adsabs/AstroCLIMB huggingface dataset:
Paper: Finding Multiply Lensed and Binary Quasars in the DESI Legacy Imaging Surveys
Authors: C. Dawes, C. Storfer, X. Huang, G. Aldering, Aleksandar Cikota, Arjun Dey, D. J. Schlegel
Figure caption: Each column shows an observed wavelength slice from SNIFS, corresponding to emission features in ascending wavelength, from Lyα to Mg II (see the text). We impose the contour from the Legacy Survey images (set to 80% of the brightest pixel for each image) on each of the slices. For each system, the extent, shape, and orientation of the contour matches the brightest pixels in the SNIFS slices, suggesting the presence of two or more source images. For each of these 11 systems (one per row), these wavelength slices show that there are multiple quasar images at the same redshift. The emission features of the last row do not align with the rest, given its lower redshift. Note the effects of the ADR (see the text).
Paper: Finding Multiply Lensed and Binary Quasars in the DESI Legacy Imaging Surveys
Authors: C. Dawes, C. Storfer, X. Huang, G. Aldering, Aleksandar Cikota, Arjun Dey, D. J. Schlegel
Figure caption: The redshift distributions for the lenses and quasars of our candidate systems. The redshifts of our quasars are from SDSS DR16 and, for 17 additional systems, from the SNIFS instrument on the University of Hawaii 88 inch (2.2 m) telescope. Photometric redshifts for the lenses are from Zhou et al. (2020).
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Variation of the disk fraction as a function of the local EUV (bottom left panel) and FUV fields (top left panel) experienced by the low-mass members. The spatial distribution of the stars falling in each bin is shown in the right panels, with the different colors marking those stars falling in the corresponding bin in the left panels. The stars mark the positions of the O stars.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Spitzer/IRAC [8.0] image of the Cyg OB2 area. The field observed with ACIS-I is marked, as well as the positions of known O stars (filled circles) and B stars (crosses).
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Left panel: maps showing the spatial variation of the disk fraction as in Figure 7. The overplotted contours mark the local stellar surface density. The contour levels are 0.7, 5, 17, 22, and 33 N pc−2. Right panel: disk fraction vs. stellar surface density flux in the bins of the same grid, showing only the values measured in bins with the relative error of the disk fraction smaller than 0.25.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Maps showing the spatial variation of the disk fraction coded with red tones. The values are indicated only in those bins where the relative error of the disk fraction is smaller than 0.25. The overplotted contours mark the 8.0 μm emission.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Left panel: maps showing the spatial variation of the disk fraction as in Figure 7. The overplotted contours mark the local FUV flux. The contour levels are 710.2, 2262.8, 3536.7, 6163.4, 11,087.3, 24,043.4 G0. Right panel: disk fraction vs. FUV flux in the bins of the same grid, showing only the values measured in bins with the relative error of the disk fraction smaller than 0.25.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Spatial distribution of stars with disks (left) and without disks (right), showing the position of the O stars (blue stars) and the 8 μm continuum emission contours in red.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Variation of the disk fraction as a function of the local FUV radiation field obtained in the 5000 simulated 3D configurations of the association. The solid histogram is obtained from the median disk fractions observed in the FUV bins, the dotted histograms are obtained from the 25% and 75% quantiles, and the dashed lines show the minimum and maximum disk fractions observed in each FUV bin.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Each histogram represents the age distribution of the stars falling in the bins in Figure 3. The plot titles show the median age of each distribution.
Paper: Photoevaporation and Close Encounters: How the Environment around Cygnus OB2 Affects the Evolution of Protoplanetary Disks
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, J. F. Albacete-Colombo, C. Clarke, B. Ercolano, E. Flaccomio, V. Kashyap, G. Micela, T. Naylor, N. Schneider, S. Sciortino, J. S. Vink
Figure caption: Simulated 3D stellar spatial distribution of the association.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: (Top two rows) Transient D21-S1 in the D21 (first row) and Dc1 (second row) difference images. The size of the images is labeled. The transient location is marked by the red arrow in each image. It is most prominent in the D21 images and becomes weaker in Dc1 images (but still visible), indicating that it reached maximum in Ep2 and then rapidly declined (disappearing from Ep3 entirely). It is almost invisible in the difference images in the SW bands. (Bottom row) Photometric information of this transient, similar to those presented in Figure 3 but without the light curves in SW as it was not seen in these blue bands. The photometry in Ep2 and Ec is based on the D21 and Dc1 difference images, i.e., it assumes the object was invisible in Ep1.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: (Top row) Color images of SN01 in four epochs. Scale and orientation are labeled. The position of the SN is indicated by the red arrow in each image. The nearby irregular galaxy, which is at z = 2.205, is presumably the host. (middle two rows) D21 and D23 (negative) difference images. The location of the source is indicated by the red circle (0.″5 radius) in each image. The change in color from blue to green/yellow is obvious in the D21 images, where its location shows negative signals in the three bluest bands and positive signals in the rest. It largely maintained the same color from Ep2 through Ep3 (although becoming dimmer) as seen in the D23 images. (Bottom row) SED evolution over four epochs (left panel) and the light curves in the SW bands (middle) and the LW bands (right). In Ep1, this transient was invisible in the three reddest bands, and the downward arrows in its Ep1 SED indicate the 5σ upper limits (calculated on the rms maps within a 0.″165 radius circular aperture to best match the size within which the PSF fitting was done; see the Appendix). In F200W and the redder bands, the transient reached the maximum in Ep2 and then gradually faded.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: (Top) Transient D31-S4 in the D31 (negative) difference images. The size of the images is labeled. The transient location is marked by the green arrow in each image. It was only seen in the difference images involving Ep3, indicating that it appeared only in that epoch. (Bottom) SED of this transient in Ep3 as measured on the D31 difference images.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: Locations of the transients found in the Spock region. The upper panel shows the color images of this region in the four epochs, while the lower panels show the inverted F356W difference images of the same region. All images are 5″ on a side and are oriented north-up and east-left.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: Mothra transient identified in an unnamed arc. The top row shows the color images (4.″8 on a side) of this region in four epochs. The red arrow in each image points to the knot that gave rise to the event. The second row zooms into the arc and shows the Ep1 images (1.″2 on a side) in the eight bands. The next three rows show the difference images between other epochs and Ep1, all displayed in negative. The last row shows the photometric information. See Section 3.2.3 and the Appendix for details of the photometry.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: (Top row) Color images of SN02 in four epochs. Scale and orientation are labeled. The two red bars in each of the color images indicate SN02's location. It was not visible in Ep1. The host redshift is z = 0.7093. (Middle two rows) D21 and D23 (negative) difference images. The location of the source is indicated by the red circle (0.″5 radius) in each image. From the difference images involving Ep2, it seems that this transient reached the maximum in Ep2 and then faded. (Bottom row) SED evolution over four epochs (left panel) and the light curves in the SW bands (middle) and the LW bands (right).
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: (Top three rows) Transient D21-S2 in the D23 (first row), D2c (second row), and D31 (third row) difference images (negative). The size of the images is labeled. The location of the transient is marked by the red arrow in each image. It is visible in the difference images involving Ep2 but not otherwise, indicating that the event was caught only in Ep2. (Bottom row) SED of the transient in Ep2 as measured from the D23 images.
Paper: JWST's PEARLS: Transients in the MACS J0416.1−2403 Field
Authors: Haojing Yan, Zhiyuan Ma, Bangzheng Sun, Lifan Wang, Patrick Kelly, José M. Diego, Seth H. Cohen, Rogier A. Windhorst, Rolf A. Jansen, Norman A. Grogin, John F. Beacom, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Dan Coe, Madeline A. Marshall, Anton Koekemoer, Christopher N. A. Willmer, Aaron Robotham, Jordan C. J. D'Silva, Jake Summers, Mario Nonino, Nor Pirzkal, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Rachana A. Bhatawdekar, Cheng Cheng, Adi Zitrin, S. P. Willner
Figure caption: Transient D23-S3 in the D23 (first row) and D21 difference images. The images have the same size as labeled. The transient location is marked by the red arrow in each image. This transient, however, is the most complicated of all, and the difference images of different epoch pairs reveal some inconsistencies. See text for details.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Source detection probability as a function of the number of source counts, calculated from the results of a large suite of MARX simulations. All sources were positioned at an off-axis angle of ﹩{6}^{{\prime} }﹩ and detected using CIAO WAVDETECT at a threshold of 10−5. The circles show the results of the source detection simulations, which were performed for various source count intensity levels, while the lines show best-fitting detection curves of the form ﹩P=1-\exp \left[\tfrac{-{C}^{{\lambda }_{1}}}{{10}^{{\lambda }_{2}}}\right]﹩ (Equation (1)), where the constants λ 1 and λ 2 are provided in Table 1. Each color represents a different background level, which are (from left to right) 0.00072, 0.0014, 0.0030, 0.0060, 0.012, 0.024, 0.048, 0.096, 0.192, 0.384, and 0.768 counts pixel−1.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Broadband background maps for ObsID 4511 from the Chandra Cygnus OB2 Legacy Survey produced by subtracting all detected sources using WAVDETECT (left) and extracted from the properties of the source catalog following our method (right). The color scale is the same in both images and uses a logarithmic scaling that ranges from 7 × 10−4 counts s−1 arcmin−2 (white) to 7 × 10−2 counts s−1 arcmin−2 (black). Differences between the two images are due to the differences between WAVDETECT's and AE's methods for extracting the local background, correcting for emission from the PSF wings of nearby bright stars (see the better backgrounds method employed by AE; Broos et al. 2012), and calculating reliable background estimates.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Broadband background map for the Chandra Cygnus OB2 Legacy Survey extracted from the properties of the source catalog. The background shown is equivalent to C  b (A  s /A  b ), or the background count rate per source PSF (see text for more information). For sources observed in multiple ObsIDs we show the lowest background level of all observations for illustrative purposes. The resulting background map shows the tiling strategy adopted by the survey, which leads to a low background level over a large area.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Image showing the arrangement of simulated sources on CCD3 of Chandra's ACIS detector. The sources are arranged in groups at off-axis angles of ﹩{0}^{{\prime} }﹩ (six sources in the lower left corner at Chandra's aim point), ﹩{2}^{{\prime} }﹩, ﹩{4}^{{\prime} }﹩, ﹩{6}^{{\prime} }﹩, ﹩{8}^{{\prime} }﹩ (10 sources at each off-axis angle arranged in concentric circles), and ﹩{10}^{{\prime} }﹩ (three sources in the upper right corner). X-ray events (photons) are shown in black, and the detected sources (for this example simulation, for which all sources were detected) are marked using green ellipses that illustrate the size enclosing 99.7% (at 1.49 keV) of Chandra's PSF at each off-axis angle.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Survey completeness as a function of stellar mass for sources across the Chandra Cygnus OB2 Legacy Survey area. All sources were modeled at a distance to Cyg OB2 of 1.4 kpc, with sources verification assessed in all three energy bands. The black line shows the completeness over the entire 1 deg2 area, while the red line shows the completeness in the deep 0.5 deg2 area. The black dashed line shows the completeness of our observations over the entire survey area assuming that the sources are not randomly distributed but are clustered in the same way as that of the massive stars in Cyg OB2.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Survey completeness as a function of stellar X-ray luminosity for sources across the Chandra Cygnus OB2 Legacy Survey area. All sources were modeled at a distance to Cyg OB2 of 1.4 kpc, with source verification assessed in all three energy bands. The black line shows the completeness over the entire 1 deg2 area, while the red line shows the completeness in the inner 120 ks deep 0.5 deg2 area.
Paper: Simulating the Sensitivity to Stellar Point Sources of Chandra X-Ray Observations
Authors: Nicholas J. Wright, Jeremy J. Drake, Mario G. Guarcello, Vinay L. Kashyap, Andreas Zezas
Figure caption: Survey completeness as a function of the X-ray source count rate in the broad (0.5–7 keV; black), soft (0.5–2 keV; red), and hard (2–7 keV; blue) bands. The solid lines show the completeness over the entire 1 deg2 area, while the dashed lines show the completeness in the inner 120 ks deep 0.5 deg2 area.
Paper: PEARLS: Near-infrared Photometry in the JWST North Ecliptic Pole Time Domain Field 
Authors: Christopher N. A. Willmer, Chun Ly, Satoshi Kikuta, S. A. Kattner, Rolf A. Jansen, Seth H. Cohen, Rogier A. Windhorst, Ian Smail, Scott Tompkins, John F. Beacom, Cheng Cheng, Christopher J. Conselice, Brenda L. Frye, Anton M. Koekemoer, Nimish Hathi, Minhee Hyun, Myungshin Im, S. P. Willner, X. Zhao, Walter A. Brisken, F. Civano, William Cotton, Günther Hasinger, W. Peter Maksym, Marcia J. Rieke, Norman A. Grogin
Figure caption: Distribution of the seeing FWHM in arcseconds measured for sources classified as stars in each individual image. The left panel shows the distributions for Y, J, and H, and the right panel the distributions for the low- and high-gain K 2.68 and K 0.95 short K filters and K spec, as indicated in the key. The median seeing values for the different configurations are (Y, J, H, K 0.95 , K 2.68 , K spec) = (0.″90, 0.″96, 0.″85, 0.″80, 1.″06, 0.″86). The distribution of K 2.68 values reflects the variation of sky conditions over the several nights the data were collected. When making mosaics for the whole field, a maximum seeing cut at 2.″1 was adopted as a compromise between attaining depth and maintaining resolution; this cut mainly affects the K 2.68 measurements.
Paper: PEARLS: Near-infrared Photometry in the JWST North Ecliptic Pole Time Domain Field 
Authors: Christopher N. A. Willmer, Chun Ly, Satoshi Kikuta, S. A. Kattner, Rolf A. Jansen, Seth H. Cohen, Rogier A. Windhorst, Ian Smail, Scott Tompkins, John F. Beacom, Cheng Cheng, Christopher J. Conselice, Brenda L. Frye, Anton M. Koekemoer, Nimish Hathi, Minhee Hyun, Myungshin Im, S. P. Willner, X. Zhao, Walter A. Brisken, F. Civano, William Cotton, Günther Hasinger, W. Peter Maksym, Marcia J. Rieke, Norman A. Grogin
Figure caption: Color–color plot of sources matching the PEARLS HSC-MMIRS with a preliminary JWST-TDF catalog measured from the first two NEP TDF spokes. The magnitudes of the latter were measured using SExtractor with a fixed aperture determined from the F444W filter. The 174 plotted NIR sources have no HSC counterparts, and the key identifies the different characteristics, i.e., sources that have at least one NIR measurement (gray dots; sources with measurements in all NIR filters (blue upward-pointing triangles); sources with measurements in H and K (orange downward-pointing triangles) and only in K (red circles). The five galaxies that match SCUBA2 sources are noted by open black squares, and the 28 MMIRS-detected galaxies with no HEROES counterparts are represented by green open diamonds.