Figure 6 from Dark Energy Survey Year 3 Results: Photometric Data Set for Cosmology

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Dark Energy Survey Year 3 Results: Photometric Data Set for Cosmology

Authors: I. Sevilla-Noarbe, K. Bechtol, M. Carrasco Kind, A. Carnero Rosell, M. R. Becker, A. Drlica-Wagner, R. A. Gruendl, E. S. Rykoff, E. Sheldon, B. Yanny, A. Alarcon, S. Allam, A. Amon, A. Benoit-Lévy, G. M. Bernstein, E. Bertin, D. L. Burke, J. Carretero, A. Choi, H. T. Diehl, S. Everett, B. Flaugher, E. Gaztanaga, J. Gschwend, I. Harrison, W. G. Hartley, B. Hoyle, M. Jarvis, M. D. Johnson, R. Kessler, R. Kron, N. Kuropatkin, B. Leistedt, T. S. Li, F. Menanteau, E. Morganson, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, C. Pond, M. Rodriguez-Monroy, J. Allyn Smith, K. M. Stringer, M. A. Troxel, D. L. Tucker, J. de Vicente, W. Wester, Y. Zhang, T. M. C. Abbott, M. Aguena, J. Annis, S. Avila, S. Bhargava, S. L. Bridle, D. Brooks, D. Brout, F. J. Castander, R. Cawthon, C. Chang, C. Conselice, M. Costanzi, M. Crocce, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, J. P. Dietrich, P. Doel, K. Eckert, A. E. Evrard, I. Ferrero, P. Fosalba, J. García-Bellido, D. W. Gerdes, T. Giannantonio, D. Gruen, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, E. M. Huff, D. Huterer, D. J. James, T. Jeltema, K. Kuehn, O. Lahav, C. Lidman, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, R. Miquel, J. J. Mohr, R. Morgan, E. Neilsen, A. A. Plazas, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, E. Suchyta, G. Tarle, D. Thomas, C. To, T. N. Varga, R. H. Wechsler, J. Weller, and R. D. Wilkinson

2021 The Astrophysical Journal Supplement Series 254 24.

Provider: AAS Journals

Caption: Figure 6.

Left: detection completeness for extended objects in the SN-X3 field (α, δ ∼36.°5, − 4.°5; approximately 3 deg² in area) in the i band, comparing three methodologies: using a deeper external data set (HSC-SSP DR2, ∼360 thousand matches to Y3 GOLD), the Deep Field catalog in that region, and simulations from Balrog processing, which inject realistic images onto co-added Y3 images. Similar agreement is obtained in other bands. Right: detection completeness for extended objects in the HSC-SSP W05 field (α ∼ 330°–360°, δ ∼ 0°; approximately 90 deg² in area of overlap) in the i band, comparing Y1 GOLD and Y3 GOLD vs. the Wide Field HSC-SSP DR2 data set (∼4.9 million matches to Y3 GOLD). Note that this region is wider and more representative of Y3 GOLD than the comparison shown in Figure 6(a) and is 0.23 magnitudes deeper. Errors are 95% containment errors computed using a Bayesian approach for efficiencies as detailed in Paterno (2004) but cannot be visualized as they are small compared to the data markers themselves. The black solid horizontal line represents the 90% level for visual reference.

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