Presentation on theme: "(and especially Robert Lupton and Dustin Lang)"— Presentation transcript:
1(and especially Robert Lupton and Dustin Lang) DeblendingJim Boschfor Data Management(and especially Robert Lupton and Dustin Lang)
2There Will Be Blends LSST will go deep: LSST is on the ground: We’ll detect fainter objects.We’ll see the low surface brightness wings of everything.LSST is on the ground:Even under the best conditions, image quality won’t be as good as what we’d get from space
6Case 1: Unknown Unknowns If sources are so close we can’t tell they’re blended, there’s nothing the DM pipelines can do.Data from space could help, but using this will likely be Level 3.Mostly, we’ll have to deal with these statistically in the science analysis.
8Case 2: Known UnknownsWe believe there may be more than one source in a particular region.We want to measure the properties of the sources in as if they were isolated.Simultaneous model-fitting is one option, but it may not be the best one.Some popular measurements (e.g. aperture fluxes, image moments) require that we actually try to split up the pixels.We don’t have good models for some kinds of sources (e.g. galaxies).
9Deblending StarsThis is easy, if we have a good PSF model: just fit models simultaneously.Because stars (at any given epoch) are completely represented by positions and fluxes, there’s no need to do additional measurements.If we don’t have enough isolated stars to build a PSF model, we need a crowded field code.
10Deblending GalaxiesUnlike stars, we don’t have good models for galaxies.This is clearly bad new for bright, well-resolved galaxies.It might also be bad news for faint or poorly-resolved galaxies.
12The SDSS Deblender: Detection In each band, we smooth the image, then detect above-threshold regions (Footprints). We then grow these regions by the size of the smoothing kernel.Within each Footprint, we find one or more Peaks.SDSS
13The SDSS Deblender: Merging/Culling We compute the spatial union of all the Footprints from different bands, epochs, smoothing kernels.Within each Footprint, we merge all the Peaks from the different detection images, culling those that appear to represent the same source.
14The SDSS Deblender: Symmetric Templates true source profilespixel values 𝑧templates 𝑇For each Peak 𝑖 and pixel 𝑥, create a template 𝑇 𝑖,𝑥 that is the minimum of the pixel value 𝑧 𝑥 and its reflection about the peak 𝑧 ~𝑥 . Do a linear fit for the amplitudes 𝛼 𝑖 of all templates by minimizing: 𝑥 𝑧 𝑥 − 𝑖 𝛼 𝑖 𝑇 𝑖,𝑥 2 Compute deblended pixel values: 𝑧 𝑥,𝑖 ∗ = 𝛼 𝑖 𝑇 𝑖,𝑥 𝑧 𝑥 𝑗 𝛼 𝑗 𝑇 𝑗,𝑥residualsdeblended pixels 𝑧 ∗
16The SDSS Deblender: Heuristics If the dot product of any two templates is close to one, drop one of them.If a template looks a lot like the PSF model, use the PSF model as the template instead.Put limits on how sharp a template’s features can be.
17The SDSS Deblender: Measurement We call the outputs of the deblender HeavyFootprints: they’re Footprints that also hold the pixels of the deblended children.When we measure a source, we replace every other source’s Footprint with noise first.In addition to measuring the child sources, we also measure the parents (because we might have been wrong about it being a blend, or the deblender may have done more harm than good).
18Features of the SDSS Deblender We can run any measurement algorithm we can run on isolated sources.Flux is conserved as it is split up.No simple assumptions about galaxy morphology: not only is 180˚ rotation a weak constraint, it’s only enforced on the templates, not the deblended pixels.
19Weaknesses of the SDSS Deblender Only Peaks are shared between bands; no good way to generate reasonable templates for drop-out sources.No way to account for multiple epochs with different PSF.Doesn’t handle uncertainty rigorously.Vetted on a survey with a much less severe blending problem.
21Detection for LSST Detection will happen on multiple coadds: different bands (or weighted combinations of bands)different smoothings (i.e. morphological filters)...and difference images.We need to merge these detections in order to deblend consistently.We need to transfer the deblender outputs back to images with different bands, PSFs, WCSs, and observation dates.
22Going Multi-EpochWe can convolve templates derived in one band or image with a difference kernel to generate one appropriate for a different band or image.We can use point-source templates for drop-outs.We can use PSF-convolved analytic models as templates.
23...or Simultaneous Fitting? We’re going to use simple galaxy models for many of our most important measurements; do we gain anything (or lose anything!) by redistributing pixel flux using a more flexible model first?Can we make galaxy models flexible enough to make model biases unimportant?Flux redistribution with templates may still be useful as a starting point – it’s a lot faster than a high-dimensional nonlinear fit.
24More on Galaxy Modeling What should we let vary between bands?How flexible should models be?If they’re very flexible, how do we handle low SNR sources?Can we afford to sample rather than fit?If we need priors, where do they come from?Do we fit a star model and a galaxy model to everything?Come to the breakout session at 1:30pm today!
25Using Colors?There’s a lot more information in the spectral dimension that could be used in deblending.We don’t want to bias downstream algorithms (e.g. photo-zs) or make it less likely to find new and interesting objects that don’t have “normal” colors.
26SDSS functionality visit images simultaneous fitting final models coadditionimage subtractionpreliminary modelscoaddimagesreplace neighbors with noise, measuredifferenceimagesdetectSDSS functionalitydetectFootprints & Peaksgenerate templates, reapportion pixel fluxesFootprints & Peaksmerge/cullcoadd Heavy FootprintsFootprints & Peaks
27The LSST Prototype Deblender The LSST DM Stack includes a limited reimplementation of the SDSS Deblender.We don’t have any code for the peak merge/cull stage, so we can’t deblend across multiple bands in a consistent way.We don’t have some of the heuristics that were used in SDSS.
28What We Don’t Know Can Hurt Us The presence of a LRG affects the measurement of the properties of sources arcminutes away.This is because undetected galaxies cluster with the galaxies we do detect, and that upsets the measurement algorithms in a systematic way.Error in measurements of simulated galaxies injected into real data.Huff and Graves (2014)