adsabs/AstroCLIMB huggingface dataset:
Paper: Impact of Anomalous Active Regions on the Large-scale Magnetic Field of the Sun
Authors: Shaonwita Pal, Prantika Bhowmik, Sushant S. Mahajan, Dibyendu Nandy
Figure caption: Qualitative comparison of the net change in solar dipole moment in our SFT simulation with the mathematical approximations. Panel (a) depicts the latitudinal (λ) dependency of different analytical functions contributing to the ultimate dipole moment. High-, mid-, and low-latitudinal regions are denoted by cyan, violet, and yellow. Panel (b) shows a change in dipole moment (Δ DM) of our simulations (violet triangles) that are compared with the mathematically derived approximated values (orange circles) for six different cases labeled on the horizontal axis.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Constraints from the size function of voids identified in the BOSS DR12 data set, for ΛCDM (left) and wCDM (right) flat cosmologies. For both panels, the 2D contours indicate the 68% and 95% confidence levels on the posterior distribution of the main model parameters, while the 1D distributions show the marginalized posteriors of each parameter with the 68% confidence interval indicated as a shaded band. In dark blue we report the results obtained by fixing the parameters C slope and C offset to their maximum posterior values obtained from the model calibration with PATCHY mocks (fixed calibration). In light blue we show the constraints when assuming an uncertainty on C slope and C offset, given by their posterior distribution reported in the right panel of Figure 3 (relaxed calibration).
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Theoretical linear matter power spectrum (left), void size function (center), and halo mass function (right) at z = 0.5, computed with Planck2013 parameters (Planck Collaboration et al. 2014), and normalized to have σ 8 = 0.83. We represent in different colors the results of varying Ωm and highlight with a dotted vertical line the pivot points that separate opposite trends. The bottom subplots show the residuals from the fiducial model with Ωm = 0.3.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Same as in Figure 6, but for the test constraints obtained from the size function of voids identified in the 100 mock catalogs of the MultiDark PATCHY simulations. Dark and light green colors indicate the results obtained by fixing and relaxing the calibration of the parameters C slope and C offset, respectively. The white star shows the input cosmological parameters of the simulation.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Shown here are 68% and 95% confidence contours obtained from the modeling of PATCHY void counts. Top: confidence contours in the C slope–C offset parameter plane, computed by increasing the void count uncertainty by factors of 2, 3, and 4. Bottom: confidence contours in the parameter planes Ωm–σ 8 (right) and Ωm–w (left). These contours are derived using the distributions shown in the top panel as 2D priors for the calibration parameters. The white star indicates the true cosmological values of the PATCHY simulations.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: MultiDark PATCHY and BOSS DR12 measurements of the redshift-space galaxy 2PCF multipoles, in the two redshift ranges considered in this analysis: 0.2 < z ≤ 0.45 (left) and 0.45 < z < 0.65 (right). Solid lines show the data obtained from the 100 PATCHY mock catalogs, while round markers indicate the measures from the BOSS data set. The correlation function monopole (ξ 0), quadrupole (ξ 2), and hexadecapole (ξ 4) are represented in green, orange, and violet, respectively. The shaded regions outside the range 15 < s [h −1 Mpc] < 55 are those excluded from the statistical analysis.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Covariance matrix (normalized by its diagonal components) of the MultiDark PATCHY redshift-space galaxy 2PCF multipoles, for the two redshift selections considered in this analysis: 0.2 < z ≤ 0.45 (left) and 0.45 < z < 0.65 (right). The galaxy separation bins (i, j) are divided by vertical and horizontal white lines to separate the measures of the monopole (ξ 0), quadrupole (ξ 2), and hexadecapole (ξ 4) moments of the correlation function.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Shown here are 68% and 95% confidence contours computed by assuming different fiducial cosmologies in the modeling of PATCHY void counts, for the ΛCDM cosmology (Ωm–σ 8 plane, right) and the wCDM (Ωm–w plane, left). In blue and red, we report the results derived for a flat cosmological model with Ωm = 0.279 and Ωm = 0.335, respectively. The white star indicates the true cosmological parameters of the PATCHY simulations.
Paper: Cosmological Constraints from the BOSS DR12 Void Size Function
Authors: Sofia Contarini, Alice Pisani, Nico Hamaus, Federico Marulli, Lauro Moscardini, Marco Baldi
Figure caption: Same as in Figure C2, but for different void radius selections. We represent in green, blue, and red the test constraints derived by modeling the PATCHY void counts with ﹩{R}_{\min }=35,37.5,40\,{h}^{-1}\ \mathrm{Mpc}﹩, respectively. The first radius selection is slightly lower than that used in the analysis presented in Appendix B.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: The CH3OH J  K  = 5 K  –4 K  binned visibility spectra (real component) with the best-fitting model overlaid in red. Each panel shows the average spectrum for a range of uv distances (antenna baselines), given in the upper-left corner, which correspond to a range of angular scales (θ) on the sky.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: The CH3CN J  K  = 14 K  –13 K  binned visibility spectra (real component) with the best-fitting model overlaid in red. Each panel shows the average spectrum for a range of uv distances (antenna baselines), given in the upper-left corner, which correspond to a range of angular scales (θ) on the sky.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: SUBLIME model geometry used in the present study showing the conical jet (Ω1) and ambient coma (Ω2) in Cartesian coordinates. Here θ jet is the half-opening angle of the conical jet, ϕ is the (phase) angle of the jet axis with respect to the observer (z), and ψ is the jet position angle in the plane of the sky (x is north, y is east).
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: The HNC J = 4–3 binned visibility spectra (real component) with the best-fitting model overlaid in red. Each panel shows the average spectrum for a range of uv distances (antenna baselines), given in the upper-left corner, which correspond to a range of angular scales (θ) on the sky.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Parent scale length χ 2 analysis for our observed species in 46P, showing the change in χ 2 value (Δχ 2) as a function of parent scale length (L  p ). Dotted horizontal lines show the Δχ 2 = 1 threshold (1σ), corresponding to 68% confidence, and dashed horizontal lines show the Δχ 2 = 6.63 threshold (2.6σ), corresponding to 99% confidence.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Observed, spectrally averaged real interferometric visibilities for CH3OH zoomed in on the region of shortest baselines to show the improved fit of the parent + daughter model (blue circles) compared with the pure parent model (orange circles).
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: The H2CO ﹩{J}_{{K}_{a},{K}_{c}}={5}_{\mathrm{1,5}}﹩–41,4 binned visibility spectra (real component) with the best-fitting model overlaid in red. Each panel shows the average spectrum for a range of uv distances (antenna baselines), given in the upper-left corner, which correspond to a range of angular scales (θ) on the sky.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: The HCN J = 4–3 binned visibility spectra (real component) with the best-fitting model overlaid in red. Each panel shows the average spectrum for a range of uv distances (antenna baselines), given in the upper-left corner, which correspond to a range of angular scales (θ) on the sky.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: The CS J = 5–4 binned visibility spectra (real component) with the best-fitting model overlaid in red. Each panel shows the average spectrum for a range of uv distances (antenna baselines), given in the upper-left corner, which correspond to a range of angular scales (θ) on the sky.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: The pre- and post-irradiation spectra for the NH3:C2H6 ice mixtures (a), NH3:C2H4 ice mixtures (b), NH3:C2H2 ice mixtures (c). Because the initial ice mixture spectra only depend weakly on temperature we only show the 10 K initial ice spectra for each ice mixture.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Top: log stretch of a weighted map. The sky pixel width is 0.°2, and the map is smoothed with a Gaussian kernel of σ = 0.°5. Only stars fainter than 17.5 mag are plotted. The blue circle and red dashed line represent M3 and the median positions of the model stream as displayed in Figure 3. Bottom: similar to the top panel but only for stars between 17.5 and 19.3 mag.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: The left panel is a CMD of the stars within M3's tidal radius, shown with blue dots. The red dashed line is the locus of the red giant branch and main sequence, obtained by calculating median values along G 0. The right panel shows the model stream (green dots) in planes of decl., heliocentric distance, ﹩{\mu }_{\alpha }^{* }﹩, and μ  δ  as a function of R.A. from top to bottom. The red dashed lines represent computed medians along R.A. The blue circle indicates M3.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Left: zoom-in look at the leading tail. Here the blue dotted line is a second-order polynomial fit to the trajectory. The area enclosed by orange solid lines is a mask parallel to the fit used to create the lateral profile. Right: lateral profile of the leading tail. Red straight lines indicate the average level of background and 1σ extent.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: The upper and lower panels show the construction of the filters in CMD and PM space. From left to right, the columns are distributions (linear stretch) of the target, background, and filters. The CMD bin size is 0.02 mag in color and 0.2 mag in G 0 magnitude. The PM bins are both 0.1 mas yr−1. Filters are smoothed with a Gaussian kernel of σ = 1 pixel.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Weighted map with linear stretch of the M3 surrounding area. The pixel size is 0.°1 × 0.°1, and the map is smoothed with a Gaussian kernel of σ = 0.°2. The contours represent an S/N of 3 (purple), 6 (orange), and 9 (red). The blue circle indicates the M3 tidal radius.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: The top and bottom panels present the dust extinction map extracted from Schlegel et al. (1998) and Gaia's scanning pattern covered by the DR3, respectively. The blue circle and red dashed line are the same as in Figure 4.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: Rest-frame UVJ color–color diagram for selecting rapidly quenched candidates. The UVJ colors are from the UVISTA catalog, where the rest-frame colors are calculated with the EAZY code (Brammer et al. 2008). The gray triangles are the parent sample of massive galaxies (﹩\mathrm{log}({M}_{\mathrm{stellar}}/{M}_{\odot })\gt 10.6﹩ at 1.25 < z < 1.75) from the UVISTA catalog. The diagonal black line divides galaxies into quiescent and star-forming galaxies, and the dashed lines are additional constraints used in Muzzin et al. (2013b). The black arrow shows the effect of dust attenuation in the UVJ space, assuming the Calzetti et al. (2000) extinction law. We apply the method used in Belli et al. (2019) and identify 12 rapidly quenched candidates (the youngest non-star-forming galaxies), which are marked as filled circles and are color-coded by their stellar mass. We perform Magellan/FIRE observations of seven of these rapidly quenched candidates, marked as magenta pentagons. We highlight two galaxies, UVISTA 169610 and 174150, with their IDs, for which we have detected absorption features. The lime green and green lines are the evolutionary tracks for dust-free stellar population models with SFH exponentially declining with the e-folding timescales of 100 Myr and 1 Gyr, respectively. For each timescale, the three tracks correspond to three different values of stellar metallicity (﹩\mathrm{log}(Z/{Z}_{\odot })=-0.2,0.0,0.2﹩).
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: SFHs of 12 UVISTA galaxies derived from Prospector fitting on photometric data. The MAP distribution is shown as the solid navy line, while the shade indicates 95% of the SFH distribution from 1000 random posteriors. The orange horizontal bar indicates the formation timescales (﹩{t}_{50}^{90}﹩, the time it takes for the stellar mass of a galaxy to increase from 50% to 90% of the total stellar mass). We find that all of our 12 rapidly quenched candidates, solely selected based on their location in the UVJ diagram, are PSBs that are rapidly formed (with average formation timescale of ﹩{t}_{50}^{90}\sim 320\,\mathrm{Myr}﹩).
Paper: Differences between the Pierre Auger Observatory and Telescope Array Spectra: Systematic Effects or Indication of a Local Source of Ultra-high-energy Cosmic Rays?
Authors: Pavlo Plotko, Arjen van Vliet, Xavier Rodrigues, Walter Winter
Figure caption: Results representing the second minimum shown as white filled triangles in Figure 3 when considering a cosmological source distribution, a local source in the Northern Hemisphere that emits cosmic rays of the iron-56 mass group, and allowing energy-dependent shifts in the energy scales of the experiments. We use SIBYLL 2.3c as the air shower model. In the left panels we see the parameter space of the local source in this scenario. The best-fit parameters are shown as white filled circles; a second solution for the local source, discussed in Appendix D, is marked with red filled squares. The meaning of the contour colors and gray part is as in Figure 3. In the right panels, spectra (upper plots) and composition observables (lower plots) correspond to the best-fit scenario of the joint fit for the second minimum. The best-fit parameters values are given in Table 5.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: Magellan/FIRE spectroscopic data of UVISTA 169610 (top) and UVISTA 174150 (bottom). The smoothed data (smoothed with 29 pixels, corresponding to ∼15 Å) are in green in both panels. The magenta lines show the best-fit stellar models from the Prospector fitting. The right panels show the resulting SFH of each galaxy. The red line shows the MAP distribution, and the hatched region includes 95% of the posterior distribution. The blue shade in the background shows 95% of the posterior distribution of SFH from Prospector fitting on photometric data only (the same as is shown in Figure 2). We confirm that both galaxies are rapidly formed with starbursts ∼500 Myr before being rapidly quenched.
Paper: Differences between the Pierre Auger Observatory and Telescope Array Spectra: Systematic Effects or Indication of a Local Source of Ultra-high-energy Cosmic Rays?
Authors: Pavlo Plotko, Arjen van Vliet, Xavier Rodrigues, Walter Winter
Figure caption: Left: parameter space of a local source for a joint fit to PAO and TA data when considering a cosmological source distribution and a local source in the Northern Hemisphere that emits a pure proton composition. Right: spectra (upper plots) and composition observables (lower plots) predicted by the models corresponding to the best-fit case for an extreme accelerator scenario.
Paper: Differences between the Pierre Auger Observatory and Telescope Array Spectra: Systematic Effects or Indication of a Local Source of Ultra-high-energy Cosmic Rays?
Authors: Pavlo Plotko, Arjen van Vliet, Xavier Rodrigues, Walter Winter
Figure caption: Left: parameter space of a cosmological source distribution, based on a fit to the TA spectrum and composition data. The best-fit parameters, listed in Table 8, are shown as a brown circle, and for comparison we show as a red circle the best fit to PAO data (Heinze et al. 2019). The solid yellow, green, and blue contours correspond to the 1σ, 2σ, and 3σ regions of our TA-only fit, respectively, while the dashed yellow line is the 1σ region of the PAO-only fit. A direct comparison is not possible because of the different values of ﹩{\chi }_{\min }^{2}﹩ and numbers of dof for the two combined fits. Right: spectra (upper plots) and composition observables (lower plots) corresponding to the best-fit parameters of our TA-only fit.
Paper: Differences between the Pierre Auger Observatory and Telescope Array Spectra: Systematic Effects or Indication of a Local Source of Ultra-high-energy Cosmic Rays?
Authors: Pavlo Plotko, Arjen van Vliet, Xavier Rodrigues, Walter Winter
Figure caption: Spectra (upper plots of each panel) and composition observables (lower plots of each panel) predicted by the models, resulting from a joint fit to TA and PAO data when considering a cosmological source distribution and additionally a local source in the Northern Hemisphere, only observable by TA. The panels show the case where this local source emits protons (top left), helium-04 (top right), nitrogen-14 (bottom left), and iron-56 (bottom right). For the gray shaded energy range, only the spectra data are used as upper limits.
Paper: Differences between the Pierre Auger Observatory and Telescope Array Spectra: Systematic Effects or Indication of a Local Source of Ultra-high-energy Cosmic Rays?
Authors: Pavlo Plotko, Arjen van Vliet, Xavier Rodrigues, Walter Winter
Figure caption: Energy-loss lengths (for redshift z = 0) of the four tested isotopes as a function of the nucleus energy. This includes adiabatic cooling, photopair production, photopion production, and photodisintegration off the cosmic microwave background and EBL (Heinze 2020). The orange band shows the energy range relevant for the joint fit.
Paper: Examining the Source Regions of Solar Energetic Particles Using an AI-generated Synchronic Potential Field Source Surface Model
Authors: Jinhye Park, Hyun-Jin Jeong, Yong-Jae Moon
Figure caption: The full-Sun running difference images (STEREO-A, B EUVI 195 Å and SDO AIA 193 Å) with the AIHMI-PFSS extrapolations at the times given: (a) the N1 event (2011 September 21), (b) the N2 event (2011 September 22), (c) the N3 event (2012 September 27), (d) the N4 event (2013 March 5), (e) the N5 event (2013 June 21), and (f) the N6 event (2014 January 6). The black arrows indicate EUV wave propagations associated with the SEP events.