adsabs/AstroCLIMB huggingface dataset:
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The correlations between the averaged line intensities (﹩{T}_{\mathrm{averl}{,}^{12}\mathrm{CO}}﹩ vs. ﹩{T}_{\mathrm{aver}{,}^{13}\mathrm{CO}}﹩), peak (﹩{W}_{\mathrm{peak}{,}^{12}\mathrm{CO}}﹩ vs. ﹩{W}_{\mathrm{peak}{,}^{13}\mathrm{CO}}﹩) and averaged (﹩{W}_{\mathrm{averl}{,}^{12}\mathrm{CO}}﹩ vs. ﹩{W}_{\mathrm{aver}{,}^{13}\mathrm{CO}}﹩) velocity-integrated intensities, and integrated fluxes (﹩{F}_{\mathrm{loc},{\ }^{12}\mathrm{CO}}﹩ vs. ﹩{F}_{{}^{13}\mathrm{CO}}﹩) of 12CO and 13CO emission toward the same areas where both 12CO and 13CO emissions are detected in each 13CO-detect. Each dot represents a single 12CO cloud with 13CO structures. The parameters of 12CO line emission are the physical parameters toward the 13CO-emitting regions within the 12CO clouds. The 13CO emission parameters are derived from all the 13CO structures inside a single 12CO cloud. The black lines show the linear least-squares fits to the data. The colors on the points show the distribution of the probability density function of the 13CO-detects’ counts (2D-PDF).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The number distributions of angular areas (﹩{{ \mathcal A }}_{{}^{12}\mathrm{CO}}﹩) and averaged velocity-integrated intensities (﹩{W}_{\mathrm{aver},{\ }^{12}\mathrm{CO}}﹩) of 12CO line emission for 12CO molecular clouds in near and far groups. The near 12CO clouds are in a velocity range of (−30 to 25) km s−1, and the far 12CO clouds are at (−95 to −30) km s−1. The green histograms represent 12CO molecular clouds not having 13CO structures (non-13CO-detects). The magenta ones are the 12CO molecular clouds having 13CO structures (13CO-detects).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The number distributions of angular sizes, mean velocity spans, integrated fluxes of 13CO line emission, and peak intensities of 13CO(1–0) line emission for the 13CO structures extracted by the three techniques. For clipping, extracted 13CO emission structures with a pixel in spatial scale or a velocity channel in velocity are determined as noise spikes and shown as blue histograms.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The number distributions of the angular areas (﹩{{ \mathcal A }}_{{}^{12}\mathrm{CO}}﹩), velocity spans (﹩{V}_{\mathrm{span},{\ }^{12}\mathrm{CO}}﹩), peak intensities (﹩{T}_{\mathrm{peak},{\ }^{12}\mathrm{CO}}﹩), and integrated fluxes (﹩{F}_{{}^{12}\mathrm{CO}}﹩) of 12CO line emission for 12CO molecular clouds with and without 13CO structures. The green histograms represent 12CO molecular clouds not having 13CO structures (non-13CO-detects). The magenta ones are the 12CO molecular clouds having 13CO structures (13CO-detects).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The distribution of the 13CO structure counts in a single 12CO cloud for the 13CO-detects in the near (left panel) and far (right panel) groups. In the top-right corner of each panel, a pie chart illustrates the percentages of 12CO clouds in this sample with one 13CO structure, two 13CO structures, and multiple (more than two) 13CO structures.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The count distributions (left panel) and cumulative fractions (right panel) of the ratios between the parameters of 13CO structures and those of 12CO line emission for the 2851 13CO-detects; these parameter ratios include the angular sizes (black), velocity spans (blue), peak intensities (cyan), and integrated fluxes (magenta).
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The number distributions of the angular sizes, velocity spans, total fluxes, and peak intensities of 13CO(1–0) and 12CO(1–0) line emission for the 2851 13CO-detects. The green histograms represent parameters of the 12CO line emission. The magenta ones are the parameters of the 13CO line emission.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The number distributions of the angular sizes, velocity spans, total fluxes, and peak intensities of 13CO(1–0) line emission for the 13CO-detects classified as filaments and nonfilaments.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: We show the distributions of the physical parameters (T eff, ﹩\mathrm{log}g﹩, [Fe/H], and [α/Fe]) in a set of paired diagrams and histograms for the full sample of 30k star spectra with good determinations of stellar properties (GSL+MaStarDR1, gray values), together with the 99% confidence regions (contours) of the adopted training (solid lines) and testing (dashed lines) subsets, corresponding to the GSL (blue) and MaStarDR1 (red) libraries. Clearly, GSL spans a wider range of stellar properties than MaStarDR1. See the text in Section 2.3 for details.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: Distributions of the internal precision of COSHA for each predicted property in the ﹩\mathrm{log}g﹩ vs. T eff plane. The contours represent the density distributions at the quartiles (solid lines) and 95th percentile (dashed lines). The map of the T eff precision (upper left) shows increasingly large imprecision toward higher temperatures. The ﹩\mathrm{log}g﹩ map (upper right) reveals more imprecise results for the coolest stars. Both the [Fe/H] and [α/Fe] maps (bottom panels) show increasing imprecision toward hotter and cooler stars. See the text in Section 4.2 for details.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: Similar to Figure 3, the joint distribution of the stellar parameters for MaStar, as estimated by COSHA. In light and dark purple, respectively, we show the original and volume-corrected distributions, as explained in Section 5.1. The contours are as in Figure 5. The corresponding average spectrum of the MaStar library and the volume-corrected one are shown in the inset axes. The inhomogeneity in the MaStar sampling of the parameter space becomes apparent: (i) T eff becomes flatter after correction; (ii) ﹩\mathrm{log}g﹩ is corrected for the undersampling of giant stars; and (iii) [Fe/H] and [α/Fe] become more biased toward solar abundance patterns. See the text in Section 5 for details.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: Spatial distributions of the MaStar stars (purple) in the [α/Fe] vs. [Fe/H] plane, segregated by the vertical distance to the MW disk plane, z. As a reference, we use the corresponding distribution for APOGEE–ASPCAP (gray). In the top panels, we compare only the matched subset of stars between the two surveys, and in the bottom panels we compare the trends found in the full samples for both surveys. In the top panels, it is appreciated that MaStar and APOGEE are statistically indistinguishable from each other, for any vertical distance. The full samples are still compliant, despite the larger scatter in MaStar, with the expected trends: stars become more Fe-poor and α-enhanced toward the thick disk, while stars with solar abundances dominate in the thin disk. See the text in Section 5.3 for details.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: Similar to Figure 6, but comparing our estimates to those derived by the APOGEE spectral analysis pipeline (ASPCAP). The systematic discrepancies with APOGEE are larger than those found with MaStarDR1. In summary, COSHA predicts systematically cooler stars, more dwarf stars, and marginally Fe-poorer stars than APOGEE, with essentially no bias in the [α/Fe] estimates. See the text in Section 4.4 for details.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: The spatial distribution of the MaStar stars in the cleaned sample (purple) compared to that of Gaia DR2 (orange). Top panel: the distribution in R.A. (RA) and decl. (DEC) shows the inhomogeneous spatial sampling of MaStar. Bottom panels: the distribution of MaStar in the galactic projections x–y (left) and x–z (right), demonstrating that MaStar extends well beyond the solar neighborhood. The plots in the bottom panels were generated using the Python package https://pypi.org/project/mw-plot/0.3.0/.
Paper: CoSHA: Code for Stellar Properties Heuristic Assignment—for the MaStar Stellar Library
Authors: Alfredo Mejía-Narváez, Gustavo Bruzual, Sebastian. F. Sánchez, Leticia Carigi, Jorge Barrera-Ballesteros, Mabel Valerdi, Renbin Yan, Niv Drory
Figure caption: CMDs of the MaStar library (left), Gaia DR2 (middle), and the volume-corrected version of MaStar (right) are shown. The similarities in the shapes of the middle and right distributions show that the volume correction is accurate.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Upper panels: The mean spectrum of 12CO (black) and 13CO (magenta) spectral lines along the boundaries of 13CO structures extracted in the molecular cloud G139.73 by clipping at cutoff levels of 2σ, 3σ, 4σ, and 5σ. The 13CO spectral lines are from the raw chopped 13CO data cube without any clipping, as shown in Figure C2. The 12CO spectral lines are from the extracted 12CO cloud of G139.73. The Num in each panel is the number of spectra along the corresponding boundary. S/N is the ratio of the peak intensity to the noise rms for the averaged-boundary 13CO spectrum. Lower panels: The mean spectrum of the extracted 12CO cloud (blue) in Yan et al. (2021) and the mean spectrum of the 13CO structures (red) extracted by clipping at cutoff levels of 2σ, 3σ, 4σ, and 5σ. The vertical dashed lines illustrate the velocity span for the extracted 13CO structures within G139.73 by clipping at the corresponding cutoff levels of 2σ, 3σ, 4σ, and 5σ. All the 13CO spectra are multiplied by a factor of 3. The σ value is estimated from the raw data and is equal to 0.27 K.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Comparisons among the integrated intensity ratios between 13CO and 12CO lines (W(13CO)/W(12CO)). The colored points show the average or median values of W(13CO)/W(12CO). The error bars on the individual points reflect the distributions for the ratios. From left to right, we present the literature results of W(13CO)/W(12CO) in local regions of the Milky Way and in nearby galaxies. W(13CO)/W(12CO), which is presented in Figure 12 of Torii et al. (2019), is calculated through the total velocity-integrated intensity of 13CO emission in a Galactic longitude of 1° divided by that of 12CO emission in the same bin. The presented values in this work are the ratio of the total integrated intensity of 13CO emission to that of 12CO emission in each molecular cloud. The W(13CO)/W(12CO) for Orion B is the mean integrated intensity of 13CO emission divided by that of 12CO emission, whose values are listed in Table 2 of Gratier et al. (2021). The values of W(12CO) and W(13CO) in Roman-Duval et al. (2016), Cormier et al. (2018), Gallagher et al. (2018), and Méndez-Hernández et al. (2020) correspond to their total luminosities in a Galactocentric radius bin, divided by the surface areas covered by the surveys in that bin, further projected onto the Galactic disk.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Top panel: The velocity-integrated intensity map of 13CO(1–0) emission in the near group. This map is derived by integrating the 13CO emission over the velocity range between −30 and 25 km s−1. The sensitivity for this velocity-integrated map is about 0.77 K km s−1. Bottom panel: The latitude-integrated intensity map of 13CO(1–0) emission in the near group. This map is derived by integrating the 13CO emission over the latitude range of −5.°25 to 5.°25.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The velocity-integrated intensity map (upper) and latitude-integrated intensity map (lower) of 13CO emission extracted within the 12CO cloud G139.73 using clipping at the cutoff level of 3σ (0.81 K). The white contours are the boundaries of the 12CO molecular cloud. The cyan contours are the determined boundaries of 13CO line emission.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The velocity-integrated intensity map (upper) and latitude-integrated intensity map (lower) of 13CO emission for the molecular cloud G139.73, which are derived by the raw chopped 13CO data cube without any clipping.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: Top panel: The velocity-integrated intensity map of 13CO(1–0) emission in the far group. This map is derived by integrating the 13CO emission over the velocity range between −95 and −30 km s−1. The sensitivity for this velocity-integrated map is about 0.83 K km s−1. Bottom panel: The latitude-integrated intensity map of 13CO(1–0) emission in the far group. This map is derived by integrating the 13CO emission over the latitude range of −5.°25 to 5.°25.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The distribution of the 13CO molecular structure counts in a single 12CO cloud for the 13CO-detects classified as nonfilaments (left panel) and filaments (right panel). In the top-right corner of each panel, a pie chart illustrates the percentages of molecular clouds in this sample with one 13CO molecular structure, two 13CO molecular structures, and multiple (more than two) 13CO molecular structures.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The velocity-integrated intensity map (upper) and latitude-integrated intensity map (lower) of 12CO emission for the molecular cloud G139.73, which are derived by the raw chopped 12CO data cube without any clipping.
Paper: Molecular Gas Structures Traced by 13CO Emission in the 18,190 12CO Molecular Clouds from the MWISP Survey
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Xunchuan Liu, Shaobo Zhang, Yan Sun, Xin Zhou, Qing-Zeng Yan, Yuehui Ma
Figure caption: The distribution of the background noise rms in the second Galactic quadrant with 104.°75 < l < 150.°25 and ∣b∣ < 5.°25.
Paper: The DECam Local Volume Exploration Survey Data Release 2
Authors: A. Drlica-Wagner, P. S. Ferguson, M. Adamów, M. Aguena, S. Allam, F. Andrade-Oliveira, D. Bacon, K. Bechtol, E. F. Bell, E. Bertin, P. Bilaji, S. Bocquet, C. R. Bom, D. Brooks, D. L. Burke, J. A. Carballo-Bello, J. L. Carlin, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, W. Cerny, C. Chang, Y. Choi, C. Conselice, M. Costanzi, D. Crnojević, L. N. da Costa, J. De Vicente, S. Desai, J. Esteves, S. Everett, I. Ferrero, M. Fitzpatrick, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, W. G. Hartley, D. Hernandez-Lang, S. R. Hinton, D. L. Hollowood, K. Honscheid, A. K. Hughes, A. Jacques, D. J. James, M. D. Johnson, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, C. Lidman, H. Lin, M. March, J. L. Marshall, D. Martínez-Delgado, C. E. Martínez-Vázquez, P. Massana, S. Mau, M. McNanna, P. Melchior, F. Menanteau, A. E. Miller, R. Miquel, J. J. Mohr, R. Morgan, B. Mutlu-Pakdil, R. R. Muñoz, E. H. Neilsen, D. L. Nidever, R. Nikutta, J. L. Nilo Castellon, N. E. D. Noël, R. L. C. Ogando, K. A. G. Olsen, A. B. Pace, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, J. Prat, A. H. Riley, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, M. Sako, J. D. Sakowska, E. Sanchez, F. J. Sánchez, D. J. Sand, L. Santana-Silva, B. Santiago, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, J. D. Simon, M. Smith, M. Soares-Santos, G. S. Stringfellow, E. Suchyta, D. J. Suson, C. Y. Tan, G. Tarle, K. Tavangar, D. Thomas, C. To, E. J. Tollerud, M. A. Troxel, D. L. Tucker, T. N. Varga, A. K. Vivas, A. R. Walker, J. Weller, R. D. Wilkinson, J. F. Wu, B. Yanny, E. Zaborowski, A. Zenteno
Figure caption: (Top) Offset in the stellar locus (r − i) color at (g − r) = 0.7 fit in each nside=128 HEALPix pixel relative to the DES value of (r − i)DES = 0.221 mag. Offsets in this distribution at large spatial scales are likely due to changing stellar populations. (Middle) Polynomial fit to the (r − i) offset map smoothed with a σ = 5° Gaussian kernel. (Bottom) Map of residuals after the polynomial fit has been subtracted. This residual map highlights variations in the location of the stellar locus at smaller scales and is an estimate of the color uniformity.
Paper: The DECam Local Volume Exploration Survey Data Release 2
Authors: A. Drlica-Wagner, P. S. Ferguson, M. Adamów, M. Aguena, S. Allam, F. Andrade-Oliveira, D. Bacon, K. Bechtol, E. F. Bell, E. Bertin, P. Bilaji, S. Bocquet, C. R. Bom, D. Brooks, D. L. Burke, J. A. Carballo-Bello, J. L. Carlin, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, W. Cerny, C. Chang, Y. Choi, C. Conselice, M. Costanzi, D. Crnojević, L. N. da Costa, J. De Vicente, S. Desai, J. Esteves, S. Everett, I. Ferrero, M. Fitzpatrick, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, W. G. Hartley, D. Hernandez-Lang, S. R. Hinton, D. L. Hollowood, K. Honscheid, A. K. Hughes, A. Jacques, D. J. James, M. D. Johnson, K. Kuehn, N. Kuropatkin, O. Lahav, T. S. Li, C. Lidman, H. Lin, M. March, J. L. Marshall, D. Martínez-Delgado, C. E. Martínez-Vázquez, P. Massana, S. Mau, M. McNanna, P. Melchior, F. Menanteau, A. E. Miller, R. Miquel, J. J. Mohr, R. Morgan, B. Mutlu-Pakdil, R. R. Muñoz, E. H. Neilsen, D. L. Nidever, R. Nikutta, J. L. Nilo Castellon, N. E. D. Noël, R. L. C. Ogando, K. A. G. Olsen, A. B. Pace, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, J. Prat, A. H. Riley, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, M. Sako, J. D. Sakowska, E. Sanchez, F. J. Sánchez, D. J. Sand, L. Santana-Silva, B. Santiago, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, J. D. Simon, M. Smith, M. Soares-Santos, G. S. Stringfellow, E. Suchyta, D. J. Suson, C. Y. Tan, G. Tarle, K. Tavangar, D. Thomas, C. To, E. J. Tollerud, M. A. Troxel, D. L. Tucker, T. N. Varga, A. K. Vivas, A. R. Walker, J. Weller, R. D. Wilkinson, J. F. Wu, B. Yanny, E. Zaborowski, A. Zenteno
Figure caption: (Left) Distribution of PSF magnitude limits for pointlike sources at S/N = 5. The double-peaked structure in r band comes from the different exposure times used in DES and DECaLS. (Right) DELVE DR2 survey area in each band as a function of the limiting PSF magnitude (S/N = 5). These distributions look similar when calculated from the mag_auto limiting magnitude for all sources, but are shifted brighter by ∼0.4  mag.