adsabs/AstroCLIMB huggingface dataset:
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Optical spectra for the two AGN-Gxy pairs ((a) and (b)), one galaxy pair (c), and one pair of sources of unknown type (d). The spectroscopically observed pair of sources are marked with a red and a peach crosshair corresponding to the spectrum (black and peach), or a red and a green crosshair if one of the sources is the CatWISE20 counterpart. See Figure 18 for the symbol key.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption:  NuSTAR   flux distributions in the soft (top), hard (middle), and full (bottom) energy bands for the NSS40 (blue) and NSS80 (green) samples. For each band, the filled histogram shows the flux distribution for sources independently detected in that band (the number of these sources, N det, is indicated in the upper-right corner), and the open histogram shows the distribution of flux upper limits for sources undetected in that band, but independently detected in at least one other band (N undet).
Paper: LADDER: Revisiting the Cosmic Distance Ladder with Deep Learning Approaches and Exploring Its Applications
Authors: Rahul Shah, Soumadeep Saha, Purba Mukherjee, Utpal Garain, Supratik Pal
Figure caption: Testing Pantheon+: relative redshift distribution of the Pantheon and Pantheon+ data sets (left panel); comparison between Pantheon-trained LADDER reconstruction vs. Pantheon+ (right panel).
Paper: LADDER: Revisiting the Cosmic Distance Ladder with Deep Learning Approaches and Exploring Its Applications
Authors: Rahul Shah, Soumadeep Saha, Purba Mukherjee, Utpal Garain, Supratik Pal
Figure caption: Calibration of BAO: colored contours are LADDER predictions; dashed ones correspond to benchmark ΛCDM calibration.
Paper: LADDER: Revisiting the Cosmic Distance Ladder with Deep Learning Approaches and Exploring Its Applications
Authors: Rahul Shah, Soumadeep Saha, Purba Mukherjee, Utpal Garain, Supratik Pal
Figure caption: GRB calibration output and comparisons.
Paper: LADDER: Revisiting the Cosmic Distance Ladder with Deep Learning Approaches and Exploring Its Applications
Authors: Rahul Shah, Soumadeep Saha, Purba Mukherjee, Utpal Garain, Supratik Pal
Figure caption: Cosmological parameter constraints obtained from the Pantheon and Pantheon+ data sets vs. LADDER predictions.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: rms scatter in the light curves as a function of mean magnitude (for stars in the field LMC502.11). Left: OGLE-III data (2001–2009). Right: OGLE-IV data (2010–2020). The black dashed (solid) line marks the lower envelope of the distribution for OGLE-III (OGLE-IV) data. The color scale is logarithmic.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Comparison between the new OGLE-III and OGLE-IV mean magnitudes for one of the analyzed fields (LMC502.11), as a function of color (upper diagram) and mean magnitude (lower diagram). The black data points represent the median difference calculated in several color (magnitude) bins. The error bars are calculated as the median absolute deviation divided by ﹩\sqrt{2}{\mathrm{erf}}^{-1}(\tfrac{1}{2})﹩. The color scale is logarithmic.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Light curves of detected events. The solid blue line shows the best-fit PSPL model (with or without the parallax). For events with detected annual parallax effects, the dotted line shows the best-fit model without the parallax.
Paper: Microlensing Optical Depth and Event Rate toward the Large Magellanic Cloud Based on 20 yr of OGLE Observations
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Mateusz Kapusta, Igor Soszyński, Łukasz Wyrzykowski, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Dorota Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Milena Ratajczak
Figure caption: Dereddened color–magnitude diagram of the field LMC516.14. Blue circles mark the positions of the detected microlensing events in the baseline. Empty circles mark three events that do not enter the final statistical sample.
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Example diagram of triple-mode 2O/1O/F δ Sct stars for r-band LCs (right) and PSDs (left). Top left: PSD of original data with maximum PSD marked in red. Top right: original LC folded by F-mode period (red dots) with the best Fourier fit shown as a green line. Middle left: PSD of residual LC after prewhitening using the period corresponding to the F mode, the maximum PSD marked is in red. Middle right: residual LC folded by 1O-mode period (red dots) with the best Fourier fit shown as a green line. Bottom left: PSD of residual LC after prewhitening using the period corresponding to the 1O mode, the maximum PSD is marked in red. Bottom right: residual LC folded by 2O-mode period (red dots) with the best Fourier fit shown as a green line.
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Example diagram of 1O/F double-mode δ Sct stars for a g-band LC and PSD. Top left: PSD of the original data; the red filled circle shows the maximum PSD. Top right: red dots are the original LC folded by the first period, the green line is the best Fourier fit. Bottom left: PSD of the residual LC after prewhitening; the red filled circle shows the maximum PSD. Bottom right: red dots are the residual LC after prewhitening folded by the second period; the green line is the best Fourier fit to the residual LC.
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Example diagram of quadruple-mode 3O/2O/1O/F δ Sct stars for r-band LCs and PSDs. The left panels show the PSD plots for the corresponding mode period, with the maximum PSD marked in red. The right panels show the LCs folded by the corresponding mode period, with the best Fourier fit line shown in green. The panels correspond to modes 1O, F, 3O, and 2O from top to bottom.
Paper: Multimode δ Sct stars from the Zwicky Transient Facility Survey
Authors: Qi Jia, Xiaodian Chen, Shu Wang, Licai Deng, Yangping Luo, Qingquan Jiang
Figure caption: Other examples of g-band LCs. The left panels are the original LCs folded by P 1, and the right panels are the residual LCs after prewhitening folded by P 2.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Magnitude and color distributions (integrated to unity) of the CatWISE20 (top) and Pan-STARRS (bottom) matched samples from Round #1, which are used to evaluate priors in Round #2 to identify the “best” IR counterpart for each  NuSTAR   serendipitous source. WISE magnitudes are Vega and optical magnitudes are AB. Top left: the W1-magnitude distribution for the best matches vs. all sources (gray shaded area), splitting the former by Galactic latitude; high-Galactic-latitude sources (∣b∣ > 20°) in red and low-Galactic-latitude sources (∣b∣ < 20°) in blue. The black line is a generalized logistic distribution fit to the data of the high-Galactic-latitude sources. The W1 distribution of the low-Galactic-latitude sources follows a similar shape to that of the high-Galactic-latitude sources, with a slightly brighter W1 tail. Top right: the W1 – W2 color distribution following the same color code as in the first panel. Here the WISE color of the high-Galactic-latitude sources, driven by the presence of AGNs, is distinct from the low-Galactic-latitude sources. Moreover, the peak of the distribution is around W1 – W2 ≈ 0.8, which is the Stern et al. (2012) criterion for selecting MIR AGNs. Therefore, the W1 – W2 color distribution can be used as a prior to identifying AGN candidates for optical/IR follow-up spectroscopy. Bottom left: the i-magnitude distribution following the same color code as in the previous panels. The distribution of the low-Galactic-latitude sources follows a similar shape to that of the high-Galactic-latitude sources, peaking at a slightly less bright magnitude. Bottom right: the g–i color distribution following the same color code as in the previous panels.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: A flowchart of the principal adopted optical counterparts to the NSS80 sources. The actions in green represent NSS80 sources with lower-energy X-ray + CatWISE20 counterparts with an optical match within 2.″7 from the WISE position. Optical matches are retrieved from PS1-DR2 (either from our NWAY matching or manually), SDSS, NSC2, DES2, or USNOB1. The purple actions indicate lower-energy X-ray + optical matches which lack a CatWISE20 association. For these sources, we matched the Chandra, XMM-Newton, or Swift-XRT positions (softX ≡ lower-energy X-ray) to the aforementioned optical catalogs using characteristic positional uncertainties of 2.5″, 5″, or 6″, respectively. The blue actions represent NuSTAR-only X-ray + CatWISE20 positions matched to the aforementioned optical surveys (prioritizing NWAY matches where available) using a matching radius of 2.″7; these optical matches are only used for the purposes of spectroscopic follow-up. NSS80 sources that lack any optical association (some of which may be too faint/distant) are indicated with gray actions. In red is shown the contribution of objects with a visually selected optical match—these include, for example, objects where crossmatching limits for other branches are exceeded slightly but on visual inspection a clear match is found. This results in an optical completeness of ∼86% (1098/1274) for the NSS80 catalog: 844/964 lower-energy X-ray and 254/310 NuSTAR-only X-ray associations. This information is available in the NSS80 catalog; see Appendix A.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Example image of the NSS80 survey library. The online library will be accessible at https://www.nustar.caltech.edu/page/59. Left cutout: the 3−24 keV coadded  NuSTAR   image of one of the 894 NSS80 unique fields, Kepler (field ID 413); ﹩{N}_{\exp }=3﹩ individual exposures (each 12’ × 12’) are combined with a total exposure time of ﹩{t}_{\exp }=364.36﹩ ks. For comparison, the NSS40 field ID and total exposure time is recorded in the top-right corner. NSS80 detections are marked with white circles and the corresponding serendip number and NSS40 detections are shown with teal-green diamonds—three additional  NuSTAR   serendipitous sources are detected in the new post-NSS40 data. The science target is marked with a green cross at the center of each field (aim point). Fields which are masked postprocessing due to excess background contamination (e.g., stray light, ghost rays, bright science target) are flagged in the bottom-left corner, and the Galactic latitude of the science target is shown in the bottom-right corner. Right cutout: DSS2 R-band image centered on the  NuSTAR   science target position. The same labeling as on the left is used to indicate NSS40 and NSS80 serendipitous sources. Galactic plane fields with latitudes ∣b∣ < 10° are flagged in the bottom-left corner.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: The positional accuracy of  NuSTAR   as a function of source-detection significance for the 956 NSS80 sources with lower-energy counterparts in pointed archival observations; all matched lower-energy counterparts are plotted. Top: astrometric offsets between the  NuSTAR   source and its matched lower-energy X-ray counterpart coordinates from (a) Chandra/CSC2.0 (circles), (b) XMM-Newton/4XMM-DR10/s (squares and diamonds), and (c) Swift-XRT/2SXPS (stars), color coded by source-detection significance. The negligible mean positional offsets are shown with white markers. Bottom: the radial offset between the  NuSTAR   source and its best lower-energy X-ray counterpart as a function of the minimum source-detection significance (﹩{\rm{\Delta }}{p}_{\mathrm{False},\min }﹩) which increases toward the right (color coded from green to purple). The solid and dashed–dotted black lines indicate the 90% and 68% confidence limits, respectively, on the  NuSTAR   positional uncertainty for bin sizes of ﹩\mathrm{log}({p}_{\mathrm{False},\min })=-10﹩. The number of sources that each bin contains is given above the solid lines. Since the number of sources becomes small toward high ﹩{p}_{\mathrm{False},\min }﹩ values, we only plot bins for ﹩\mathrm{log}({p}_{\mathrm{False},\min })\lt -50﹩.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Flowchart illustrating our NWAY-matching strategy, which we used to identify CatWISE20 and PS1-DR2 counterparts to the NSS80 sources. (a) Round #1 entails the generation of the magnitude and color priors required for Round #2 (magenta outlined box; see Figure 10(b)), by using astrometric information including source positions and their associated uncertainties, and the sky density as a function of magnitude (green outlined boxes) to identify counterparts to the best X-ray position (blue outlined box). Lines are dashed or shown in different colors purely for clarity. (b) Round #2 of NWAY that utilizes the priors (magenta) from the matching to lower-energy X-ray counterparts (blue) with ∣b∣ > 20° in Round #1 and flat priors for sources with ∣b∣ < 20°. All matches with probabilities >10% are stored in the final postprocessed catalog, which includes X-ray information, multiband positions and photometry, and key NWAY information such as the Bayesian match probabilities.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Bottom: Comparison of the 3−8 keV  NuSTAR   and <10 keV X-ray mission fluxes (F soft) for the best Chandra/CSC2.0 (green circles), XMM-Newton/4XMM-DR10/s, (purple squares and diamonds, respectively), or Swift-XRT/2SXPS (blue stars) counterpart matched to the primary NSS80. The different energy bands used to calculate the 3−8 keV fluxes for the CSC2.0 are indicated with different symbols, i.e., 2−7 keV (solid green circles), 0.1−10 keV (white filled, green-edged circles), and 0.5−7 keV (white filled, green-edged stars). Top: distribution of  NuSTAR   to <10 keV X-ray mission fluxes for each instrument. In both panels, the black solid line shows the 1:1 relation, the black dashed–dotted lines show a factor of 3 from this relation, and the red dotted line indicates a factor of 5 below the 1:1 relation. Ten sources have  NuSTAR   3−8 keV flux measurements below the 1:5 relation.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: A histogram of the distribution of match probabilities for the NWAY CatWISE20 (top panel) and Pan-STARRS (bottom panel) candidates before applying the >10% p Cat/PS1,best cut at the end of Round #2, both for NuSTAR-only (open) and improved lower-energy X-ray positions (filled). The high-quality probability cut (p Cat/PS1,best ≥ 0.4) is plotted with a dashed–dotted line. Evidently, in the absence of more reliable lower-energy X-ray positions, NWAY returns low probabilities for the CatWISE20/PS1-DR2 matches. The left panel shows all sources; the middle and right panels show high- and low-Galactic-latitude sources, respectively.
Paper: The NuSTAR Serendipitous Survey: The 80 Month Catalog and Source Properties of the High-energy Emitting Active Galactic Nucleus and Quasar Population
Authors: Claire L. Greenwell, Lizelke Klindt, George B. Lansbury, David J. Rosario, David M. Alexander, James Aird, Daniel Stern, Karl Forster, Michael J. Koss, Franz E. Bauer, Claudio Ricci, John Tomsick, William N. Brandt, Thomas Connor, Peter G. Boorman, Adlyka Annuar, David R. Ballantyne, Chien-Ting Chen, Francesca Civano, Andrea Comastri, Victoria A. Fawcett, Francesca M. Fornasini, Poshak Gandhi, Fiona Harrison, Marianne Heida, Ryan Hickox, Elias S. Kammoun, Lauranne Lanz, Stefano Marchesi, Gaël Noirot, Encarni Romero-Colmenero, Ezequiel Treister, C. Megan Urry, Petri Väisänen, Brian van Soelen
Figure caption: Example DSS R-band cutouts centered on the  NuSTAR   aim point for a given observation (green cross). Sources within the radius of RC3 galaxies (Third Reference Catalog of Bright Galaxies; de Vaucouleurs et al. 1995), Milky Way (Galactic) globular clusters (MWGC), or Abell clusters are flagged as secondary sources and indicated with blue circles. The white circles and the teal-green diamonds mark primary and L17 serendipitous sources, respectively (see Figure 7 for further details).