adsabs/AstroCLIMB huggingface dataset:
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Color–magnitude diagram showing extinction-corrected absolute g-band magnitudes vs. g − r color for spider counterparts, overlaid on a background of three million Pan-STARRS field stars crossmatched with Gaia to obtain accurate distance and absolute magnitude measurements. Spider systems predominantly occupy a region between the main sequence and WD branch. Outliers are, in most cases, either HM systems (with giant companions), tMSPs (which may include optical emission from an accretion disk), or potentially unassociated stars (where the optical counterpart is uncertain due to a large angular separation from the pulsar or candidate). Most spider systems are located between the two dashed lines, where the upper boundary is defined by Mg = 4.5 × (g − r) + 4.5, and the lower by Mg = 2.7 × (g − r) + 10.3. We also draw two representative blackbody tracks with different temperatures from 3000 K to 16,000 K separated by 1000 K (marked as stars) for BW-type (with radius RBW = 0.08 R⊙) and RB-type stars (with radius RRB = 0.37 R⊙).
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Spin period (P) vs. spin period derivative (﹩\dot{P}﹩) diagram for ATNF pulsars, highlighting binaries and confirmed spider systems. Lines of constant ﹩\dot{E}﹩, B, and τ are superposed. Also, the classical and outer magnetosphere “death lines” are shown as dashed blue and dashed–dotted green lines, respectively (see text). Histograms of P and ﹩\dot{P}﹩ are shown above and to the right of the plot, respectively, on a logarithmic scale for clarity. Spiders occupy the lower-left region of the ﹩P/\dot{P}﹩-diagram, corresponding to the fastest-spinning, most weakly magnetized, and oldest pulsars. Two outlier systems, PSR J2129−0429 and PSR J1932+2121, lie above the main population, likely representing mildly recycled systems with longer spin periods and higher ﹩\dot{P}﹩, indicative of alternative evolutionary paths.
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Spider spin periods as a function of orbital period (panel (a): RBs, panel (b): BWs). Data points are color coded by K-means clusters (black indicates no available estimate for ﹩\dot{P}﹩): Cluster 1 (violet data points) features fast spins and a wider range in orbital periods, while Cluster 2 (green data points) comprises systems with short orbital periods and a broader range of spin periods. Upper panels display box plots of derived parameters for the two clusters: spin-down luminosity (left), characteristic age (middle), and magnetic field strength at the light cylinder (right).
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: The relationship between X-ray (LX) and γ-ray (Lγ) luminosities for spider systems. γ-ray luminosities are not significantly different between spider types. On the other hand, RBs exhibit systematically higher X-ray luminosities likely due to stronger IBSs. BWs follow a relation of ﹩{L}_{{\rm{X}}}\propto {L}_{\gamma }^{0.5\pm 0.2}﹩, while RBs may follow a steeper trend of ﹩{L}_{{\rm{X}}}\propto {L}_{\gamma }^{0.9\pm 0.3}﹩, suggesting differing emission contributions across populations.
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Minimum companion mass vs. orbital period for spider systems, color coded by spider subclass. RBs and BWs are clearly separated by their characteristic companion masses, with RBs generally having Mc,min ≳ 0.1 M⊙ and BWs Mc,min ≲ 0.06 M⊙. The areas of tidarren and HM systems are highlighted at the low-period and low-mass and high-period and high-mass corners, respectively. PSR J1908+2105 is labeled as an outlier RB with an anomalously low minimum companion mass, explained by a low orbital inclination.
Paper: SpiderCat: A Catalog of Compact Binary Millisecond Pulsars
Authors: Karri I. I. Koljonen, Manuel Linares
Figure caption: Histogram of the logarithm of the ratio of γ-ray (Fγ) to X-ray (FX) fluxes for spider systems (bin size: 0.25 dex), color coded by spider type. The flux ratios for BWs are more narrowly distributed and generally higher. For ﹩\mathrm{log}\,({F}_{\gamma }/{F}_{{\rm{X}}})\lt 2﹩, it becomes increasingly likely that the system is an RB.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Left: dust temperature map of NGC 7023 derived from Herschel maps of L1172/1174 cloud (J. Di Francesco et al. 2020). The central star is marked in black with PDRs labeled. The solid black circle marks the POL-2 field of 6﹩{}^{{\prime} }﹩ radius. The cyan box shows the area of interest that is considered in later figures. Right: SCUBA-2 850 μm Stokes I map obtained with our polarization observations. The clump C1 is labeled. The SCUBA-2 dust continuum emission contours in white range from 0.1 (10σ) to 1.1 mJy arcsec−2 in the intervals of 20σ, σ = 0.01 mJy arcsec−2.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Extracted filament shown as a black dotted line overplotted on the SCUBA-2 image, with magnetic field lines shown in white. The magenta triangles show three cores, labeled as P17 21, P17 23, and P17 24. The names were adopted from K. Pattle et al. (2017). The circles show the regions I, II, and III, chosen to calculate the average magnetic field around the three cores.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Non-debiased polarization fraction as a function of Stokes I intensity, fitted with a single-power-law distribution and a Ricean noise model, as described in the text. All data points in the central 3′-diameter region of the image are shown and fitted. Those at p/dp > 2 are shaded in gray; those at p/dp > 3 are shaded in black. The best-fit model, with a power-law index α = 0.62 ± 0.04, is shown as a solid maroon line. The behavior in the absence of true polarized signal, ﹩p^{\prime} =\sqrt{\pi /2}{(I/{\sigma }_{\mathrm{QU}})}^{-1}﹩, is shown as a dashed maroon line.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Left: Herschel dust column density map of NGC 7023. The white star marks the position of the intermediate-mass star HD 200775. The magenta lines show the magnetic fields derived from Planck polarization data, and the yellow lines show the magnetic field lines measured using optical polarization vectors (P. Saha et al. 2021). Right: SCUBA-2 850 μm Stokes I map toward C1. The zoomed-in region is marked with a cyan box in the main image. The integrated intensity contours of N2H+ (1–0) in cyan are in the range from 0.5 to 1.4 K km s−1 (step size ∼0.1 K km s−1). Red vectors show our POL-2 observations toward C1 with pdb/dp > 3.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Left: the POL-2 dust polarization map at 850 μm toward NGC 7023 reflection nebula near the Herbig Ae Be star, HD 200775. The background image shows the Stokes I intensity. The black lines show the polarization angles, and the degree of polarization in their length is proportional to polarization percentages. A reference vector with a polarization percentage of 10% is shown. Right: the magnetic field map toward NGC 7023 with equal length vectors that have been rotated by 90° to trace the plane-of-sky magnetic field direction.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Average profile of N2H+ in blue over the clump. The vertical line shows the systematic velocity of the clump derived using a hyperfine fitting of the N2H+ line.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: The distribution of polarization angles, rotated by 90∘ to infer the magnetic field orientations obtained using JCMT POL-2, is shown in green. The B-field orientations from optical R-band P. Saha et al. (2021) and from Planck polarization data (rotated by 90∘) are plotted in gray and red, respectively. The black and red vertical lines around the R-band (∼0.6 μm) and Planck distribution are the mean magnetic field direction with their range of dispersion.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: The angular dispersion function for the polarization angles obtained from the POL-2 data. The best-fit parameters were found by fitting Equation (12) and are shown in the top-right legend.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Examples of preprocessing steps applied to the OGLE data. The original data for OGLE-II and OGLE-III are plotted in red, while black points represent the adjusted light curve. The median valued of the sections with low disk activity (top) and selected by the user (middle) are shown in the legends and are graphically represented by horizontal lines (red ones for original OGLE-II and OGLE-III data, while black represents OGLE-IV level). The identified outliers are plotted as red stars, and gray horizontal bands display the range of 2 times the detection threshold of 0.06 mag (see Section 3.4 for more details). Vertical purple bands mark transition times among different observational phases. Top: SMC_SC3_71445 light curve, with automatic offset values of ΔO−II = 16.575−16.605 = −0.030 and ΔO−III = −0.024 mag. Middle: data for SMC_SC10_94551 target, with offset valued equal to ΔO−II = −0.027 mag, estimated from manual selection (outlined by green areas), and outliers identified by sigma clipping with the parameters Σ = 2σ and NI = 3. Bottom: LMC_SC15_294 light curve with outliers identified by sigma clipping (Σ = 3σ and NI = 3).
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Herschel dust column density map of the region with red- and blueshifted high-velocity 12CO gas around the star. The red contours show the integrated 12CO emission in the velocity range 5–7.5 km s−1 and blue dotted contours in the velocity interval −2.5 to 0 km s−1. The contour levels for red contours range from 1.25 to 7 K km s−1 in steps of 5σ with σ as 0.15 K km s−1, and for blueshifted gas, the levels range from 1.3 to 6 K km s−1 in steps of 3σ (σ ∼ 0.18 K km s−1). The yellow box marks the extent of the Spitzer data shown in Figure 9. The systematic velocity of the cloud is ∼2.7 km s−1.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Panel (A) shows the light curve of LMC_SC1_164770, featuring an initial stable phase, followed by a bump that gradually decays over approximately 5000 days. The corresponding CMD traces a loop: it starts in a bluer and dimmer region, shifts toward brighter and redder areas, and ultimately returns to its original position. The second light curve, from target LMC_SC3_400956, begins with a slow brightness increase and is followed by two dips; while the associated CMD shows a vertical excursion with small changes in color. Panel (C) (LMC_SC1_340178) presents a very active star with (quasi)-periodic bumps and a CMD structure similar to one find in the first panel. The next panel displays the light curve of LMC_SC15_294, exhibiting a more complex behavior; the CMD does not present a clear structure. The light curve presented in panel E (LMC_SC3_113787) shows no activity and small CMD variations. The last panel presents SMC_SC2_33373, a quite periodic star with no clear CMD structure.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Spitzer 8 μm emission map of NGC 7023 taken from the c2d catalog (N. J. Evans et al. 2003). The red contours and yellow vectors show the SCUBA-2 emission contours and the magnetic field orientation derived from our POL-2 measurements, respectively. The dotted cyan curves mark the outer periphery of the biconical structure of the nebula, and the magenta star shows the central source HD 200775. The extent of the emission region around HD 200775 corresponds to the yellow box marked in Figure 10.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Synthetic light curve of disk events for a dense disk (Σ0 = 4.00 g cm−2), generated for different buildup times as indicated in the legend. The abscissa represents time, referenced to the beginning of dissipation, while the ordinate shows the variation in brightness, relative to the diskless value, caused by the disk’s presence. The gray band represents the detection threshold, as introduced in Figure 1. The transition to the dissipation phase is marked by filled black circles. The upper panel shows a pole-on view (i = 0°), while the edge-on view (i = 90°) is at the bottom.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Schematic view of the clump C1 in the NGC 7023 region. Black solid lines show the bipolar outflow, and the double arrow shows the direction of the outflow axis. The central source HD 200775 is marked by a blue star. The black ellipses show three cores in the blue-colored clump. The dashed lines show the derived magnetic field direction in the clump using POL-2. Black arrows show the direction of the compression across the outflow walls. The red and blue structures show the red- and blueshifted gas traced in outflow wings.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: SCUBA-2 dust continuum emission maps of the observed region with overplotted molecular line emission contours for (a) N2H+ (1–0), with the contour levels ranging from 0.5 to 1.3 K km s−1 in steps of ∼0.1 K km s−1; (b) C18O (1–0) line with the contour levels ranging from 0.3 to 1.3 K km s−1 in steps of 0.14 K km s−1; (c) CS(2–1) with the contour levels ranging from 0.2 to 0.8 K km s−1 in steps of ∼0.1 K km s−1.
Paper: Imprints of Stellar Feedback on Magnetic Fields in the Iris Nebula NGC 7023
Authors: Ekta Sharma, Kate Pattle, Di Li, Chang Won Lee, Maheswar Gopinathan, Tao-Chung Ching, Mehrnoosh Tahani, Shinyoung Kim
Figure caption: Average profiles of N2H+ in black, C18O in red, and CS (2–1) in blue toward the clump. The gray lines show the fitted Gaussians. The vertical line shows the systematic velocity of the clump derived using a hyperfine fitting of the N2H+ line.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Examples of light curves categorized according to the definitions in Section 5. The colors of data points and error bars represent different categories of variability: gray (1—baseline), blue (2—buildup), orange (3—dissipation), magenta (4—plateau), green (5—isolated buildup), red (6—isolated dissipation). Horizontal red lines show the average baseline (dashed), and the respective standard deviation limits (dotted), when available. Their respective values are shown in the legend. Vertical magenta bands show the transition times among different observational phases. Top: light curve for target SMC_SC2_29957 for which the values of DC and DDC estimated were DC = 0.55 and DDC = 1.0. Middle: light curve for LMC_SC10_40703 with DC = 0.78 and DDC = 0.92. Bottom: light curve for LMC_SC1_164770, with DC = 0.13 and DDC = 0.83. The dashed line shows the fit of Equations (5) and (6) (bottom panel). Vertical black lines represent times marking the beginning and end of each category selected.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Similar to Figure 8 for the masses obtained for 468 stars of groups 2 and 3 (LMC population in purple and yellow represents SMC targets). The expected Be star distributions estimated from the literature (see the text) are shown by thick lines. The purple line uses data from C. Martayan et al. (2006), the yellow from C. Martayan et al. (2007), and the dotted black line was extracted from F. Navarete et al. (2024).
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: V − I CMD for different models and inclinations. The ordinate shows the brightness variations in the I band, taking a diskless star as a reference. The abscissa represents the change in color due to the disk’s presence, with zero indicating a diskless star. Top: shown are models for Σ0 = 4.00 g cm−2, selected buildup times (different line styles as seen in the top left legend), and inclination angles (indicated by different colors in the bottom right legend). Bottom: same as the top panel, but keeping tb = 1800 days fixed and varying the base density. The transition to the dissipation phase is marked by filled circles, colored according to i. Dashed horizontal and vertical lines represent the CMD position for a diskless star. As in Figure 1, the horizontal gray area represents the adopted detection threshold, while the vertical gray band indicates the equivalent limit for the color, taking into account the error propagation for both bandpasses.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Box plots for the DC (top), DDC (middle), and Nout (bottom), combining the subsample that exhibits a baseline (groups 2 and 3), separated into three mass intervals (see text) for both galaxies (purple for LMC and yellow for SMC stars). Box plots summarize the distribution of the data, with the box indicating the IQR and the line inside the box representing the median. The whiskers extend to 1.5 times the IQR. The dotted lines represent the median values of the entire sample, with all mass bins combined. The K-S test was run to compare the distributions of each mass bin from different metallicities, resulting in ﹩{\rho }_{{M}_{{\rm{1}}}}=0.36﹩, ﹩{\rho }_{{M}_{{\rm{2}}}}=0.36﹩, ﹩{\rho }_{{M}_{{\rm{3}}}}=0.21﹩ (for DC), ﹩{\rho }_{{M}_{{\rm{1}}}}=0.81﹩, ﹩{\rho }_{{M}_{{\rm{2}}}}=0.47﹩, ﹩{\rho }_{{M}_{{\rm{3}}}}=0.61﹩ (for DDC), ﹩{\rho }_{{M}_{{\rm{1}}}}=0.25﹩, ﹩{\rho }_{{M}_{{\rm{2}}}}=1.5\times 1{0}^{-4}﹩, and ﹩{\rho }_{{M}_{{\rm{3}}}}=0.42﹩ (for Nout).
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Maximum disk excess for the I band, ﹩{\rm{\Delta }}{I}_{{\rm{\max }}}﹩, observed as a function of inclination angle for models with different disk densities (represented by colors shown in the central legend box) and feed times (line styles as seen in the bottom left legend). The horizontal gray band indicates the detection threshold limit of 0.06 mag. The vertical bars indicate the inclination range for which ﹩{\rm{\Delta }}{I}_{{\rm{\max }}}﹩ is below the detection limit, colored according to the model density and with the respective numerical range at the top.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Normalized histogram of the number of outbursts per year (Nout) for LMC (purple) and SMC (yellow) stars of the entire Be star sample. The numbers of light curves of each sample are shown in the legend: 1154 for LMC and 597 SMC light curves. Median values are shown by vertical dashed lines. The cumulative distribution functions, assisted by horizontal dashed lines for 20%, 40%, and 80%, are represented by dotted lines (right-hand axis). The value of the K-S test applied to both samples is ρLMC − SMC).
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: CMD of simulated diskless stars (Table 3) for LMC (left) and SMC (right). The colors ranging from dark red to dark blue correspond to the eleven values of M⊙, as shown in the upper-right legend. The 10 rotation values are represented by symbol sizes (middle right legend). The different symbols represent the stellar MS age (bottom left legend). The data for stars of groups 2 and 3 are represented by the green dots with error bars.
Paper: Be Star Demographics: A Comprehensive Study of Thousands of Light Curves in the Magellanic Clouds
Authors: André Luiz Figueiredo, Alex C. Carciofi, Jonathan Labadie-Bartz, Matheus L. Pinho, Tajan H. de Amorim, Pedro Ticiani dos Santos, Igor Soszyński, Andrzej Udalski
Figure caption: Schematic view of the samples defined in the paper. In the upper-right box, we list the characteristics of the light curves that were removed to obtain the raw sample.