adsabs/AstroCLIMB huggingface dataset:
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Distribution of the MWL flux values in different time intervals: 1 day binned unabsorbed XRT-band flux (A-panel); LAT-band fluxes with 1 week integration (B); 1 day binned UVW2-band flux (C); 1 week binned MAXI and BAT-band fluxes (panels (D1) and (D2), respectively); 1 day binned TeV-band excess rates (FACT observations; panel (D3)); 1 day binned fluxes in the UVOT bands U and V (panels (D4) and (D5), respectively). The red and green curves show the log-normal and Gaussian fits to the histograms, respectively.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Correlation between the MWL fluxes. (a) Unabsorbed 0.3–2 keV and 2–10 keV fluxes; (b)–(c) 0.3–10 keV flux vs. the 0.3–300 GeV (1 week binned) and UVW2 fluxes; (d)–(f) UVW2 flux vs. the 0.3–300 GeV, UVW1 and V fluxes. The black, red, and blue points correspond to the data from Intervals 1a, 1b and 1c, respectively.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Unabsorbed fluxes and spectral parameters plotted vs. time. (a) 0.3–2 keV flux, (b) 2–10 keV flux, (c) curvature parameter, (d) photon index at 1 keV (black points) and the 0.3–10 keV photon index (blue points), and (e) position of the synchrotron SED peak. The Intervals presented in Section 3.1.1 are located between the vertical dashed lines. The downward gray triangles in the bottom panel indicate the upper limit to the intrinsic position of the synchrotron SED peak. The vertical dashed lines represent the boundaries between Intervals 1a, 1b, and 1c.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Statistical properties of the 0.3–10 keV IDVs: distribution of the related unabsorbed 0.3–10 keV fluxes (panel (a)) and photon indices (panel (b)); fractional variability amplitude plotted against the corresponding 0.3–10 keV flux (panel (c)). The red and green curves show the log-normal and Gaussian fits to the histograms, respectively.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: WWZ (left column) and LSP (right column) plots in different spectral bands: Panels (a) and (c) are based on the 1 day binned 0.3–10 keV and UVW2 band light curves, respectively; panel (b) is based on 1 week binned 0.3–300 GeV flux values.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption:                         Same as Figure 6 for the LAT-band photon index.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Magnitude–color diagrams for the observations performed with UVOT.
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: Left: exposure map of the XMM-Newton observations around M31. The color denotes the effective exposure time accounting for the vignetting. The pink circles represent observations that are excluded from the data reduction and analysis due to background flaring. Right: the sky coverage of the observations above the given all-EPIC exposure time. The sky coverages of this work, Stiele et al. (2011), and Pietsch et al. (2005a) are shown by the black solid line, the blue dashed line, and the green dotted line, respectively.
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: Mosaicked false-color image of the XMM-Newton observations of M31. We also show three zoom-in ﹩30^{\prime} \times 30^{\prime} ﹩ regions in the center, disk, and halo. The count-rate images are background-subtracted, exposure-corrected, and adaptively smoothed, but not vignetting-corrected. The scale bars of ﹩10^{\prime} =2.2\,\mathrm{kpc}﹩ in the inserted panels are calculated at the distance of M31 (761 kpc). Because the center region is much brighter, we adjust the color scale of the upper left panel to capture more details.
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: a) The fraction of matched sources and matches of shifted X-ray sources as the function of p_any (the probability of matching defined in NWAY) based on the distance. (b) The fraction of the matched sources as the function of the fraction of matches of shifted sources. (c) The estimated number of secure matches as the function of the fraction of false-positive matches. In (b) and (c), we present comparisons of the matching performance between different priors: no prior (distance only), Gmag, F X/G, and F X/G with HR2.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Same as Figure 2, but for SNR G16.0−0.5. Two integrate intensity maps of 12CO (J = 1–0) emission in the upper row are in the velocity ranges of +35 to +50 km s−1 (left) and +60 to +80 km s−1 (right). Locations of broad lines at velocities of +43.7 and +67.9 km s−1 are denoted by tiny stars on the corresponding left and right integrated intensity maps, respectively. Broad lines identified by partial criteria are in pink, those by full criteria are in red, and those by full criteria plus the clean subbackground region condition are in blue. Cyan contours in both integrated intensity maps are at half the column density maximum of shocked molecular gas obtained by Beaumont et al. (2011). The GLEAM 200 MHz radio continuum emission map in power-law scale is superimposed on the upper left corner of the left integrated intensity map, overlaid with the same red dashed circle as in integrated intensity maps. In the index-velocity maps in the bottom row, broad lines identified by full criteria plus the clean subbackground region condition (left), full criteria (middle), and partial criteria (right) are in red.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Distributions of heights from the Galactic plane for SNR–MC associations. Fixed SNR–MC associations in known SNRs except for those within 10° of l ∼ 0° and 5° of l ∼ 180° are shown in the left panel. All fixed and possible SNR–MC associations in all known and candidate SNRs are shown in the right panel. The position of the Galactic midplane is derived from the fixed SNR–MC associations by the least-squares fitting. The height of the Sun above the Galactic midplane is estimated as ∼15.7 pc. The same position of the Galactic midplane is also used to calculate heights of all SNR–MC associations. Black dotted lines indicate fitting results by a Gaussian function in the left panel and by two Gaussian functions in the right panel (separated components shown by red dotted lines). Note that all distances estimated for possible SNR–MC associations are used. However, if we use only the smallest distance for each possible SNR–MC association, the height distribution still has two components.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Radius (left) and progenitor initial mass (right) distributions for SNRs associated with MCs. Fixed SNR–MC associations in known SNRs are in blue except for those within 10° of l ∼ 0° and within 5° of l ∼ 180°. All fixed and possible SNR–MC associations in all known and candidate SNRs are in black. The numbers of fixed SNR–MC associations are multiplied by 4 for better visibility. Radii are mostly estimated based on SNRs’ bright radio continuum shells. The progenitor initial mass is estimated based on its linear relationship with the size of the main-sequence interstellar bubble in a molecular environment reflected by the size of SNRs associated with MCs (see details in Chen et al. 2013). Lognormal fitting results of radius distributions and power-law fitting results of progenitor initial mass distributions are shown as dotted lines. SNR radius distributions peak at ﹩{9.7}_{-2.2}^{+2.8}﹩ and 8.1 ± 0.5 pc, for the fixed and all SNR–MC associations, respectively. Progenitor initial mass distributions have indices of −2.6 ± 0.6 and −2.3 ± 0.1, for the fixed and all SNR–MC associations, respectively.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Maximum spatial correlation coefficients (SCCs) at each velocity channel and 12CO (J = 1–0) intensity maps at the corresponding velocity channel at the SCC peak for SNR HB 3. Dashed and dotted lines in panels in the left column denote 5σ and 3σ levels, respectively. Black circles in panels in the right column indicate the annular template applied in the calculation to obtain the maximum SCC. The red dashed circle is the same as in Figure 3. Upper panels show SCC results considering pixels inside the ring template or within twice the SNR radius, which has a significant peak at ∼−42.2 km s−1. For comparison, the peak of the SCC at ∼−41.6 km s−1 in lower panels, considering pixels inside the ring template or within the SNR radius, is not above 5σ; however, it distinguishes the molecular shell structure around the SNR more precisely.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Radius vs. height from the Galactic plane for fixed (red pluses) and all (blue tiny stars) SNR–MC associations. Fixed SNR–MC associations are selected from known SNRs except for those within 10° of l ∼ 0° and 5° of l ∼ 180°. All SNR–MC associations, including fixed and possible ones, are selected from all known and candidate SNRs. The position of the Galactic plane is the same as that applied in Figure 10. Two histograms respectively show the average radius of corresponding SNR–MC associations, which are binned with the number of sources to be at least 10 and the step of the height to be at least 5 pc.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption:  12CO (J = 1–0) intensity maps of PWN G18.00-0.69, at the +5.4 km s−1 velocity channel (left) and integrated over the velocity range of +54.1 to +69.8 km s−1 (right). Minimum values of 12CO emission intensity shown in colorbars are at 3σ confidence level. Red tiny stars denote locations of broad lines identified by full criteria. Red dashed circles denote the extent of the PWN. Black solid circles delineate the cavity edge (left) and the surrounding shell (right).
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Ratios of SNRs associated with MCs along the Galactic longitude. Each histogram is adaptively binned with the number of corresponding SNRs as sixteen. Black and blue histograms show ratios of all and fixed SNR–MC associations, respectively. Solid lines are for known SNRs, and dotted lines for all known and candidate SNRs. Red dashed line is the ratio of previously detected SNR–MC associations in known SNRs.
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Type distributions of SNRs associated with MCs and all SNRs. For each pair of bars, the left one is for SNRs of certain type, and the right one for all SNRs of certain and possible type. The histogram of possible SNR–MC associations (dark gray) is stacked on top of that of fixed SNR–MC associations (light gray), and they are contained in that of all SNRs (black).
Paper: A Systematic Study of Associations between Supernova Remnants and Molecular Clouds
Authors: Xin Zhou, Yang Su, Ji Yang, Xuepeng Chen, Yan Sun, Zhibo Jiang, Min Wang, Hongchi Wang, Shaobo Zhang, Ye Xu, Qingzeng Yan, Lixia Yuan, Zhiwei Chen, Yiping Ao, Yuehui Ma
Figure caption: Same as Figure 4, but for SNR G16.0−0.5. The red dashed circle in the right panel is the same as in Figure 5. The peak of the SCC at ∼+63.3 km s−1 in upper panels is above 0.5; nevertheless, the peak of the SCC in lower panels at ∼+37.6 km s−1 is not so significant.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: Select NIRCam CMDs of M92, along with HST WFC3/IR (HST-GO-11664) and ACS/WFC (GO-9453, GO-10775, GO-12116, and GO-16298) CMDS. Overplotted are solar-scaled PARSEC stellar models at a fixed age (13 Gyr) over a select range of [Fe/H] values, which have been corrected to match the known α-enhancement of M92 (Mészáros et al. 2020). The SW NIRCam CMD extends from our saturation limit (F090W ∼ 18) to below the lowest-mass star from the standard PARSEC models (M = 0.09 M ⊙) and into the expected hydrogen-burning limit regime (0.078 ≤ M < 0.08 M ⊙). The LW CMDs reach slightly higher limits (M = 0.12 M ⊙). These are among the deepest CMDs of a GC in existence and highlight how JWST will easily enable the study of prominent features for low-mass stars such as the MS kink and lowest-mass stars. The double MS in panel (d) and broadness of the CMDs in panels (b) and (c) are in part due to an 0.1 mag offset in the flux calibrations of LW modules A and B. While the stellar models are in excellent agreement with the more-luminous stellar evolutionary phases (e.g., RGB and MSTO) in the HST CMDs, they are ∼0.05 mag too blue for the lower-mass stars in the SW JWST filters. This offset could be due to the complex atmospheres of low-mass stars or the in-progress nature of the absolute flux calibrations.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: The locations of our M92 and Draco II NIRcam and NIRISS observations (plotted in red) for each ERS target, overplotted on a Pan-STARRS optical image. The orange dotted lines indicate 2 and 5 half-light radii (r h) for M92 and 1 and 2 r h for Draco II. We show additional pointings for each system: (a) M92: select HST optical (green; HST-GO-10775) and IR (pink; HST-GO-11664). (b) Draco II: HST/ACS optical data (HST-GO-14734; PI: Kallivayalil) are shown in green. We opted not to undertake large dithers to fill the NIRCam chip and module gaps, which would have substantially increased the program time while only marginally enhancing our science goals.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: CMDs from all eight NIRCam chips for each of our targets. (a) M92 extends from our bright saturation limit without Frame 0 data (F090W ∼ 18) near the MSTO and reaches just fainter than the hydrogen-burning limit (F090W > 28.2). The inflection point of the MS at F090W ∼ 21 is the MS kink. (b) The CMD of Draco II includes the MS kink at F090W ∼ 23 and reaches the bottom of the stellar sequence provided by the standard PARSEC models (0.09 M ⊙). (c) The CMD of WLM displays a wide variety of stellar sequences that span a range of ages including young stars (e.g., the upper MS and red core helium burning stars), intermediate-age stars (e.g., AGB and RGB stars), and ancient stars that span a wide range of colors and magnitude (e.g., RGB, SGB, MSTO, and lower MS). This CMD of WLM (S/N = 10 at M F090W = +4.6) is the deepest taken for a galaxy outside the immediate vicinity of the MW.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: The locations of our NIRcam and NIRISS observations (plotted in red) for WLM overplotted on a Pan-STARRS optical image. The orange dotted lines indicates 1 r h. An exhaustive, though not complete set of HST observations including HST/WFPC2 UV and optical imaging in blue (HST-GO-11079; Bianchi et al. 2012), HST/WFC3 UVIS UV imaging in purple (HST-GO-15275, PI: Gilbert), HST/ACS and HST/UVIS optical imaging in green (HST-GO-13768, PI: Weisz; Albers et al. 2019), and HST/WFC3 IR imaging in pink (HST-GO-16162, PI: Boyer). We opted not to undertake large dithers to fill the NIRCam chip and module gaps which would have substantially increased the program time while only marginally enhancing our science goals.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: NIRCam color composite of M92. F090W was used as the blue channel, F150W as the green, and a combination of the two LW filters (F277W and F444W) as the red channel. The red and orange boxes highlight the stellar densities at ∼1 r  h  and ∼0.5 r  h . The blue box shows the presence of member stars as well as prominent background galaxies (red and yellow extended sources). The central black bar is the intermodule gap, over which we opted not to dither.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. II. Survey Overview
Authors: Daniel R. Weisz, Kristen B. W. McQuinn, Alessandro Savino, Nitya Kallivayalil, Jay Anderson, Martha L. Boyer, Matteo Correnti, Marla C. Geha, Andrew E. Dolphin, Karin M. Sandstrom, Andrew A. Cole, Benjamin F. Williams, Evan D. Skillman, Roger E. Cohen, Max J. B. Newman, Rachael Beaton, Alessandro Bressan, Alberto Bolatto, Michael Boylan-Kolchin, Alyson M. Brooks, James S. Bullock, Charlie Conroy, M. C. Cooper, Julianne J. Dalcanton, Aaron L. Dotter, Tobias K. Fritz, Christopher T. Garling, Mario Gennaro, Karoline M. Gilbert, Léo Girardi, Benjamin D. Johnson, L. Clifton Johnson, Jason S. Kalirai, Evan N. Kirby, Dustin Lang, Paola Marigo, Hannah Richstein, Edward F. Schlafly, Judy Schmidt, Erik J. Tollerud, Jack T. Warfield, Andrew Wetzel
Figure caption: NIRCam color composite of Draco II. F090W was used as the blue channel, F150W as the green, and a combination of the two LW filters (F360M and F480M) as the red channel. The central black bar is the intermodule gap, over which we opted not to dither. The stellar density of Draco II is so low that background galaxies by far dominate the image. Only software like DOLPHOT is able to locate the faint stars that are members of Draco II.