adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Demonstration of the DEM technique applied to SIRS (T. N. Woods et al. 2009). The top-left panel shows the median DEM value across 105 draws from the posterior distribution (solid green line) with shading spanning the interval between the 16th–84th percentile of the DEM draw values and the horizontal bars are the flux constraints discussed in Section 2.2. The bars labeled with ion species correspond to measured integrated line fluxes from that species while the unlabeled bars correspond to spectral bins where the contribution function is a sum from unresolved blends of lines and continuum processes. The top-right panel and its associated color bar show the Gλ(T) contribution function matrix calculated using atomic data, with the position of dark patches along a single wavelength column corresponding to the plasma temperature that contributes more observed emission at that wavelength (assuming an equal distribution of plasma at all temperatures). The bottom panel compares the model-generated DEM spectrum (green) to the original data (black) with the shaded interval representing the model uncertainty determined by sampling from the posterior distribution of DEM shapes and systematic uncertainty inflation s-factors.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for AD Leo. The top-left panel shows the median DEM value as a function of temperature in a solid red line with a translucent red swath spanning the 16th–84th percentile interval of DEM values. Horizontal lines approximate the DEM value within a temperature interval implied by an individual input integrated flux, left unlabeled if associated with a spectral bin and labeled by ion species if associated with a set of resolved emission lines. The top-right panel, analogous to the right panel of Figure 1, shows how the median DEM combines with atomic data to contribute flux as a function of both wavelength and temperature. The intensity of color is proportional to the product Ψ(T) × G(T), which can be integrated along a single wavelength column across temperature to arrive at a quantity proportional to the integrated flux observed for that wavelength bin. The bottom panel shows the flux constraints from emission lines with the data in black points with error bars and the DEM model fluxes in red crosses with error bars extending from the 16th–84th percentile values of the predictions obtained by sampling from the posterior distribution of DEM function shapes and systematic uncertainty parameters. Appendix A contains similar DEM summary figures for the other stars analyzed in this work.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: Spectrum summary figure for AD Leo. The top panel shows the flux densities of the EUVE spectrum post-background subtraction and ISM correction at the wavelengths that satisfy S/N and G(T) threshold cuts to use as inputs while fitting the DEM, corresponding to the unlabeled horizontal lines in the top-left panel of Figure 2, the DEM summary figure for AD Leo. The middle panel plots the model spectrum divided by the EUVE data. The bottom panel plots the post-processed EUVE spectrum and DEM model EUV spectrum at 5 Å wavelength resolution. Appendix A contains similar spectrum summary figures for the other stars analyzed in this work.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: This figure summarizes three tests of how the presence/absence of data affects the uncertainties in the DEM and output spectrum using ﹩{ \mathcal E }﹩ Eri as an example. The top four rows correspond to different data inputs used for the fit, titled standard, only EUVE, no EUVE and coarse with further description in Section 3.4. The four columns are from left to right: the DEM and the flux constraints used for the fitting, a comparison to EUVE data, the output EUV spectrum, and a comparison to the mean EUV spectrum from the standard fitting process (the titles of each column are the y-axis labels for the column). Each panel plots 250 sample draws from the posterior distribution to show how the model uncertainties propagate. The bottom row has three panels for different bandpasses within the spectral interval plotted above, showing histograms of the integrated fluxes of the sample draws from the four models above.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: The solid black line with error bars represents the coadded EUVE spectrum of AD Leo with its observational uncertainties while the dotted red line shows the most flare-enhanced observation from 1993 March 1. The gray swath spans the 16th–84th percentile (here the second-lowest to second-highest) value of the flux density in each wavelength bin. Some transitions from Fe XVIII–Fe XXII and a single transition from He II are marked with small vertical lines. The hotter lines are more variable overall, but not all flares heat the same lines so there are a couple of spectral bins where the observed variability across all nine AD Leo EUVE spectra exceeds the enhancement of the 1993 March 1 spectrum relative to the median. The excess variability around 300 Å plot corresponds to the drop off in sensitivity at the edge of the medium-wave detector.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: The DEM-generated EUV spectra produced by this work are plotted with each star in the labeled panels compared to the T. N. Woods et al. (2009) SIRS in gray, scaled to the Earth-equivalent instellation distance (1 au ﹩\times \sqrt{\frac{{L}_{\star }}{{L}_{{\rm{Sun}}}}}﹩; E. Mamajek & K. Stapelfeldt 2024).
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: The DEM models fit by this work are plotted with each star in the labeled panels with shared axes and laid out with the same grid and color scheme as in Figure 6. The Sun’s DEM plotted earlier in Figure 1 is plotted in gray for comparison.
Paper: Stellar Library of Differential Emission Measures and Extreme Ultraviolet Spectra: Dwarf Stars Observed by the Extreme Ultraviolet Explorer
Authors: Girish M. Duvvuri, Zachory K. Berta-Thompson, J. Sebastian Pineda, Kevin France, Alexander Brown, Allison Youngblood, David J. Wilson, Cynthia S. Froning, P. Christian Schneider, Thomas Ayres, Keivan G. Stassun
Figure caption: DEM summary figure for Procyon in the same style as Figure 2.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Left panel: cumulative star formation rate. Our measurements for SDSSJ0819 and for all of our quasar fields are shown as orange and blue squares, respectively. Since only bright sources are targeted by our observations, these measurements are likely lower limits. The green solid diamonds show the observed cumulative SFRs of other protocluster candidates: PCL1002 (C. M. Casey et al. 2015), COSMOS(z = 2.1) (C.-L. Hung et al. 2016), SMMJ004224 (I. Oteo et al. 2018), MRC1138-256 (H. Dannerbauer et al. 2014), HS1549+19 (G. C. P. Wang et al. 2025), and SPT2349-56 (T. B. Miller et al. 2018). The hollow symbols represent the values derived from the corresponding samples but limited to sources located within the light-of-sight depth of 28.6 cMpc, as defined by the FOREVER22 simulation. The gray region represents the predicted range from all simulated halos with masses comparable to those of quasars in the FOREVER22 simulation (H. Yajima et al. 2022). Right panel: star formation rate density as a function of redshift. The orange and blue solid squares are the results of calculations based on the confirmed member galaxies that are located within the volume centered at quasars with a size specified by the FOREVER22 simulation, (25.7 cMpc)3, for SDSSJ0819 and the average for all of our quasar fields, respectively. Again, they are likely lower limits. The green points show some of the measurements from the literature (D. L. Clements et al. 2014; Y. Kato et al. 2016). The gray region represents the predicted region based on all simulated halos with masses comparable to those of quasars in the FOREVER22 simulation. Furthermore, the cosmic mean curve reported by P. Madau & M. Dickinson (2014) is shown as a black dashed line.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Probability distributions of projected distances (∣dis∣) between the SMGs and the probable large-scale spine structures, in both the projected sky plane (x–y; upper panel) and the projected line-of-sight plane (x–z; lower panel). The error bars are calculated from Poisson error. Red curves represent the fitting results of our sources for the filament widths, green curve represents the outcome after applying our methods to sources reported in G. C. P. Wang et al. (2025), and black curves represent the x–y distribution results from F. Arrigoni Battaia et al. (2023).
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: CO luminosity functions in various transitions. Black curves show the fitting results of Schechter functions reported by L. A. Boogaard et al. (2023), while the blue and green blocks show the results from the ASPECS (R. Decarli et al. 2020) and HDFN (L. A. Boogaard et al. 2023) survey, respectively. Orange blocks show our results for the supplementary sources, which are consistent with those reported in the field, confirming that the supplementary sources are likely field line emitters.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: An example for axis rotation based on the field SDSSJ0819. The green crosses represent the relative locations for primary samples to the central quasar. The red line shows the direction of filament reported by F. Arrigoni Battaia et al. (2023). The left panel show the real distribution, whereas the right panel shows the case after rotating the field such that the direction of filament is aligned with the x-axis.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: Modified blackbody (MBB) fitting results for primary sources. The blue line shows the best-fitting result. Black points represent the flux density for ALMA and JCMT/SCUBA-2 (from left to right, 450, 850 μm (SCUBA-2), 3 mm (ALMA)), while green points represent those for Herschel (from left to right, 250, 350, 500 μm).
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: CO emission maps for all the 28 primary (pri) and supplementary (sup) detections. The plotting style follows that of the lower panels of Figure 1.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: JCMT/SCUBA-2 850 μm SNR maps of quasar field hosting Lyα nebulae. The plotting style follows that of the upper panel in Figure 1.
Paper: A Multiwavelength Study of ELAN Environments (AMUSE2): The Impact of Dense Environment on Massive Dusty Star-forming Galaxies at Cosmic Noon
Authors: Yu-Jan Wang, 禹然 王, Chian-Chou Chen, 建州 陳, Fabrizio Arrigoni Battaia, Roberto Decarli, Helmut Dannerbauer, Po-Feng Wu, 柏鋒 吳
Figure caption: CO spectra of all the 28 primary and supplementary detections. The plotting style follows that of the lower panels of Figure 2.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Multiwavelength comparison of Region E in NGC 4258 observed with JWST and HST. The top row shows smoothed images of the PAH emission at 3.3 μm (left), the H2 emission at 2.12 μm (center), and the [Fe II] emission at 1.64 μm (right) captured by JWST. The bottom row displays the Brα emission at 4.05 μm (left), an optical image from HST (center), and the HST UV F275W imaging from LEGUS (right). All images are aligned to the same celestial coordinates, with the field of view centered at R.A. = 12h18m57﹩\mathop{.}\limits^{{\rm{s}}}﹩2 and decl. = +47° 18’07﹩\mathop{.}\limits^{\unicode{x02033}}﹩8. The VLA 4.8 GHz emission is overplotted as the black contours. The color bars indicate the flux density in MJy str−1 for each corresponding image, highlighting the spatial distribution of the different emission features across the region.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Multiwavelength comparison of Regions A and B in NGC 4258 observed with JWST and HST. The top row for each region shows smoothed images of the PAH emission at 3.3 μm (left), the H2 emission at 2.12 μm (center), and the [Fe II] emission at 1.64 μm (right) captured by JWST. The bottom row for each region displays the Brα emission at 4.05 μm (left), an optical image from HST (center), and the HST UV F275W imaging from LEGUS (right). The VLA 4.8 GHz emission is overplotted as the black contours. The color bars indicate the flux density in MJy str−1 for each corresponding JWST image, highlighting the spatial distribution of the different emission features across each region.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Multiwavelength comparison of Regions C and D in NGC 4258 observed with JWST and HST. The top row for each region shows smoothed images of the PAH emission at 3.3 μm (left), the H2 emission at 2.12 μm (center), and the [Fe II] emission at 1.64 μm (right) captured by JWST. The bottom row for each region displays the Brα emission at 4.05 μm (left), an optical image from HST (center), and the HST UV F275W imaging from LEGUS (right). The VLA 4.8 GHz emission is overplotted as the black contours. The color bars indicate the flux density in MJy str−1 for each corresponding JWST image, highlighting the spatial distribution of the different emission features across each region.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Top panel: bar chart showing normalized emission-feature flux measurements from Table 2 across the six measured regions in Figures 6–  9 for the four imaged emission features: PAH (orange), Brα (red), H2 (green), and [Fe II] (blue). The fluxes are normalized within each region to the brightest detected feature, and the additional “Total” column on the right shows the relative line strengths integrated across all six regions. Regions with missing flux measurements indicate negligible or undetectable emission for the corresponding feature. Bottom panel: scatter plot of the Brα/[Fe II] ratio for each region (N through E), plotted on a logarithmic scale. The dashed horizontal line at 0.3 indicates the approximate threshold above which photoionization is expected to dominate over shock excitation (A. Alonso-Herrero et al. 1997; D. E. Osterbrock & G. J. Ferland 2006).
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Each row shows a 35″ × 35″ cutout of a region selected from the NGC 4258 field: Region A (top) and Region B (middle) contain bright [Fe II] emission arcs, while the selected empty region (bottom) is devoid of obvious line emission. From left to right, the columns show the medium-band continuum image (F162M), the narrow-band line + continuum image (F164N), and the continuum-subtracted [Fe II] emission. The cutouts are oriented with north to the top and east to the left. The color scales for [Fe II] are symmetric about zero, to highlight both positive and negative residuals. A scale bar of 5″ is shown in the final column. The results demonstrate the successful subtraction of continuum across both emission-dominated and line-free regions.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Comparison of [Fe II] and H2 emission from JWST imaging with Chandra X-ray and VLA radio emission. The top panel shows the [Fe II] emission, while the bottom panel presents the H2 emission, both mapped onto the same field of view. The magenta contours represent the X-ray emission, highlighting regions of high-energy activity, while the cyan contours trace the radio emission. The varying contour thicknesses reflect the emission intensity, with thicker lines indicating higher flux levels. JWST imaging artifacts are visible in both images, particularly the striping patterns and abrupt intensity variations. These features are consistent across both data sets, suggesting systematic origins rather than astrophysical structures.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Schematic illustration of the proposed outflow-driven shock scenario in NGC 4258. The blue and red arrows represent the path of the outflows from opposite sides of the AGN. The thick arrows indicate regions where [Fe II] emission is observed, tracing the most energetically shocked areas. These [Fe II] regions appear roughly 180° apart and are encased by lower-energy H2-emitting regions (indicated by the thin solid arrows). The dashed blue lines represent areas where H2 observations are unavailable. The curved white boundary marks the shock/ISM interface, showing how the outflows interact with the surrounding ISM.
Paper: JWST NIRCam Imaging of NGC 4258. I. Observation Overview
Authors: Travis C. Fischer, Nicholas F. Cothard, Omnarayani Nayak, Henrique R. Schmitt, Erin C. Smith, Jason Glenn
Figure caption: Histograms show the flux density distribution of the [Fe II] emission after continuum subtraction in Regions A, B, and C. The vertical lines mark the mean (black dashed), median (red solid), and ±3σ (orange dotted) levels. The distributions are sharply peaked and symmetric about zero, including Region C, which lacks line emission. The measured 1σ residual scatter in Region C (0.10 MJy sr−1) provides an estimate of the systematic uncertainty from the subtraction process.
Paper: NIRC2 Interferometric Imaging of the HD 34282 Transition Disk’s Small Grain Structure
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Top left: the L′ image reconstruction from the observed closure phases and squared visibilities. The brightness distribution of the central star (located at the plus symbol) has been suppressed in the image. However, it has a fractional flux of f* = 0.83. Top middle: the best-fit geometric single-ring model. Top right: the image reconstruction from the single-ring model closure phases and squared visibilities, with the position of the star marked by the plus symbol (fractional flux f* = 0.84). The single-ring model fails to reproduce the close-in asymmetries located east and northwest of the star (with east being left and north being up in the images). Bottom left: the same as top left. Bottom middle: the best-fit geometric double-ring model. The double-ring model has a lower χ2, and we find the significance of the preference over the single-ring model to be >5σ. Bottom right: the image reconstruction from the double-ring model closure phases and squared visibilities. This model successfully reproduces the close-in asymmetries. In this panel, the central star is again removed and represented by the plus symbol, with a fractional flux of f* = 0.81.