Evolution of asymptotic giant branch stars. II. Optical to far-infrared isochrones with improved TP-

By P. Marigo, L. Girardi, A. Bressan, M. Groenewegen, Laura Silva, G. G. A. Department, P. University, Italy., Astronomical Observatory of Padova, -INAF and 7 more. 2007

1,277 citations recorded by the source corpus.

We present a large set of theoretical isochrones, whose distinctive features mostly reside on the greatly-improved treatment of the thermally-pulsing asymptotic giant branch (TP-AGB) phase. Essentially, we have coupled the TP-AGB tracks described in Paper I, at their stages of pre-flash quiescent H-shell burning, with the evolutionary tracks for the previous evolutionary phases from Girardi et al. (2000, AA the bell-shaped sequences in the Hertzsprung-Russell (HR) diagram for stars with hot-bottom burning; the changes of pulsation mode between fundamental and first overtone; the sudden changes of mean mass-loss rates as the surface chemistry changes from M- to C-type; etc. Theoretical isochrones are then converted to about 20 different photometric systems - including traditional ground-based systems, and those of recent major wide-field surveys such as SDSS, OGLE, DENIS, 2MASS, UKIDSS, etc., - by means of synthetic photometry applied to an updated library of stellar spectra, suitably extended to include C-type stars. Finally, we correct the predicted photometry for the effect of circumstellar dust during the mass-losing stages of the AGB evolution, which allows us to improve the results for the optical-to-infrared systems, and to simulate mid- and far-IR systems such as those of Spitzer and AKARI. We illustrate the most striking properties of these isochrones by means of basic comparisons with observational data for the Milky Way disc and the Magellanic Clouds. Access to the data is provided both via a web repository of static tables (http://stev.oapd.inaf.it/ dustyAGB07 and CDS), and via an interactive web interface (http://stev.oapd. inaf. it/cmd), which provides tables for any intermediate value of age and metallicity, for several photometric systems, and for different choices of dust properties.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/58be1ab5a2386e59694ff764045c7a5fbc1e2243

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Citations in the corpus

• A COMPACT DEGENERATE PRIMARY-STAR PROGENITOR OF SN 2011fe (2011, background): “The hydrogen main sequence, shown using solar-metallicity isochrones from Marigo et al. (2008), is excluded as the SN 2011fe primary.”
• Stellar Population Inference with Prospector (2020, methodology): “Isochrone libraries are available from the MIST (Choi et al. 2016), PARSEC (Bressan et al. 2012), BaSTI (Cordier et al. 2007), Padova (Marigo et al. 2008), Geneva (Meynet et al. 1994), and BPASS (Eldridge et al. 2017) models.”
• OBSERVING THE NEXT GALACTIC SUPERNOVA (2013, methodology): “To find the progenitor luminosity for a given mass, we rely on an interpolation of the Padova isochrones (Marigo et al. 2008), taking the progenitor luminosity to be the luminosity of the most massive star left on the isochrone.”
• THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME (2011, methodology): “…index of −1.30 over a mass range of 0.1 to 120 M⊙, a binary fraction of 0.35 with a flat secondary mass distribution, 71 equally spaced logarithmic time bins ranging from log t = 6.6–10.15, color and magnitude bins of 0.05 and 0.1 mag, and the Padova stellar evolution models (Marigo et al. 2008).”
• Metallicity gradients in disks - Do galaxies form inside-out? (2012, methodology): “…by deriving the absolute magnitude of each simulated star particle, making use of its age, metallicity, andinitial mass function, alongside the Marigo et al. (2008) isochrones.13 As expected from the Sánchez-Blázquez et al. (2011) analysis, the mean abundance shifted by∼0.1 dex depending…”
• THE APOKASC CATALOG: AN ASTEROSEISMIC AND SPECTROSCOPIC JOINT SURVEY OF TARGETS IN THE KEPLER FIELDS (2014, methodology): “2008) and the Padova group (Marigo et al. 2008; Girardi et al. 2000), the set of YY isochrones (Demarque et al. 2004), a grid constructed using the Yale Stellar Evolution Code (YREC; Demarque et al. 2008) and described by Gai et al. (2011) (we refer to this set as YREC), and another set of models…”
• Nebular Continuum and Line Emission in Stellar Population Synthesis Models (2016, methodology): “Within FSPS, there are four isochrone sets to choose from: Padova (Bertelli et al. 1994; Girardi et al. 2000; Marigo et al. 2008) + Geneva (Schaller et al. 1992; Meynet & Maeder 2000); BaSTI (Pietrinferni et al. 2004; Cordier et al. 2007); PARSEC (Bressan et al. 2012); and MESA Isochrones and…”
• StarHorse : a Bayesian tool for determining stellar masses, ages, distances, and extinctions for field stars (2017, result): “The underlying stellar models of TRILEGAL are from Marigo et al. (2008), which are similar but not identical to our default PARSEC 1.2S models.”
• Resolved stellar mass maps of galaxies. I: method and implications for global mass estimates (2009, background): “…& Charlot 2003, CB07 hereafter), which includes revised prescriptions for the TP-AGB evolutionary phase, following Marigo & Girardi (2007) and Marigo et al. (2008).3 An accurate modelling of this phase is of particular relevance to correctly predict fluxes (hence colours and M/L) that…”
• The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars (2017, methodology): “While one could, in principle, improve the agreement between spectroscopic and asteroseismic radii with an 16 ASTEC (Christensen-Dalsgaard 2008), BaSTI (Pietrinferni et al. 2004), DSEP (Dotter et al. 2008), Padova (Marigo et al. 2008), Yonsei-Yale (Demarque et al. 2004), and YREC (Demarque et al. 20”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, positive): “…(BaSTI; Pietrinferni et al. 2004), the Dartmouth Stellar Evolution Database (DSEP; Dotter et al. 2008), the Padova stellar evolution code (Marigo et al. 2008), the Yonsei–Yale isochrones (YY; Demarque et al. 2004), and the Yale Rotating Stellar Evolution Code (YREC; Demarque et al. 2008).”
• Fitting the integrated spectral energy distributions of galaxies (2010, background): “…past few decades, much work has gone into providing homogeneous sets of stellar tracks from different groups, e.g. Padova (Marigo and Girardi 2007; Marigo et al. 2008), Geneva (Lejeune and Schaerer 2001), Yale (Demarque et al. 2004), MPA (Weiss and Schlattl 2008), BaSTI (Pietrinferni et al. 2009).”
• COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, methodology): “We therefore use the Padova isochrones (Marigo et al. 2008) for horizontal branch (HB) and AGB evolution4.”
• THE K2 ECLIPTIC PLANE INPUT CATALOG (EPIC) AND STELLAR CLASSIFICATIONS OF 138,600 TARGETS IN CAMPAIGNS 1–8 (2015, methodology): “The isochrones used in Galaxia to predict the stellar properties are from the Padova database (Marigo et al. 2008).”
• Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, background): “They found significant discrepancies with results from Marigo et al. (2008) (2007) and Weiss & Ferguson (2009) have shown that, although the use of opacity tables that properly include the enhancements of C is more appropriate, the predictions of the behaviour with time of Teff as provided by fully…”
• A NEW GENERATION OF PARSEC-COLIBRI STELLAR ISOCHRONES INCLUDING THE TP-AGB PHASE (2017, methodology): “PARSEC tracks PARSEC (the PAdova and tRieste Stellar Evolutionary Code) represents a deeply-revised version of the Padova code used in many popular sets of isochrones (e.g. in Bertelli et al. 1994; Girardi et al. 2000, 2010; Marigo et al. 2008).”
• SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED STARS (2011, background): “A set of Padova isochrones (Marigo et al. 2008) are shown for reference.”