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Emiliano Merlin with the ASTRODEEP consortium ADASS XXIV Calgary, Oct 8 th 2014 T-PHOT: Advanced techniques of precision photometry for present and future multiwavelength surveys

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INAF – OAR: A. Fontana, E. Merlin, R. Amorin, M. Castellano, P. Santini, K. Boutsia INAF – OABO: A. Comastri+ CEA – Saclay: D. Elbaz+ Univ. of Edinburgh: J. Dunlop+ STScI – Baltimore: H. Ferguson+ Immagine sito www.astrodeep.eu

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5 CANDELS fields + 4x2 FRONTIER fields FIR: Herschel MIR / NIR: Spitzer NIR / Opt / UV: HST, ground X: Chandra ASTRODEEP goal #1: Produce complete, up to date multiwavelength photometric catalogs of observed deep fields

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ASTRODEEP goals: 1) produce multiwavelength (FIR to X) catalogs on a wide set of fields; 2) set a “best” standard procedure, develop and publicly release the necessary software tools Main concern: confusion/blending/overlapping of sources at decreasing resolution and increasing wavelength T-PHOT (Merlin+2014, in prep.) : A code for PSF-matched photometric analysis of multiwavelength data using priors

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PSF-MATCHED MULTIWAVELENGTH PHOTOMETRY: BASIC METHOD k k = F‾¹ [F(PSF_LRI) / F(PSF_HRI)]

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TFIT (STScI – Papovich+ 1999, Laidler+ 2007): - C++ core (fitting) + Python envelop - 10,500 lines.py +.cc (plus external libraries) - Requires many external tools (Python modules, IRAF, etc.) - Cell fitting + Dithering; best flux chosen geometrically - 24 hours on a typical field (mostly because of Python slowness in preparation and post-fit stages) CONVPHOT (OAR – DeSantis+ 2007): - C - 4,200 lines.c (plus external libraries) - Single fit on whole image - No FFT convolution - 24 hours on a typical field (mostly because of pixels summation convolution and of fitting procedure) * Python envelop, C/C++ cores * Clearly organized in “stages” similarly to TFIT (with improvements) * Fast: ca. 30 mins. on a “standard” CANDELS field with TFIT parameters * Robust, and can handle large datasets with smart memory allocation * Only needs Python modules Numpy, Astropy and Matplotlib, plus CFITSIO and FFTW3 (no IRAF, STDAS, anfft) * Versatile: includes all different choices and methods already present in TFIT and CONVPHOT concerning smoothing (pixel summation or FFT), fitting (cells vs. single fit, three methods for matrix solving, threshold, clipping of negative sources, dance stage for kernel registration) * Includes a cells-on-objects method, which combines the computational efficiency of TFIT cells approach and the robustness of CONVPHOT single fit method * Can operate with three different types of priors: real 2-d cutouts from HRI, analytical models, or unresolved point-like sources T-PHOT (Merlin et al. 2014, in prep.)

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Real 2-d profile cutouts from HRI [catalog + HRI + segmentation] Analytical 2-d (multicomponent ) models, e.g. Galfit [catalog + FITS stamps] Unresolved point- like sources [catalog] Priors input Convolved templates Convolution kernel (and/or LRI PSF) LRI + RMS map Linear system minimization FLUX CATALOG + DIAGNOSTICS Measure input { - Options for matrix decomposition - Options for fitting - Options for enhancing the fit Locally registered kernels Uses WCS info to automatically compute image shifts (must be aligned and have integer pixel ratio)

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Left: simulated HRI (fwhm=0.2”). Right: simulated LRI (fwhm=1”) and residuals image [T-PHOT whole image fit using “real” priors]

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Left: simulated LRI (SPIRE). Right: residuals image [T-PHOT whole image fit using unresolved point-like priors]

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1 2 3 4 5 CELLS-ON-OBJECTS method: * One cell per object * Include all first order contaminants * Higher order contaminants are all included unless: - they are fainter than given fraction of the total flux of the central object (use the Detection image flux as a proxy) - OR they only overlap to the previous level contaminant with a small fraction of their total area * Once the central object is fitted, it is subtracted from the Measure image; catasptrophic contamination is excluded * NOTE: trying to keep fits for other “non central” objects in a given cell proves unsatisfactory

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1 2 3 5 CELLS-ON-OBJECTS method: * One cell per object * Include all first order contaminants * Higher order contaminants are all included unless: - they are fainter than given fraction of the total flux of the central object (use the Detection image flux as a proxy) - OR they only overlap to the previous level contaminant with a small fraction of their total area * Once the central object is fitted, it is subtracted from the Measure image; catasptrophic contamination is excluded * NOTE: trying to keep fits for other “non central” objects in a given cell proves unsatisfactory

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2 3 5 CELLS-ON-OBJECTS method: * One cell per object * Include all first order contaminants * Higher order contaminants are all included unless: - they are fainter than given fraction of the total flux of the central object (use the Detection image flux as a proxy) - OR they only overlap to the previous level contaminant with a small fraction of their total area * Once the central object is fitted, it is subtracted from the Measure image; catasptrophic contamination is excluded * NOTE: trying to keep fits for other “non central” objects in a given cell proves unsatisfactory

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Comparison of measured flux using single image fitting and cells-on-object method on the same simulated field

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ASSUMPTIONS, CAVEATS, ANALYSIS - PSF dependence - Prone to assumptions: – → no morphology dependence on wavelength (for real priors... how about multicomponent models?); no priors blending

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Comparison between residual images for an IRAC simulation. Left to right, top to bottom: Detection simulated image (HST F160W); Segmentation image; Measure simulated image (IRAC ch1); Residual images (TFIT with 100x100 pixels cells; TPHOT with 100x100 pixels cells, identical to TFIT; TPHOT 200x200 pixels cells; CONVPHOT; TPHOT with single cell fitting; TPHOT with adaptove-cells-on-objects fitting).

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Regions from UDS I band residual images. Left: TFIT “official” catalog; right: T-PHOT with cells-on-object method and revised kernel registration

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Euclid: T-PHOT vs. APERTURE PHOTOMETRY on simulated data

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HOW TO GET T-PHOT: http://www.astrodeep.eu/t-phot/ emiliano.merlin@oa-roma.inaf.it SUMMARY: - T-PHOT is fast, robust, versatile and accurate :) - Works fine on FIR to UV datasets, uses three types of priors - It is promising as the weapon of choice for future (large, demanding) surveys (… Euclid?)

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Spitzer pointings to Frontier Fields. Blue line: ACS, red line: WFC3

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Frontier Fields: Abell 2744 Parallel (HSTf814w, IRAC1, SExtractor segmetation and zoom)

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Frontier Fields: Abell 2744 (HSTf814w, IRAC1, SExtractor segmetation and zoom on cluster)

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Frontier Fields: Abell 2744 Possible approach: model sources (Galfit) and use models as priors

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Figure 5: Example of stacked images. Figure 6: Number count plot where the diamonds are the simulated data assuming no evolution from z=3-4 to z=5 and.

Figure 5: Example of stacked images. Figure 6: Number count plot where the diamonds are the simulated data assuming no evolution from z=3-4 to z=5 and.

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