adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The distribution of eclipse separations in phase space. Eclipse separations serve as proxies for the tangential component of eccentricity, ﹩e\cos \omega ﹩.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The distributions of primary and secondary eclipse widths, and their correlation, derived from the polyfit and two-Gaussian models. Eclipse widths serve as proxies for the radial component of the eccentricity, ﹩e\sin \omega ﹩.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The TESS combined differential photometric precision (CDPP). The top panel depicts the measured CDPP with a 0.5 hr running average, in ppm. The second panel provides a crowding measure per target, i.e., the fraction of light in the aperture from the observed target. The third panel corrects the original CDPP for crowding: corrected CDPP = CDPP/crowding. This assumes that the contribution of background light does not vary with time, which may or may not be true. Depicted in blue are all observed targets, and in red are the EBs. The bottom panel is the flattened version of the previous panel, divided by the bottom envelope.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The number of EB targets (top) compared to all Sector 1 targets (bottom) as a function of flattened CDPP. Note the logarithmic y scale.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The distribution of TESS magnitudes for all 2 minute targets observed in sectors 1–26 (blue) and all 4584 EBs (amber).
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Detection frequency of EBs as a function of Galactic latitude. The frequency is computed by counting all detected 2 minute cadence EBs in a given 10° Galactic latitude strip and dividing the count with the number of all 2 minute cadence targets observed in the same strip.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The comparison of orbital period distributions from TESS, Kepler, and OGLE. All distributions are normalized by their surface areas for comparison purposes.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Examples of single-transit EBs, TIC 190630888 and TIC 198385324.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Distributions of the Gaia EDR3 brightness, color, distance, and RUWE for the eclipsing binaries in the catalog. The histograms are truncated on the right (and some on the left) for clarity.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The color–magnitude diagram in the Gaia passbands. The grayscale denotes the renormalized unit weight error (RUWE) parameter for ∼1 million Gaia EDR3 targets within ∼400 pc. Left: Gaia-only targets, with the piecewise linear line showing the fit to the lowest RUWE values. Right: TESS EBs plotted over Gaia targets; most EBs are displaced to the brighter, redder region of the CMD.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: EB sample in the color–magnitude diagram with theoretical evolutionary tracks spanning 1–10 solar masses and boxes indicating evolutionary states of particular interest (see, e.g., Belokurov et al. 2020), including white dwarfs (WD), hot subdwarfs (sd), extreme horizontal branch (EHB) stars, RS CVn systems, and a remarkably large number of bright giants (BGs; i.e., giant stars of intermediate mass).
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Galactic coordinates of each of the 460,000+ EB candidates found using a neural network on all TESS light curves up to 15th magnitude in sectors 1–26.
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 high-level overview of how the Deep Fields (DF) and Y3 image processing pipelines interact to create the Balrog catalogs. The raw DECam exposures are used as the basis for both tracts, with the much deeper DF data being represented by the larger image stacks. The null-weight images, weight maps, PSF models, and zero-point solutions are computed from the raw exposures after calibrations are applied and are the starting point of the sampled transfer function. The DF exposures are not dithered and thus single-CCD coadds are created in place of the much larger Y3 coadds. The fiducial DF catalog is created by fitting CModel profiles to detections with Multi-Object Fitting (MOF), which simultaneously models the light profiles of detected neighbors. These fitted model profiles (after a few limited cuts discussed in Section 3.4) are used as the Balrog injection catalog, which are added to the Y3 null-weight images directly. Afterwards, the injected null-weight images are processed in a nearly identical way to the real images including coaddition, detection, and photometric measurements. Finally, we match the output object catalog to truth tables containing the injected positions. As all sources are remeasured, there is some ambiguity in the matching; this is discussed further in Section 3.5. See Hartley et al. (2021) and Morganson et al. (2018) for further DF and Y3 pipeline details, respectively.
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: High-level overview of the injection processing for a single realization. Green boxes are inputs to the injection framework while red boxes are outputs. The length of each loop is determined by the number of exposures and tiles considered in the full simulation. While the main runs used for Y3 cosmology calibration modify only the position, orientation, and flux normalization of the truth inputs, there are many optional transformations that can be applied such as a constant shear or magnification. The main output of our injection package is a multidocument configuration file with detailed injection specifications that is then executed by GalSim, with each step being executed in the physically correct order. Additional realizations replicate all steps, other than the initial configuration parsing, and produce unique outputs.
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 series of plots highlighting aspects of the noiseless blank image test described in Section 2.3. (a) The first panel shows the difference in input bdf_fracdev vs. measured cm_fracdev for detected objects. The additional peak at 0.5 for bdf_fracdev is a result of the slightly different model definition; for bdf, the relative size ratio between the bulge and disk components is forced to be 1. This constraint does not exist for cm and thus it has a different prior on the parameter. (b) This panel shows the i-band magnitude response of these objects, where there are clearly two different populations. The first is well calibrated with the majority of detections well within ±2.5 mmag of the truth. The second population is biased toward fainter measurements by ∼7.5 mmag on average. (c) The g − r color response for these objects. The bias in recovered magnitude is nearly identical in griz and so does not translate to the recovered colors. The mean color response for g − r, r − i, and i − z is 0.1, 0.3, and 0.2 mmag, respectively. (d) The final panel shows that the biased magnitude population is a result of injections with input bdf_fracdev ∼ 0.5 scattering to 0 or 1 to match the expected cm_fracdev prior. As we do not believe this differential response to be of physical origin, it contributes to a lower bound on the precision in which Balrog can calibrate Δmag—though importantly this does not contribute a bias to recovered colors.
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 mean (solid circle) and median (hollow diamond) difference in measured vs. injected magnitude (〈Δmag〉) as a function of input magnitude for the final blank image runs with zero-mean Gaussian background noise. The vertical bars correspond to the mean of the standard deviations of griz magnitude responses in each truth magnitude bin, centered at the mean magnitude response. The vertical bars represent the average of the standard deviations of griz magnitude responses in each bin of size 0.5 mag, centered at the mean magnitude response. The overall calibration is excellent, with the median response less than 5 mmag in all bins except for g < 18.5 and 22.5 < z < 23. We expect significant biases past magnitude 23 due to selection effects near the detection threshold. However, the mean responses show some bias—particularly on the bright end. As discussed in the text, this is due to an asymmetric tendency for SOF to measure the fluxes of bright, extended galaxies to be too large when neighbors are contained in the object’s MEDS stamps. The errors in 〈Δmag〉 do not substantially decrease past input magnitudes of 20 for the same reason. This is discussed in greater detail in Section 4.3.1.