adsabs/AstroCLIMB huggingface dataset:
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Solid lines show the numeric plasma temperature profiles as a function of optical depth at different shock radii, for R14 = 1 and v9 = 1. Analytic approximations for key temperature features that describe the profile are shown in dashed lines: the RMS temperature TRMS, Equation (20); the CLS temperature TCLS, Equation (21); the temperature to which upstream plasma is heated by the diffusing radiation TUS, Equation (22); and the thermal equilibrium temperature achieved in the dense shell TTE, Equation (23). The approximations for TUS and TTE are obtained using the numeric radiation temperature (see text).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Radiation hydrodynamics profiles at the CLS for ﹩{\tilde{r}}_{{\rm{sh}}}=6﹩, R14 = 1, and v9 = 1: density, velocity, plasma temperature, bolometric luminosity, bolometric radiation energy density, and radiation temperature, as functions of optical depth, normalized to their analytic shock values. The analytic CLS temperature and luminosity are given by Equations (21) and (17), respectively. The analytic radiation energy density profile is given by Equation (18) (dashed line). All profiles presented are nearly independent of ﹩{\tilde{r}}_{{\rm{sh}}}﹩, Rbo, and vbo, with the exception of the evolving radiation temperature (which is normalized by 1 keV), and of the thickness of the postshock hot layer (see text), which depends on the shock radius according to Equation (27).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Plasma density (upper panel) and velocity (lower panel) profiles as a function of optical depth at different shock radii (normalized by Equation (4), except the velocity, which is normalized to the piston velocity). At small shock radii, the radiation diffusing upstream accelerates the plasma to the postshock velocity. When the RMS approaches the breakout radius, the plasma is accelerated by the radiation diffusing upstream to a smaller velocity, ﹩{\rm{\Delta }}{\tilde{v}}_{{\rm{RMS}}}﹩ (see text) described analytically by Equation (19) (dashed line), and then further accelerated by ﹩{\rm{\Delta }}{\tilde{v}}_{{\rm{CLS}}}﹩ by the CLS.
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Plasma temperature profiles as a function of (normalized) optical depth, for ﹩{\tilde{r}}_{{\rm{sh}}}=6﹩, R14 = 1, and v9 = 0.5, 1, 2. For v9 = 1, we also show R14 = 0.1 and 10. Analytic approximations describe well the variations in TCLS, Equation (21), TUS, Equation (22), TTE, Equation (23), and τhot, Equation (27).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Radiation spectral energy density normalized to the bolometric energy density at different locations downstream, between the piston (red) and the shock (dark blue), for ﹩{\tilde{r}}_{{\rm{sh}}}=6﹩, R14 = 1, and v9 = 1. The shaded area represents the variation of the (energy-weighted) average photon energy, ﹩\mathop{\varepsilon }\limits^{\unicode{x00304}}﹩, defined in Equation (15).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Plasma density (upper panel) and velocity (lower panel) profiles as a function of optical depth at different shock radii, normalized to their breakout value. We present calculations for star radius R⋆ = 0.1 Rbo and mass M⋆ = 10 M⊙, which become independent of these parameters as the shock propagates beyond a few R⋆. The shock deceleration is then well fitted by Equation (36) (red dashed). During the RMS–CLS transition, the RMS velocity difference, ﹩{\rm{\Delta }}{\tilde{v}}_{{\rm{RMS}}}﹩, is described analytically by Equation (19) (black dashed).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: A CSM density profile with a finite RdCSM, similar to the one inferred from observations of the nearby SN 2023ixf (see Section 1.1 below), and the wind density profile considered in this paper. A qualitative discussion of the impact of a finite RdCSM is given in Section 5.
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Solid lines show the average photon energy at the shock ﹩{\bar{\varepsilon }}_{{\rm{sh}}}﹩ (energy weighted, Equation (15)) at ﹩{\tilde{r}}_{{\rm{sh}}}=10﹩ (left axis), and the “X-ray radius,” defined in the text (right axis), as a function of vbo. ﹩{\bar{\varepsilon }}_{{\rm{sh}}}(10)﹩ is insensitive to Rbo, with variations of the order of the plotted line width, and the X-ray radius is weakly sensitive to Rbo, with the shaded area representing a spread of 1013–1015 cm. ﹩{\bar{\varepsilon }}_{{\rm{sh}}}(10)﹩ is well described by Equation (38) (red dashed curve). Also shown in black dashed lines (corresponding to right axis): the shock radii beyond which there is negligible upstream X-ray absorption (by photoionization or Compton scattering, Equations (B7) and (B8)) beyond which there is electron–proton equipartition at the shock, Equation (C4).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Average photon energy (energy weighted, Equation (15)) emitted from the photosphere, normalized to ﹩{\bar{\varepsilon }}_{{\rm{sh}},{\rm{late}}}({\tilde{r}}_{{\rm{sh}}}=10)﹩ of Equation (38), as a function of photospheric time, defined by Equation (37), for R14 = 1 and v9 = 0.5, 1, and 2. For v9 = 1, we also show the results for R14 = 0.1 and 10 (dashed blue lines). The purple line shows the bolometric luminosity curve, normalized to L given by Equation (17), while the red dashed line is an analytic fit of a Crystal Ball function (see Equation (37) and the text following it). The black line shows the “X-ray time,” after which >1 keV photons compose a significant (>10%) part of the luminosity, where the black dots correspond to v9 = 0.6–2 with a step size of 0.2.
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: The equilibrium upstream plasma temperature Teq, obtained by numerically solving for the steady-state solution of Equation (B4), as a function of the photon energy εr of a monochromatic incident radiation, for ﹩\tilde{r}=3﹩ and v9 = 0.4. We also present the Compton–bremsstrahlung equilibrium, Equation (22) (with its limiting behaviors for  Tr higher or lower than Tc1), and the photoionization–bremsstrahlung equilibrium, Equation (B6). Tc2 separates regions where Compton or photoionization heating dominates.
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Spectral luminosity, Lε ≡ ∂L/∂ε, emitted from the photosphere, normalized to L given by Equation (17), at different photospheric times, defined by Equation (37). Results are shown for R14 = 1 and v9 = 0.5, 1, and 2.
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Solid lines show the peak plasma temperature at the CLS, obtained in numeric calculations with (“CL”) and without (“NCL”) a cooling limiter for various spatial grid resolutions, as a function of the optical depth ahead of the shock location, for R14 = 1 and a constant piston velocity v9 = 1. rsh/Δrsh is the ratio of the shock radius to the numeric spatial width of the shock. Black dashed lines show the analytic estimate for the peak temperature expected for different shock resolutions without a cooling limiter, Equation (A3). The red dashed line shows the analytic estimate of the CLS temperature, Equation (21).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Comparison of the radiation spectral energy density from dynamic and different static calculations, normalized to the bolometric energy density at the shock position, for ﹩{\tilde{r}}_{{\rm{sh}}}=6﹩, R14 = 1, and v9 = 0.5, 1, and 2 for constant velocity piston-driven shocks. Solid lines represent numeric calculations: dynamic calculation (blue), static calculation (i.e., No Hydrodynamics, orange), static calculation with only bremsstrahlung (yellow), and static calculation with only bremsstrahlung in the far downstream near the dense shell (purple). Dashed lines represent analytic approximations: the reprocessed component of thermal radiation (blue, Equation (23)) and bremsstrahlung cooling (magenta, Equation (28)).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Comparison of the radiation spectral energy density from static calculations, normalized to the bolometric energy density at the shock position, for ﹩{\tilde{r}}_{{\rm{sh}}}=2﹩, R14 = 1, and v9 = 1 for a constant velocity piston-driven shock. Solid lines represent static numeric calculations with varying optical depths (manually adjusted) for Compton scattering of the thermal radiation seeds emitted far downstream near the dense shell. Dashed lines represent analytic approximations: unsaturated Comptonization (red dashed, Equation (31)) and thermal radiation (blue, Equation (23)).
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: The convergence with spatial resolution (increasing by a factor of 2 between the different curve colors) of the radiation spectrum (right) and of the thermodynamic trajectory of the cooling plasma (middle) when using a cooling limiter as described in the text (results shown for the case of R14 = 1 and a constant velocity v9 = 1 piston-driven shock, at ﹩{\tilde{r}}_{{\rm{sh}}}=1﹩). While the spatial width of the hot plasma layer, which extends over ∼20 grid points, changes with resolution (left), the thermodynamic profiles and radiation spectrum converge.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: Unfolded spectra obtained from the first GTI of Exposure ID P061433801402, P061433802003, and P061433802703. Results from the spectral model (thcomp⨂diskbb+relxillCp) are shown in the left column, and those from the spectral model (diskbb+xillver) in the right column. In the left panels, the convolution component (thcomp⨂diskbb) is shown in purple, and the reflection component in sky blue. In the right panels, the diskbb, Compton, and reflection components are plotted in orange, purple, and sky blue. The LE, ME, and HE data are plotted in green, blue, and red, respectively. All spectra are rebinned for visual clarity.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: Temporal evolution of the QPO centroid frequency (upper panel) and fractional rms (lower panel). Red circles, green triangles, and blue squares represent data in the LE (2–10 keV), ME (10–30 keV), and HE (30–100 keV) bands, respectively. The transition from the normal state to the flare state is indicated by the dashed vertical line.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: Schematic of the potential coevolution geometry between the inner hot flow and the accretion disk. For clarity, only half of the accretion flow is depicted. The black hole is marked as a solid black circle, the inner hot flow is shown as a blue ellipse, and the accretion disk is colored brown.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: The QPO frequency as a function of (a) disk truncation radius and (b) covering fraction. The radius ﹩{R}_{{\rm{tr}}}﹩ is normalized by the gravitational radius Rg. The dashed curves represent the best-fitting results. The MJD is mapped to the colors of the points.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: The correlations between QPO frequency and (a) unscattered disk luminosity, (b) Compton luminosity, and (c) intrinsic disk luminosity during flare state. The MJD is mapped to the colors of the points. The dashed curves indicate the best-fit results.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: The fractional rms as a function of energy. The three observations are colored with sky blue, orange, and pink, respectively, corresponding to the highlighted regions in Figure 1. Labels indicate MJD, QPO frequency (Hz), and disk fraction fdisk.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: Key fitting parameters of thcomp and relxillCp, which are taken from the spectral fits in H. He et al. (2025). (a) The power-law photon index. (b) The electron temperature. (c) The covering fraction. (d) The ionization of the accretion disk. (e) The normalization of relxillCp.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: The correlations between QPO frequency and intercepted disk luminosity during the flare state. The MJD is mapped to the colors of the points. The dashed curve indicates the best-fitting result.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: Derived component luminosities in 0.01–1000 keV and the covering fraction cf based on the spectral model constant∗tbabs∗(thcomp⨂diskbb+relxillCp). The data points are taken from the spectral fits in H. He et al. (2025).
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: The correlation between QPO frequency and the unscattered disk, and Compton luminosity during the flare state. The MJD is mapped to the colors of the points. The dashed curves indicate the best-fitting results.
Paper: Temporal Evolution of Quasiperiodic Oscillations in an Accreting Black Hole Swift J1727.8-1613: Coevolution of the Disk–Corona during the State Transition
Authors: Sai-En Xu, Bei You, Yi Long, Han He
Figure caption: Derived component luminosities in 0.01–1000 keV based on the spectral model constant∗tbabs(diskbb+xillver).
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Top panels: comparison between the derived photometric metallicity values in this work and in spectroscopic work in the literature by M. A. C. de los Reyes et al. (2022; left) and E. Tolstoy et al. (2023; right). Median values and median absolute deviations (MMAGIC,  MR22,  and MT23) are indicated in the top-left corner of each panel. Bottom panels: difference between the [Fe/H]MAGIC and the spectroscopic estimates. MΔ[Fe/H] indicates the median value.
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Left panel: color–magnitude diagram with DECam g, r photometry of selected members (blue) and the complete field observed by our DECam pointings (gray) around the Scl dSph. A BaSTI isochrone with [Fe/H] = −1.8 and 12 Gyr is overlaid. Right panel: spatial distribution of selected members (blue) and the complete field (gray). The inner ellipse indicates the half-light radius for the Scl dSph galaxy (﹩{{\rm{r}}}_{{\rm{h}}}=11.1{7}^{{\prime} }﹩). Dashed ellipses mark 2 and 3 half-light radii. The outer ellipse covers 7 half-light radii, showing the extent of our data. The structural parameters used were obtained by R. R. Muñoz et al. (2018) assuming a Plummer profile.
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Top panel: metallicity uncertainties reported by the original works as a function of g0 magnitude for members observed by the MAGIC survey (blue points), and stars in common with M. A. C. de los Reyes et al. (2022, R22; yellow triangles) and with E. Tolstoy et al. (2023, T23; green squares). Bottom panel: normalized difference histograms comparing MAGIC estimates with R22 (yellow thick line) and T23 (green thin line). The gray curve illustrates a Gaussian function with mean μ = 0 and standard deviation SD = 1 for comparison.
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: A color–color plot of the MAGIC data on the Scl dSph galaxy (black data points), in which the y-axis color term includes the CaHK magnitude and the x-axis is the (g − i)0 color. Stars at different metallicities occupy different regions of this color–color space. To indicate this, we overplot as upside-down triangles synthetic photometry from the TSLTE grid (described in Section 3.1), fixing ﹩{\rm{log}}\,{\rm{g}}=2.0﹩. As seen by the color scale, stars at different metallicities separate into well-behaved trend lines.
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Comparison of photometric metallicities and spectroscopic metallicities from T23, separating the sample between stars with (bottom panel) and without (top panel) deblended photometry. Contours corresponding to nonblended sources are plotted over the deblended sample and vice versa. The color bar indicates the radial distance.
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Radial (top panel) and g0 magnitude distribution (bottom panel) for deblended stars (blue thick line) and nondeblended stars (gray thin line). The radial distribution is presented in units of half-light radius, using rh = 11.17′ for the Scl dSph galaxy (R. R. Muñoz et al. 2018).
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Difference between photometric metallicity and spectroscopic values, colored according to the measured carbon abundance for each star. The spectroscopic [Fe/H] values were obtained by E. Tolstoy et al. (2023) and the [C/Fe] values by A. Chiti et al. (2018).
Paper: The DECam MAGIC Survey: A Wide-field Photometric Metallicity Study of the Sculptor Dwarf Spheroidal Galaxy
Authors: F. O. Barbosa, A. Chiti, G. Limberg, A. B. Pace, W. Cerny, S. Rossi, J. L. Carlin, G. S. Stringfellow, V. M. Placco, K. Atzberger, J. A. Carballo-Bello, A. Chaturvedi, Y. Choi, D. Crnojević, A. Drlica-Wagner, A. P. Ji, N. Kallivayalil, C. E. Martínez-Vázquez, G. E. Medina, N. E. D. Noël, A. H. Riley, D. J. Sand, A. K. Vivas, C. R. Bom, P. S. Ferguson, B. Mutlu-Pakdil, M. Navabi, J. D. Sakowska, A. Zenteno
Figure caption: Panel (a): cumulative distribution function (CDF) as a function of half-light radius. The blue line indicates the data obtained with MAGIC observations, the yellow thick line with M. A. C. de los Reyes et al. (2022, R22), and the green thin line with E. Tolstoy et al. (2023, T23). Panel (b): comparison of the MDF for the different studies of the Scl dSph galaxy. Panel (c): comparison between photometric (MAGIC) and spectroscopic (T23) data for members in common. Panel (d): comparison between photometric (MAGIC) and spectroscopic (T23) data for members in common.