adsabs/AstroCLIMB huggingface dataset:
Paper: Comparative Analysis of TRGBs (CATs) from Unsupervised, Multi-halo-field Measurements: Contrast is Key
Authors: J. Wu, D. Scolnic, A. G. Riess, G. S. Anand, R. Beaton, S. Casertano, X. Ke, S. Li
Figure caption: (Left) Following Table 2, for NGC 3031, tip residuals to the mean for all tip measurements. The residuals are shown sequentially for the different analysis steps. The range of green dashed lines shows the standard deviation of the TRGB detection set of each step. (Right) The same as the left, but with the R cut applied as the second cut. From both panels, we find that all analysis steps contribute to decreasing the overall dispersion, with the cut on the contrast ratio R as the strongest step.
Paper: Comparative Analysis of TRGBs (CATs) from Unsupervised, Multi-halo-field Measurements: Contrast is Key
Authors: J. Wu, D. Scolnic, A. G. Riess, G. S. Anand, R. Beaton, S. Casertano, X. Ke, S. Li
Figure caption: For the methods described in Table 2, the optimization is to determine the best values/choices for the different parameters. For each of our parameters (color bandwidth and slope, smoothing, weighting), we show trends of our three metrics when varying the values. The color bandwidth and slope are, respectively, w and s defined in Equation (2). The smoothing is discussed in Section 3.4 Equation (3), and the three weighting techniques are listed in Equations (4)–(6). The dashed horizontal lines are referential lines for better visual localization.
Paper: Comparative Analysis of TRGBs (CATs) from Unsupervised, Multi-halo-field Measurements: Contrast is Key
Authors: J. Wu, D. Scolnic, A. G. Riess, G. S. Anand, R. Beaton, S. Casertano, X. Ke, S. Li
Figure caption: The Padova isochrones (version CMD3.7) were used to calculate LFs for the ACS F814W passband in the range of ±0.5 around the TRGB to calculate the contrast ratio. The calculations were done for single-age populations ranging from 1.5–10 Gyr at a low metallicity of [M/H] = −2 and −1.5. We plot the same RGB to AGB ratio R used throughout the empirical analysis vs. the age of the stellar population. As shown, the tip contrast increases with the age of the population, with a different dependence but the same general trend for different metallicities. The TCR relation found in Figure 9 may therefore show a relation between the inferred luminosity and the age of the stellar population.
Paper: Comparative Analysis of TRGBs (CATs) from Unsupervised, Multi-halo-field Measurements: Contrast is Key
Authors: J. Wu, D. Scolnic, A. G. Riess, G. S. Anand, R. Beaton, S. Casertano, X. Ke, S. Li
Figure caption: Histogram of the raw CMD properties discussed in Section 3.4 for the GHOSTS fields and the SN fields used in Anand et al. (2022). The lightly shaded blue and orange bars show the numbers for fields with either R < 3 or N +,1.0 < 50. We find generally good agreement between the distributions for the GHOSTS sample and SN hosts.
Paper: Comparative Analysis of TRGBs (CATs) from Unsupervised, Multi-halo-field Measurements: Contrast is Key
Authors: J. Wu, D. Scolnic, A. G. Riess, G. S. Anand, R. Beaton, S. Casertano, X. Ke, S. Li
Figure caption: The dispersion of TRGB measurements from individual fields relative to the mean TRGB across fields for that galaxy. This is done for all 10 GHOSTS galaxies in which more than two fields are observed. A minimum R cut of 4 and N +,1.0 cut of 200 are applied for this calculation (after which two of the hosts no longer have two valid fields).
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: The difference between the disk and stellar inclinations (i  d  − i  s ) plotted vs. different system parameters. The color of each point corresponds to the median value of the minimum obliquity. The top left shows T eff on the bottom axis while the right has the mass, the bottom left shows ﹩v\sin i﹩, and the bottom right the number of confirmed planets in the system.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Stellar parameters for the systems in our sample. The color of each point corresponds to the absolute value of the median of Δi = i  d  − i  s , where blue indicates a well-aligned system and red indicates a large misalignment. The top left figure shows mass vs. T eff, the top right shows radius vs. T eff, the bottom left gives ﹩v\sin i﹩ vs. T eff, and the bottom right gives the rotation period vs. T eff.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Disk inclinations plotted against the stellar inclination for each system in our sample. The color of each point corresponds to the absolute value of the median of Δi = i  d  − i  s , where blue indicates a well-aligned system and red indicates a large misalignment. Capped error bars represent the range of values that a parameter falls within (assuming a uniform distribution), while the rest represent the 68% credibility interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the AU Mic TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 1 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 129590 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 11 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 141943 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 12 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 104860 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 14 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 10647 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 2 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: Merged (MOS1 and MOS2), QPB-subtracted, exposure-corrected, and smoothed XMM image in 2–6 keV. PSR J2021+3651 and WR 141 are marked with a cross (X) and a plus sign (+), respectively. The extent of the outer nebula ﹩\sim 10^{\prime} ﹩ is marked with dashed lines. A “ring” is marked with a dotted line.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: Merged (Obs IDs 8502 and 7603) and exposure-corrected Chandra images of the Dragonfly in 2–6 keV. The scales were adjusted for better legibility. PSR J2021+3651 is marked as a cross (X) in both images. Top: ﹩1^{\prime} \times 1^{\prime} ﹩ image after Gaussian smoothing with σ = 1.5 pixel =0.″7. The 20″ × 10″ inner nebula and the pulsar jet stretching out to ∼30″ from the pulsar are marked with dashed lines. Bottom: ﹩21^{\prime} \times 11^{\prime} ﹩ image after Gaussian smoothing with σ = 3 pixel =3.″0. The arc in length ﹩\sim 7\buildrel{\,\prime}\over{.} 7﹩ is traced with a dotted line. The extent of the outer nebula seen by XMM is marked as a dashed line.
Paper: White Dwarfs Revealed in Gaia’s Candidate Compact Object Binaries
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Comparison of mass estimated in this study vs. those reported in the SHA23 and ATF22 catalogs for the LCs (left) and DRs (right). Blue (orange) dots show candidates from the ATF22 (SHA23) catalogs. The black solid line shows the x = y line. While more or less consistent, our estimated M LC and M DR are typically slightly lower.
Paper: White Dwarfs Revealed in Gaia’s Candidate Compact Object Binaries
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Eccentricity vs. M DR for the 49 sources with identified UV counterparts. Circles denote the 15 sources with significant UV excess. Red + (blue x) denotes sources identified as WDs (NSs) in the SHA23 catalog. In all cases, we use M DR estimated by this study (Section 3.3) and the eccentricities given by SHA23. All the magenta triangles show where we have both FUV and NUV data.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption:                          ﹩4^{\prime} \times 4^{\prime} ﹩ NuSTAR images of the inner nebula. The images were created following the same procedures described in the caption of Figure 2. PSR J2021+3651 is marked with a cross (X). A dashed circle of radius ﹩1^{\prime} ﹩ is shown as a reference.
Paper: Hard X-Ray Observation and Multiwavelength Study of the PeVatron Candidate Pulsar Wind Nebula “Dragonfly”
Authors: Jooyun Woo, Hongjun An, Joseph D. Gelfand, Charles J. Hailey, Kaya Mori, Reshmi Mukherjee, Samar Safi-Harb, Tea Temim
Figure caption: Merged (FPMA and FPMB) and exposure- and vignetting-corrected ﹩21^{\prime} \times 11^{\prime} ﹩ NuSTAR images after Gaussian smoothing with σ = 1.5 pixel =4.″7. The scales were adjusted for better legibility. PSR J2021+3651 and WR 141 are marked with a cross (X) and a plus (+), respectively. The extent of the outer nebula seen by XMM is marked with a dashed line.
Paper: White Dwarfs Revealed in Gaia’s Candidate Compact Object Binaries
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Probability distribution functions for L bol (top) and T eff (bottom) for the WDs (red dashed) and MS stars (orange solid) for sources showing significant UV excess.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: The results of theoretical modeling and the results of the POD and DMD analyses obtained for sunspot NOAA 11366 are presented for time intervals T  c6 (top panel) and T  c7 (bottom panel). The first column displays the spatial structure of the theoretically modeled fundamental slow-body sausage mode for the same shape as the umbra shape of sunspot NOAA 11366 at the particular time interval. The second column shows the spatial structure of the first (top and bottom) POD modes, where the dominant frequency of their time coefficient is in the range between 3.1 and 4.8 mHz. The cross correlation between the model and the determined POD mode is shown in the third column. The fourth column displays the spatial structure of the DMD modes that correspond to 3 mHz (top) and 4.3 mHz (bottom). Finally, the last column contains the cross correlation between the model (first column) and the DMD mode (fourth column). The solid black line shows the umbra/penumbra boundary. The same configuration was used for Figures 4 and 5. The color bars in the first column display the density perturbation obtained from the theoretical model, while the second and fourth columns display the magnitude of the Doppler velocity after being analyzed by POD and DMD, respectively. The color bars in the third and fifth columns denote the correlation/anticorrelation.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: The results of theoretical modeling and the POD and DMD analyses obtained for sunspot NOAA 12146 are presented for the time intervals T  e5 (top panel) and T  e10 (bottom panel). The first column displays the spatial structure of the theoretically modeled fundamental slow-body sausage mode for the same shape as the umbra shape of sunspot NOAA 12146 at two time intervals. The second column shows the spatial structure of the fourth POD mode (top) and the fifth POD mode (bottom), where the dominant frequency of their time coefficient is in the range between 3.3 and 4 mHz. The cross correlation between the model and the determined POD mode is shown in the third column. The fourth column displays the spatial structure of the DMD modes that correspond to 3.8 mHz (top) and 3.4 mHz (bottom). Finally, the last column contains the cross correlation between the model (first column) and the DMD mode (fourth column). The solid black line shows the umbra/penumbra boundary. The same configuration was used for Figures 7 and 8.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Same as Figure 3, but here the first row shows the first POD mode and the spatial structure of the DMD mode that corresponds to 3.4 mHz at T  c1. The second row shows the second POD mode and the spatial structure of the DMD mode that corresponds to 3.1 mHz at T  c1. The third row shows the second POD mode and the spatial structure of the DMD mode that corresponds to 3.9 mHz at T  c7. The first column shows the morphology of the theoretical fundamental slow-body kink mode that corresponds to T  c1 (M 3 top panel and M 2 middle panel) and T  c7 (M 3; bottom panel).
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: First 10 POD modes of the circular sunspot. Every column shows a POD mode, and the rows show how the modes change at each time interval, T  ci , of the data time series. Every time interval contains 50 images and has a duration of 37.5 minutes. Every time interval is shifted by 20 images, i.e., the initial time of T  ci+1 is after the initial time of T  ci  by 20 images, which corresponds to 15 minutes.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Same as Figure 6, but here the first row shows the ninth POD and the spatial structure of DMD mode that corresponds to 2.8 mHz at T  e1. The second row shows the ninth POD and the spatial structure of DMD mode that corresponds to 4.6 mHz at T  e3. The first column shows the slow-body fluting (n = 2) mode that corresponds to T  e1 (M 4; top panel) and T  e3 (M 5; bottom panel).
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Wave contribution from the observed MHD modes to the total variance of the signal in the case of the circular sunspot, WE c , as a function of time. The values of WE c  correspond to the contribution of the POD mode linked to MHD wave mode in each time interval, T  ci . Different modes are shown by different colors, as indicated by the legend in the upper part of the plot. Here, FSBS stands for the fundamental slow-body sausage (n = 0) mode, FSK for the fast-surface kink (n = 1) mode, and SBF for the slow-body fluting (n = 2) mode, while (I) and (II) refer to two different (perpendicular) directions of the wave polarization.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Wave contribution from the observed MHD wave modes to the total variance of the signal for the elliptical sunspot, WE e , as a function of time. The values of WE e  correspond to the contribution of the POD mode linked to MHD wave mode at each time interval, T  ei . The identified MHD modes are shown by different colors and specified by the legend in the upper part of the plot. The abbreviation of possible modes is identical with the one used in Figure 9.
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Same as Figure 6, but here the first row shows the sixth POD and the spatial structure of the DMD mode that corresponds to 3.3 mHz at T  e1. The second row shows the sixth POD and the spatial structure of the DMD mode that corresponds to 3.5 mHz at T  e5. The first column shows the fundamental slow-body kink mode that corresponds to T  e1 (M 2; top panel) and T  e5 (M 3; bottom panel).
Paper: The Temporal and Spatial Evolution of Magnetohydrodynamic Wave Modes in Sunspots
Authors: A. B. Albidah, V. Fedun, A. A. Aldhafeeri, I. Ballai, D. B. Jess, W. Brevis, J. Higham, M. Stangalini, S. S. A. Silva, C. D. MacBride, G. Verth
Figure caption: Same as Figure 3, but here the first row shows the eighth POD mode and the spatial structure of the DMD mode that corresponds to 4 mHz at T 6. The second row shows the seventh POD and DMD modes that correspond to 3 mHz at T 7. The first column shows the slow-body fluting (n = 2) that corresponds to T 6 (M 5; top panel) and T 7 (M 4; bottom panel).
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: Molar fraction of N2 at different thermal diffusion factors (a) and Molar fraction of N2 at different mass relative factors (b).
Paper: Mass Transfer Theory Based Analysis of Influencing Factors on Component Gradient of Near-surface Atmosphere on Venus
Authors: Wen Gao, Xiaoning Yang, Jing Wang, Yanqiang Bi, Boying Lin, Yonghong Shang, Xinguang Cui
Figure caption: Molar fraction of N2 at different surface temperatures (a) and Molar fraction of N2 at different gravity (b).
Paper: Striped Jets in Post–Neutron Star Merger Systems
Authors: Emma Kaufman, I. M. Christie, A. Lalakos, A. Tchekhovskoy, D. Giannios
Figure caption: The duration τ of field reversals on the BH, determined from ϕ BH,north (see Figure 1) for all models considered (see legend), shows a general increase with increasing simulation time. For times t ≳ 5 × 10−2 s, our BT-LD, BT-LDN, and BT-NR models no longer exhibit flips in polarity up to the cessation of the simulation, denoted by the horizontal lines of the same color. Reversals produced at times ≳0.015 s, i.e., times at which polar outflows begin to form (horizontal black line), will propagate and reconnect at various distances z rec with the jet (see top axis). Here we use a fiducial value of Γj = 100 for the jet Lorentz factor in computing z rec (see Equation (1)).
Paper: Striped Jets in Post–Neutron Star Merger Systems
Authors: Emma Kaufman, I. M. Christie, A. Lalakos, A. Tchekhovskoy, D. Giannios
Figure caption: Time-averaged power 〈P Φ〉 (see Equation (2)) of each stripe propagating within the jet (see also Figure 2). Here 〈P Φ〉 is highly scattered for all models (see legend) as a function of τ, with the BT model displaying additional fluctuations as a function of simulation time (see color bar). The BT-LDN model, which neglects all nuclear physics, contains the stripes with the largest power. The black dashed (dotted) line shows the minimum (maximum) photospheric radius (see Equation (3)) using fiducial values of Γ∞ = 300 and Γ j  = 100.
Paper: Striped Jets in Post–Neutron Star Merger Systems
Authors: Emma Kaufman, I. M. Christie, A. Lalakos, A. Tchekhovskoy, D. Giannios
Figure caption: Time-averaged energy 〈E〉 per stripe (top panel) and cumulative energy 〈E〉c of all stripes (bottom panel) as a function of radial distance z within the jet. The BT-LD model (see legend) dissipates all available energy within the estimated upper bound of the photospheric radius ﹩{z}_{\mathrm{ph},\ \max }﹩ (vertical line), while the remaining models dissipate only a small fraction (≲1.6%) of 〈E〉c. Here 〈E〉 (〈E〉c) appears to constitute a power law as a function of radial distance and, equivalently, τ. Fitting each model, the slope can be estimated as (〈E〉: 1.7, 〈E〉c: 1.8) for the BT model, (〈E〉: 1.5, 〈E〉c: 1.7) for BT-NR, (〈E〉: 2.5, 〈E〉c: 3) for the BT-LD model, and (〈E〉: 2.2, 〈E〉c: 2.2) for the BT-LDN model.