ASCL.net

Astrophysics Source Code Library

Making codes discoverable since 1999

Searching for codes credited to 'Cullen, F.'

Tip: Author search checks name variants (e.g., Smith, John, Smith J). Last names are still best when results are broad.

Found 2 codes.

[ascl:1804.008] EGG: Empirical Galaxy Generator
Schreiber, C.; Elbaz, D.; Pannella, M.; Merlin, E.; Castellano, M.; Fontana, A.; Bourne, N.; Boutsia, K.; Cullen, F.; Dunlop, J.; Ferguson, H. C.; Michałowski, M. J.; Okumura, K.; Santini, P.; Shu, X. W.; Wang, T.; White, C.
The Empirical Galaxy Generator (EGG) generates fake galaxy catalogs and images with realistic positions, morphologies and fluxes from the far-ultraviolet to the far-infrared. The catalogs are generated by egg-gencat and stored in binary FITS tables (column oriented). Another program, egg-2skymaker, is used to convert the generated catalog into ASCII tables suitable for ingestion by SkyMaker (ascl:1010.066) to produce realistic high resolution images (e.g., Hubble-like), while egg-gennoise and egg-genmap can be used to generate the low resolution images (e.g., Herschel-like). These tools can be used to test source extraction codes, or to evaluate the reliability of any map-based science (stacking, dropout identification, etc.).
[ascl:2508.019] FiCUS: FItting the stellar Continuum of Uv Spectra
Saldana-Lopez, A.; Schaerer, D.; Chisholm, J.; Calabrò, A.; Pentericci, L.; Cullen, F.; Saxena, A.; Amorín, R.; Carnall, A. C.; Fontanot, F.; Fynbo, J. P. U.; Guaita, L.; Hathi, N. P.; Hibon, P.; Ji, Z.; McLeod, D. J.; Pompei, E.; Zamorani, G.
FiCUS (FItting the stellar Continuum of Uv Spectra) fit the stellar continuum of extragalactic ultraviolet (UV) spectra. The code takes observed-frame wavelength, flux density (with errors) and user-defined mask arrays as inputs, and returns an estimation of the galaxy stellar age, metallicity and dust extinction, as well as other secondary Spectral Energy Distribution (SED) parameters. FiCUS has two scripts; the first reads the INPUT file provided by the user and performs the fit according to selected options. It then gives the best-fit parameters and creates the OUTPUT files and figures. The second script includes pre-defined routines for spectral analysis, loading INPUT files and handling with data and models, as well as functions for the fitting routine, SED-parameters calculations and plotting, and imports functions into the first script.