adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Two sectors of ELEANOR data for TIC 21159577, an EB showcasing an evolving pattern of starspot-induced rotational modulations.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Pronounced apsidal motion exhibited by TIC 189281140 (upper panel) and TIC 470715046 (lower panel).
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Slope (left panel, named C1) and y-intercept (right panel, named C) distribution obtained after the photometric calibration fit for all three photometric bands, specifically g band in green, r band in red and i band in orange. The two values have been provided by the photometric calibration fit, i.e., mATLAS = C1mDECam + C0. On the x-axis the investigated DECam fields are reported labeled as F*, where the asterisk stands for the number of the field, from 1 to 23. The y-axis shows the slope and y-intercept values to which the calibration fit converged. The dashed lines indicate the mean values for each band. In order to make the figure readable, a vertical shift of 0.2 and 1.0, for the slope and y-intercept distributions respectively, has been applied for the r-band and i-band distributions, taking the g-band values as reference. Each panel includes, in the upper left box, the mean values and corresponding uncertainties, calculated as the standard deviation, for each filter.
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Magnitude distributions of the detected sources in the three photometric bands used in this study: g (green), r (red), and i (yellow). The legend in the top-left corner indicates the number of detections per band. The upper-right subpanel shows an enlargement around the histogram peaks, along with linear fits (colored lines) used to estimate the completeness magnitudes. For clarity, the resulting completeness values are listed in Table 3.
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Signal-to-noise ratio (SNR) as a function of magnitude in the g (top), r (middle), and i (bottom) bands. The data are fitted with a decaying exponential function, shown as a yellow line. The adopted SNR threshold (S/N = 5) is marked by the red horizontal dashed line, while the corresponding limiting magnitude is indicated by the green vertical dashed line. Each panel includes an upper-right subpanel that zooms into the region around the limiting magnitude.
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Photometric uncertainties as a function of magnitude in the g, r, and i bands (top to bottom) for all sources in the COSMIC-L catalog. The red horizontal line indicates the mean photometric error in each band. Photometry is based on PSF fitting.
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Spatial distribution of the completeness (left panel) and limiting (right panel) magnitudes across the LMC region, based on the COSMIC-L catalog. The color bars indicate the magnitude values for each of the 23 DECam fields, labeled according to the field-numbering convention (i.e., F1 to F23). See the text for further discussion.
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Chemical composition of the ejecta of a generation of stars in the mass range 9.22−120 M⊙ averaged over a Salpeter IMF compared to the solar composition. The gray band corresponds to a variation by a factor of 2 with respect to ﹩{\rm{Log}}{(}^{16}{\rm{O}}{/}^{16}{{\rm{O}}}_{\odot })﹩. For stars more massive than 15 M⊙ we have used the yields provided by M. Limongi & A. Chieffi (2018) under the assumption that all the stars with initial mass lower than 30 M⊙ eject 0.07 M⊙ of 56Ni while all the more massive ones fully collapse to a black hole and hence contribute to the chemical enrichment only through the mass ejected by stellar wind.
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Bolometric light curves computed assuming the initial energy–initial mass and ejected 56Ni–initial mass relations reported in Table 3. In all these calculations we assume that the 56Ni synthesized during the explosion is mixed from the inner edge of the exploding mantle to about half of the H-rich envelope (M. Limongi & A. Chieffi 2020).
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Comparison between the chemical composition of the ejecta of a generation of massive stars averaged over a Salpeter IMF in the mass interval 9.22−120 M⊙ (〈Yield〉9.22−120) and the one averaged over the same IMF but in the mass range 13−120 M⊙ (〈Yield〉13−120). The gray band corresponds to a variation of a factor of 2.
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Same as Figure 7 but for the 15 M⊙ star.
Paper: SageNet: Fast Neural Network Emulation of the Stiff-amplified Gravitational Waves from Inflation
Authors: Fan Zhang, Yifang Luo, Bohua Li, Ruihan Cao, Wenjin Peng, Joel Meyers, Paul R. Shapiro
Figure caption: Similar to Figure 2, except that the lower left panel displays the variable defined in Equation (A1). The vertical shades in the upper right panel indicate the sensitive frequency band of PTAs and that of Advanced LIGO/Virgo (R. Abbott et al. 2021), respectively. The vertical shades in all other panels indicate the integration time spans of the illustrative modes.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Example 5 × 5 pixel sector-averaged difference images used for photocenter measurements of TESS EB candidates. The red star symbols represent the pixel position of the target star, the open black circles represent the sector-averaged photocenter, and the small red symbols represent nearby field stars that are bright enough to produce the detected eclipses as contamination to the target star. The first three columns from the left (labels (A), (B), and (C)) show difference images that are reasonably well suited for photocenter measurements. The photocenters in the first column (A) indicate that the detected eclipses are on-target, whereas the second (B) and third (C) columns show false positives due to significant photocenter offset. Column (B) highlights the case for a well separated target and contaminator, while the two are within the same pixel in column (C)—and also reside in crowded fields. Column (D) shows difference images that are dominated by systematic effects, thus making them inadequate for reliable photocenter measurements.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: An example issue associated with the automated ephemeris measurements of the TESS FFI ELEANOR lightcurve and difference image for TIC 33521833. The upper panel shows one sector of TESS data with the automatically detected periodic signal highlighted by the green vertical bands. Lower left panel: corresponding phase-folded data from all available sectors. Lower right panel: corresponding difference image and photocenter measurements. Here, the lightcurve is dominated by stellar variability and the automatically measured period is incorrect.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Same as Figure 12 but for TIC 187172446. Here, the lightcurve shows a clear EB signal, the measured period is correct, the difference image is adequate for reliable photocenter analysis, and the measured photocenter offset is ∼0.14 pixels. However, there is a nearby field star, TIC 510123334, that is bright enough to be the source of the eclipses and too close to the target (projected separation of about 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩71) for the photocenter measurements to pinpoint the source of the detected eclipses. Such targets are not included in our catalog.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: An example screenshot highlighting the first question of the EBP workflow. The upper panel in the figure shows one sector of TESS data, highlighting the detected eclipses in green, and listing the measured period. The lower left panel shows the corresponding phase-folded lightcurve, and the lower right panel shows the difference image used for the photocenter measurements. The difference image also shows the pixel position of the target (red star) and the sector-averaged measured photocenter (open black circle). The user decides whether the target shows clearly visible periodic dips (indicating an EB), answers “yes” or “no,” and is then taken to the second question.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Examples of several different types of false positives returned by our neural network shown by TESS Sector 14 lightcurves. The TIC 120693310 lightcurve (upper left) demonstrates scattered light resembling eclipses, a particularly difficult false positive to train against. The TIC 120426180 lightcurve (upper right) shows pulsations with local minima broad enough to be classified an an eclipse. The TIC 26656569 lightcurve (bottom left) shows a clear EB, but this lightcurve is contaminated by the nearby TIC 26656583 (KIC 11560447), which is in the Kepler EB catalog. The TIC 123447105 lightcurve (bottom right) shows a noise pattern with several features that could be mistaken for eclipses.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Left: number of TESS targets exhibiting eclipse-like features from Sectors 1–82 as a function of TESS magnitude. Right: corresponding R.A. vs. decl.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Same as Figure 12 but for TIC 823000. Here, the primary and secondary eclipses have similar depths (130 parts per thousand (ppt) and 120 ppt, respectively) and the automatically measured period is off by a factor of 2.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Distributions of the TESS magnitudes, preliminary measured periods, and respective photocenter offsets for the 60K sample. The lower right panel is a zoomed-in version of the lower left panel, highlighting the distribution of measured photocenters smaller than 2 pixels. See text for details.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: An example screenshot of the workflow and interface of Exogram EB vetting, enabling rapid image classification.
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Left panel: color–magnitude diagram (i vs. g − r) for LMC sources, highlighting the main sequence (left) and the giant branch (right). A dense population with g − r > 1.2 corresponds to foreground K-type and M-type stars in the Milky Way. Right panel: color–color diagram (r − i vs. g − r) for the same sources. Spectral types (O, B, A, F, G, K, M) are labeled along the bottom, while luminosity classes (V, III, I) are shown in orange, green, and fuchsia, respectively. The main sequence is marked by a black line. A total of 18,676,294 sources are included. For details, see Table 2. Both diagrams use 1000-bin 2D histograms, discarding bins with fewer than three sources to reduce noise. The color bars indicate source density per pixel.
Paper: COSMIC-L: A Photometric Catalog of Observed Stars in the Large Magellanic Cloud
Authors: Antonio Franco, Achille A. Nucita, Francesco De Paolis, Francesco Strafella
Figure caption: Distance distribution of the 76,267 stars with g − r > 1.2, identified in Figure 6. Distances are derived from Gaia EDR3, with corrections applied using C. A. L. Bailer-Jones et al. (2021). The Gaia nominal detection limit at ∼2 kpc is marked by the pink vertical line (E. Sánchez 2010), while the extended detection limit adopted in this work is indicated by the red vertical line. Approximately 91% of the sources lie within 5 kpc, confirming their classification as foreground stars in the thin and thick disks of the Milky Way. The top-right inset contains the corresponding legend.
Paper: A White Dwarf Catalog from LAMOST DR11 Using Deep Learning
Authors: Shengwen Zhang, Yanxia Zhang, Chao Liu
Figure caption: Accuracy as a function of SNR for the eight-class classification model.
Paper: A White Dwarf Catalog from LAMOST DR11 Using Deep Learning
Authors: Shengwen Zhang, Yanxia Zhang, Chao Liu
Figure caption: Confusion matrix of the eight-class classification model.
Paper: A White Dwarf Catalog from LAMOST DR11 Using Deep Learning
Authors: Shengwen Zhang, Yanxia Zhang, Chao Liu
Figure caption: Confusion matrix of the two-class classification model.
Paper: A White Dwarf Catalog from LAMOST DR11 Using Deep Learning
Authors: Shengwen Zhang, Yanxia Zhang, Chao Liu
Figure caption: The architecture of the ensemble model.
Paper: A White Dwarf Catalog from LAMOST DR11 Using Deep Learning
Authors: Shengwen Zhang, Yanxia Zhang, Chao Liu
Figure caption: Screening and validation flowchart of white dwarf candidates.
Paper: A White Dwarf Catalog from LAMOST DR11 Using Deep Learning
Authors: Shengwen Zhang, Yanxia Zhang, Chao Liu
Figure caption: Comparison of magnitude and color for both the training (yellow) and predicted (blue) white dwarfs, along with non–white dwarfs (gray).
Paper: Probing Obscured Star Formation in Galaxy Clusters Using JWST Medium-band Images: 3.3 μm PAH Emitter Sample in A2744
Authors: Cheng Cheng, Xin Wang, Piaoran Liang, Fengwu Sun, Edo Ibar, Malte Brinch, Haojing Yan, Jia-Sheng Huang, Jun Li, Juan Molina
Figure caption: magcontinuum − F430M vs. F444W - F430M for the F430M emitters, where magcontinuum = ﹩28.9-2.5\times {\mathrm{log}}\,(0.6\times {f}_{{\rm{F410M}}}+0.4\times {f}_{{\rm{F460M}}})﹩. Since the F444W flux includes the emission lines captured by F430M, and magcontinuum more closely represents the line-free continuum for the F430M emitters, the color F444W − F430M is offset from magcontinuum − F430M for more extreme emitters when F444W − F430M ≳0.4. Therefore, assuming F444W as the continuum of the emission line lowers the significance of emitter selection. We highlight the PAH emitters in this work with red dots, which are closer to the 1:1 line in black. The scatter of the color difference for the PAH emitters is 0.022, which has little effect on PAH emitter selection. The scatter in color difference introduces an uncertainty in PAH flux of approximately ﹩{\rm{\Delta }}{\mathrm{log}}\,({f}_{\mathrm{PAH}})\sim 0.02\mbox{--}0.04﹩, depending on the F444W − F430M color (see Section 4.2).