adsabs/AstroCLIMB huggingface dataset:
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: Locations of detected X-ray sources. The sources detected in different areas as defined in Table 1 are plotted in different colors.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: The probability density distribution of different types sources in Figure 4 at different hardness ratios. The vertical dashed line marks our criteria for separating fg star from AGNs and XRBs. The HR1–HR2 criterion in the upper panel is used in the source classification, as summarized in Table 2.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: The X-ray contours and optical images of eight extended galaxies. The contours are 2σ  (background uncertainty) and above of the 0.5–4.5 keV X-ray count-rate images smoothed with a 5″  Gaussian kernel. The ﹩1\times 1\,{\mathrm{arcmin}}^{2}﹩ optical images are from the PS1 g, r, and z bands.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: False-color image of the newly discovered superbubble candidate J004436.8+412514. It is composed of Hα (red) and [O III] λ5007Å (green), and the X-ray (blue, 0.2–1.0 keV) image is smoothed with a 20″  Gaussian kernel. A dashed circle with a diameter of 30″ (∼110 pc at a distance of 761 kpc) has been superimposed on the location of the superbubble candidate.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: The probability density of Gaia Gmag, F X/G (the flux ratio between 0.5 and 2.0 keV and the Gaia G band), and HR2 for secure matches and nonmatches based on distance. Also shown are the corresponding ratios of the kernel densities of these parameters.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: The stacked PN, MOS1, and MOS2 spectra of AGN candidate J004442.8+415340 are shown in black, red, and green, respectively. Also shown are the corresponding best-fit absorbed power-law model and the residuals.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: Comparison between the parallax and kinematic distances. The young stellar population is shown in the left panel, and the masers are shown in the right panel. D  π  is the distance converted from the measured parallax. D  k  is the kinematic distance. The standard kinematic distance is obtained without considering the peculiar motion. The revised kinematic distance is obtained by adding the offsets to radial velocity to counteract the peculiar motion.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: (a) l–v diagram. Colored dots are the sources of masers (orange dots), YOCs (red triangles), and O–B2-type stars (cyan diamonds). (b) Variations in the average V LSR per 20° for the masers (orange), YOCs (red), and O–B2-type stars (cyan) along Galactic longitude. Each interval must have more than five sources.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption:  V LSR values of the YOCs (triangles) and O–B2-type stars (diamonds) being assigned to the corresponding spiral arms (lines) as a function of Galactic longitude. The magenta, blue, and green lines represent the Perseus Arm, the Local Arm, and the Carina Arm, respectively, whose ﹩{V}_{\mathrm{LSR}}^{\mathrm{mod}}﹩ values are calculated by using Equation (2).
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: The average peculiar motions of the YOCs as a function of Galactocentric distance, R. The black solid lines indicate all sources, and shaded areas represent the uncertainties. The magenta, blue, and green lines represent the sources located in the Perseus, Local, and Carina Arms. The average is calculated within a window of 1 kpc width in steps of 0.25 kpc, and R 0 is 8.15 kpc. Each interval must have more than five sources.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: Histograms of peculiar motions of the O–B2 type stars.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: Histograms of peculiar motions of the YOCs.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: The average peculiar motions of the O–B2-type stars as a function of Galactocentric distance, R. The others are the same as Figure 5.
Paper: Kinematics of the Local Spiral Structure Revealed by Young Stars in Gaia DR3
Authors: Dejian Liu, Ye Xu, Chaojie Hao, Shuaibo Bian, Zehao Lin, Yingjie Li, Jingjing Li
Figure caption: Schematic depiction of the source and Galactic parameters.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Input artificial star CMDs showing how the model SEDs cover the relevant color space. The color bar is in units of stars per CMD bin. Blue lines mark the approximate depth of the observed photometry. The models extend to much fainter fluxes than any detections in some bands due to very red colors of some models. Specifically, some of the oldest ages, highest metallicities, and high reddenings are potentially detectable in the IR but extremely faint in the UV. Further, the very faint blue feature in the UV bands is due to red leaks in the UV filters, which result in small fluxes for red stars that are not detectable in the UV bands.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Exposure map of all exposures included in a typical half-brick run, where photometry was only performed on the area indicated with the black box, but all exposures that had pixel falling within that area were included in the run, resulting in our seamless final catalog.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: The location of the 23 bricks of the PHAT survey. Each of these bricks consists of 18 HST pointings, each of which contains data in all three HST cameras. A full survey observing strategy description is provided in W14.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: The new optical CMDs for the six colored regions shown in Figure 4 with the W14 CMDs of the same regions subtracted away. The color bar indicates the significance of the difference between the two CMDs, calculated as the new CMD minus the old CMD divided by the square root of the sum of the two CMDs in each CMD bin. The rows go from lower to higher stellar density to show the decrease in photometric quality as stellar density increases. The photometry extends slightly deeper than W14 at all but the highest stellar density region, as shown by the larger number of stars at fainter magnitudes. Furthermore, the red clump feature (the strip starting at F814W = 24, F475W−F814W = 1.5 and extending to the red) appears tighter when it is detected.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Map of the six levels of model stellar densities used to define the six regions that were used to make the different CMDs shown in Figures 11–18. Numbers refer to the log of the stellar density of red giant branch stars. The numbers are relative and determined from a model disk, making the normalization irrelevant. The areas covered by the defined regions are 770, 481 349, 113, 106, and 31 arcmin2 from lowest to highest stellar density, respectively. We divided our results in this way to account for the changing completeness limits with stellar density in the same way as W14 for easy comparison.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Example star-by-star comparison for all six bands, taken from Brick 8 of the survey. The color bar is in units of log of the number of stars per Δmag–-mag bin. The median of the residual is shown by the thick line, while the interquartile range is shown with the thin lines. The residuals show general consistency between the measurements. The UV bands show significant offsets, which is expected from updates to calibrations and CTE corrections, indicated by the yellow shading. The IR bands show slightly fainter new photometry, likely partially due to better deblending. Furthermore, all bands show systematic bias to fainter magnitudes at the faint end, as expected from improved deblending.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: The new IR CMDs for the six colored regions shown in Figure 4 with the W14 CMDs of the same regions subtracted away. The color bar indicates the significance of the difference as calculated in Figure 11. The rows go from lower to higher stellar density to show the decrease in photometric quality as stellar density increases. The new photometry is slightly redder, likely due mostly to the improved deblending from including all overlapping data in the star finding, as well as the different IR PSF. Furthermore, the red clump is detected in the third and fourth density bins (middle row) in the new photometry at more than 5σ greater significance than in W14.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Color–color relations of red clump and red giant branch stars from matched regions of Brick 8 in the W14 catalog and our new catalog. The color bar is in units of the log of the number of stars per color–color bin. The thick lines mark the median F814W−F160W color as a function of F475W−F814W color. While the results are clearly similar, the width of the 16th to 84th percentile of the F814W−F160W color as a function of F475W−F814W color, shown with the thinner lines, is slightly narrower (by a few hundredths of a magnitude) in the new photometry, confirming improved photometric precision over W14.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Optical CMDs for the six colored regions shown in Figure 4. The color bar is in units of stars per CMD bin. The rows go from lower to higher relative stellar density to show the decrease in photometric quality as stellar density increases. The photometry extends slightly deeper (∼0.2 mag) than W14 at all but the highest stellar density region.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: IR CMDs for the six colored regions shown in Figure 4. The color bar is in units of stars per CMD bin. The rows go from lower to higher stellar density to show the decrease in photometric quality as stellar density increases.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: UV CMD for the entire survey. The color bar is in units of stars per CMD bin. The photometry extends slightly deeper (∼0.2 mag) than W14  due to the inclusion of overlapping imaging when performing the photometry.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Optical-IR CMDs for the six colored regions shown in Figure 4. The color bar is in units of stars per CMD bin. The rows go from lower to higher stellar density to show the decrease in photometric quality as stellar density increases. The photometry extends slightly deeper than W14 at all but the highest stellar density region.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Maps of the spatial distribution of four CMD features that are proxies for different age populations. The top row provides a summary of the population selection used to create the maps. The white dot in the lower left of each map shows the size of the smoothing kernel used. The color bar is in units of stars per CMD bin. The left panel shows outlines of the areas of the optical CMD from which the MS (red polygon) and helium-burning (cyan polygon) populations were extracted, while the right panel shows outlines of the areas of the infrared CMD from which the RGB (red polygon) and AGB (green polygon) populations were extracted. The MS probes ∼3–200 Myr, and the HeB probes ∼30–500 Myr. The AGB probes ∼0.8–2 Gyr, and the RGB probes ≳2 Gyr. The bottom two rows show the resulting maps showing that the two younger populations are more highly structured than the two older populations.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: UV, optical, and IR plots showing the median number of bands with good measurements per star as a function of color and magnitude in three radial bins of the survey, representing high (top row), medium (middle row) and low (bottom row) stellar density regions. The CMD space is color coded to show the number of bands with good measurements. In all panels, yellow, orange, magenta, purple, and blue points show stars with good measurements in two, three, four, five, and six bands, respectively. Left: UV CMD produced from all measurements where both bands passed our GST criteria. Center: optical CMD produced from all measurements where both bands passed our GST criteria. Right: IR CMD produced from all measurements where both bands passed our GST criteria.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Bias and scatter results of our ASTs in all six bands as a function of input magnitude. The bias is the median difference of the ASTs (output – input). Scatter is calculated as the difference between the 84th and 16th percentile (output – input) differences divided by 2. In all bands, scatter increases with magnitude, and in the IR bands, the bias is for recovered stars to be brighter than input, as expected from crowding effects. In uncrowded regions, the bias is for recovered stars to be fainter than input, suggesting slight background overestimation when optimizing for crowded fields.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Comparison of the spatial distributions of a small section of the survey from W14 (left) and this work (right). The color bar is in units of the log of the number of stars per spatial bin. Top row: a crowded region of the survey (Brick 2). There is improved depth, except at the IR detector edges (example labeled), and there is improved homogeneity in this legacy reduction. Bottom row: an uncrowded region (Brick 22). There is improved depth in the overlapping ACS frames (example labeled) and improved homogeneity in this legacy reduction.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Completeness as a function of magnitude for all six bands at six levels of stellar density. Higher stellar densities show lower completeness due to crowding, with the effect showing up more strongly in redder bands. The statistics at the bright end are essentially unaffected by the small number of outliers detected.
Paper: The Panchromatic Hubble Andromeda Treasury. XXI. The Legacy Resolved Stellar Photometry Catalog
Authors: Benjamin F. Williams, Meredith Durbin, Dustin Lang, Julianne J. Dalcanton, Andrew E. Dolphin, Adam Smercina, Petia Yanchulova Merica-Jones, Daniel R. Weisz, Eric F. Bell, Karoline M. Gilbert, Léo Girardi, Karl Gordon, Puragra Guhathakurta, L. Clifton Johnson, Tod R. Lauer, Anil Seth, Evan Skillman
Figure caption: Same as Figure 13, but these maps are constructed only including stars with F475W < 28.3 so that the patterns due to the improved depth in the new photometry are not visible.