adsabs/AstroCLIMB huggingface dataset:
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Each panel in this figure represents a redshift interval, as indicated above each plot. Completeness and purity are shown as a function of the probability of galaxies being dominant. The solid red curve and the dashed green curve denote completeness for BCGs and protoBCGs, respectively. Meanwhile, the blue curve represents purity considering both BCGs and protoBCGs. At high probability thresholds, the number of objects becomes small not only in the numerator but also in the denominator when computing purity, leading to increased statistical fluctuations. This effect is particularly noticeable in the 1.3 < z < 1.5 panel, but the noise is similar in other redshift intervals for Pdominant ≳ 0.7.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: i-band magnitude, r − i color, stellar mass, and transverse angular diameter distance from the dominant galaxy (ddominant) as a function of photometric redshift. The markers denote the medians in redshift bins, and the bars are delimited by the 16th and 84th percentiles. Green, blue, and red colors stand for real (proto)cluster members, foreground, and background galaxies, respectively. A slight horizontal shift was applied to the different markers to improve visualization.
Paper: Selecting Clusters and Protoclusters via Stellar Mass Density. I. Method and Tests on Mock HSC-SSP Catalogs
Authors: Marcelo C. Vicentin, Pablo Araya-Araya, Laerte Sodré, Michael A. Strauss
Figure caption: Halo mass–richness relations for different redshift intervals, as indicated above each panel. The Y-axis represents the true halo masses from the Millennium simulation. The red shaded area corresponds to bootstrap resampling of the fits, where the estimated parameters are varied within their respective uncertainties, illustrating the statistical dispersion of the relation.
Paper: Detection of Diffuse Radio Emission inside the Supernova Remnant G338.3-0.0 Associated with the γ-Ray Source HESS J1640-465
Authors: Moaz Abdelmaguid, Joseph D. Gelfand, J. A. J. Alford
Figure caption: Multiwavelength comparison of a zoomed-in view of SNR G338.3−0.0 and the interior radio diffuse emission region. The leftmost panel shows the MeerKAT 816 MHz image, with the interior radio diffuse emission (yellow ellipse) and SNR G338.3−0.0 (green circle). The remaining panels display the corresponding FOVs from MIR and FIR surveys, including ATLASGAL at 870 μm (F. Schuller et al. 2009), Herschel-SPIRE at 500, 350, and 250 μm (M. J. Griffin et al. 2010), Herschel-PACS at 160 and 70 μm (A. Poglitsch et al. 2010), MIPSGAL at 24 μm (S. J. Carey et al. 2009), and Spitzer-GLIMPSE at 8.0, 5.8, 4.5, and 3.6 μm (E. Churchwell et al. 2009). The color bar scale is linear, with the units indicated in each subplot.
Paper: Detection of Diffuse Radio Emission inside the Supernova Remnant G338.3-0.0 Associated with the γ-Ray Source HESS J1640-465
Authors: Moaz Abdelmaguid, Joseph D. Gelfand, J. A. J. Alford
Figure caption: Multiwavelength comparison of the region surrounding SNR G338.3−0.0 to ensure a representative background choice. The leftmost panel shows the MeerKAT 816 MHz image, with the interior radio diffuse emission (yellow ellipse), one of the selected background regions (blue), and SNR G338.3−0.0 (green circle). The remaining panels display the corresponding FOVs from MIR and FIR surveys, including ATLASGAL at 870 μm (F. Schuller et al. 2009), Herschel-SPIRE at 500, 350, and 250 μm (M. J. Griffin et al. 2010), Herschel-PACS at 160 and 70 μm (A. Poglitsch et al. 2010), MIPSGAL at 24 μm (S. J. Carey et al. 2009), and Spitzer-GLIMPSE at 8.0, 5.8, 4.5, and 3.6 μm (E. Churchwell et al. 2009). The color bar scale is linear, with the units indicated in each subplot.
Paper: Spatiotemporal Low First Ionization Potential Abundance: A Catalyst for Coronal Condensation
Authors: Luke Fushimi Benavitz, Jeffrey W. Reep, Lucas A. Tarr, Andy S.H. To
Figure caption: Impulsive nanoflare-heated coronal loop. The rows of plots show electron density, electron temperature, radiative losses, radiative timescale, and bulk flow velocity along the loop length as a function of time. Positive velocity indicates flows moving toward the right and vice versa. The columns of plots show the three simulations, each with different assumptions of abundances (photospheric, coronal, and variable). The loop heats up and cools down almost uniformly, except in the model with variable elemental abundances, which forms a condensation at the apex of the loop.
Paper: Detection of Diffuse Radio Emission inside the Supernova Remnant G338.3-0.0 Associated with the γ-Ray Source HESS J1640-465
Authors: Moaz Abdelmaguid, Joseph D. Gelfand, J. A. J. Alford
Figure caption: The selected (a) background and (b) PS and radio diffuse emission regions listed in Tables A1 and A2, respectively. The intensity scale of the color maps is linear and in units of Jy per beam.
Paper: Spatiotemporal Low First Ionization Potential Abundance: A Catalyst for Coronal Condensation
Authors: Luke Fushimi Benavitz, Jeffrey W. Reep, Lucas A. Tarr, Andy S.H. To
Figure caption: The top row shows the abundance factor as a function of position on the loop (for the full duration of the simulation), and the bottom row similarly shows the radiative losses (for the first 200 s). The left column shows the nanoflare-heated case, while the right is the beam-heated case. The corona starts at coronal abundances, but the abundance factor decreases rapidly in the corona due to chromospheric evaporation. The initial low-FIP material is pushed to the apex, however, leaving a localized spike in f and thus in radiation.
Paper: Spatiotemporal Low First Ionization Potential Abundance: A Catalyst for Coronal Condensation
Authors: Luke Fushimi Benavitz, Jeffrey W. Reep, Lucas A. Tarr, Andy S.H. To
Figure caption: Electron-beam-heated coronal loop, similar to Figure 2. The loop heats up and cools down almost uniformly, except in the HYDRAD model with variable elemental abundance, which forms coronal rain at the apex of the loop.
Paper: Detection of Diffuse Radio Emission inside the Supernova Remnant G338.3-0.0 Associated with the γ-Ray Source HESS J1640-465
Authors: Moaz Abdelmaguid, Joseph D. Gelfand, J. A. J. Alford
Figure caption: Evolution of the PWN radius (RPWN; blue solid line) and the PWN magnetic field (BPWN; red solid line) over the model’s true age (tage ∼ 3100 yr) for (a) the radio size and (b) the γ-ray size. The green dashed lines mark the times of collision between the PWN and the SNR RS, occurring at tRS ∼ 1900 yr for the radio size and tRS ∼ 3000 yr for the γ-ray size.
Paper: Detection of Diffuse Radio Emission inside the Supernova Remnant G338.3-0.0 Associated with the γ-Ray Source HESS J1640-465
Authors: Moaz Abdelmaguid, Joseph D. Gelfand, J. A. J. Alford
Figure caption: The selected (a) SNR regions and (b) SNR cutout regions listed in Table A2. The intensity scale of the color maps is linear and in units of Jy per beam.
Paper: Chondrule Dust Rim Growth: Influence of Restructuring Using Molecular Dynamics Simulations
Authors: Chuchu Xiang, Nina Merkert (Née Gunkelmann), Lorin S. Matthews, Augusto Carballido, Truell W. Hyde
Figure caption: Snapshots of a sample collision with views from the side (a)–(c) and from above (d)–(f). Panels (a) and (d) show the positions of the particles when the incoming particle (in purple) first touches the rim. Panels (b) and (e) are mid-collision, and panels (c) and (f) show the end result. The incoming aggregate has an equivalent radius of 13.3 μm and collision energy KE of 1.53 × 10−8 J.
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: Detailed ionization structure changes (innermost zone) for the five elements with new recombination rates, at t = 10 days.
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: Spectrum at 10 days of model using old rates (left) and new rates (right), showing the significant impact of the new recombination rates. Specific contributions by Se I (yellow, dashed line) and Se III (blue, dotted line) are plotted.
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: The total recombination rates (DR calculated from HULLAC + RR ground calculated from the analytical formula for Fe from T. S. Axelrod 1980) for different ions at five different temperatures. The different panels represent different recombination stages (upper left: II to I, upper right: III to II, bottom: IV to III).
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: Same as Figure 10, at 25 days.
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: Impact on electron fraction (left) and temperature (right) of using the new recombination rates, at t = 10 days.
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: Same as Figure 9, but at t = 25 days.
Paper: Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light r-process Composition
Authors: Smaranika Banerjee, Anders Jerkstrand, Nigel Badnell, Quentin Pognan, Niamh Ferguson, Jon Grumer
Figure caption: Same as Figure 8, at 25 days.
Paper: Chondrule Dust Rim Growth: Influence of Restructuring Using Molecular Dynamics Simulations
Authors: Chuchu Xiang, Nina Merkert (Née Gunkelmann), Lorin S. Matthews, Augusto Carballido, Truell W. Hyde
Figure caption: (a) Predicted growth of chondrule rims as a function of number of collisions. (b) Rim growth during the first 200 collisions.
Paper: Chondrule Dust Rim Growth: Influence of Restructuring Using Molecular Dynamics Simulations
Authors: Chuchu Xiang, Nina Merkert (Née Gunkelmann), Lorin S. Matthews, Augusto Carballido, Truell W. Hyde
Figure caption: Average rate of growth of the chondrule rim mass. The growth rate is calculated from the predicted rim mass shown in Figure 13 for turbulence levels ranging from α = 10−6 to 10−1.
Paper: Chondrule Dust Rim Growth: Influence of Restructuring Using Molecular Dynamics Simulations
Authors: Chuchu Xiang, Nina Merkert (Née Gunkelmann), Lorin S. Matthews, Augusto Carballido, Truell W. Hyde
Figure caption: Average change in (a) rim thickness and (b) rim porosity for high-energy collisions (KE > 10−11 J) as a function of the incident angle. The blue lines correspond to increased thickness or porosity and the red lines correspond to decreased thickness or porosity. The data is grouped by the original rim porosity, where darker shades represent lower porosity and lighter shades represent greater porosity.
Paper: Chondrule Dust Rim Growth: Influence of Restructuring Using Molecular Dynamics Simulations
Authors: Chuchu Xiang, Nina Merkert (Née Gunkelmann), Lorin S. Matthews, Augusto Carballido, Truell W. Hyde
Figure caption: The average size of the monomers that are lost (red) and remain attached (blue) during each collision event.
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Example MSEP spectra. The top row are L2 MSEP data without any corrections from Section 3.2 applied. The vertical white regions in the top panels correspond to when MAVEN is at its periapsis. The bottom row are the results obtained from correcting for attenuator state, Mars-shine contamination, and plasma regime. Each telescope and look direction for each spectra are indicated in the plots’ titles (e.g., 1R, 1F, 2R, and 2F).
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Summary of solar wind and particle observations at STEREO-A and MAVEN during CR2214. (A) Solar wind IMF magnitude observed at STEREO-A is plotted in blue. The MAVEN IMF profile in orange is time-shifted relative to the STEREO-A observation and scaled (﹩{B}_{1\,{\mathrm{au}}}={B}_{M}\,{r}_{M}^{1.59}﹩). (B) Solar wind proton density observed at STEREO-A is plotted in blue, while the time-shifted, scaled density (﹩{n}_{1\,{\mathrm{au}}}={n}_{\mathrm{MAVEN}}\,{r}_{M}^{1.96}﹩) observed at MAVEN is shown in orange. (C) Solar wind bulk speed observed at STEREO-A and at MAVEN, time-shifted by ∼4.14 days. (D) Omnidirectional average ion flux observed with STEREO-A SEPT. (E) Time-shifted ion flux observed by MSEP 1F. White vertical regions are the result of correcting for plasma regime, attenuator state, and Mars-shine. The vertical black dashed line indicates the start time of the CIR. The vertical blue dashed line indicates the end time of the CIR as observed by STEREO-A. The vertical dotted orange line indicates the end time of the CIR as observed by MAVEN.
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Summary of solar wind and particle observations at STEREO-A and MAVEN during CR2215. (A) Solar wind IMF magnitude observed at STEREO-A is plotted in blue. The MAVEN IMF profile in orange is time-shifted relative to the STEREO-A observation and scaled (﹩{B}_{1\mathrm{au}}={B}_{M}\,{r}_{M}^{1.59}﹩). (B) Solar wind proton density observed at STEREO-A is plotted in blue, while the time-shifted, scaled density (﹩{n}_{1\mathrm{au}}={n}_{\mathrm{MAVEN}}\,{r}_{M}^{1.96}﹩) observed at MAVEN is shown in orange. (C) Solar wind bulk speed observed at STEREO-A and at MAVEN, time-shifted by ∼2.82 days. (D) Omnidirectional average ion flux observed with STEREO-A SEPT. (E) Time-shifted ion flux observed by MSEP 1F. The white vertical regions are the result of correcting for plasma regime, attenuator state, and Mars-shine. The vertical black dashed line indicates the start time of the CIR. The vertical blue dashed line indicates the end time of the CIR as observed by STEREO-A. The vertical dotted orange line indicates the end time of the CIR as observed by MAVEN.
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Time-averaged ratio of 1F and 1R MSEP Compton–Getting-corrected intensities vs. MSEP energy. Each point is the result of averaging each energy channel’s intensity over the entirety of the event and then plotting against the centroid of each MSEP energy channel. The average ratio for the suprathermal and energetic populations is reported in the upper-right corner. The primary direction of particle flow is indicated in the blue and light orange regions. Ratios greater than 1 indicate preferential antisunward flow (blue), while ratios less than 1 indicate preferential sunward particle flow (orange).
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Spacecraft geometry and particle spectra for CR2214. The left panel shows the position of STEREO-A (blue) and MAVEN (red) at the beginning of the observation. The angle of separation is indicated in the upper-left corner. The right panel shows the omnidirectional, averaged fluences for STEREO-A (blue) and MAVEN (red). The fluences from each MSEP telescope are plotted and indicated in the legend. The curves of best fit are overplotted on each spectra, with the spectral transition energies (E0) for each fit indicated by the vertical dotted lines.
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Spacecraft geometry and particle spectra for CR2215. The left panel shows the position of STEREO-A (blue) and MAVEN (red) at the beginning of the observation. The angle of separation is indicated in the upper-left corner. The right panel shows the omnidirectionally averaged fluences for STEREO-A (blue) and MAVEN (red). The fluences from each MSEP telescope are plotted and indicated in the legend. The curves of best fit are overplotted on each spectra, with the spectral transition energies (E0) for each fit indicated by the vertical dotted lines.
Paper: A Deep, High-angular-resolution 3D Dust Map of the Southern Galactic Plane
Authors: Catherine Zucker, Andrew K. Saydjari, Joshua S. Speagle, 佳士 沈, Edward F. Schlafly, Gregory M. Green, Robert Benjamin, Joshua Peek, Gordian Edenhofer, Alyssa Goodman, Michael A. Kuhn, Douglas P. Finkbeiner
Figure caption: Schematic overview of the process of turning images of the sky into a 3D map of dust. The DECaPS2 survey forms the foundation of our 3D dust map, whose photometric colors are combined with complementary photometric (VVV, 2MASS, unWISE) and astrometric surveys (Gaia) where available and fed into our stellar inference framework. We use the brutus stellar inference framework to infer the distance, extinction, and stellar type of hundreds of millions of stars. We then group stars into pixels and fit the set of distance–reddening measurements along the line of sight in each pixel to generate a 3D map of dust.
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Summary of the 1F/1R intensity ratio vs. time for each energy channel in the suprathermal range measured by MSEP. The intensity ratio scale is shown on the left side of each panel, and overplotted in black is the measured solar wind speed at MAVEN. The horizontal gray dotted line is placed at unity to indicate equivalent sunward and antisunward flow.
Paper: Examining the Radial Evolution of a Corotating Interaction Region Observed at STEREO-A and MAVEN
Authors: Sarah A. Henderson, Rachael J. Filwett, Christina O. Lee, Rebecca Jolitz, Robert C. Allen, Maher A. Dayeh, Ali Rahmati, Davin Larson, Jasper S. Halekas, Jacob R. Gruesbeck, Antoinette Galvin, Hanying Wei, Bernd Heber
Figure caption: Summary of the 1F/1R intensity ratio vs. time for each energy channel in the energetic range measured by MSEP during CR2214. Each subpanel shows the 1F/1R ratio for a given energy channel with corresponding scale on the left y-axis. Overplotted is the solar wind speed profile in black with a scale shown on the right y-axis. The horizontal gray dotted line is placed at unity to indicate equivalent sunward and antisunward flow.
Paper: The Electron Temperature Distribution and the High Ionization Just behind the Shock in the Cygnus Loop
Authors: Masahiro Ichihashi, Aya Bamba, Dai Tateishi, Kouichi Hagino, Satoru Katsuda, Hiroyuki Uchida, Hiromasa Suzuki, Ryo Yamazaki, Yutaka Ohira
Figure caption: The 0.15–12.0 keV image observed by metal-oxide-semiconductor (MOS) in EPIC of XMM-Newton (ObsID:0741820101; left) and the Hα image of the northeastern region of the Cygnus Loop observed at the Rozhen National Astronomical Observatory by M. Vučetić et al. (2023; right). These images are shown on a logarithmic scale. Some shapes in these figures show the regions for spectral analysis below. The cyan square shows the CCD1 of MOS. The magenta polygon shows the background region from which we made the CXB model. Green fan-shaped regions show the source region. These regions are labeled as layer 1, 2, ..., and 24 from the filament toward downstream. The red box region shows the outer shell region, which is located between the two outermost Hα filaments, as an indicator of the physical parameters of the shock front.
Paper: The Electron Temperature Distribution and the High Ionization Just behind the Shock in the Cygnus Loop
Authors: Masahiro Ichihashi, Aya Bamba, Dai Tateishi, Kouichi Hagino, Satoru Katsuda, Hiroyuki Uchida, Hiromasa Suzuki, Ryo Yamazaki, Yutaka Ohira
Figure caption: The comparison of the temperature in our result to the temperature structure of the Sedov solution. The red region shows the case without radiative cooling, and the blue region shows the case with radiative cooling of the cooling function in J.-G. Kim et al. (2023). The brown region is the overlapping region of both cases.
Paper: The Electron Temperature Distribution and the High Ionization Just behind the Shock in the Cygnus Loop
Authors: Masahiro Ichihashi, Aya Bamba, Dai Tateishi, Kouichi Hagino, Satoru Katsuda, Hiroyuki Uchida, Hiromasa Suzuki, Ryo Yamazaki, Yutaka Ohira
Figure caption: The spatial distribution of kT (left) and net (right) of the low-temperature component in the northeastern region of the Cygnus Loop. The blue points and the black point show the result of the annulus regions and the outer shell region, respectively. The red region in the left figure shows the range of an electron temperature estimated from both a proper motion and the distance of the Cygnus Loop. The red region of the right figure shows the range of a net estimation from an electron density and a shock velocity of the Cygnus Loop.
Paper: The Electron Temperature Distribution and the High Ionization Just behind the Shock in the Cygnus Loop
Authors: Masahiro Ichihashi, Aya Bamba, Dai Tateishi, Kouichi Hagino, Satoru Katsuda, Hiroyuki Uchida, Hiromasa Suzuki, Ryo Yamazaki, Yutaka Ohira
Figure caption: The spectra and best-fit model of fan-shaped regions. Cyan, red, orange, gray, and blue lines show the model of the low-temperature component, the high-temperature component, Fe L line, the source background, and the NXB fluorescent lines, respectively. We adopt the one nei model to the spectra of layer 1–16 and two nei model to the spectra of layer 17–24.