adsabs/AstroCLIMB huggingface dataset:
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: Gas-to-dust mass distribution. The blue points represent our z ∼ 2–3 SMGs around quasars, with a median value of gas-to-dust mass ratio of 57 ± 14 (black point). The orange triangles represent the field SMGs from J. E. Birkin et al. 2021, with a median of 59 ± 12 (red triangle). The purple stars represent the brightest field SMGs from AS2COSPEC (C.-L. Liao et al. 2024), with a median of 44 ± 11 (purple star). The diagonal lines represent various gas-to-dust mass ratios, with the corresponding values indicated next to the lines.
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: Eight-filter composite optical imaging of NGC 4258. The orange outline depicts the approximate footprint of the NIRCam LW channel field of view. The cyan outline depicts the footprint of archival HST WFC3/F275W imaging from the LEGUS survey (D. Calzetti et al. 2015). The green contours represent VLA 4.89 GHz radio continuum emission from NVAS (image credit: NRAO/VLA Archive Survey, © 2005–2009 AUI/NRAO). The yellow boxes highlight several regions of interest detailed in Figures 6–  9.
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 the NGC 4258 nuclear region, Region N, 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), the optical imaging 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 the nuclear region. The typical aperture extent used in the photometry across each region is shown in cyan over the optical imaging, with the masked nuclear region shown in magenta.
Paper: Calcium Excess in Novae: Beyond Nuclear Physics Uncertainties
Authors: Mallory K. Loria, Pavel A. Denissenkov, Chris Ruiz, Falk Herwig
Figure caption: Comparison between the elemental mass fractions of the premixed accreted envelope (blue line) and the postexplosion mass-averaged envelope composition from our multizone nova models (red line). The dashed line shows the solar composition and the dotted line shows the fraction of H in the initial composition compared to the H at the end of the simulation. The top panel shows this for Model 1 and the bottom panel shows this for Model 5. For both of the models shown the premixed material is assumed to be 50% solar material and 50% WD material.
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: Two-color composite mosaics of continuum-subtracted PAH (yellow) and Brα (blue). The VLA 4.8 GHz emission is overplotted as a contour line. The PAH emission traces dust lanes and outlines the star formation 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: Two-color composite mosaics of continuum-subtracted [Fe II] (blue) and H2 (yellow). The VLA 4.8 GHz emission is overplotted as a contour line. The shock-tracing [Fe II] and H2 emission lines follow the anomalous radio arc structure rather than the spiral structure of the galaxy. 1/f noise and stray light artifacts are amplified by the continuum-subtraction process, due to the faint [Fe II] and H2 emission.
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: NIRCam filter bandpasses, emission lines, and PAH band. Top: bandpasses for the F164N, F162M, F187N, F182M, F212N, and F210M filters. Bottom: bandpasses for the F335M, F300M, F360M, F405N, F466N, and F430M filters. The locations of the emission lines are identified with the red dashed lines, and the approximate position of the PAH 3.3 μm feature is highlighted as the red shaded region in the bottom panel.
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: Three-color near-IR composite mosaic of NGC 4258 using the NIRCam filters F466N (blue), F300M (green), and F335M (red). VLA 4.8 GHz images are overplotted as the contour lines. Diffuse continuum emission is observed throughout the galaxy. At a distance of 7.2 Mpc, NIRCam resolves star clusters and potentially individual stars. Bands of PAH and Paschen-α emission trace the spiral structure of the galaxy.
Paper: Calcium Excess in Novae: Beyond Nuclear Physics Uncertainties
Authors: Mallory K. Loria, Pavel A. Denissenkov, Chris Ruiz, Falk Herwig
Figure caption: Distributions of the abundances for the selected elements relative to their default value in the multizone MC simulation for nova Model 5. The size and color of the circles represent the number of MC runs with that abundance.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: The variations of the K values with different H I surface density profiles. (a) H I surface density profiles, with the color bar showing the s values. From bottom to top, the H I surface density at the center of the galaxy goes from deficient to enriched, corresponding to the red to purple solid lines. (b) The normalized CoG obtained from the spectra corresponding to each H I surface density distribution in panel (a) with all other parameters fixed. The area enclosed by the CoG and the diagonal line is the corresponding K value with the colors coded in the same way as in panel (a). (c) Relationship between H I surface density profiles and K values. s represents the slope of H I surface density in the galactic center, with a larger s indicating a higher central H I surface density. The colors are coded in the same way as in panel (a).
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: The distributions of CV for misaligned galaxies and aligned controls. (a) The blue and gray histograms show the CV distributions for SF misaligned galaxies and their aligned controls, respectively. The blue and gray bars on the top mark the corresponding median values. The p-value from the KS test of this distribution is marked by blue text in the plot. (b) The red and gray histograms show the CV distributions for QS misaligned galaxies and their aligned controls, respectively. The red and gray bars on the top mark the corresponding median values. The p-value from the KS test of this distribution is marked by red text in the plot.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: Schematic view to illustrate the CoG method. (a) Mock spectra. The solid profile shows a symmetric profile. The dashed profile shows an asymmetric profile. The blue and red colors represent the blueshift and redshift. (b) CoG for mock spectra. The colors and curves are coded the same as in panel (a), and the black solid line is the total CoG of the solid profile in panel (a). Purple and green lines mark the position of F85(V85) and F25(V25). (c) Mock spectra. The black, green, and red profiles display flat-topped, single-peaked, and double-horned shapes. (d) Normalized CoG for mock spectra. The colors and curves are coded the same as in panel (c). The light green area represents the K value for the single-peaked profile. The light red area represents the absolute K value for the double-horned profile.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: The distributions of K for misaligned galaxies and their aligned controls. (a) The blue and gray histograms show the K distribution for SF misaligned galaxies and their aligned controls, respectively. The blue and gray bars on the top mark the corresponding median values. The p-value from the KS test of this distribution is marked by blue text in the plot. (b) The red and gray histograms show the K distribution for QS misaligned galaxies and their aligned controls, respectively. The red and gray bars on the top mark the corresponding median values. The p-value from the KS test of this distribution is marked by red text in the plot. In panels (a) and (b), the vertical dashed line marks the value of K = 0, corresponding to the flat-topped shape.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: The distributions of AF for misaligned galaxies and their aligned controls. (a) The blue and gray histograms show the AF distribution for SF misaligned galaxies and their aligned controls, respectively. The blue and gray bars on the top mark the corresponding median values. The p-value from the KS test of this distribution is marked by blue text in the plot. (b) The red and gray histograms show the AF distribution for QS misaligned galaxies and their aligned controls, respectively. The red and gray bars on the top mark the corresponding median values. The p-value from the KS test of this distribution is marked by red text in the plot.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: Stacked H I spectra in misaligned galaxies and aligned controls. (a) Blue and gray profiles show the stacked H I spectra in SF misaligned galaxies and their aligned controls, respectively. (b) Red and gray profiles show the stacked H I spectra in QS misaligned galaxies and their aligned controls, respectively. In panels (a) and (b), the vertical dashed line marks the position of V = 0 km s−1, and the horizontal solid line marks the flux of FV = 0 mJy.
Paper: The Impact of External Gas Accretion on the Distribution of H I Gas in Galaxies
Authors: Qianhan Zhang, Min Bao, Yanmei Chen, Niankun Yu, Yong Shi, Luis C. Ho
Figure caption: The distributions of line widths (W50) for misaligned galaxies and aligned controls. (a) The blue and gray histograms show the line-width distributions for SF misaligned galaxies and their aligned controls, respectively. The blue and gray bars on the top mark the corresponding median values. (b) The red and gray histograms show the line-width distributions for QS misaligned galaxies and their aligned controls, respectively. The red and gray bars on the top mark the corresponding median values.