adsabs/AstroCLIMB huggingface dataset:
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Process for fitting reddening slope R or β, comparing the distribution of points in transmission, after matching PSF core widths to the F606W value, in various pairs of filter bands with curves predicted by particular reddening forms. Derived transmission values are shown in the F606W and F090W filters, for all unmasked pixels in zone 1 of Figure 8. Curves in the left panels use the CCM reddening law with values of R = 1–4 spaced by 1. The right panels use a power law in extinction A  λ  ∝ λ −β  for β = 4 to 1 in steps of 1. This zone emphasizes arm attenuation and therefore does not show the cloud of points near (1, 1) indicating an area of no attenuation, although the cloud of most common values should still fall along the best-fit curve in the absence of systematic offsets. Gray attenuation would trace a straight line from the origin through (1, 1), β = 0 or an infinite value for R. The middle panels show logarithmically spaced contours of the point distribution (after summing in bins of 0.01 on each axis), with thin lines marking the extreme curves from the top panels for reference. The bottom panels show this distribution in gray scale after filtering with a 3 × 3 bin Laplacian to trace its ridgeline, as a valley in the Laplacian gradient. The adopted fits to the ridgeline are shown as lines over the contour plots and as points over the Laplacian together with the best-fit curve for each parameterization. While a best fit can be found for either, each set of highly constrained model curves shows systematic departures from the ridgeline of these data.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Lensed arc and counterimage, shown after subtraction of the model for the foreground elliptical galaxy, with intensity scaling as appropriate for each. The top row shows HST WFC3 F606W and JWST NIRCam F090W and F150W bands, with NIRCam F356W and F444W at the bottom. The nucleus of the elliptical galaxy VV 191a is marked with a plus sign on the single-filter images. Other features discussed in the text or in Table 5 are labeled on the F444W image: the arc, counterimage (CI), diffuse feature, and weakly lensed galaxy A. “FG” indicates an outlying star-forming region in the foreground galaxy. At the lower right is a logarithmically scaled composite of F150W (blue), F356W (green), and F444W (red) data to show color structure in the arc and relative colors of arc, counterimage, and weakly lensed galaxy A (which is shown at higher contrast and magnified by a factor 1.5 in the inset for F444W). The arc has radius 2.″83. The circle on the F356W image shows the modeled Einstein radius 2.″01. Model subtraction leaves signatures of dust from the outer disk of VV 191b visible to the right of the elliptical nucleus, along with subpercent residuals from fitting the elliptical-galaxy model near the core and minor contributions from the hexagonal PSF structure. At the shortest wavelengths, foreground dust lanes cross the right side of the arc and affect its observed spatial profile.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: The F090W attenuation map with masked regions shown (black) and the five zones chosen for fitting attenuation slopes in Table 2. Left to right, they are regions 1, 4, 2, 5, and 3. Zones 1, 2, and 3 are arm regions with organized dust lanes, while zones 4 and 5 are interarm regions with minimal coverage by distinct lanes. This subimage displays north to the right, and covers an area 18.″4 × 21.″7. Zones are marked by subtracting constant values for each from the attenuation map before display. The small area with a dashed outline labeled “UV” is the region used for F336W measurements, where the brightest background and large attenuation combine to give usable S/Ns.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Point clouds for the zones in Figure 8, with the trajectories corresponding to the adopted best-fit values of R = A  V /E  B−V  and power-law index β as in Tables 2 and 3 superimposed. The derived transmission (residual intensity) in each pair of the filter bands (F606W, F090W, and F150W) is shown pixel by pixel after matching PSF widths; the central panels for F606W vs. F150W give the most leverage in fitting the overall reddening law. Typical uncertainties per point are shown for each panel; since these are mostly functions of distance from the two galaxy centers, they are nearly the same within each zone. The wide gray bands mark the ridgelines of the point clouds as traced with the Laplacian. The fitted slope values from Tables 2 and 3 are shown as curves, with the CCM values of R shown as solid curves and the power-law slope results for β shown as dashed curves.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Fits to transmission measurements in the small region used for F336W, comparing F336W and F606W transmission values. Individual pixels are show as points; the broad gray line traces the ridgeline of this point cloud using the Laplacian approach, from data in bins of 0.05 in each coordinate. For comparison, the jagged line shows a running mean over 199 points when sorted by F606W transmission, reflecting the much smaller error in F606W. The curves show the results of CCM models with the indicated R values; we claim only that the data are consistent with R = 1.7 ± 0.4 and strongly limited by the S/N in F336W.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: (Top left) Observed data in band F444W, after subtraction of the elliptical-galaxy lens. (Top right) Lensing model: a lens with a singular isothermal ellipsoid (SIE) mass distribution and external shear, with an extended source behind it. (Bottom left) Lensing geometry reconstruction: the source (black star) is near the cusp of the tangential caustic (green line) and produces two images, of which A is the brightest. A is stretched into an arc due to its proximity to the critical line (red). (Bottom right) Image-model pixel-by-pixel differences in log scale.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: Maximum angular separation of fictitious VZ planets orbiting at the runaway greenhouse boundary around nearby stars with 2500 K ≤ T eff ≤ 7500 K within 30 pc. Face-on inclination was assumed, and only planets that orbit outside the IWA/IWA0.5 while having flux ratios above the 1 × 10−10 threshold are color-coded.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: Terrestrial VZ planets colored based on their TSM value. The x-axis represents the planets’ location in the VZ, where 1 indicates the outer VZ boundary and 0 is the inner VZ boundary. Data points denoted by crosses are VZ planets that are planned to be observed by JWST.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: The relationships between various planet properties. In all plots, the black circles are all known planets regardless of size or location, while the blue squares are terrestrial VZ planets.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: The ESM values of all nontransiting, terrestrial VZ planets at both 7.5 μm (left) and 15 μm (right).
Paper: Evidence for Hidden Nearby Companions to Hot Jupiters
Authors: Dong-Hong Wu, Malena Rice, Songhu Wang
Figure caption: Selection of potential dynamical histories for hot Jupiter systems within our framework. Each path begins with a compact multiplanet system that contains at least one Jovian planet. We emphasize that the pathways shown here are intended to be representative of a broader continuum. At one extreme (top row) is a quiescent dynamical history, where hot Jupiters without strong planet–planet interactions maintain very low eccentricities (e ∼ 0), and neighboring planets remain in the system. At the other extreme (bottom row), two or more gas giants that formed further out in the disk can initialize high-eccentricity migration. Dynamical interactions between cold Jupiters launch one gas giant onto an extremely eccentric orbit, removing close-in companions from the system. The gas giant’s orbit tidally circularizes over time, producing an isolated hot Jupiter. For illustrative purposes, we show two example systems that fall between these extremes in the low-eccentricity migration regime in which some warm Jupiters may attain lower eccentricities and migrate shorter distances to ultimately become hot Jupiters. We note that some hot Jupiters that underwent eccentric migration may retain wide-orbiting companions; however, because the rate of retention for these companions is poorly constrained, we do not include them within this schematic.
Paper: Evidence for Hidden Nearby Companions to Hot Jupiters
Authors: Dong-Hong Wu, Malena Rice, Songhu Wang
Figure caption: Summary of the observed Kepler TTV rates compared with simulated TTV recovery rates to provide a final occurrence rate of hot and warm Jupiters with nearby companions. Panel (a): our full sample in period–radius space, shown in the context of Kepler planetary candidates. Panel (b): distribution of systems with Jupiter-sized planets that show detectable TTVs. Panel (c): simulated recovery rate of Jupiter-mass planets with observed TTVs. Panel (d): final combined result for the occurrence rate of Jupiter-sized planets with nearby companions as a function of the orbital period.
Paper: Evidence for Hidden Nearby Companions to Hot Jupiters
Authors: Dong-Hong Wu, Malena Rice, Songhu Wang
Figure caption: The upper panel displays the generalized Lomb–Scargle periodogram for the TTV data of KOI-202.01 from Rowe et al. (2015) and Holczer et al. (2016), shown in blue and yellow, respectively. The highest power and best-fitting period are indicated by a solid dot, while the FAP level of 0.01% is represented by a dashed line. The generalized Lomb–Scargle periodogram analysis of the TTV data from these two sources suggests a strong TTV signal with a period of 1325 days. The lower panels show the detected TTV signals for KOI-202.01 with a bin time of 100 days. The unbinned TTVs are represented by gray solid points with error bars, while the binned TTVs from Rowe et al. (2015) and Holczer et al. (2016) are depicted in blue and yellow, respectively. The binning process effectively reduces the uncertainties of the TTVs without altering the overall TTV pattern, resulting in a typical uncertainty of 0.08 minutes.
Paper: Evidence for Hidden Nearby Companions to Hot Jupiters
Authors: Dong-Hong Wu, Malena Rice, Songhu Wang
Figure caption: Comparison of TTVs derived from short-cadence data in the present study with those obtained from long-cadence data as reported in Holczer et al. (2016). The TTV differences between Holczer et al. (2016) and this study are shown in the left panel as a function of time. The rms of the differences was reduced from 0.44 to 0.074 minutes with a 50 day bin. The right panel presents the TTVs derived from long-cadence data in Holczer et al. (2016) and the corresponding TTVs derived from short-cadence data in this study. The data points are represented by yellow dots with error bars, and the blue dashed line indicates exact agreement.
Paper: Evidence for Hidden Nearby Companions to Hot Jupiters
Authors: Dong-Hong Wu, Malena Rice, Songhu Wang
Figure caption: Detected TTV signals for the Kepler Jupiter sample, broken into logarithmically spaced period bins. The top row shows where each system with TTVs lies in period–radius space, while the remaining panels show the observed TTVs. The legend is provided in the lower left corner for reference. The x-axis of each panel spans the same full time range of Kepler primary mission observations.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Distribution of ﹩R\,\sin \,i﹩/R ratios as a proxy of ﹩\sin i﹩. Top: comparison between slow and fast rotators. Middle: comparison of the sources with strong (>5% of the total flux) and weak (<1%) variability (limited to just the slow rotators with P > 2 days), as well as SB2 spectroscopic binaries from Kounkel et al. (2019). Bottom: comparison of CTTSs and WTTSs, also limited to just slow rotators.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Rate of loss of angular momentum L (top) and specific angular momentum H (bottom) as a function of temperature and age, assuming the empirical relation in Figure 6 and Table 1.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Average systematic trends in the distribution of ages as a function of T eff across Orion in different age ranges. The included models are MIST (Choi et al. 2016); PARSEC (Marigo et al. 2017); Baraffe et al. (2015); SPOTS with 0%, 17%, 34%, and 51% spot coverage (Somers et al. 2020); and Sagitta (McBride et al. 2021). The black line shows the constant age across all T eff.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Fit of angular momentum L. Yellow dots correspond to the data within each age bin. The red line shows the running median within the data. The thick blue line shows the best fit for L for a given age. Thin blue lines are offset in age by ±0.3 dex, and dotted lines are offset in age by ±0.6 dex. The typical scatter between the data and the resulting fit of L is shown in each panel. Open circles represent CTTSs, and filled circles represent WTTSs.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Top: rotational period as a function of color for the sample from Kraus et al. (2011) in Taurus with the periods from Paper I. Blue dots highlight binaries that have been resolved through high-resolution imaging, and red diamonds indicate sources in which no resolved companion has been identified to date. The black line shows the period of 2 days, delineating slow and rapid rotators (see also Figure 4 in Stauffer et al. 2018). Bottom: rotational period as a function of projected separation in resolved binaries.
Paper: Measurement of the Angular Momenta of Pre-main-sequence Stars: Early Evolution of Slow and Fast Rotators and Empirical Constraints on Spin-down Torque Mechanisms
Authors: Marina Kounkel, Keivan G. Stassun, Lynne A. Hillenbrand, Jesús Hernández, Javier Serna, Jason Lee Curtis
Figure caption: Kernel density estimate distribution of ﹩R\,\sin \,i﹩/R ratios of CTTSs and WTTSs as a function of age. Note that the last two age bins are different between the two panels due to a decreased number of CTTSs at older ages. The distribution is often bimodal; the sources that appear to be inclined are likely to be unresolved binaries.
Paper: Searching for Compact Object Candidates from LAMOST Time-domain Survey of Four K2 Plates
Authors: Senyu Qi, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Song Wang, Jifeng Liu
Figure caption: Light curves of three sources folded by orbital periods. The photometric data of J034813 is from K2 (The error bars for data points are invisibly small). The photometric data of J063350 is from ZTF. The photometric data of J064850 is from TESS. The red curve represents the best-fitting PHOEBE model.
Paper: Searching for Compact Object Candidates from LAMOST Time-domain Survey of Four K2 Plates
Authors: Senyu Qi, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Song Wang, Jifeng Liu
Figure caption: LAMOST spectra (left panels) and CCF profile (right panels) for the candidates. In each left panel, two spectra used to perform the CCF are both observational spectra but are styled with distinct colors and labels to indicate which one is used as the template. The vertical dashed lines in the right panels indicate the measured (relative) radial velocity.
Paper: Searching for Compact Object Candidates from LAMOST Time-domain Survey of Four K2 Plates
Authors: Senyu Qi, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Song Wang, Jifeng Liu
Figure caption: The minimum mass of the invisible companion ﹩{M}_{2}^{\min }﹩ at the maximum inclination (i = 90°). Two dash lines represent the cases ﹩{M}_{1}={M}_{2}^{\min }﹩ and ﹩{M}_{1}=2{M}_{2}^{\min }﹩.
Paper: Searching for Compact Object Candidates from LAMOST Time-domain Survey of Four K2 Plates
Authors: Senyu Qi, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Song Wang, Jifeng Liu
Figure caption: Parameter distributions of the light curves fitting. The top left, top right, and bottom corners correspond to J034813, J063350, and J064850, respectively.
Paper: Searching for Compact Object Candidates from LAMOST Time-domain Survey of Four K2 Plates
Authors: Senyu Qi, Wei-Min Gu, Tuan Yi, Zhi-Xiang Zhang, Song Wang, Jifeng Liu
Figure caption: The SED fitting results of J034813 (top panel), J063350 (middle panel), and J064850 (bottom panel). Cyan points are the observed fluxes, purple diamonds are the synthetic fluxes, and the black curve is the best-fit SED model.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: The ZTF g-band observed light curve data for NGC  6254 V20 fitted with various nth-order of the Fourier expansion (dark solid curves). The Baart’s condition suggested the best Fourier fit is for n = 6. The dashed red curve is a smoothed curve derived from applying the LOWESS algorithm to the duplicated observed light curve from phase 0 to 2. The two problems mentioned in the text can be seen on the smoothed curve, such that this curve is disjointed at phase 0 and 2 (i.e., nonperiodic), and a slight deviation of the smoothed curve from the data points can be seen around phase ∼0. Therefore, we only compare the smoothed curve to the fitted Fourier expansion for different n at phases between 0.5 and 1.5 (the solid red curve). Based on such approach, the best Fourier order was found to be n = 4 for this observed light curve.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Examples of the light curves for rejected SXP stars in our sample. N represents the number of data points in the light curve. The solid curves are the fitted Fourier expansion with the best-fit Fourier order given as n. Black crosses are rejected data points based on the two-step period refining process as described in Section 3.1.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for SX Phoenicis Variables in the gri Band
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Brian F. Healy, Russ R. Laher, Reed Riddle, Avery Wold
Figure caption: Amplitudes as a function of ﹩\mathrm{log}{P}_{\mathrm{LSM}}﹩ for the SXP stars in the sample. See text for further discussion on NGC  6838 P13.