adsabs/AstroCLIMB huggingface dataset:
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 dispersion of measured background fluxes using 100,000 random apertures of 12.5 pixels (2.″1) calculated for the final science-grade mosaics in K 2.68 (orange), K 0.95 (green), and K spec (gray). The numbers of apertures contributing to the histogram for each filter are proportional to the areas with exposure times greater than 600 s; these comprise 78%, 53%, and 31% of the random variates for K 2.68, K 0.95, and K spec, respectively. The higher noise level for the K 0.95 is immediately apparent; the different peaks are associated with the large contiguous regions of the mosaics with very similar exposure times. Shorter exposures shift the peaks toward higher noise values, as expected; the peaks seen for K 2.68 (from left to right) correspond to total exposures ∼9100 s, 8600 s, and 3800 s, while for K 0.95 the peaks correspond to ∼4000 s and 1000 s, and for K spec the counts peak at ∼6000 s.
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: Footprint of the imaging for different MMIRS filters in the NEP TDF using a ∼23.′9 × 22.′6 Subaru HSC g, i2, z color composite as backdrop, with north up and east to the left, and with the grid showing coordinates in sexagesimal units. The NEP TDF is centered at (R.A., decl.)J 2000 = (17:22:47.896, +65:49:21.54). The white solid line outlines the Y imaging, the green dashed line outlines J, the thick blue dashed–dotted line H, and the orange dots K. Most outlines overlap each other, with the exception of J. The K outline combines observations taken with the (short) K and K spec filters; the latter occupy the SE corner quadrant. The figure also includes the outline of the completed JWST/NIRCam observations as a thin red solid line. When the MMIRS observations were initiated, a preliminary NEP TDF pointing and set of NIRCam position angles were used. The NIRCam observations as executed use a field center offset to the W, such that the full NEP TDF is covered with MMIRS only in J.
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 in R.A. and decl. of sources in the regions where the three modes of K-band imaging overlap. Pink circles show sources in common between all modalities (K 2.68, K 0.95, and K spec). Blue points represent sources with K 2.68 and K 0.95 imaging; green points are sources with K 0.95 and K spec. Sources detected in K spec and K 0.95 only are represented by black “+” and green “x” symbols, respectively. Gray diamonds represent sources with K spec and 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: Comparisons between photometric measurements of sources for the different K-band filters and gain values. The full sample of galaxies, with no magnitude cut, is plotted as black diamonds; green dots represent sources that remain after a 3.5σ cut. The orange diamonds represent the subsample of galaxies after the magnitude cuts, and black plusses the same sample after a 3.5σ cut. The dashed lines represent the mean calculated using the resistant_mean procedure in IDL, and the horizontal dotted–dashed lines the ±1σ range for the full sample (green) and the magnitude-limited one (blue). The vertical dashed lines represent the bright and faint magnitude limits used to calculate the average offsets.
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: Completeness levels for the individual bands and for the combined K + K spec mosaic (g) for point sources (orange points and lines) and for n = 1 Sérsic profiles (blue). The vertical lines indicate (from left to right) the 95%, 80%, and 50% completeness levels.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Distribution of source models as a function of HSC r magnitude in T1. Sources are more resolved at brighter magnitudes. The unresolved PointSource model and barely resolved SimpleGalaxy model dominate fainter magnitudes of r ≳ 24. The resolved ExpGalaxy and DevGalaxy models dominate brighter magnitudes of 20 ≲ r ≲ 24. The most complex CompositeGalaxy model is mostly found at r ≲ 22.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Demonstration of model fitting and forced photometry by The Farmer. A blob containing a pair of neighboring sources separated by ∼1″ is shown. The image, model, and residual maps are shown from left to right. The HSC r, NEWFIRM K  s , and IRAC [3.6] bands are shown from top to bottom. For reference, 2″ diameter apertures centered at the source positions are shown in red. The sources are modeled simultaneously using the rizK  s  bands. Forced photometry is performed on all of the bands by fixing the source profiles convolved with the PSF of each band and only allowing the flux normalizations to vary.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: SHELA DECam ugrizY weight maps demonstrating the survey’s footprint and relative depths. The field is covered by eight DECam pointings and divided into seven tiles of 1.°98 × 2.°145, labeled T1–T7, so that the tiles are roughly square. Our survey combines ugriz images from our observations with grizY archival images released prior to 2021 March 3. We note that T1 has substantially deeper Y-band imaging due to a large number of repeated exposures in the archive.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Left: difference between the u-band instrumental DECam magnitude and the SDSS reference magnitudes for the F0 stars in T1. Right: u-band instrumental DECam magnitude vs. SDSS reference magnitudes. We apply the expected magnitude offset calculated from the filter transmission curves of the DECam and SDSS filters, as well as a −0.04 mag correction to align with the AB magnitudes. See the main text for a detailed discussion.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Exposure map of the IRAC imaging overlaid with the coverage of data from all of the surveys used in this catalog. The area included this catalog is defined by the coverage of our own DECam program, which is completely filled by the HSC grz bands and VICS82 imaging.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Relative transmission curves for the photometric bands used. The effects of the filter, atmosphere, detector, and optics are included.
Paper: Testing Modules for Experiments in Stellar Astrophysics (MESA)
Authors: William M. Wolf, Josiah Schwab, R. Farmer, Evan B. Bauer
Figure caption: An example of the test case commit view showing that the failing instances are coming from a single computer, along with links to view the logs of those instances (see Section 2.3.5). The “+” icons indicate submissions where optional inlists were run. In this example, we can see that enabling optional inlists revealed a regression in this test.
Paper: Testing Modules for Experiments in Stellar Astrophysics (MESA)
Authors: William M. Wolf, Josiah Schwab, R. Farmer, Evan B. Bauer
Figure caption: An example of the test case history view showing all submissions from the computer ScienceFurnace for the test case cburn_inward over a range of dates for all commits on the remove-deltaQ-Vs branch.
Paper: Testing Modules for Experiments in Stellar Astrophysics (MESA)
Authors: William M. Wolf, Josiah Schwab, R. Farmer, Evan B. Bauer
Figure caption: An example of an automatic daily summary e-mail developers receive from the TestHub.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: The overall structure of the detection model for solar radio burst spectrograms comprises MobileViT and SSDLite. MobileViT is the feature extractor, while SSDLite includes a neck network and detection head. Extra layers (convolutional feature layers) are added after the truncated MobileViT network to form the neck network. Figure 6 shows the details of the SSDLite structure. DSC consists of depth and pointwise convolutions. MV2 denotes the MobileNetv2 block (inverted residual structure), which performs downsampling when s = 2.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: SSDLite model structure (includes a neck network and detection head). Unlike the depiction in Figure 3, in the original SSDLite model, the extra layers are added after the truncated MobileNetV2 network to form the neck network, which produces multiscale feature maps. The detection head is responsible for classification and bounding box regression, and postprocessing with nonmaximum suppression is applied to produce the final predictions.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Data enhancement processing of the solar radio spectrogram.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Structure diagram of the MobileViTBlock module. The transformer (×L) represents the stacking of L transformer structures, where L is specified by the number in the MobileViTBlock box in Figure 3. X is the input tensor, and the output feature tensor Y is obtained by fusing the local and global representations with X through feature concatenation and convolution.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Schematic diagram of CIoULoss. In (a), DIoULoss considers the IoU and center point distance, and CIoULoss introduces the aspect ratio factor (b) on the basis of DIoULoss.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Solar radio burst spectrograms. Three example images are provided for each burst type. The x-axis of the image is the time axis (the recorded time length is 15 minutes because a FITS source file contains 15 minute records), and the y-axis is the frequency axis.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Global information of MobileViT.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Training loss and AP50 change curves.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: Consistency between ﹩{V}_{\mathrm{LSR},\mathrm{HCN}}﹩ and V LSR,thin. Red: red-profile spectral lines; blue: blue-profile spectral lines; black: no clear line profiles. The error bars in two directions are given by spectral line-fitting errors.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: Distribution of HCN core volume density. A total of 86.4% of HCN cores have a volume density within the range of 105 to 106 cm−3.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: (a) No data augmentation leads to poor accuracy; (b) data augmentation with RandomFlip brings more accuracy.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Comparison of GradCAM++ heat maps of solar radio burst spectrum detection images.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Error detection examples that contain noise as solar radio bursts.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Correct prediction of the model for incorrect labeling.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Solar radio burst detection results of type II, III, IIIs, IV, and V.
Paper: Solar Radio Burst Detection Based on the MobileViT-SSDLite Lightweight Model
Authors: Hailan He, Guowu Yuan, Hao Zhou, Chengming Tan, Shaojie Guo
Figure caption: Comparison of localization loss functions.
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: Magnitude distributions in the OSIRIS r (left panel) and UKIDSS J (right panel) bands for the entire OIR catalog (solid histogram), the nearby sources (dotted histogram), and the expected correlated distributions (dashed histograms) using Equation (3) (SM method).
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 EUV flux. The contour levels are 2.3 × 1010, 6.2 × 1010, 9.3 × 1010, 1.6 × 1011, 3.1 × 1011, 7.7 × 1011 photons cm−2 s−1. Right panel: disk fraction vs. EUV 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 variation of the disk fraction overplotted with contours marking the expected mass-loss rate due to the photoevaporation externally induced by EUV photons. The label shows the corresponding values of ﹩\mathrm{log}\left(\dot{M}\right)﹩ in units of M ⊙ yr−1. The disk fraction values are indicated only in those bins with good statistics.
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: Disk fraction vs. FUV flux as observed in NGC 6611.
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: Distributions of local stellar density around the simulated 3D members’ positions obtained averaging the 5000 simulations described in Section 3.1.
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: Correlation between the disk fraction and stellar surface density in the bins of the grid used in Figure 7.
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: Number of real (solid line) and spurious (dashed line) matches obtained with increasing the reliability threshold in the SM method. The numbers over the solid line show how the fraction of spurious matches decreases with increasing the threshold.
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: Disk fraction vs. distance of the low-mass members from the closest O star.
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: The r vs. r − i diagrams, with all the sources with good optical photometry marked with gray dots, the isochrones with age <10  Myr, and the ZAMS plotted using the distance and extinction as in Guarcello et al. (2012). The reddening vector and the masses corresponding to the 3.5 Myr isochrone are also shown. Different symbols and colors mark the X-ray sources matched with just one method.
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: NIR color–color diagrams with all the sources with good photometry in the involved colors (gray dots) and the “most reliable” counterparts of X-ray sources (black dots). The loci shown in the diagrams distinguish the typical colors expected from giants and normal stars at various extinctions, disk-bearing stars, and background galaxies. In the right panel, giants can be found across the entire diagram, except for the locus marked with “No giants.”
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: The r vs. r − i diagrams, with all the X-ray sources with a “reliable” OIR counterpart with good optical photometry marked with gray dots, and with the Cyg OB2 members with circumstellar disks marked with black dots. The isochrones, reddening vector, and masses are plotted as in Figure 4.
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: Optical color–color diagrams with all the sources with good photometry in the involved colors (gray dots) and the “most reliable” counterparts of X-ray sources (black dots). In the r − i vs. i − z diagram the solid lines are 3.5  Myr isochrones with A  V  = 2.6 and A  V  = 5.6; in the ﹩{r}^{{\prime} }-{\rm{H}}\alpha ﹩ vs. ﹩{r}^{{\prime} }-{i}^{{\prime} }﹩ diagram the solid lines are ZAMS with increasing E  B−V  from 0 to 4.
Paper: Optical and Infrared Counterparts of the X-Ray Sources Detected in the Chandra Cygnus OB2 Legacy Survey
Authors: M. G. Guarcello, J. J. Drake, N. J. Wright, T. Naylor, E. Flaccomio, V. L. Kashyap, D. García-Alvarez
Figure caption: Spatial distribution of the X-ray sources without OIR counterparts, with the emission contours at 8.0 μm overplotted.