adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Left column: the variation of BP/X shape parameters R pea (top), σ pea (middle), and  R bar  (bottom) with the bar pattern speed for model A (orange), model B (red), and model C (blue) over time. Note that the bar pattern speed for model A here is not scaled as it is in Figure 2. The x-axis shows the pattern speed in the inverse direction. We use only snapshots where the bar is in a relatively steady state. Right column: the variation of BP/X shape parameters with the dimensionless bar rotation parameter ﹩{ \mathcal R }\equiv {R}_{\mathrm{cor}}/{R}_{\mathrm{bar}}﹩. The vertical red dashed line indicates ﹩{ \mathcal R }=1.4﹩, the criterion below which the bar is classified as a fast bar. For model C, the ﹩{ \mathcal R }﹩ values are multiplied by a factor of 0.5 for better visualization. The numbers tagged to each point denote the sequence of time evolution, ranging from 1 (earliest snapshot) to the latest snapshot.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: SoS for 50 orbits in model B at t = 4.5 Gyr within the energy range −1.0 < E J < −0.98. Each panel displays V  y  vs. y for orbits intersecting the y- z plane with positive V  x . The colors denote various orbit families: x 1 orbits in red, OX orbits in cyan, CX orbits in blue, and box orbits in green. To alleviate overcrowding, the SoS for box orbits is plotted in the right panel.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Contours of density extracted from OX and CX orbits and their contributions to models A, B, and C in edge-on views are presented. Red lines delineate various types of X-shaped structures. The first row represents the contributions of OX/CX structures after the formation of the BP/X bulge, while the second row displays these structures at the end of the simulation, with the contribution of each species to the total structure given as a percentage.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Distributions of the frequency drift parameter ﹩{\mathrm{log}}_{10}({\rm{\Delta }}f)﹩ for 15,000 orbits integrated over durations of 20 Gyr (red) and 2 Gyr (blue). The dashed line indicates the threshold value of ﹩{\mathrm{log}}_{10}({\rm{\Delta }}f)=-1.2﹩. Orbits with ﹩{\mathrm{log}}_{10}({\rm{\Delta }}f)\gt -1.2﹩ are classified as chaotic.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Illustration of typical x 1, OX, and CX orbits in the x- y and x- z planes.
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Comparison of our orbit frequency map for orbits integrated over durations of 20 Gyr (left) and 2 Gyr (right).
Paper: Orbital Support and Evolution of CX/OX Structures in Boxy/Peanut Bars
Authors: Behzad Tahmasebzadeh, Shashank Dattathri, Monica Valluri, Juntai Shen, Ling Zhu, Vance Wheeler, Ortwin Gerhard, Sandeep Kumar Kataria, Leandro Beraldo e Silva, Kathryne J. Daniel
Figure caption: Comparison of our orbit classification for orbits integrated over durations of 20 Gyr (black) and 2 Gyr (gray).
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: Minimum planetary magnetic fields for stellar winds deflection (﹩{B}_{{\rm{p}},\min }﹩) as a function of orbit semimajor axis (a). The top and bottom panels consider, respectively, magnetospheric sizes of r M = 11.7 R p (Earth today) and r M = 5 R p (Earth, 3.4 Gyr ago). The maroon and gray colors are associated with planetary systems of the stars Kepler-186 and TOI-700, respectively. The small vertical lines at the bottom of each panel show the semimajor axis of the exoplanets around these stars. The shaded regions represent the habitable zones for each star, with IHZ determinations based on a planetary mass of 1 M ⊕. Solid, dashed, and dotted lines are the ﹩{B}_{{\rm{p}},\min }﹩ vs. a for each star, considering ratios between magnetic fields from circular polarimetry and intensity of respectively, 1%, 5%, and 10%. We also show the position of the Earth in the upper panel for comparison.
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: The top and bottom panels show, respectively, the insolation and equilibrium temperatures as a function of the orbit semimajor axis for the sample exoplanets. The exoplanets are color coded by the host star mean magnetic fields derived in this work; these are used to calculate the minimum planetary mass needed to protect the exoplanet from stellar winds. Most of the sample exoplanets are not in a habitable zone and these are shown as open symbols. The only exoplanets in the habitable zone of their stars are Kepler-186f (filled square) and TOI-700d (filled inverted triangle); the Earth is also shown for comparison.
Paper: Magnetic Fields in a Sample of Planet-hosting M Dwarf Stars from Kepler, K2, and TESS Observed by APOGEE
Authors: Fábio Wanderley, Katia Cunha, Verne V. Smith, Oleg Kochukhov, Diogo Souto, C. Allende Prieto, Suvrath Mahadevan, Steven R. Majewski, Philip S. Muirhead, Marc Pinsonneault, Ryan Terrien
Figure caption: Derived magnetic fluxes for the studied M dwarfs as a function of their rotational periods (blue circles). The M-dwarf members of the young Pleiades open cluster (F. Wanderley et al. 2024; open orange circles) and for field M dwarfs (A. Reiners et al. 2022; gray xs) are also shown. The studied M dwarfs fall in the unsaturated regime and follow other results from the literature.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: The (m F150W − m F200W) vs. m F200W color–magnitude diagram for the Cloud 2 clusters. Only point sources located in the cluster region and that are detected with more than 10σ in both the F150W and F200W bands are plotted. The gray lines show isochrone models from L. Siess et al. (2000) for the mass range 3 < M/M ⊙ ≤ 7 and from F. D’Antona & I. Mazzitelli (1997) for the mass range 0.017 ≤ M/M ⊙ ≤ 3. A distance of 7.9 kpc and an age of 0.1 Myr are assumed. The black arrows show the reddening vectors for A  V  = 5 mag from the isochrone models. Stars located in the cluster region on the sky and that are located between the orange lines on the color–magnitude diagram (2 mag ≤ A  V  ≤ 14 mag and 1 mag ≤ A  V  ≤ 18 mag for the Cloud 2-N and 2-S clusters, respectively) are identified as cluster members. Identified cluster members are shown as red circles, while sources that are located in the cluster region but that are not considered to be cluster members are shown as black circles. The dashed lines show the 10σ limits. The sensitivity limits are indicated by red lines.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Comparison of theoretical M–L (m F200W) relations. The M–L relation that is used in the modeling in Section 4.1 (F. D’Antona & I. Mazzitelli 1997, 1998; L. Siess et al. 2000) for the age of 0.1 Myr is shown with a black line, while the relation by the same reference but for the age of 0.5 Myr is shown with a gray line. The M–L relations in the JWST/NIRCam filter system by I. Baraffe et al. (2015) for the ages of 0.5, 1, and 2 Myr are shown with blue, red, and magenta lines, respectively. The distance of D = 7.9 kpc is assumed.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: The observed F200W LFs for the Cloud 2 clusters (Cloud 2-N and 2-S clusters for the left and right panels, respectively). The F200W LFs for sources in the cluster regions (the cluster region F200W LFs) are shown with thick black lines, while those for sources in the control field (the control field F200W LF) are shown with thin lines. The control field F200W LF is normalized by multiplying the ratio of the area of each cluster region to the area of the control field. The cluster F200W LFs, obtained by subtracting the normalized counts from the control field F200W LF from the counts for each cluster region F200W LF, are shown as thick red lines.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: The best-fit IMF for the Cloud 2-S cluster. The best-fit IMFs assuming the TPL and lognormal IMFs are shown as the black solid and dashed lines, respectively. The cluster IMF is also compared to IMFs previously obtained in the field and in nearby star clusters: E. E. Salpeter (1955; magenta), J. Scalo (1998; green), A. A. Muench et al. (2002; red), G. E. Miller & J. M. Scalo (1979; blue), and P. Kroupa (2002; orange). All of the IMFs are normalized to 0 on the vertical axis at a mass of 1 M ⊙.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Same as Figure 9, but for the control field. The left and right panels are for the same control field, but just apply different A  V  thresholds for each cluster, the left and right panels (2 mag ≤ A  V  ≤ 14 mag and 1 mag ≤ A  V  ≤ 18 mag) for the Cloud 2-N and 2-S clusters, respectively.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: The best-fit IMF for the Cloud 2-N cluster. The best-fit IMF assuming a lognormal IMF is shown as the black line. The cluster IMF is also compared to IMFs previously obtained in the field and in nearby star clusters: E. E. Salpeter (1955; magenta), J. Scalo (1998; green), A. A. Muench et al. (2002; red), G. E. Miller & J. M. Scalo (1979; blue), and P. Kroupa (2002; orange). All of the IMFs are normalized to 0 on the vertical axis at a mass of 1 M ⊙.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Model F200W LF with the parameters of the best-fit IMF for the Cloud 2-N and 2-S clusters. The best-fit model F200W LF is shown as the red line with 1σ standard deviation, which is from 100 trials for the best-fit lognormal/TPL IMF parameter sets for the Cloud 2-N/2-S clusters, while the observed cluster KLF for the age is shown as the blue histogram. The bins of the fit range are indicated by filled blue squares, and the others are indicated by open blue squares.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: F200W-excess distributions for stars in the regions of the Cloud 2-N cluster (left panel) and the Cloud 2-S cluster (right panel). The distributions for stars in the cluster regions are shown as thick lines, while those in the control field are shown as thin lines. The distributions for stars in the control field are normalized by multiplying the ratio of the area of each cluster region to the area of the control field. The distributions obtained by subtracting the normalized distribution for stars in the control field from the distribution for stars in each cluster region are shown as red lines.
Paper: Revealing Potential Initial Mass Function Variations with Metallicity: JWST Observations of Young Open Clusters in a Low-metallicity Environment
Authors: Chikako Yasui, Natsuko Izumi, Masao Saito, Ryan M. Lau, Naoto Kobayashi, Michael E. Ressler
Figure caption: Same as Figure 4, but for the control field.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A comparison of the cumulative distribution function best fits to the cluster and field samples. The shaded regions show the 95% confidence interval, which is calculated based on the sample size, sampling of the data, and the number of limit cases. The x-axis is in units of AB magnitudes. We show a comparison of the cumulative distributions of the inner regions (top) and the outer regions (bottom) for cluster (in green) and field (in orange) galaxies. For the FUV − NUV color, both the inner and outer comparisons show statistically significant differences based on the p-value of a log-rank comparison. For the NUV − r color, the inner and outer comparisons show no statistically significant differences based on the p-value.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A comparison of the inner (orange) and outer (pink) colors in NUV − r vs. FUV − NUV for the full (photo-z and spec-z) cluster sample used in the analysis from the main text (left), as well as a spec-z-only sample (right). Axes are in units of AB magnitudes. Right-facing triangles show aperture fluxes with limits in either the FUV flux or the NUV flux. Downward-facing arrows show limits in just the NUV flux. Open circles show aperture fluxes with limit fluxes in both FUV and NUV. Contours based on a kernel density estimate are also shown to better illustrate the comparison.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A comparison of the ΔFUV − NUV and ΔNUV − r color gradients for the full (photo-z and spec-z) cluster sample used in the analysis from the main text (right), as well as a spec-z-only sample (left). Axes are in units of AB magnitudes. We also show contours based on a kernel density estimate of the plotted points for another visual representation of the distributions. Overall, both samples have similar distributions across all four quadrants, as well as equal representation in each quadrant within the estimated error from a Monte Carlo Markov Chain.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: Here we show the CDFs of the inner region of cluster galaxies (green) and field galaxies (orange) in the FUV − NUV and NUV − r, inner and outer colors, generated with survival statistics. Survival statistics does not incorporate errors on the input values directly. Thus, to test the robustness of our results, we run a Monte Carlo with 100 iterations within the 1σ flux errors of the survival statistics CDF for both cluster and field. All iterations are plotted here. We then calculate the rms of the p-value for each pair of Monte Carlo–generated distributions, in order to calculate an error estimate for the p-value.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A comparison of the cumulative distribution function fits to the cluster and field samples. The shaded regions show the 95% confidence interval, which is calculated based on the sample size, sampling of the data, and the number of limit cases in the sample. The x-axis is in units of AB magnitudes. We show a comparison of the cumulative distributions of the outer−inner color gradient distributions for cluster and field galaxies. For the FUV − NUV color (left), only the log-rank test supports a different cluster vs. field gradient distribution, but nonetheless a number of the cluster galaxies do have steeper redder outside to bluer inside trends. For the NUV − r color (right), the overall outer−inner distribution is statistically significantly different, but without a clear bias toward more negative or positive gradients.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: When comparing the color gradients in ΔFUV − NUV (along the y-axis) and ΔNUV − r (along the x-axis), there are four possible combinations, depending on whether each gradient is positive or negative. We indicate these four quadrants here, labeled I–IV, along with an illustration of the relative color gradients. According to an analysis of very similar colors at z ∼ 0 from A. Abramson et al. (2011), actively or recently ram-pressure-stripped galaxies should fall in quadrant I. From surveys of field galaxies at z ∼ 2, showing galaxies having bluer outskirts than insides, the majority of galaxies would lie in quadrant IV, absent significant evolutionary pressure from the environment.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A comparison of the ΔFUV − NUV and ΔNUV − r color gradients of field galaxies (left) and cluster galaxies (right). Axes are in units of AB magnitudes. We also show density contours based on a kernel density estimate of the plotted points for another visual representation of the distributions. Overall, both cluster and field have similar amounts of galaxies falling in quadrants I and III. The major difference between cluster and field appears to be the number of galaxies in quadrant IV and quadrant II in the cluster. There is also an overall much wider range in color gradient values in the cluster.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: Same caption as Figure B1, but for the ΔFUV − NUV and ΔNUV − r color gradients.
Paper: Event-horizon-scale Imaging of M87* under Different Assumptions via Deep Generative Image Priors
Authors: Berthy T. Feng, Katherine L. Bouman, William T. Freeman
Figure caption: Extracted ring features of images reconstructed from simulated data. The dotted line indicates the measured quantity of the ground-truth image, and the shaded yellow region indicates the std. dev. as computed by REx (the orientation of the Ring image was manually set to span 0°–360°). For the score-based priors (CIFAR, GRMHD, RIAF, CelebA), the mean was computed across the measured quantities of 128 posterior samples. The std. dev. for all features except fractional central brightness (f  C ) was computed as the square root of the average variance across these samples. Since REx does not provide uncertainty for f  C  of a single image, the f  C  error bars were computed as the std. dev. of the f  C  values of all posterior samples. All choices of prior roughly recover the target diameter, orientation, and asymmetry. The only exceptions are that the RIAF prior overestimates the diameter of GRMHD 1 (due to the difficulty of fitting GRMHD data to a strong RIAF prior) and that the CelebA prior overbiases the orientation of GRMHD 2 (due to the CelebA prior struggling to produce a strong ring structure with such data). The width and fractional central brightness are particularly prior dependent, with the GRMHD prior providing consistently small values for these features. In contrast, the RIAF prior prefers large widths and high f  C  values. Please see Figure 3 for image samples.