adsabs/AstroCLIMB huggingface dataset:
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: Comparison between the star-forming galaxy sample in T. D. Rawle et al. (2014) and the 3.3 μm PAH sample in this work. The SFR of the y-axis is estimated from GALEX UV flux (blue) and UV+IR flux (red), where the IR flux is measured from MIPS or Herschel, which is roughly the total flux. As shown in Figure 8, the SFR from UV+IR is consistent with the SFR3.3μm PAH. We also denote the SFR of the targets that are only detected in T. D. Rawle et al. (2014) or in F430M by a horizontal or vertical black bar in the y- or x-axis. The two star-forming galaxy samples are highly consistent with each other at SFR >10M⊙ yr−1. The two targets missed by our F430M method are GLX001421-302209 and HLS001414-302240, which are classified as further spiral and red-core spiral in T. D. Rawle et al. (2014). The SEDs of the two targets do not show excess in F430M.
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: F460M − F430M vs. F444W − F430M for the F430M emitters. The solid line shows the 1:1 trace. We highlight the 3.3 μm PAH emitter by red dots as in Figure 15. The offset is caused by the intrinsic color between F444W and F460M, which suggests the continuum for the 3.3 μm PAH emission should cover the wavelength blue and redder than F430M. The scatter of the color difference between F460M − F430M and F444W − F430M is 0.069, which will affect the accuracy of the PAH flux by 0.1 dex, and still not affect the selection and SFR estimation.
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: Stellar mass and the observed Ks and 4.5 μm bands for the galaxies at 0.2 < z < 0.4 from the CANDELS catalog. The strong correlation indicates that the flux cut in the NIR flux-limited sample is also a stellar-mass-limited sample.
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: Comparison between the SFR derived from Herschel data (SFRHerschel adopted from T. D. Rawle et al. 2016) and from the SED fitting (SFRMAGPHYS). The target with the highest SFRMAGPHYS is ID 1191, which includes an AGN in the center and biases the SFR from SED fitting.
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: The SFR from the SED fitting would be affected by the uncertainty of the SFH. We compare the SFR from Bagpipes with a double power-law SFH and the nonparametric SFH, and find a consistent trend between the two SFRSED.
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: The distributions of integrated H I flux and H I mass for the dark galaxy candidates, luminous galaxies, and H I clouds, as a function of redshift. The dashed lines in the first and second panels represent SNR = 5, assuming W50 = 100 km s−1 and median rms (i.e., σrms = 2.34 mJy) of the ALFALFA spectra.
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: Selection criterion for the H I clouds based on minimum projected distance. The colored dots represent ALFALFA sources without optical counterparts, whereas black dots (i.e., Luminous) represent ALFALFA high-quality detections with optical counterparts. Blue dots represent H I clouds from the literature (step1) and red dots represent the remaining H I sources without optical counterparts. The black dashed line denotes dmin = 0.075 Mpc, and the blue dashed line denotes the Arecibo 3′ beam size as a function of redshift.
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: The sky coverage for the computation of local density. The green region represents the SDSS DR7 main survey area, while the black region represents the area covered by the ALFALFA sources. The red dots are the dark galaxy candidates within the SDSS DR7 main survey area.
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: The likelihood ratio distributions for dark galaxy candidates (red) and luminous galaxies (black).
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: The internal properties and local environments of the ALFALFA galaxies (top) and the TNG50 simulation (bottom). The black, red, and blue symbols represent the luminous galaxies, dark galaxy candidates and H I clouds, respectively. Left: H I and dynamical (total) mass distribution of the ALFALFA (TNG50) galaxies. Right: the local density and dynamical (total) mass distribution of the ALFALFA (TNG50) galaxies. The p-values from the Kolmogorov–Smirnov test are shown in each histogram panel, indicating the statistical significance of the differences between the distributions of dark galaxy candidates and other samples.
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: The distributions of H I-to-dynamical mass ratio and local density for the dark galaxy candidates and the comparison samples. In both panels, the red lines represent the dark galaxy candidates. In the left panel, the black histogram represents the mass controlled luminous galaxies in the ALFALFA sample. In the right panel, the black and green histograms represent luminous galaxies from the ALFALFA sample and SDSS DR7 galaxies, respectively; their mass and redshift distributions are matched to those of the dark galaxy candidates.
Paper: Searching for Dark Galaxies with H I Detection from the Arecibo Legacy Fast ALFA (ALFALFA) Survey
Authors: Minseong Kwon, Ho Seong Hwang, Brian R. Kent, Ilsang Yoon, Gain Lee, Hyein Yoon
Figure caption: (Left) Median-stacked r-band image of the dark galaxy candidates, smoothed with a Gaussian kernel of σ = 5″. The red solid and dashed circles represent radii of ﹩1.^{\prime} {5}^{}﹩ and ﹩0.^{\prime} 5﹩, respectively. (Right) Magnitude distribution of the median-stacked image, measured at random positions using a circular aperture with a radius of 30″. The red arrow indicates the magnitude at the center.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Comparison of the renormalized χ2 differences between single- and binary-star models for three different mock data sets: (a) mock WD–MS binary, (b) mock MS single, and (c) mock WD single. The x-axis represents the normalized difference in χ2 values, ((﹩{\chi }_{\rm{single}\,}^{2}-{\chi }_{\,\rm{WDMS}}^{2})﹩/﹩{\chi }_{\,\rm{single}\,}^{2}﹩), and the y-axis shows the number of occurrences on a logarithmic scale. The histograms are color-coded by S/N values of 5, 10, 20, 50, and 100. The percentage accuracy of correctly identifying the better fit (single or binary) is indicated in the legend for each S/N value. Vertical dashed lines at x = 0 separate regions where single or binary models provide a better fit.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Left: CMD showing the density distribution of stars of selected Gaia data, with absolute G-band magnitude (MG) plotted against Bp – Rp color (B – R). Middle: extinction-corrected CMD for the stars displayed in the left panel, accounting for interstellar reddening. Right: the CMD showing the distribution of stars in our sample within ∼300 pc that passed our initial cleaning for training the spectral emulator. The blue dotted line represents a PARSEC isochrone for [M/H] = 0.5, which serves as an upper boundary for selecting single MS stars. The blue dashed line is a hard cut to select WD stars.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Demonstration of our NN spectral emulators for WDs (top panels) and MS stars (bottom panels). Each panel shows the predicted XP spectra with different stellar parameters, where the x-axis is the wavelength and the y-axis is the logarithmic flux (10−20 W m−2 nm) normalized to 10 pc. Left panels: spectra at fixed absolute G magnitude (MG) with different B – R color. Right panels: spectra at fixed B – R color with varying MG.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Projections of the GPC predictions on single stars and WD–MS binary systems using two example features: g – r vs. r – i (top) and v – g vs. r – i (bottom). Blue circles represent single stars, while red crosses indicate binary systems. The background contours show the predicted probability of being a binary system from the trained GPC model, ranging from 0 (blue) to 1 (red).
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: Transmission curves of JWST/NIRCam filters F410M (green), F430M (blue), F460M (red), F480M (orange), and F444W (purple), overlaid with the NIRSpec spectrum of one PAH emitter in A2744 (ID: 15548 in B. Vulcani et al. 2025) at redshift z = 0.3068 (PI: M. Castellano, GO-3073). Open circles indicate the observed flux of the spectrum through each filter. The F430M filter (blue) is uniquely positioned to encapsulate the redshifted 3.3 μm PAH emission (dashed line at 4.3 μm), while the adjacent filters (F410M, F460M, F480M) sample the stellar continuum. The F444W filter has the most overlap in imaging coverage with F430M, making F430M and F444W the chosen bands for selecting sources based on PAH emission and continuum. This target is the ID 5565 in this work.
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: Stamp images of the 3.3 μm PAH bright targets (6″ × 6″). We show the F444W, F430M, and the PAH 3.3 μm images (=F430M − F444W) of each target. The IDs are denoted in the left corner. The orange line in the PAH images show the projected direction to the cluster center (R.A. = 00:14:20.7022; decl. = −30:24:00.6264, X. Wang et al. 2015; G. Mahler et al. 2018; P. Bergamini et al. 2023). The clear detection in PAH images confirms our selection method. PAH images reveal complex morphologies, including disklike, clumpy, or compact structures. Additionally, some exhibit asymmetric features, suggesting the influence of ram pressure.
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: Upper panel: F430M − F444W color vs. F430M ISO mag of the F430M selected sample. The blue line marks the 3σ detection limit of the color excess. The 3σ excess F430M emitters are highlighted with red plus signs. Lower panel: photometric redshift distribution of the F430M emitters. The photometric redshifts are separated into several redshift bins, corresponding to several emission lines that shift to the F430M filter. The brightest targets are mainly the 3.3 μm PAH emitters. We highlight the PAH targets studied in this work with red crosses.
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: The Bagpipes SED fitting results for the PAH emitter sample. The orange curves represent the model spectra, and the blue dots show the photometric data points from the SED released by UNCOVER (J. R. Weaver et al. 2024). The blue end of ID 1191 is not well fitted due to the central AGN contribution (M. S. Owers et al. 2012). A more detailed SED analysis of this target is presented by P. J. Watson et al. (2024).
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: Comparison of SFR3.3μm PAH with SFRSED estimates from SED fitting using Bagpipes and MAGPHYS. Red points indicate SFR﹩{}_{{\rm{SED}}}^{{\rm{Bagpipes}}}﹩, derived from optical-to-NIR SED fitting, which primarily traces star formation from the stellar population. Blue open circles represent SFR﹩{}_{\mathrm{SED}}^{\mathrm{MAGPHYS}}﹩ of the seven Herschel-detected PAH emitters. SFR﹩{}_{\mathrm{SED}}^{\mathrm{MAGPHYS}}﹩ values are obtained from optical-to-FIR SED fitting by MAGPHYS, incorporating dust emission and thus providing a more complete measure of total star formation. The solid black line denotes the 1:1 relation, with dashed black lines indicating a ±0.5 dex range. For the seven Herschel bright targets, SFR﹩{}_{\mathrm{SED}}^{\mathrm{MAGPHYS}}﹩ systematically exceeds SFR﹩{}_{{\rm{SED}}}^{{\rm{Bagpipes}}}﹩ and is in better agreement with SFR3.3μm PAH (blue circles). The blue dashed lines connect the two SFRSED estimates for the same source, illustrating the difference between the two methods. The overall consistency suggests that the 3.3 μm PAH flux, estimated from medium-band photometry, remains a reliable SFR tracer, immune to dust obscuration.
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: The SFR and star formation surface density distribution of the 3.3 μm PAH sample (green), as compared with normal/irregular galaxies (purple), IR-selected galaxy (red), blue compact starburst galaxies (blue), and circumnuclear star-forming ring in local barred galaxies (orange) from R. C. Kennicutt & N. J. Evans (2012). The 3.3 μm PAH sample lies near the transition region between normal and IR-selected galaxies. The lack of compact star-forming galaxies with similar star formation rates may be due to the small sample size. Another potential bias of the PAH bright sample among the star-forming population is the lack of blue compact galaxies, which may be due to the lack of PAH in dwarf galaxies (Section 4.2).
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: The star-forming main sequence of the PAH targets (orange circles for SFR3.3μm PAH, blue circles for SFRMAGPHYS, and red circles for SFRBagpipes) and the cluster member galaxies (black open dots). We link the SFR for the same target with dashed lines. Most of the cluster galaxies are quiescent, and therefore, have low SFRs. We only show cluster galaxies with SFR above 0.01M⊙ yr−1, which is enough to show the separation between the PAH sample and the SFR of other cluster members. The solid and dotted lines show the star-forming main sequence (J. S. Speagle et al. 2014) at z = 0.308 and a scatter of 0.5 dex. The PAH bright targets have a similar or higher star formation rate to the field star-forming galaxies. Most of the cluster galaxies have an SFR 1 order of magnitude lower than the star-forming galaxies. So the 3.3 μm PAH selection targets are mainly on or above the main sequence.
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: Morphology parameters of the PAH distribution (from the F430M − F444W image) and the stellar distribution (from the F444W image). Left: Gini-M20 results with the reference lines from J. M. Lotz et al. (2004). The PAH morphologies are close to the normal galaxy region, while the stellar distributions are close to the ULIRG region. The change from the stellar distribution to the PAH morphology is from compact (high Gini, low M20) to disklike (low Gini, high M20). Middle: asymmetry of the targets of PAH and stars. The PAH distribution is more asymmetric than the stellar distribution, especially for the targets with an asymmetry index >0.4. Right: half-light radius of the stellar and PAH distribution. The PAH emission region is typically more extended than the stellar continuum. The PAH morphology parameters are measured from the F430M image with the F444W image subtracted.
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: F430M image of A2744, with the 3.3 μm PAH emitters highlighted. Targets within the red circles are the Herschel-detected galaxies in the A2744 cluster. The cyan contours are the mass surface density with levels of [2, 4, 6, 8, 16] × 108 M⊙ kpc−2 from S. Cha et al. (2024), shown in cyan, green, blue, yellow, and red, respectively. The cyan box shows the region of the mass distribution released by S. Cha et al. (2024). Almost all the PAH emitters are in the region of mass surface density lower than 6 × 108 M⊙ kpc−2. Our results show that PAH bright galaxies are more frequently seen in the cluster infall regions with lower surface density than their virialized core.
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:                         Star formation surface density vs. stellar surface density of the PAH bright sample (green open circles). The blue lines represent the scaling relation of star-forming galaxies at 0.25 < z < 0.35 from the MAGPI survey project (M. Mun et al. 2024). The star formation surface density of the PAH bright sample is higher than the scaling relation. The only exception is target ID 3599, located in the lower-right corner, which is blended with nearby galaxies (see Figure 3). This blending affects the F444W size measurement, leading to an anomalously high stellar surface density.
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: SFH derived from Bagpipes SED fitting. The red curves represent the double power-law SFH, while the black stepped curves correspond to the continuity nonparametric SFH model results. The two SFH models are generally consistent, though the nonparametric SFH reveals a recent starburst feature that is smoothed out in the double power-law model. Most of the stellar mass formed around redshift 1.
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: Stellar mass and the mass-weighted formation timescale tform distribution. The cluster galaxies (dots) have a mass-weighted formation time of 4 Gyr after the Big Bang. The PAH samples (squares) formed more recently. The color bar shows the star formation rates, which are higher for the PAH sample and the most massive cluster galaxies.
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: The U − V vs. V − J distribution of the cluster galaxies (blue dots) and PAH sample (orange square). The dashed lines are the critical lines to divide the quiescent and star-forming galaxies (J. J. Fang et al. 2018). So most of the cluster members are quiescent, and the PAH sample is mainly star forming.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Comparison of WD−MS binary candidates selected by different methods in various CMDs. Left panel: Gaia CMD showing absolute G magnitude vs. dereddened B – R color. Middle and right panels: GALEX−Gaia CMD using NUV and FUV bands, respectively. In all panels, blue circles represent WD−MS binaries identified through χ2 fitting of their XP spectra (Chi2 sample in Table 3), while red circles show WD−MS candidates identified by our GPC (QC sample) but missed by the Chi2 sample. Yellow circles mark possible MS–MS binaries (flagMS–MS = 1), mostly brighter than the dotted line at MG0 = 7. The underlying gray circles show the single stars, as defined by the GPC with PWD–MS < 0.2.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: CMD showing WD−MS binary candidates identified by our GPC method (red circles). Yellow triangles denote possible MS–MS binaries. The white contours show the density distribution of the GPC WD−MS candidates. The background gray scale shows the density distribution of all stars in our sample, with the color bar indicating the logarithmic number of stars per bin, which reflects a refined sample from Figure 8.