adsabs/AstroCLIMB huggingface dataset:
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: Theoretical eigenfunctions that correspond to the changing shapes of the observed circular sunspot (see Figure 11). Every row shows the spatial structure of the models at different times and the changing shape. The columns represent different types of slow-body modes, and they are labeled by M  i , where i = 1,...,10. In particular, M 1 is for fundamental sausage (n = 0), M 2 and M 3 are for fundamental kink (n = 1), M 4 and M 5 are for fluting (n = 2), M 6 is for sausage overtone (n = 0), M 7 and M 8 are for fluting (n = 3), and the last two columns (M 9 and M 10) are for kink overtone (n = 1).
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: Theoretical eigenfunctions that correspond to the changing shapes of the observed elliptical sunspot (see Figure 13). Every row shows the spatial structure of the models at different times and the changing shape. The columns represent different types of slow-body modes, and they are labeled by M  i , where i = 1,...,10. In particular, M 1 is for fundamental sausage (n = 0), M 2 and M 3 are for fundamental kink (n = 1), M 4 and M 5 are for the fluting (n = 2), M 6 is for sausage overtone (n = 0), M 7 and M 8 are for the fluting (n = 3), and the last two columns (M 9 and M 10) are for kink overtone (n = 1).
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 elliptical sunspot. Every column shows a POD mode, and the rows show how the modes change at each time interval, T  ei , of the data time series. Every time interval contains 80 images and has a duration of 60 minutes. Every time interval is shifted by 40 images, i.e., the initial time of T  ei+1 is after the initial time of T  ei  by 40 images, which correponds to 30 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: Theoretical eigenfunctions that correspond to the changing shapes of the observed circular sunspot (see Figure 17). Every row shows the spatial structure of the models at different times and the changing shape. The columns represent different types of slow-body modes, and they are labeled by M  i , where i = 1,...,10. In particular, M 1 is for the fundamental sausage, M 2 and M 3 are for fundamental kink, M 4 and M 5 are for fluting (n = 2), M 6 is for sausage overtone, M 7 and M 8 are for fluting (n = 3), and the last two columns (M 9 and M 10) are for kink overtone.
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: Theoretical eigenfunctions that correspond to the changing shapes of the observed circular sunspot (see Figure 19). M 1 is for fundamental sausage, M 2 and M 3 denote the fundamental kink, M 4 and M 5 are for fluting (n = 2), M 6 is for sausage overtone, M 7 and M 8 are for fluting (n = 3), and the last two columns (M 9 and M 10) are are for kink overtone.
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  i , of the data time series. Every time interval contains 30 images and has a duration of 22.5 minutes. Every time interval is shifted by 15 images, which correponds to 11 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: Summation of pixels in the correlation matrix between the POD modes in Figure 13 and the theoretical models in Figure 14, for every T  ei . The color bar shows the amplitude of the summation of the correlation matrix. The maximum value of each column was normalized along all time intervals.
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: Summation of pixels in the correlation matrix between the POD modes in Figure 11 and the theoretical models in Figure 12, for every T  ci . The color bar shows the amplitude of the summation of the correlation matrix. The maximum value of each column was normalized along all time intervals.
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  i , of the data time series. Every time interval contains 80 images and has a duration of 60 minutes. Every time interval is shifted by 40 images, which correponds to 30 minutes.
Paper: A Tight Universal Relation between the Shape Eccentricity and the Moment of Inertia for Rotating Neutron Stars
Authors: Yong Gao, Lijing Shao, Jan Steinhoff
Figure caption: The ﹩{e}_{i}/\hat{R}﹩–﹩\bar{I}﹩ and ﹩{e}_{c}/\hat{R}﹩–﹩\bar{I}﹩ relations for NSs (blue) and QSs (red). Here we take the dimensionless spin χ = 0.5.
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: CMDs of individual fields in NGC 3031 with labels corresponding to the fields presented in Figure 1. The field numbers are labeled at the top left corner of each panel and match those in Figure 1, and the R.A. and decl. of each field are labeled at the bottom-right corner, in units of degree in epoch J2000. Halo Fields 01 and 08-11 are from HST external, archival data that has been involved in the analyses of the GHOSTS survey, and data of all 11 halo fields are from the GHOSTS compilation. The properties of the CMD vary from field to field; some of this can be attributed to contamination from younger stellar populations where the disk and halo overlap. This study aims to quantify the remaining differences and their impact on TRGB measurements. The red vertical line represents our separation of the MS stars from evolved stars, like the AGB and RGB, and the green line shows where the S/N reaches 10. Both lines are used in the spatial clipping algorithm, as discussed in Section 3.1. The orange lines denote the optimized color that maximizes the number of stars included on the RGB branch. The color and magnitude selections are discussed in Section 3.
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 tip magnitudes (top) and EDR (bottom) are shown for all the non-disk fields of NGC 3031. Note that the F814W magnitude ranges are different between the top panels and bottom panels, and the lower panels are zoomed in to show the wiggle patterns better and do not include the extreme outliers seen in the top panels. The left and right figures present the results for two different smoothing scales (σ = 0.05 and 0.1). In the top panels, the green lines denote the median of detections. We apply our algorithm to the individual field, labeling each tip detection with an orange diamond marker in the top panels, and the one with the highest R for each field is shaded darker, where R is the contrast defined in Equation (8). As shown in the bottom panels, there is little correlated structure of EDRs, except at the location of the best-fit line around F814W ∼ 23.85 mag in the bottom-right panel. Furthermore, for multiple fields, there are multiple peaks in this space, and an optimal algorithm must attempt to distinguish between these. Sometimes, the highest EDR peak is not aligned with the median as it is a false detection due to large absolute LF values at the faint end, and Equation (6) cannot sufficiently suppress that. We find that R is a critical indicator to characterize the quality of tip detections, which can filter out false tip detections fainter than the real tip. In this figure, only peaks with R > 3.5 are marked (top panel) and labeled (bottom panel, by the vertical line) as plausible. To further constrain the tip location, we need to apply N +,1.0, which will filter out false detections in the bright end due to a small number of statistics, see Figure 6.
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: A demonstration of the spatial clipping used for this analysis to suppress contamination from young stars and AGB stars. As shown in Figure 2, we use a red vertical line and a green horizontal line to find the location of the MS, and we calculate the number density of blue stars (i.e., stars bluer than the red line and brighter than the green line in color–magnitude space) and red stars (i.e., all other stars on the CMD) as well as the ratio of red stars to blue stars. The number densities and ratio are calculated with a resolution size of 16 arcsec2. We plot the ratio and blue star population in the top row (panel 1 and panel 2, respectively) across a spatial region of 11.1 arcmin2, which is the size of an entire field in the GHOSTS survey. The units of the panels in the first row are ACS pixels. In panel 3, we perform a 2D-GLOESS smoothing on the blue star population, and we find through optimization that cutting areas based on the smoothed number density of blue stars yields the best tip measurements, as quantified in Section 4. In the bottom row, we show in the left panel the original CMD of this field, with blue stars marked blue. The middle panel shows how this space is carved out using a 2D-GLOESS filter, the white empty space is the region clipped, and the red and blue dots elsewhere are the remaining red stars and blue stars. We present a tag of “in direction of disk” in the space showing the region near the galaxy disk, which demonstrates the efficiency of our spatial clipping algorithm. In the bottom-right panel, we show how the blue main-sequence cluster in the CMD, together with non-MS young star populations such as supergiants, is heavily suppressed after this spatial clipping.
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: A demonstration of how the TRGB magnitude is determined from the CMD for one of the halo fields in NGC 3031 (#4). For each step, analysis choices must be made including color cuts and spatial clipping (panel 1), and smoothing/weighting of the LF (panels 2 and 3). The red line crossing all three panels is the tip detection line and matches the tallest peak of the black curve in panel 3. The red “x” points in panel 1 indicate the stars cut using spatial clipping as discussed in Section 3.1. The N − and N +, as discussed in Section 3.4, indicate the range of magnitudes 0.5 mag brighter and fainter than the red TRGB magnitude, respectively. The gray distribution in panel 2 represents the LF and the bold black curve the smoothed LF. In panel 3, the raw EDR is with no color band or spatial clipping applied; the spatial EDR is with only a spatial clipping applied; the “spatial&color” EDR is with both a color band and spatial clipping applied.
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: A footprint of NGC 3031 produced from SDSS gri data (Alam et al. 2015), generated with the online Imaging Mosaics tools (https://dr12.sdss.org/mosaics/). The locations of the fields observed as part of the GHOSTS program are indicated and labeled. The GHOSTS fields are each 1 pointing of HST+ACS corresponding to 11.1 arcmin2. All halo fields are located at or past a 25 mag arcsec−2 isophot.
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: Theoretical eigenfunctions that correspond to the changing shapes of the observed elliptical sunspot (see Figure 21). M 1 is for fundamental sausage, M 2 and M 3 are for fundamental kink, M 4 and M 5 are for fluting (n = 2), M 6 is for sausage overtone, M 7 and M 8 are for fluting (n = 3), and the last two columns (M 9 and M 10) are for kink overtone.
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: Theoretical eigenfunctions that correspond to the changing shapes of the observed elliptical sunspot (see Figure 23). M 1 is for fundamental sausage, M 2 and M 3 are for fundamental kink, M 4 and M 5 are for fluting (n = 2), M 6 is for sausage overtone, M 7 and M 8 are for fluting (n = 3), and the last two columns (M 9 and M 10) are for kink overtone.
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 elliptical sunspot. Every column shows a POD mode, and the rows show how the modes change at each time interval, T  i , 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 30 images, which correponds to 22.5 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: First 10 POD modes of the elliptical sunspot. Every column shows a POD mode, and the rows show how the modes change at each time interval, T  i , of the data time series. Every time interval contains 100 images and has a duration of 75 minutes. Every time interval is shifted by 50 images, which correponds to 37.5 minutes.
Paper: A Tight Universal Relation between the Shape Eccentricity and the Moment of Inertia for Rotating Neutron Stars
Authors: Yong Gao, Lijing Shao, Jan Steinhoff
Figure caption: The ﹩{e}_{i}/\hat{R}﹩–﹩\bar{I}﹩ universal relation for fast-rotating models with the dimensionless spin χ = 0.6. The upper panel shows the fitted universal relations for both NSs and QSs. The middle (lower) panel presents the relative deviation for NSs (QSs).
Paper: A Tight Universal Relation between the Shape Eccentricity and the Moment of Inertia for Rotating Neutron Stars
Authors: Yong Gao, Lijing Shao, Jan Steinhoff
Figure caption: The ﹩{e}_{* }/\hat{R}﹩–﹩\bar{I}﹩ universal relation for slowly rotating models. The upper panel shows the fitted universal relations for both NSs and QSs. The middle (lower) panel presents the relative deviation for NSs (QSs).
Paper: A Tight Universal Relation between the Shape Eccentricity and the Moment of Inertia for Rotating Neutron Stars
Authors: Yong Gao, Lijing Shao, Jan Steinhoff
Figure caption: The mass–radius relation for selected EOS models of NSs (solid) and QSs (dashed). The 1σ regions of the mass measurements of PSR J0348+0432 (Antoniadis et al. 2013) and PSR J0740+6620 (Fonseca et al. 2021) are illustrated.
Paper: A Tight Universal Relation between the Shape Eccentricity and the Moment of Inertia for Rotating Neutron Stars
Authors: Yong Gao, Lijing Shao, Jan Steinhoff
Figure caption: The surface of the fitting formula Equation (12) for NSs (blue) and QSs (red). Models of NSs and QSs fall on two well-defined surfaces.
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: Frequency-resolved lags computed in each band with respect to the UVW2 reference band, with corresponding bias-corrected coherence values below. The (non-frequency-resolved) CCF lags computed from the original light curves are shown with 1σ uncertainties in blue, and those computed from the detrended light curves in orange. The 3 day binning of the X-ray light curves limits us to frequencies below ∼0.2 day−1 (the Nyquist frequency).
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: The frequency-resolved lags in the lowest three frequency bins, fit with a τ ∝ λ 4/3 relation with best-fit normalization values (τ 0) shown (dashed blue line). The dashed orange line shows the expected lag–wavelength relation for this source using the disk reprocessing model in each frequency range. At higher frequencies, the lags rapidly approach the expected lag–wavelength relation for this source, with the lags in the 0.09–0.18 day−1 range roughly consistent with the disk reprocessing model. If this discrepancy is due to contamination from a distant reprocessor, then it is occurring on timescales longer than 1/0.09 = 11.5 days, consistent with the radius of the BLR based on the 13.9 day Hβ lag (Grier et al. 2012).
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: An exemplar band (the i band) for comparing the lags computed with respect to the UVW2 band using Fourier techniques (black) and the (non-frequency-resolved) CCF using the original light curves (blue) and the detrended light curves (orange), with 1σ uncertainties shown. The non-detrended CCF lag is consistent with the low-frequency component of the Fourier lags, whereas the detrended CCF lag is consistent with those at higher frequencies. See Figure 4 for the lags computed in all bands.
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: Left: light curves from the 100 day reverberation campaign presented by Kara et al. (2023) with Swift and ground-based telescopes from MJD 2458770–2458865. The average of 1000 GP realizations is shown by solid orange and blue lines, with shaded regions indicating 1σ in the distribution. In practice, we do not average over the realizations to compute the lags (see Section 3). Right: the CCF (solid black line) and the distribution of ICCF centroid lags (colored histograms), both with respect to the UVW2 band.(The data used to create this figure are available.)
Paper: X-Ray/UVOIR Frequency-resolved Time Lag Analysis of Mrk 335 Reveals Accretion Disk Reprocessing
Authors: Collin Lewin, Erin Kara, Edward M. Cackett, Dan Wilkins, Christos Panagiotou, Javier A. García, Jonathan Gelbord
Figure caption: Distributions of lags and bias-corrected coherence from simulated light curves with a 2 day lag in the g, z band (left, middle), and a 10 day lag in the soft X-ray band (right), with respect to the simulated UVW2 reference band. We compare the simulated lag recovery from unevenly sampled light curves, with time bins matching those of the observations and thus require the use of GPs (orange), to evenly sampled light curves (black) allowing immediate use of Fourier techniques. Shaded regions are used to visualize the overlapping lag uncertainties. The effect of applying GPs to compute the lags and their uncertainties are the most (z, soft X-ray) and least pronounced (g) in these bands in terms of error from the simulated lag and uncertainties compared to those computed from regularly sampled data.
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: Values of the metrics defined in Section 4.1, as functions of different R and N +,1.0, where R is the contrast ratio defined in Equation (8) and N +,1.0 is the number of stars within one mag below tip as defined in Equation (9). In each panel, trend lines for different N +,1.0 cuts are given. (Left) For each trend line, the metric is plotted with varying R cut (i.e., the minimum R as labeled on the x-axis), starting from 1.5–6.5. Note that for a specific R cut, the data which passes through this cut has a mean ratio typically 2–3 times greater than the cut limit. Likewise, the mean number of stars is a factor of a few greater than the minimum, see Section 4.3. (Left, top) The trend of the dispersion of field-tip magnitudes σ tot as a function of the minimum ratio of R. (Left, middle) Similarly, the percentage of fields P valid passes the cuts from the above panel. (Left, bottom) The number of detected tips per field N TPF as a function of the minimum ratio of R. (Right) Changing the x-axis to be mean R instead of minimum, using a running bin size of 3 to make the set (e.g., for a minimum R = 3, we calculate the mean R of detections whose ratio 3 ≤ R < 6). (Right, top) Analogous to the left, but we add on one more curve which is the predicted σ tot from Equation (11). (Right, middle/bottom) Analogous to the left.
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 relationship between measured tip-brightness residual for detected field TRGBs and R, using a σ = 0.1 smoothing and R ≥ 3, N +,1.0 ≥ 200 cut, where R is the contrast ratio defined in Equation (8), and N +,1.0 is the number of stars within one mag below tip as defined in Equation (9). For each galaxy, we calculate each detection’s residual to the median of all the TRGB measurements within that galaxy. Note that for each field of that specific galaxy, it is also likely to have multiple detections. The residuals are plotted vs. the detection’s R, with error bars derived from Equation (11). The orange line is an error-weighted fitting of the blue data points, and the shaded region represents the error of this fitting. We find the slope of the orange fitting line to be −0.023 ± 0.0046 mag/unit ratio. Consequently, we find a TCR, which shows higher R is related to brighter tip magnitude.