-band image. The center of the galaxy is classified as weak AGN ionization while the remaining regions are consistent with the retired galaxy category (Section 4.2).
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: The middle panel shows the v NaD map (in kilometers per second, with respect to the galaxy systemic velocity) on top of the HST V-band image, while the surrounding panels show the normalized NaD ISM profiles overplotted with the best-fit models (black lines with shaded areas representing uncertainties), in the same color as the corresponding bin on the map. The outflow bin is marked with an arrow. The y-axes of all panels are set to the same scale. The blueshifted wing (red line) around the systemic component (green line) of the NaD absorption in the bottom left panel indicates the presence of an outflow, and the corresponding bin on the map overlaps with the dust cone. The vertical dashed lines in the small panels mark the stellar rest-frame vacuum wavelengths of the NaD doublet.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: One of the spectra from the combined IFS data cube after binning, overplotted with its best-fit continuum (Section 3.1). This spectrum is from the bin at the center of the galaxy. The gray shaded areas are masked during the continuum fitting, and the zoomed-in views for some important spectral features are shown in the smaller panels. The overall weak emission lines and strong Balmer absorption lines reflect the post-starburst nature of IC 860. There appears to be a small mismatch between the spectrum and the fitted continuum between 5400 and 5700 Å, where the original blue and red data cubes overlap, which could be caused by the noisy data in the original red cube. This small mismatch should not affect our results since there are no prominent spectral features within this region, and we test that our data combination is reliable in Section 2.3.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: FUV to FIR SED of the entire galaxy plotted with the median posterior model spectrum from the MCMC SED fitting technique (Section 3.4.1), with shaded regions showing the 16th–84th percentile uncertainties. The colored squares represent the actual data while the gray circles represent the model predictions. Decomposition of the model is plotted with different colors, and the residual is calculated as (F obs − F model)/F obs.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Examples of spatially resolved SEDs constructed from HST imaging data plotted with their best-fit models (Section 3.4.2). The left panel is a colormap showing the binning scheme, and the right panels are SEDs from different galaxy regions marked by colored points on the bin map. The color of the data points on the SED matches the color of its location markers on the bin map.
Paper: A Multiwavelength View of IC 860: What Is in Action inside Quenching Galaxies 
Authors: Yuanze Luo, Kate Rowlands, Katherine Alatalo, Elizaveta Sazonova, Abdurro'uf, Timothy Heckman, Anne M. Medling, Susana E. Deustua, Kristina Nyland, Lauranne Lanz, Andreea O. Petric, Justin A. Otter, Susanne Aalto, Sabrina Dimassimo, K. Decker French, John S. Gallagher III, Joel C. Roediger, Sofia Stepanoff
Figure caption: Integrated CO spectrum of IC 860 created using the moment0 map as a mask. The spectrum (black) is well fitted by a Gaussian function centered at the systemic velocity of the galaxy (red), and the lower panel shows the residuals.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Data to best-fit model ratios for the simulated observations with i = 30° and 70◦, assuming the Kerr metric (α 13 = 0) or without such an assumption (α 13 free). Red and blue bars are, respectively, the data from FPMA and FPMB.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Surface of the accretion disk obtained from the GRMHD simulation and employed for the calculations of the iron-line profiles and the reflection spectra.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Disk–corona model. The reflection spectrum is generated by the illumination of a cold, geometrically thin, and optically thick disk by a hot corona. Figure taken from Bambi (2022) under the terms of the Creative Commons Attribution 4.0 International License.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Iron-line profiles generated by a Novikov–Thorne accretion disk (solid red curves) and our GRMHD-simulated accretion disk (dashed blue curves). The viewing angles of the disks are i = 30° (left panels) and i = 70° (right panels). The emissivity profile of the disks is described by a power law with emissivity indices of q = 3 (top panels) and q = 6 (bottom panels).
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Constraints on the spin parameter a * and the Johannsen deformation parameter α 13 from the simulated observations with i = 30°. The red, green, and blue curves are, respectively, the 68%, 90%, and 99% confidence level contours for the two relevant parameters. The gray region is excluded in our analysis because this parameter space contains pathological spacetimes.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Angular velocities of the gas on the surface of the disk for a Novikov–Thorne accretion disk (solid red curve) and our GRMHD-simulated accretion disk (dashed blue curve).
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Initial setup of the Fishbone–Moncrief torus. The black lines denote the magnetic fields. Density is normalized.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: As in Figure 8 for the simulations with i = 70°.
Paper: Testing Relativistic Reflection Models with GRMHD Simulations of Accreting Black Holes
Authors: Swarnim Shashank, Shafqat Riaz, Askar B. Abdikamalov, Cosimo Bambi
Figure caption: Disk averaged out over time 16,000–25,000 M. The black lines denote the magnetic fields. Density is normalized.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: 1.3 mm continuum images of the 130 disks detected in our ALMA Cycle 7 program, ordered by decreasing continuum flux density (as reported in Table 1). Each panel is 7″ × 7″ and is scaled from −0.3 mJy to the maximum pixel value of the primary. This causes a few bright secondary sources to be saturated in some fields. White plus signs are plotted at the location of maximum intensity for binary companions (defined in Section 4). A representative beam size is shown in the bottom left panel, and the infrared spectral classification for all sources is noted in the lower right corner of each panel.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: The cumulative dust mass distribution for Serpens disks around YSOs in different evolutionary stages. The shading represents the 68% confidence interval. For the Class II distribution, the small number of low-mass detections below the typical detection threshold produces the flattened region below 10 M ⊕.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: J18275472–0342384 and a nearby Class 0 source. Left: the background image is a three-color composite of the 2MASS J, H, and K filters. Yellow contours represent the 1.3 mm continuum. The central source is illuminated in both near-IR and continuum, and a binary companion is identified in the continuum in a portion of the near-IR image that contains significant nebulosity. Right: the 12CO moment 0 map. The 12CO was integrated along channels from −5 to 17 km s−1 with respect to the rest frame of the source.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: Location of observed disks in the Serpens region. Four different groups are visually identified and labeled as Serpens Northeast, Serpens Main, Serpens South, and Serpens Far-South, each with the mean distances from Gaia EDR3 parallaxes. An additional two sources are present in our sample but reside at an RA of nearly 270° and so are not shown here.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: Spitzer IRAC [3.6] – [24.0] vs. [3.6] – [5.8] color–color diagram used for classifying YSOs. The dashed black lines in this magnitude plot correspond to the α IR slopes that we use to group objects into their evolutionary classes (Spitzer IRAC [3.6] – [24.0] colors of 2.75, 5.42, and 6.66). Transition disk candidates are indicated by the points with white circles inset.
Paper: Protostellar and Protoplanetary Disk Masses in the Serpens Region
Authors: Alexa R. Anderson, Jonathan P. Williams, Nienke van der Marel, Charles J. Law, Luca Ricci, John J. Tobin, Simin Tong
Figure caption: Cumulative dust mass distributions for disks around Class II YSOs in young star-forming regions. The Serpens sample is substantially less sensitive than the others, and a small number of low-mass detections below the typical detection threshold produce the flattened region below 10 M ⊕.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Mass combination of WD–WD mergers, and candidates for the ignition processes. He and C–O WDs are assumed to have <0.5 M ⊙ and 0.5–1.2 M ⊙, respectively. C–O WDs are allowed to have He shells on their surfaces. The primary WDs are limited to C–O WDs. Double detonation with any WD combinations in DD systems has been suggested by Guillochon et al. (2010), Fink et al. (2010), Woosley & Kasen (2011), Pakmor et al. (2013, 2021, 2022), Shen & Bildsten (2014), and Tanikawa et al. (2018, 2019). The (carbon-ignited) violent merger is numerically demonstrated by Pakmor et al. (2010, 2012) and Tanikawa et al. (2015). The spiral instability is reported by Kashyap et al. (2015, 2017). Double detonation in a DD system with an ONe WD can also occur according to Marquardt et al. (2015).
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Schematic of the relation between ignition process and WD–WD phase, where Δt is defined as the difference between the ignition time and merger time. Note that, for negative Δt, the merger time would be given if the ignition did not occur. Double detonation can occur before WD–WD mergers. The violent merger initiates at the moment of the merger. Spiral instability can ignite explosive carbon burning at an early and asymmetric accretion disk phase, where the accretion disk is made of the lighter WD that was tidally disrupted. In the late accretion disk phase, magnetic viscosity heats the system, although there is no scenario for WD explosion in this phase. In the neutrino cooling phase, the classical DD scenario (or near-Chandrasekhar-mass explosion) may work. The double detonation, violent merger, and spiral instability are studied in the references cited in the caption of Figure 8. Dan et al. (2015) investigated WD explosion at a similar phase to the phase of magnetically viscous heating, although they artificially put a hot spot to start carbon detonation. The classical DD was suggested by Webbink (1984) and Iben & Tutukov (1984).
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Median vales of the logarithms of the fractional estimation errors of the primary WD component mass ﹩{\mathrm{log}}_{10}({\rm{\Delta }}{m}_{1}/{m}_{1})﹩ for m 1−m 2 WD–WDs at 11 Mpc. One Ia supernova event is expected per year within this distance from Equation (3). The full observations during the 3 yr operation period are assumed.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Peak magnitudes and decline rates in the B band for normal Ia supernovae and subclasses of Ia supernovae, which is reproduced from Figure 1 in Taubenberger (2017). The solid black curve shows the Phillips relation. The dashed black curves indicate counterpart candidates of WD–WD mergers supposed in the main text.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Estimation errors vs. observational time for 1.0 M ⊙–0.8 M ⊙ WD–WDs at 11 Mpc. The dots correspond to 2 yr, 1 yr, 6 months, 1 month, 1 week, and 1 day before coalescence. The lower cutoff frequency is fixed to 3 yr before the coalescence.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Similar to Figure 3 but for the secondary WD component mass.
Paper: Probe for Type Ia Supernova Progenitor in Decihertz Gravitational Wave Astronomy
Authors: Tomoya Kinugawa, Hiroki Takeda, Ataru Tanikawa, Hiroya Yamaguchi
Figure caption: Median vales of the logarithms of the sky localization errors ﹩{\mathrm{log}}_{10}({\rm{\Delta }}{{\rm{\Omega }}}_{s})﹩ for m 1−m 2 WD–WDs at 11 Mpc. The full observations during the 3 yr operation period are assumed.