adsabs/AstroCLIMB huggingface dataset:
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The distribution of differences in recovered the griz SOF CModel magnitude vs. the injected DF magnitude (ΔmagDF) as a function of input magnitude for the y3-deep sample. The density is overplotted where the contour lines correspond to the percentiles of the first three sigmas of a 2D Gaussian, containing 39.2%, 86.5%, and 98.9% of the data volume, respectively. The mean (solid), median (dotted), and standard deviation of the magnitude responses in bins of size 0.25 mag are shown in the overlaid black bars. These are compared to the reported SOF CModel errors by the solid white lines, which do not attempt to account for systematic effects. The marginal distributions of Δmagδ are included to highlight the small relative volume of the outlier tails.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: A few examples of injections that contribute to the long scatter tail in the magnitude response of bright y3-deep objects, due to the blending of extended DF injections discussed in Section 4.3.1. Each injection had a true g-band magnitude between 17 and 19, and we include the tile name and magnitude response Δm at the top of each panel. The red lines correspond to the 50th and 95th percentile flux contours of the measured profile. The extended profiles of these injections cause the MEDS image cutout size (based on the fitted SExtractor FLUX_RADIUS value) to be relatively large, which increases the probability of including real neighbors in the MEDS stamp. This in turn can cause SOF to significantly overestimate the cm_T size, which leads to a much larger Δm than one would naively expect for objects with these bright magnitudes. This is discussed further in Section 4.3.3. The final panel shows a typical bright but compact object that is very well calibrated for comparison. Note the presence of a nearby source in the bottom that could have potentially caused the same failure mode if the box size had been slightly larger. The stretch in each panel runs from −3σsky to +10σsky.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The distribution of differences in the measured SOF CModel g − r, r − i, and i − z color vs. the injected DF color (ΔcDF) as a function of input color for the y3-deep sample. The density is overplotted where the contour lines correspond to the percentiles of the first three sigmas of a 2D Gaussian, containing 39.2%, 86.5%, and 98.9% of the data volume, respectively. The mean (solid), median (dotted), and standard deviation of the magnitude responses in bins of size 100 mmag magnitude for g − r and r − i and 50 mmag for i − z are shown in the overlaid black bars.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The distribution of differences in the recovered i-band SOF CModel magnitude vs. the injected DF magnitude (ΔmagDF) as a function of input magnitude. The inset corresponds to the i-band panel in Figure 16 where the density contours still contain 39.2%, 86.5%, and 98.9% of the data volume, respectively. While most of the density is captured in the inset, it misses many of the rich features of the full magnitude response—particularly the long outlier tail of injections measured to have magnitudes up to 10 greater than truth. We explore some of the causes of this in Section 4.3.3.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The MEDS image cutouts for a few injection realizations of the same DF object with true r magnitude of 21.42 in eight distinct WF tiles (bal_id of 10034605248852). The red contours give the 50% and 95% enclosed light apertures for the injected object as modeled in each tile. The difference between the measured and injected magnitude Δm is listed next to each tile name, with the cutouts ordered by the magnitude response. The box sizes are in 0.″263 pixels. Not all cutouts are the same size, as the box size expands based on the initial SExtractor FLUX_RADIUS measurement. The true scale length of the object (after PSF deconvolution) is 0.″77. The fitted profile for the object on tile DES0149–4123 is 1.″0 and while that on tile DES0346–5248 is an unrealistic 17″, leading to an overestimate of the object flux corresponding to an error of 2.32 mag. The stretch in each panel runs from  −3σsky to +10σsky.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The MEDS image cutouts for eight Balrog objects with extremely large differences between the measured and injected magnitude Δm. The red lines correspond to the 50th and 95th percentile flux contours of the measured profile. These injections happened to be placed in regions of rapidly varying sky brightness, in the spiral arm of a large spiral galaxy, in a rich cluster, near a stellar diffraction spike, in between two extended galaxies, or simply in crowded fields. In all cases, the fitted size is far too large for the source, which in turn leads to an overestimate of the object’s flux. This process is discussed in detail in Section 4.3.3. The stretch in each panel runs from  −3σsky to + 10σsky.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The full i-band magnitude response ΔmagDF for y3-deep shown in Figure 19 but now colored by the logarithmic absolute error in recovered size parameter cm_T vs. input size bdf_T. The response scatter is largely correlated by error in recovered size; injections with small ΔmagDF values typically have small errors in recovered T as well (in blue), while nearly all of the extreme magnitude outliers have correspondingly large size errors. The correlation is less strong past the detection threshold at i ∼ 23 where other systematic effects increase in importance.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The efficiency (in blue) and contamination (in red) of the Balrog stellar sample (a) and galaxy sample (b). We use the δ injections of δ-stars as our population of true stars for (a) as it is a nearly pure sample, with only ambiguous matches as potential contaminates. We use the DF injections classified as galaxies from the DF k-nearest neighbor (knn) classifier described in Section 3.3 as our true galaxy sample, which has intrinsic uncertainty as detailed in Hartley et al. (2021). For (b), we cannot use the δ injections as the contamination measurement requires a realistic ratio of galaxy and stars sources in the sample so we instead use the classified DF stars. Each line corresponds to the fraction of objects above or below the noted EXTENDED_CLASS_SOF threshold value. We do not expect the galaxy efficiency to be 100% even at magnitudes where complete due to small impurities DF knn classifier.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The magnification bias from the boosted detection efficiency Csample estimated on samples with a uniform i-band flux magnitude limit. The Balrog estimates in blue use the magnified Balrog runs with a 2% magnification applied to every input object. The data estimate applies the same artificial magnification to the galaxy magnitudes in the data and reapplies the selection. The Balrog estimates of Csample are consistent with the flux-only estimates for this very simple selection, indicating that the contributions from additional selection effects are small. However, the Balrog Csample estimates are systematically lower than the simple data estimate for the real Y3 samples used in J. Elvin-Poole et al. (2021, in preparation), where the selections are significantly more complicated.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: Reproduced from Eckert et al. (2020), Figure 3. The Gaussian mean offset μ in the BFD flux moment pull distribution as a function of object density for the 48 used Balrog tiles in blue. The green points show the mean offset for the tiles after a local sky subtraction that mitigates the flux bias. While the g band is relatively unaffected, the redder riz bands show statistically significant sky oversubtraction that is correlated with object density.
Paper: Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog
Authors: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, and R. D. Wilkinson
Figure caption: The difference in measured CModel z-band magnitude vs. the injected DF magnitude ΔmagDF as a function of input magnitude for the high-density clusters run in a redshift range of 0.2–0.3. The three columns present the ΔmagDF responses binned by their radial distances to nearby cluster centers as specified at the top of the columns. The median response biases across the range of the injected magnitude are displayed as solid red lines, with the first and second ﹩{\sigma }_{{\mathrm{mag}}_{\mathrm{DF}}}﹩ contours indicated by the dashed lines above and below. As the injections approach the center of a cluster, the median bias becomes increasingly negative, indicating that the objects are measured to be progressively brighter than injected truth the closer they are to the bright central galaxy (BCG). In the three rows we color the magnitude responses as a function of (a) measured object size cm_T, (b) cluster richness, λ, and (c) the magnitude of the cluster’s BCG. The measured object size appears to have the strongest influence over magnitude bias among the three quantities, though richer clusters also show larger ΔmagDF responses. We use cm_T+1 for the color scale as the ngmix T sizes are allowed to be slightly negative. This preliminary analysis will be followed up in more detail in A. Masegian et al. (2021, in preparation).