adsabs/AstroCLIMB huggingface dataset:
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Similar to Figure 20, but for the distribution of the complete magnitude in the SAGES v  s  passband, with a median value of v  s  = 20.3 mag.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Similar to Figure 17 but for complete magnitude of the SAGES v s  passband, which is ∼2.4 mag deeper than that in Figure 17.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Similar to Figure 16 but for complete magnitude (which is defined as the turnover in the magnitude histogram) of the SAGES u  s  passband, which is ∼2.4 mag deeper than that in Figure 16.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Similar to Figure 16 but for the SAGES v  s  passband, limiting magnitude of S/N = 100, and corresponding to a photometry error of 0.01 mag.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Examples of raw M2FS (HiRes configuration) images obtained during exposures of a calibration LED source (top left), evening twilight (top right), ThArNe arc lamp (bottom left), and a science field (bottom right). Single-order spectra appear as horizontal bands, each spanning 5130–5190 Å over columns ∼300–1400 (signal outside this column range is contributed by light from adjacent orders and is not used). The separation into eight groups of 16 apertures reflects the physical bundling of fiber ends at the spectrograph.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Examples of Magellan/M2FS HiRes spectra (black, main panels; sky-subtracted counts are scaled to the dimensions of the plotting window), which for our observing configuration cover 5125–5190 Å at resolution ﹩{ \mathcal R }﹩ ≈ 24,000. Text indicates Gaia ID and Gaia G-band magnitude. Overplotted (red) are best-fitting model spectra. Smaller panels display normalized (by the count error propagated through the processing pipeline) residual with respect to the best fit. In the top panels, hash marks identify wavelengths (redshifted to match the observed spectrum) of known Fe I (solid gray), Fe II (broken gray), and Mg I (solid black) lines. Left-hand (right-hand) panels depict spectra for likely red giant (dwarf) stars, with surface gravity measured to be ﹩\mathrm{log}g﹩ < 1 (﹩\mathrm{log}g﹩ > 4).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Mean value of ﹩{\chi }_{1}^{2}\equiv {(S-{S}_{\mathrm{in}})}^{2}/{\hat{\sigma }}_{N}^{2}﹩ as a function of expected signal S in, from 106 realizations at each input signal, assuming read noise σ  r  = 2.6 e−; see Section 3.1 for details. Curves show results for different estimators of the variance, ﹩{\hat{\sigma }}^{2};﹩ black uses the true variance, blue uses a commonly used estimator, and red uses the estimator we use for real M2FS data (Equation (2)).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Same as Figure 5, but for example MMT/Hectochelle spectra, which span 5150–5300 Å at ﹩{ \mathcal R }﹩ ≈ 32,000. The larger numbers of counts (see Figures 5 and 6) reflect the fact that the Hectochelle pipeline calculates the sum of counts across subexposures, while the M2FS pipeline calculates the average.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Change in wavelength per change in temperature (as measured at the detector), from emission lines observed in calibration exposures acquired immediately before and immediately after M2FS (HiRes configuration) observations of one example science field. Left/right panels show results for the blue and red channel, respectively.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Identification of spectral apertures in an example M2FS frame. Plotted for each row on the detector is the mean count recorded in columns 1013–1032 (the middle 20 columns). Local maxima signify the centers of spectral apertures.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Same as Figure 5, but for example Magellan/M2FS MedRes spectra, which span 5115–5300 Å at ﹩{ \mathcal R }\approx 7000﹩.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Top three panels: χ 2 per pixel vs. median S/N per pixel, from the best-fitting model for each individual spectrum obtained with M2FS HiRes, M2FS MedRes, and Hectochelle. Red points identify observations that pass our crude quality-control filter, with raw velocity error ≤5 km s−1. Outliers having χ 2/pix above the dashed curves tend to correspond to anomalous sources, primarily carbon stars, background galaxies, and quasars. Bottom three panels: ratio of median flux in the 5160–5167 Å bandpass to the median flux in the 5176–5183 Å bandpass, vs. median S/N. Outliers having flux ratios below the dashed curves are flagged in our data catalogs as likely carbon stars.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Internal validation of formal uncertainties. For each of the spectroscopic observables V LOS, T eff, ﹩\mathrm{log}g﹩, [Fe/H], and [Mg/Fe], the panels indicate distributions of pair-wise deviations between independent measurements of the same target, normalized by the combined error in both measurements. Errors are calculated using the standard deviation taken directly from the marginal posterior PDFs returned by MultiNest (blue “before” histograms), and using the formal errors obtained by fitting the error model described in Section 4.2 (red “after” histograms). Individual panels in the top, middle, and bottom rows show results from 6830 pairs of M2FS HiRes observations, 259 pairs of M2FS MedRes observations, and 6301 pairs of Hectochelle observations, respectively. In all panels, the solid black curve is the standard normal distribution.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Top row: comparison of stellar-atmospheric parameters measured (before applying zero-point adjustments) by M2FS HiRes and either M2FS MedRes (cyan) or Hectochelle (blue), for stars common to both samples. Bottom three rows: comparison of parameters that we measure (before applying zero-point adjustments) using M2FS (red) and Hectochelle (blue) to those measured in external surveys by Kirby et al. (2010, second row), APOGEE (DR17; Abdurro’uf et al. 2022, third row), and the H3 survey (Conroy et al. 2019, fourth row). In all panels of the bottom three rows, the quantity plotted along the horizontal axis is the measurement from M2FS (red) and/or Hectochelle (blue).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Examples of M2FS HiRes (left) and Hectochelle (right) spectra from anomalous sources, with text indicating celestial coordinates, HJD of observation, and Gaia G-band magnitude (if available). The top two M2FS spectra, and the top Hectochelle spectrum, come from stars showing various levels of carbon enhancement, with the prominent Swan (1857) C2 bandhead near 5165 Å. The second (from top) Hectochelle spectrum is dominated by emission lines from an extragalactic source. Spectra in the third row are from cool M giant stars, with the TiO bandhead apparent near 5170 Å. Spectra in the bottom row are from known quasars, at redshift z ∼ 3.7 (Boutsia et al. 2021, left) and z ∼ 3.4 (Pâris et al. 2014, right).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Comparison of current M2FS+Hectochelle measurements of [Fe/H] (left) and [Mg/Fe] (right) to previously published values derived from high-resolution spectra.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Top row: difference between line-of-sight velocities measured by M2FS HiRes and either M2FS MedRes (cyan) or Hectochelle (blue), for stars common to both samples. Bottom three rows: differences between line-of-sight velocities we measure using M2FS HiRes (red), M2FS MedRes (cyan), or Hectochelle (blue) and those measured in external surveys by Walker et al. (2009, second row), APOGEE (DR17; Abdurro’uf et al. 2022, third row), and the H3 survey (Conroy et al. 2019, fourth row).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Validation of template spectra. Top panels compare observed solar (left) and Arcturus (right) spectra with synthetic spectra generated using the same tools as for our template grid. Data points represent the observed spectra, resampled to the resolution of our models, Δλ = 0.05 Å, which are shown by the red lines. Bottom panels illustrate the differences in percent.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Histograms of metallicities we infer from archival Hectochelle observations of targets in the star clusters (top to bottom) M92, M13, M3, M107, M71, and M67. In each panel, the dashed vertical line indicates the metallicity tabulated by Harris (1996), except for the metallicity of M67, which we adopt from Pace et al. (2008).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Distribution of number of independent measurements (having line-of-sight velocity error <5 km s−1), for M2FS HiRes (blue), M2FS MedRes (cyan), and Hectochelle (red) samples. The bump in the M2FS HiRes sample at N obs > 10 is contributed entirely by repeated observations of the Tucana II dwarf galaxy.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Sky maps, color–magnitude diagrams (CMDs; middle), proper-motion coordinates, and spectroscopic [Fe/H] vs. V LOS, from Gaia photometry/astrometry and Magellan/M2FS spectroscopy of point sources toward Galactic satellites. Colored points indicate sources for which we report spectroscopic measurements, with bluer colors identifying likely red giant stars belonging to the satellites. In sky maps, dashed ellipses have semimajor axis ﹩a=2{R}_{\mathrm{half}}/\sqrt{1-\epsilon }﹩, where R half is the projected half-light radius and ϵ ≡ 1 − b/a is the measured ellipticity, both adopted from the compilation by Pace et al. (2022). In CMDs, gray points indicate unobserved point sources within 1◦ of the satellite center; in sky maps, gray points indicate unobserved sources within ﹩\delta =\max (0.15,\sqrt{{\sigma }_{{\rm{G}}}^{2}+{\sigma }_{\mathrm{BP}}^{2}+{\sigma }_{\mathrm{RP}}^{2}})﹩ magnitudes of the theoretical isochrone (Morton 2015; Dotter 2016) overplotted in the corresponding CMD (chosen for typical age = 10 Gyr and according to previously published mean metallicity). Dashed lines indicate previously measured mean systemic proper motions and line-of-sight velocities.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Chemo-dynamic substructure within the Milky Way halo: metallicity vs. line-of-sight velocity, from Magellan/M2FS and MMT/Hectochelle spectra acquired for 16,369 stars observed toward 38 Galactic Halo objects. Marker color indicates spectroscopically estimated surface gravity. Given our color/magnitude criteria for spectroscopic target selection, redder marker colors tend to identify dwarf stars in the Galactic disk, while bluer marker colors indicate giant stars in the Galactic halo and its substructures. The halo objects that are most obvious here are the “classical” dwarf spheroidal galaxies Draco (V LOS ∼ −290 km s−1), Ursa Minor (−250 km s−1), Fornax (+55 km s−1), Leo II (+80 km s−1), Sculptor (+110 km s−1), Carina/Sextans (both at +220 km s−1), and Leo I (+280 km s−1).
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Distributions of the ratio of weighted standard deviation to weighted mean uncertainty of spectroscopically measured parameters, for stars having multiple independent measurements passing our quality-control filter. Red (blue) histograms correspond to sources that do (do not) appear in Gaia’s (DR3) RR Lyrae catalog. The leftmost panel demonstrates the intrinsic variability of V LOS for RRL stars.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Surface gravity vs. effective temperature (both estimated spectroscopically), for the 7416 stars in our M2FS+Hectochelle data set that have observational errors ≤0.5 in each of ﹩\mathrm{log}g﹩, [Fe/H], and [Mg/Fe]. Marker color indicates spectroscopically estimated metallicity. Overplotted, for comparison, are theoretical isochrones (Morton 2015; Dotter 2016) calculated for age = 10 Gyr and a range of [Fe/H].
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Examples of M2FS (top left) and Hectochelle (all other panels) spectra corresponding to spurious measurements of extremely low metallicity ([Fe/H] ≲ −3.6), high surface gravity (﹩\mathrm{log}g﹩ ≳ 4.5), and alpha-enhanced [Mg/Fe]. Overplotted in red are best-fitting models, which tend to find absorption features but fail to reproduce their broadness. Text indicates target coordinates, Gaia G-band magnitude, and values of spectroscopically inferred parameters.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption: Magnesium abundance vs. metallicity, for the 7416 stars in our M2FS+Hectochelle data set that have observational errors ≤0.5 in each of ﹩\mathrm{log}g﹩, [Fe/H], and [Mg/Fe]. Marker color indicates spectroscopically estimated surface gravity.
Paper: Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo 
Authors: Matthew G. Walker, Nelson Caldwell, Mario Mateo, Edward W. Olszewski, Andrew B. Pace, John I. Bailey, Sergey E. Koposov, Ian U. Roederer
Figure caption:                         Same as Figure 22, but for Galactic satellites observed with MMT/Hectochelle.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: Color–color diagrams of the detected X-ray sources with hardness ratio errors σ HR < 0.2. Identified fg stars, AGNs, and galaxies are plotted in the top panels ((a1), (a2), and (a3)), with the firmly identified ones plotted with filled circles and the candidates plotted with open circles. Identified GlCs, XRBs, and SNRs are plotted in the middle panels ((b1), (b2), and (b3)). All the sources detected in the present work are plotted in the bottom panels ((c1), (c2), and (c3)). The underlying false-color images are the probability distributions of the crossmatched sources between 4XMM-DR11s (Traulsen et al. 2020, 2022) and SIMBAD (top row: AGNs in blue, galaxies in green, fg stars in red; middle row: XRBs in blue, GlCs in green, and SNRs in red). The dotted contours enclose 68% of the crossmatched sources. We also overlay different power-law (in blue) and APEC (in red) models in the mesh grids. The colors of the thick solid curves denote N H, which changes from 0 to 3 × 1021 cm−2, with the three dashed curves marking N H = 0, 5 × 1020, and 3 × 1021 cm−2, respectively. The upper limit of N H is roughly consistent with the peak value in the M31 disk. When computing the models, the response files of PN, MOS1, and MOS2 are used for the top, middle, and bottom rows, respectively. The dashed–dotted lines show our criteria for classifying different types of objects (SSSs, “hard,” and “soft” sources; see Table 2 for details).
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: Left: the probability density function of the offset Δpos between XMM-Newton X-ray sources and Gaia optical sources at the different ranges of the position statistical uncertainty σ pos of the X-ray sources. The corresponding best-fit models are shown with dashed lines. The distributions have been shifted vertically for ease of comparison. Right: total position uncertainty σ combined as the function of σ pos. The σ combined is the σ of the Rayleigh distribution. The measured σ combined is shown with the black dots, while the red dashed line shows the best-fit model and the black dotted line represents the uncorrected σ pos.
Paper: An XMM-Newton View of the Andromeda Galaxy as Explored in a Legacy Survey (New-ANGELS). I. The X-Ray Source Catalog
Authors: Rui Huang, Jiang-Tao Li, Wei Cui, Joel N. Bregman, Xiang-Dong Li, Gabriele Ponti, Zhijie Qu, Q. Daniel Wang, Yi Zhang
Figure caption: The X-ray-to-IR flux ratio (X-ray flux is calculated in 0.2–12 keV, while the IR flux is the WISE 3.4 μm flux) and X-ray variability of different X-ray source populations. The symbols are the same as in Figure 4, except that the firmly identified LMXBs and HMXBs in the literature (not limited to M31; e.g., Zhang et al. 2011; Binder et al. 2015) are plotted with the plus and cross symbols. The vertical dashed–dotted line roughly separates fg stars and AGNs, while the horizontal dashed line defines “highly variable” sources, which is a key criterion for firmly identifying XRBs (Table 2).