adsabs/AstroCLIMB huggingface dataset:
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Drawings reporting the observation of the transit of Mercury over the solar disk on 1868 November 5 (top) and of the solar eclipse that occurred on 1867 March 6 (bottom).
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Examples of drawings made by Secchi (left) and his close collaborator Lais (right) on 1871 May 9. The top panels show the full-disk drawing made by the two observers. The lower panels show enlarged areas around group #98 to highlight the different techniques in drawing sunspots by the two observers.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Examples of drawings made prior to 1858 December, reporting the results of the solar observation performed on 1857 May 17 (left) and 1858 January 11 (right).
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Number of solar full-disk observations per year in the collection. Number of days per year with group counts (either from full-disk drawings or annotations; black), number of days per year with information on group counts in annotations (yellow), total number of drawings (dashed green), number of drawings of enlarged regions (dashed light blue), and number of images that included enlarged regions within a full-disk drawing (red). The days with information on group counts are also expressed as the fraction of days within a year as shown in the right y-axis.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Example of a mask derived by recounting sunspot groups in Secchi’s drawing of 1870 June 30. The outermost green circle marks the solar disk, while each group is marked with a colored circle.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Infographic summarizing information about the instruments employed by Secchi (yellow boxes), the solar features reported in the drawings (green boxes), and Secchi’s assistants (blue boxes) over the period of 1850–1878. Find more details in Section 3.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: Examples of successful scene-modeling measurements for a few objects. The columns, from left to right for each object are: (1) a postage stamp of the data centered on the detection; (2) the best-fit model in Equation (2); (3) the difference between the data and the background portion of the model (i.e., without subtracting the model of the TNO itself); (4) the difference between the data and the point-source portion of the model (i.e., without subtracting the background model); and (5) the residuals of data minus the full model. The first row shows an example measurement of our brightest object, the magnitude m  r  ≈ 19.5 Eris.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: The best-fit β-distributions q(A) of the LCA for the marked subsets are plotted in the lower panels as solid lines, and the corresponding cumulative distributions are shown in the upper panels. The dotted lines are the posterior distributions for A of the observed sample when using these best-fit functions as priors. The agreement between the data and the β distributions is good, with larger deviations seen (as expected) in the samples with fewer members. The top axis converts our sinusoidal flux variation amplitude A into the peak-to-peak magnitude change of the light curve (under the sinusoidal assumption), for easier comparison to the literature. The upper axis only applies to the upper panels.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: The results of the modeling of the LCA and determination of mean flux and color are summarized for (612620) 2003 SQ317 (top), a source with well-characterized variability; and 2016 SD106 (bottom), a source consistent with no variability. For each source, the upper panel plots the measured fluxes over the 6 yr of the survey, in particular the flux variation ﹩f/{\overline{f}}_{b}﹩ relative to the mean flux in each band. The bottom panels for each object shows histograms of the MCMC samples drawing from the inferred posterior probabilities of the absolute magnitude H  r  (left), the LCA A (middle), and the colors (right) for the object. The horizontal band in the relative-flux figure and the dashed line in the LCA figure for (612620) 2003 SQ317 show the light curve peak-to-peak amplitude measured by Lacerda et al. (2014). Our method underestimates the LCA, likely because the true light curve is not sinusoidal. The vertical bands in the 2016 SD106 color histograms show the 68% limits from Chen et al. (2022), which are in good agreement with our inferred colors.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: For each of six disjoint subsamples of TNOs described in Table 2, the top plot shows their 68% and 95% posterior credible regions of the ﹩(\bar{A},s)﹩ distribution parameters as used in Equation (17). The maximum posterior likelihood of each is marked with an “X.” The bottom panel projects these posterior distributions onto the single parameter ﹩\bar{A}﹩ that gives the mean of the inferred distribution of noiseless LCAs for that population. It is immediately clear that larger TNOs (Big) with H  r  < 6 are less variable than the smaller members of all of the dynamical populations, with the possible exception of detached TNOs. Furthermore, the hot classicals (HCs) are less variable than the cold classicals (CC), with the resonant population being consistent with either and our constraints on the scattering population being weaker. Detached TNOs are also decisively less variable than resonant or scattering TNOs in the same H  r  range.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: Same columns as in Figure 1, but the four examples show failures of the scene-modeling procedure. The first row shows a case where the TNO (with a small expected S/N) was near an extended background galaxy with a much more significant flux contribution. This example is remarkable because, even though there is no usable photometry for the TNO, the model reproduces the spiral structure of the galaxy really well, leading to a near perfect subtraction. The second row shows a similar case of a bright background source near the TNO, but in this case the model failed to reproduce this background. The third row corresponds to a bright source near the edge of the stamp, with its scattered light precluding any photometric measurement nearby. The final row is a rare case where the least-squares procedure of Equation (3) led to an incorrect solution (namely, the model predicts a large negative flux for the central point source), possibly due to excess noise fluctuations in the background and the low S/N of the target source.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: Δχ 2 between the single source and binary models vs. S/N of the fainter source for a randomly chosen subset of 10% of the ≈25,000 photometric measurements (in gray) in the DES data. The two binary objects are shown with different colors, and the acceptance region is shaded in yellow. The other cases of objects where the binary fit yields a statistically significant improvement in the χ 2 arise when there is a poorly subtracted background object in the single-source fit, or when the binary fitting corrects small errors in the assumed pixel position of the primary object caused by atmospheric turbulence.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption: Single (upper row of each object) and binary (bottom row) point-source scene-modeling photometry applied to the same detections of two high-confidence binary TNOs identified in the DES data. In the first case (Δχ 2 = 130.6), a distinct quadrupole pattern is present in the residual image, a strong indication that this source is a binary. The second object (Δχ 2 = 12.8), while less visually apparent, is statistically significant across several images.
Paper: Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
Authors: Pedro H. Bernardinelli, Gary M. Bernstein, Nicholas Jindal, T. M. C. Abbott, M. Aguena, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. E. S. Pereira, T. M. Davis, S. Desai, H. T. Diehl, P. Doel, S. Everett, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, A. Palmese, A. Pieres, A. A. Plazas Malagón, M. Raveri, E. Sanchez, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, P. Wiseman, Y. Zhang
Figure caption:  g − r (blue), r − i (red), i − z (green), and g − i (purple) colors and corresponding uncertainties measured from sequential exposures of each component of the 2014 LQ28 system. The dashed gray diagonal line corresponds to the regime where the colors are equal in both members. The colors scatter around this diagonal line, and are all within 3σ of the nominal identity, implying that each member has the same colors (and therefore, similar surface composition).
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption:  The Farmer provides detailed statistics to readily select problematic sources such as blends, poor model fits, and artifacts that are difficult to identify from χ 2 alone. The red, yellow, and green sources are well fit with a small variation in negative and positive flux. The cyan source contains features not well described by our smooth model profiles, the blue source is an unidentified blend, and the purple source is a point-source model assigned to a resolved galaxy. Each of these six sources is selected from unique regions of a 3D statistic space (left). Each statistic is measured within the residual segment pixels of each source and includes the χ 2, the median χ distribution μ(χ), and the standard deviation of the χ distribution σ(χ). χ 2 and σ(χ) are closely related; gray curves indicate the allowed regions of the joint distributions. The colored histograms show their observed distributions while solid curves indicate expectation: 〈χ 2〉 = 1, μ(χ) = 0, and σ(χ) = 1.
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption: Example of a decision tree process for a group containing two identified sources. The input z-band image is shown in the top left with colored ellipses around the two detected objects beside the final residual constructed from subtracting the best model determined by The Farmer. Shown rightward are the residuals and models for two of the three tiers in the decision tree from which the best model types were determined. This particular pair of sources satisfied the decision tree before reaching the CompositeGalaxy in tier (3). While model images are scaled by ﹩{\mathrm{log}}_{10}﹩ to highlight morphologies, the science image and residuals are scaled to ±3σ to highlight faint signal and any oversubtraction.
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption: Schematic of the three-tiered decision tree used by The Farmer to determine the most suitable model type for a given source. The five models are tested in order of increasing number of parameters. Values shown are examples, and should be configured by the user to suit their data set.
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption: Eight similarly bright point sources are injected into a simulated noise field over six scenarios of increasing degrees of circularly symmetric crowding. Assuming source positions are known beforehand, fluxes are measured in four ways: 2″ apertures, profile-fitting each source independently, profile-fitting each source with successive model subtraction, and jointly fitting all models simultaneously. The degree of success of each method is shown on the right measured in the difference in magnitude Δmag between the input and measured magnitudes as a function of source crowding, with a median Δmag and 68% ranges indicated for each scenario. Only joint fitting provides both precise and accurate recovery of crowded sources.
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption: Example of results from forced photometry for the brightest source in Figure 3 measured in i and channel (2). The image of each band is shown next to the best-fit model from The Farmer. Brightness contours and principal axes are overlaid on the model in blue. The residuals are shown ±3σ (same as the image) to highlight faint signal and any over subtraction. The rightmost panel shows the per-pixel χ image scaled ±3 computed within the bounds of source segment; bottom rows for each band show a wire-mesh representation of the PSF profile; slices although the source (black), best-fit model (red), and residual (green); and the distribution of χ values over the group pixels on expectation should be normally distributed. The median and 68% range of the distribution is shown for illustration.
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption: Fraction of unresolved (resolved) sources correctly assigned an unresolved (resolved) model by The Farmer as a function of apparent i-band magnitude is shown by the solid green curve, and broken down into resolved and unresolved subsets by the dashed and dotted curves, respectively. The in recovery fraction at i ∼ 25 is expected as sources at that brightness are typically only marginally resolved and so challenge the decision tree. We consider only sources with χ 2 < 3 in the i band as they are considered reliable, the fraction of which is shown by the gray dashed curve. Our simulated field at i > 25 uses mostly pointlike sources to reflect real conditions in a COSMOS-like survey; the total resolved fraction is shown by the solid gray curve.
Paper:  The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys
Authors: J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Figure caption: Results of forced photometry by The Farmer on simulated fields of depths similar to COSMOS. Sources are izK  s -detected and modeled on i, z, and K  s  jointly, then forced on other bands including channel (1). Models can be compared to input images in the two leftmost panels in ﹩{\mathrm{log}}_{10}﹩ scaling where morphology is visible. Insets show a zoom-in of a smaller region. Residuals can be compared to input images in the two rightmost panels in ±3σ scaling to highlight faint signal above (black) and below (red) the background. While some sources were skipped as they were too complex, other notable oversubtractions are driven by blends and/or injected sources that are not well-described by the five model types.