Revised Bolometric Corrections and Interstellar Extinction Coefficients for the ACS and WFPC2 Photometric Systems

Girardi, L.; Dalcanton, Julianne J.; Williams, Benjamin F.; Jong, Roelof de; Gallart, Carme; Monelli, M.; Groenewegen, M. A. T.; Holtzman, Jon A.; Olsen, Knut; Seth, Anil; Weisz, Daniel R.; Angrrr,

doi:10.1086/588526

Cited by 139 publications

(155 citation statements)

References 41 publications

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“…The formalism that we follow to derive bolometric corrections in these systems is described in Girardi et al (2002). The definition of zeropoints was revised as described in a paper by Girardi et al (2008), a description that is not repeated here. Suffice it to say that the bolometric correction tables are based on an updated and extended library of stellar spectral fluxes.…”

Section: Bolometric Correctionsmentioning

confidence: 99%

“…For lower T eff , the library is completed with spectral fluxes for M, L, and T dwarfs from Allard et al (2000), M giants from Fluks et al (1994), and finally C star spectra from Loidl et al (2001). Details about the implementation of this library, and in particular about the C star spectra, are provided in Marigo et al (2008) and Girardi et al (2008).…”

Section: Bolometric Correctionsmentioning

confidence: 99%

“…-ACS-WFC photometric system (bolometric corrections from Girardi et al 2008). In the tables, the absolute magnitudes for the following 12 filters are listed: F435W, F475W,F550M,F555W,F606W,F625W,F658N,F660N,FF775W,F814W,F850LP,F892N.…”

Section: Description Of Isochrone Tablesmentioning

confidence: 99%

“…In the tables, the absolute magnitudes for the following 12 filters are listed: F435W, F475W,F550M,F555W,F606W,F625W,F658N,F660N,FF775W,F814W,F850LP,F892N. -ACS-HRC photometric system (see Girardi et al 2008). The absolute magnitudes listed in the tables are for the following 16 filters: F220W, F250W,F330W,F344N,F435W,F475W,F550M,F555W,F606W,F625W,F658N,F660N,F775W,F814W,F850LP,F892N. In the case of the Johnson-Cousins-Glass system, the isochrone tables contain the following information:…”

Section: Description Of Isochrone Tablesmentioning

confidence: 99%

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Scaled solar tracks and isochrones in a large region of theZ–Yplane

Bertelli¹,

Nasi²,

Girardi³

et al. 2009

A&A

252

348

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We extend our theoretical computations for low-mass stars to intermediate-mass and massive stars, for which few databases exist in the literature. Evolutionary tracks and isochrones are computed for initial masses 2.50−20 M for a grid of 37 chemical compositions with metal content Z between 0.0001 and 0.070 and helium content Y between 0.23 and 0.40 to enable users to obtain isochrones for ages as young as about 10 7 years and to simulate stellar populations with different helium-to-metal enrichment laws. The Padova stellar evolution code is identical to that used in the first paper of this series. Synthetic TP-AGB models allow stellar tracks and isochrones to be extended until the end of the thermal pulses along the AGB. We provide software tools for the bidimensional interpolation (in Y and Z) of the isochrones from very old ages down to about 10 7 years. This lower limit depends on chemical composition. The extension of the blue loops and the instability strip of Cepheid stars are compared and the Cepheid mass-discrepancy is discussed. The location of red supergiants in the H-R diagram is in good agreement with the evolutionary tracks for masses from 10 to 20 M . Tracks and isochrones are available in tabular form for the adopted grid of chemical compositions in the extended plane Z − Y in three photometric systems. An interactive web interface allows users to obtain isochrones of any chemical composition inside the provided Z − Y range and also to simulate stellar populations with different Y(Z) helium-to-metal enrichment laws.

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Section: Bolometric Correctionsmentioning

confidence: 99%

Section: Bolometric Correctionsmentioning

confidence: 99%

Section: Description Of Isochrone Tablesmentioning

confidence: 99%

Section: Description Of Isochrone Tablesmentioning

confidence: 99%

See 2 more Smart Citations

Scaled solar tracks and isochrones in a large region of theZ–Yplane

Bertelli¹,

Nasi²,

Girardi³

et al. 2009

A&A

252

348

View full text Add to dashboard Cite

show abstract

“…We have generated synthetic integrated magnitudes and colours from models based on Padova isochrones (Marigo et al 2008;Girardi et al 2008) and a Monte Carlo method following Santos & Frogel (1997) in order to assess the influence of stochastic effects on the integrated colours of the clusters. Padova isochrones for g, z, and K were retrieved in a manner similar to the SSPs described in Sect.…”

Section: Stochastic Effectsmentioning

confidence: 99%

An optical/NIR survey of globular clusters in early-type galaxies

Chies-Santos

Larsen

Küntschner

et al. 2010

A&A

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Context. Some photometric studies of extragalactic globular cluster (GC) systems using the optical and near-infrared colour combination have suggested the presence of a large fraction of intermediate-age (2−8 Gyr) GCs. Aims. We investigate the age distributions of GC systems in 14 E/S0 galaxies. Methods. We carried out a differential comparison of the (g − z) vs. (g − K) two-colour diagrams for GC systems in the different galaxies in order to see whether there are any indications of age differences. We also compared the different GC systems with a few simple stellar population models. Results. No significant difference is detected in the mean ages of GCs among elliptical galaxies. S0 galaxies, on the other hand, show evidence for younger GCs. Surprisingly, this appears to be driven by the more metal-poor clusters. The age distribution of GCs in NGC 4365 seems to be similar to that of other large ellipticals (e.g. NGC 4486, NGC 4649). Padova SSPs with recently released isochrones for old ages (14 Gyr) show less of an offset with respect to the photometry than previously published models. Conclusions. We suggest that E type galaxies assembled most of their GCs in a shorter and earlier period than S0 type galaxies. The latter galaxy type seems to have a more extended period of GC formation/assembly.

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Recovery of the star formation history of the LMC from the VISTA survey of the Magellanic system

Kerber

Girardi

Rubele

et al. 2009

A&A

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The VISTA near infrared survey of the Magellanic System (VMC) will provide deep Y JK s photometry reaching stars in the oldest turn-off point throughout the Magellanic Clouds (MCs). As part of the preparation for the survey, we aim to access the accuracy in the star formation history (SFH) that can be expected from VMC data, in particular for the Large Magellanic Cloud (LMC). To this aim, we first simulate VMC images containing not only the LMC stellar populations but also the foreground Milky Way (MW) stars and background galaxies. The simulations cover the whole range of density of LMC field stars. We then perform aperture photometry over these simulated images, access the expected levels of photometric errors and incompleteness, and apply the classical technique of SFH-recovery based on the reconstruction of colour-magnitude diagrams (CMD) via the minimisation of a chi-squared-like statistics. We verify that the foreground MW stars are accurately recovered by the minimisation algorithms, whereas the background galaxies can be largely eliminated from the CMD analysis due to their particular colours and morphologies. We then evaluate the expected errors in the recovered star formation rate as a function of stellar age, SFR(t), starting from models with a known age-metallicity relation (AMR). It turns out that, for a given sky area, the random errors for ages older than ∼0.4 Gyr seem to be independent of the crowding. This can be explained by a counterbalancing effect between the loss of stars from a decrease in the completeness and the gain of stars from an increase in the stellar density. For a spatial resolution of ∼0.1 deg 2 , the random errors in SFR(t) will be below 20% for this wide range of ages. On the other hand, due to the lower stellar statistics for stars younger than ∼0.4 Gyr, the outer LMC regions will require larger areas to achieve the same level of accuracy in the SFR(t). If we consider the AMR as unknown, the SFHrecovery algorithm is able to accurately recover the input AMR, at the price of an increase of random errors in the SFR(t) by a factor of about 2.5. Experiments of SFH-recovery performed for varying distance modulus and reddening indicate that these parameters can be determined with (relative) accuracies of Δ(m− M) 0 ∼ 0.02 mag and ΔE B−V ∼ 0.01 mag, for each individual field over the LMC. The propagation of these errors in the SFR(t) implies systematic errors below 30%. This level of accuracy in the SFR(t) can reveal significant imprints in the dynamical evolution of this unique and nearby stellar system, as well as possible signatures of the past interaction between the MCs and the MW.

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Revised Bolometric Corrections and Interstellar Extinction Coefficients for the ACS and WFPC2 Photometric Systems

Abstract: We present extensive tables of bolometric corrections and interstellar extinction coefficients for the WFPC2 and ACS (both WFC and HRC) photometric systems. They

Cited by 139 publications

References 41 publications

Scaled solar tracks and isochrones in a large region of theZ–Yplane

Scaled solar tracks and isochrones in a large region of theZ–Yplane

An optical/NIR survey of globular clusters in early-type galaxies

Recovery of the star formation history of the LMC from the VISTA survey of the Magellanic system

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