A JavaScript Passive Evolution Calculator When there is no new star formation, galaxies evolve “passively”, i.e., they redden and fade as stars turnoffof themain sequence. In principle,thisevolutioncan bemeasured by comparingthe mass-to-lightratios and colors of distantpassivelyevolving galaxies to thoseof nearby ones. The measured evolution can then be compared to predictions from stellar population syntesis models, todetermineages andotherparameters. Thistechniquehasbeenappliedsuccessfullytodeterminetheagesofearly-typegalaxiesinthe 5 0 fieldand clusters,outtoredshiftsz∼1.25(e.g., vanDokkum&Franx 1996;Treuetal.2002;van 0 der Wel et al. 2004). However, there is growing evidence that the number of early-type galaxies 2 is not stable with time, but decreases with redshift (e.g., Dressler et al. 1997; van Dokkum et al. n 2000; Bell et al. 2004). The implication of such complex evolution is that the sample of early- a J type galaxies at high redshift is a biased subset of the sample at z =0, containing only the oldest 2 progenitors of today’s early-types. This “progenitor bias” leads us to overestimate the ages of 1 today’searly-typegalaxies. 1 In van Dokkum & Franx (2001), we quantified the effects of progenitor bias on the observed v 6 luminosity and color evolution of early-type galaxies, and developed a simple model which can 3 providethebias-correctedagesofearly-typegalaxiesforanassumedrateofmorphologicalevolu- 2 1 tion. Here we present a JavaScript calculator for predicting the luminosity and color evolution of 0 passivelyevolvinggalaxies,basedon thevanDokkum& Franx (2001)parameterization. 5 0 / Simpleevolution h p In its simplest form, the calculator provides the evolution of a stellar population with a given - o luminosity-weightedformationredshift (“Default 1”). Figure 1 shows examples of theoutput, for r t astellarpopulationformedat z=6. s a : v i X r a Figure1: Exampleoutputforasinglestellarpopulation formedatz=6. 1 Complex evolution The calculator can also incorporate morphological evolution (i.e., progenitor bias) and complex star formation histories of individual galaxies. The calculator provides the luminosity evolution, scatter in luminosity, color evolution, scatter in color, the fraction of today’s early-type galaxies formedatagivenredshift,andtheluminosity-weightedstellarformationredshiftoftheearly-types atthatredshift. Theexamplebelowshowssomeoftheoutputfor“Default3”,amodelwithstrong morphologicalevolution. Figure 2: Model with strong morphological evolution. Although only ∼20% of present-day early-types wereinplacebyz=2,theluminosityevolutionisverysimilartothatinFig.1,andthescatterinV- K color issmallatallredshifts. Thesecounter-intuitive trendsareexplained invanDokkum&Franx(2001). Web location: www.astro.yale.edu/dokkum/evocalc/ Pleaserefer to vanDokkum&Franx (2001)ifyouusethiscalculator. Bell,E.,etal.2004,ApJ,608,752 Dressler, A.,etal.1997,ApJ,490,577 Treu,T.,Stiavelli,M.,Casertano, S.,M/oller, P.,&Bertin,G.2002, ApJ,564,L13 vanderWel,A.,Franx,M.,vanDokkum,P.G.,Rix,H.-W.2004,ApJ,601,L5 vanDokkum,P.G.,&Franx,M.1996, MNRAS,281,985 vanDokkum,P.G.,Franx,M.,Fabricant,D.,Illingworth, G.D.,&Kelson,D.D.2000,ApJ,541,95 vanDokkum,P.G.,&Franx,M.2001, ApJ,553,90 2