TFIT: A Photometry Package Using Prior Information for Mixed‐Resolution Data Sets

By V. Laidler, C. Papovich, Norman Grogin, R. Idzi, Mark Dickinson, H. Ferguson, B. Hilbert, K. Clubb, S. Ravindranath. 2007

158 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Ecology

View Paper: https://www.semanticscholar.org/paper/ae57c6f03a5faeb0df7307f9583f957ea06728bb

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Citations in the corpus

The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field (2014, methodology): “We refer the reader to Laidler et al. (2007), Lee et al. (2012) and the citations within for further details of the TFIT process and the improvements gained on mixed wavelength photometry.”
COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs (2021, methodology): “Of recent popularity are prior-based techniques (e.g., De Santis et al. 2007; Laidler et al. 2007; Merlin et al. 2016) which use the highest resolution image as a prior, convolve it with the corresponding PSF kernel of the lower resolution images and utilize the normalization of the PSF convolved…”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, methodology): “In past works using TFIT (e.g. Laidler et al. 2007), this region was defined by the SExtractor segmentation map.”
GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z ∼ 2 (2011, methodology): “We use a catalog of z-band selected objects with photometry in all of the optical-NIR bands measured using TFIT (Laidler et al. 2007).”
A CENSUS OF STAR-FORMING GALAXIES IN THE Z ∼ 9–10 UNIVERSE BASED ON HST+SPITZER OBSERVATIONS OVER 19 CLASH CLUSTERS: THREE CANDIDATE Z ∼ 9–10 GALAXIES AND IMPROVED CONSTRAINTS ON THE STAR FORMATION RATE DENSITY AT Z ∼ 9.2 (2012, methodology): “Fortunately, there are well-established procedures to use the positions and spatial profiles of sources in available HST observations to model the IRAC image observations and extract fluxes (e.g., Shapley et al. 2005; Labbé et al. 2006; Grazian et al. 2006; Laidler et al. 2007).”
THE EVOLUTION OF THE GALAXY STELLAR MASS FUNCTION AT z = 4–8: A STEEPENING LOW-MASS-END SLOPE WITH INCREASING REDSHIFT (2015, methodology): “Another source of uncertainty is that TFIT/t-phot assumes no morphological k-corrections (no variation in the surface profile or morphology) between short- and longwavelength images, which is likely not the case (although we attempted to mitigate this by using the reddest HST image as our high-resol”
GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 < z < 2 FROM THE S-COSMOS SURVEY (2009, methodology): “However, we caution the reader that specific software like CONVPHOT (De Santis et al. 2006) or TFIT (Laidler et al. 2007) could provide flux measurements less affected by the confusion by using the K band image as a prior.”
The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “The authors rely on F160W images (∼1.6 µm) from the HST/WFC3 camera and extract IRAC sources using the software TFIT (Papovich et al. 2001; Laidler et al. 2007).”
The many flavours of photometric redshifts (2018, methodology): “AJ 144, 188 (2012) [100] Laidler V. G., et al. TFIT: A Photometry Package Using Prior Information for Mixed-Resolution Data Sets.”
THE NEWFIRM MEDIUM-BAND SURVEY: PHOTOMETRIC CATALOGS, REDSHIFTS, AND THE BIMODAL COLOR DISTRIBUTION OF GALAXIES OUT TO z ∼ 3 (2011, methodology): “Laidler et al. (2007) use the best-fit fluxes directly to calculate flux ratios (colors), whereas our method adds back in the residuals of the fit before performing aperture photometry.”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, methodology): “For the ground-based and IRAC bands, the catalog uses TFIT (Laidler et al. 2007) to measure photometry of these lower-resolution images using the HST WFC3 imaging as a high-resolution template for the galaxies.”
The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, methodology): “The ISAAC and IRAC photometry are measured using TFIT (Laidler et al. 2007) using the ACS z850 data as a prior for source positions.”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, methodology): “As has become stan- dard procedure (e.g., Shapley et al. 2005; Labbé et al. 2005, 2015; Grazian et al. 2006; Laidler et al. 2007; Merlin et al. 2015), we use the HST observations as a template to model the fluxes of sources in the Spitzer/IRAC observations and thus perform photometry below the…”
UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD (2015, methodology): “First, if the PSF FWHM’s are very different (by a factor of a few or more), then a template-fitting method is typically used to match a convolved galaxy ‘model’ to the measured flux (Laidler et al. 2007; de Santis et al. 2007).”
STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS (2014, methodology): “In brief, TFIT uses the a priori information on the source location and surface brightness profile on the F160W image to measure its photometry on the low-resolution image.”
THE MOST LUMINOUS z ∼ 9–10 GALAXY CANDIDATES YET FOUND: THE LUMINOSITY FUNCTION, COSMIC STAR-FORMATION RATE, AND THE FIRST MASS DENSITY ESTIMATE AT 500 Myr (2013, methodology): “HST imaging and convolving these to the IRAC PSF (see, e.g., Labbé et al. 2006; Grazian et al. 2006; Laidler et al. 2007).”
3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, unknown): “Like alternative methods such as TFIT (Laidler et al. 2007), our approach uses high-resolution images as priors to model sources in lower-resolution images.”
THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, methodology): “We utilized the TPHOT software (Merlin et al. 2015), an updated version of TFIT (Laidler et al. 2007), to model low-resolution images (IRAC images) by convolving HST imaging with empirically derived IRAC PSFs and simultaneously fitting all IRAC sources.”