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: Power spectra of the mean airmass and associated interpolated Balrog and Y3 GOLD galaxy count variations, as in Figure 12. The left panels show the angular power spectrum of the noted survey property (in green) and the corresponding power spectra of the number densities of the Balrog (in blue) and Y3 GOLD (in gold) MAGLIM-like galaxies across the Y3 footprint using the interpolated trends described in Sections 4.1.3 and 4.1.4. The reference CAMB nonlinear matter power spectrum in black is at z = 0.7 with a linear galaxy bias parameter of 1. The right panels show the difference in power between Y3 GOLD and Balrog as a fraction of the fiducial cosmological power spectrum shown on the left.
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: Power spectra of the mean exposure time and associated interpolated Balrog and Y3 GOLD galaxy count variations, as in Figure 12. The left panels show the angular power spectrum of the noted survey property (in green) and the corresponding power spectra of the number densities of the Balrog (in blue) and Y3 GOLD (in gold) MAGLIM-like galaxies across the Y3 footprint using the interpolated trends described in Sections 4.1.3 and 4.1.4. The reference CAMB nonlinear matter power spectrum in black is at z = 0.7 with a linear galaxy bias parameter of 1. The right panels show the difference in power between Y3 GOLD and Balrog as a fraction of the fiducial cosmological power spectrum shown on the left.
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: Power spectra of the mean PSF FWHM and associated interpolated Balrog and Y3 GOLD galaxy count variations, as in Figure 12. The left panels show the angular power spectrum of the noted survey property (in green) and the corresponding power spectra of the number densities of the Balrog (in blue) and Y3 GOLD (in gold) MAGLIM-like galaxies across the Y3 footprint using the interpolated trends described in Sections 4.1.3 and 4.1.4. The reference CAMB nonlinear matter power spectrum in black is at z = 0.7 with a linear galaxy bias parameter of 1. The right panels show the difference in power between Y3 GOLD and Balrog as a fraction of the fiducial cosmological power spectrum shown on the left.
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: Power spectra of the mean error on the gray zero-point correction and associated interpolated Balrog and Y3 GOLD galaxy count variations, as in Figure 12. The left panels show the angular power spectrum of the noted survey property (in green) and the corresponding power spectra of the number densities of the Balrog (in blue) and Y3 GOLD (in gold) MAGLIM-like galaxies across the Y3 footprint using the interpolated trends described in Sections 4.1.3 and 4.1.4. The reference CAMB nonlinear matter power spectrum in black is at z = 0.7 with a linear galaxy bias parameter of 1. The right panels show the difference in power between Y3 GOLD and Balrog as a fraction of the fiducial cosmological power spectrum shown on the left.
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: Power spectra of the mean sky brightness and associated interpolated Balrog and Y3 GOLD galaxy count variations, as in Figure 12. The left panels show the angular power spectrum of the noted survey property (in green) and the corresponding power spectra of the number densities of the Balrog (in blue) and Y3 GOLD (in gold) MAGLIM-like galaxies across the Y3 footprint using the interpolated trends described in Sections 4.1.3 and 4.1.4. The reference CAMB nonlinear matter power spectrum in black is at z = 0.7 with a linear galaxy bias parameter of 1. The right panels show the difference in power between Y3 GOLD and Balrog as a fraction of the fiducial cosmological power spectrum shown on the left.
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: Power spectra of the variance from the sky background and associated interpolated Balrog and Y3 GOLD galaxy count variations, as in Figure 12. The left panels show the angular power spectrum of the noted survey property (in green) and the corresponding power spectra of the number densities of the Balrog (in blue) and Y3 GOLD (in gold) MAGLIM-like galaxies across the Y3 footprint using the interpolated trends described in Sections 4.1.3 and 4.1.4. The reference CAMB nonlinear matter power spectrum in black is at z = 0.7 with a linear galaxy bias parameter of 1. The right panels show the difference in power between Y3 GOLD and Balrog as a fraction of the fiducial cosmological power spectrum shown on the left.
Paper: Give Me a Few Hours: Exploring Short Timescales in Rubin Observatory Cadence Simulations
Authors: Eric C. Bellm, Colin J. Burke, Michael W. Coughlin, Igor Andreoni, Claudia M. Raiteri, and Rosaria Bonito
Figure caption: Histogram (top) and normalized cumulative histogram (bottom) of the time gaps between visits to the same sky position for several representative LSST simulations and ZTF observations. Shaded regions highlight the 2–14 hr and 14–38 hr ranges for which we compute metrics (Table 1).
Paper: Give Me a Few Hours: Exploring Short Timescales in Rubin Observatory Cadence Simulations
Authors: Eric C. Bellm, Colin J. Burke, Michael W. Coughlin, Igor Andreoni, Claudia M. Raiteri, and Rosaria Bonito
Figure caption: Histogram (top) and normalized cumulative histogram (bottom) of the time gaps between visits to the same sky position in the same filter in the baseline_nexp1 simulation excluding the Deep Drilling Fields. Shaded regions are as in Figure 1.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: (A) Raw X-ray time-series data (0.1–0.8 nm). Minimum nominal values are scaled to 0. (B) Log scaled X-ray time-series data. (C) 3D visualization for five samples taken from the random split test data set.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: (A) M-class training data set visualization using the chronological split approach, 1 hr after an event. (B) M-class test data set visualization using the chronological split approach, 1 hr after. (C) M-class training data set visualization using the random split approach, 1 hr after. (D) M-class test data set visualization using the random split approach, 1 hr after.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: General classification deep CNN stack of layers. Red shows the convolutional kernel. Orange shows feature maps and activation function layer. Blue represents the pooling kernel. Green shows the pooling layers. Gray are fully conncected layers. The output tensor is passed through the softmax activation function and converted into a probability space.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: The suggested CNN architecture uses four convolutional layes with ReLU activation function, four max pooling layers, and one fully connected layer with softmax activation function.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: Random split approach for M-class vs. no-flare class data set. The number of events in the data set counts for 1772 (886 M-class events and 886 No-flare class events). Every row constitutes 144 hr of prprocessed X-ray data prior to an event, e.g., hour 145 (not included in the data set) is an M-class flare event (in case of an M-class label) or no-flare class event (in case of a no-flare label). In order to train the architecture for various time frames, we pulled 48 hr (our model input length) sequence data out of the 144 hr shifted by a prediction window, marked by different colors: blue shows the 1 hr prediction window prior to an event, orange shows the 3 hr prediction window prior to an event, green shows the 6 hr prediction window prior to an event, red shows the 12 hr prediction window prior to an event, purple shows the 24 hr prediction window prior to an event, brown shows the 48 hr prediction window prior to an event, pink shows the 72 hr prediction window prior to an event, and gray shows the 96 hr prediction window prior to an event.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: Validation loss graphs for all the 48 trained models. (A) Validation loss for eight different time prediction frames for X-class flare vs. no-flare event with random data split. (B) Validation loss for eight different prediction window frames for M-class flare vs. No-flare event with random data split. (C) Validation loss for eight different prediction window frames for M-class flare vs. no-flare event with chronological data split. (D) Validation loss for eight different prediction window frames for X-class flare vs. no-flare event with chronological data split. (E) Validation loss for eight different prediction window frames for M-class flare vs. X-class flare event with random data split. (F) Validation loss for eight different prediction window frames for M-class flare vs. X-class flare event with chronological data split.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: ROC curve visualization for different split type and classification model by hours before the event. (A) ROC curves for X-class solar flare event vs. no-flare event classification with random split. (B) ROC curves for X-class solar flare event vs. no-flare event classification with chronological split. (C) ROC curves for M-class solar flare event vs. no-flare event classification with random split. (D) ROC curves for M-class solar flare even vs. no-flare events classification with chronological split.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: Visualization for random and chronological split types metric evaluation. Left: metric evaluation for an X-class solar flare event vs. no-flare event classification model. Right: metric evaluation for an M-class solar flare event vs. no-flare event classification model.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: Statistical visualization for the different metrics by data split method using the box-chart method, where Q1 is the candle upper boundary (equal to −0.6745σ) and Q3 is the candle lower boundary (equal to 0.6745σ). (A) Metric statistics for an X-class solar flare event vs. no-flare event classification. (B) Metric statistics for an M-class solar flare event vs. no-flare event classification.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: M-class solar flare classifier model metric visualization comparison.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: X-class solar flare classifier model metric visualization comparison.
Paper: Low-dimensional Convolutional Neural Network for Solar Flares GOES Time-series Classification
Authors: Vlad Landa, and Yuval Reuveni
Figure caption: ROC curve graph of the distinguishing abilities of the models for X-class and M-class solar flares with different prediction time frames. Left: random data split trained and tested model ROC curve. Right: chronological data split trained and tested model ROC curve.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Schematic of the COSMOS field. The background image corresponds to the izYJHKs detection image. The solid lines represent survey limits, and the dashed lines indicate the deepest regions of the images. In the case of UltraVISTA, the dashed lines illustrate the “ultradeep” stripes. In the case of CLAUDS, the solid line shows the limit of the u-band image, and the dashed line shows the deepest region of the u*-band image.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Relative transmission curves for the photometric bands used. The effects of the atmosphere, telescope, camera optics, filter, and detector are included. The black curves represent medium and narrow bands. The profiles are normalized to a peak transmission of 1.0 for the broad bands, and to 0.3 for the medium and narrow bands.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Depths at 3σ measured in empty 3″ diameter apertures in PSF-homogenized images, except for NUV and IRAC images. The NUV depth is from Zamojski et al. (2007) and the F814W 3σ depth is derived from the 5σ value in Koekemoer et al. (2007). For the Y, J, H, and Ks bands, the depths in the ultradeep regions are indicated. The length of each segment is the FWHM of the filter transmission curve. The thin black segments show the depths of the medium and narrow bands. The gray segments indicate the depths of the images used in Laigle et al. (2016) for comparison.