Proceedings of the Workshop
"The Magellanic Clouds and Other Dwarf Galaxies"
of the Bonn/Bochum-Graduiertenkolleg

The Star Formation History

of Nearby Dwarf Galaxies:

problems, methods and results

Antonio Aparicio

Instituto de Astrofísica de Canarias, E-38200 La Laguna, Canary Islands, Spain

Received 01st April 1998
Abstract. The synthetic color-magnitude diagram (CMD) methodology to study the star formation history (SFH) of nearby galaxies is briefly reviewed. Firstly the most significant features of the CMD for this task are discussed. Then, the procedure of computing synthetic CMDs is explained and the main results obtained by our group in the last few years summarized. Finally, for the purpose of showing the potentiality of the synthetic CMD methodology, sketches of the SFHs of Carina and Fornax are used to build-up synthetic CMDs qualitatively reproducing the observed CMDs of these two galaxies.

1. Star Formation History and color-magnitude diagram

The most powerful way of studying stellar populations and the star formation history (SFH) of a galaxy is by analyzing the distribution of stars in the color magnitude diagram (CMD). Comparison with synthetic CMDs computed on the basis of a consistent stellar evolution library and simulating different SFHs, is an efficient way to extract the information about the SFH (see Gallart et al. 1996a, 1996b, 1996c; Aparicio et al. 1997a, 1997b).

The accuracy and time-resolution of the resulting SFH is quite dependent on the depth and quality of the observed CMDs and on the quality and coverage of the stellar evolutionary models. Observation of low main sequence (MS) and subgiants stars together with the horizontal branch (HB) and the red clump (RC) of core He-burning stars is crucial to have a good time resolution for the oldest ages and, in particular for the HB and the RC, to constrain the chemical enrichment law (CEL). In any case, the ability of resolving the short time-scale structure in the SFH necessarily worsens for older ages. Keeping this in mind, it is not surprising that the latest improvements in the quality of data resulting from the use of the HST and of the new high sensitivity, wide-field CCDs operating in ground-based telescopes are producing an increasing interest on the detailed analysis of the SFH of nearby galaxies. On the other hand, the latest improvements in the stellar evolutionary theory and the availability of new stellar evolutionary libraries (see Bertelli et al. 1994 and references therein), covering all the stellar evolutionary phases and a wide range of masses and metallicities, is making possible accurate and comprehensive studies of the SFH in these systems.

The potentiality of the CMD and the comparison with synthetic diagrams to derive the SFH can be grasped from Aparicio et al. (1996) and from Fig. 1 (a more clear and detailed color figure can be seen at http://www.iac.es/galeira/aaj/fig1_color.html). It shows four synthetic CMDs (including observational effects) computed for constant star formation rate (SFR), ψ(t), spanning the intervals of time quoted in the labels. Two main trends are evident:

But it is also interesting to note a few more subtle things:

[Click here to see Fig. 1!]

2. Synthetic color-magnitude diagrams

For the purposes of computing synthetic CMDs, the SFH can be considered divided into three simpler functions: the SFR, ψ(t), the initial mass function (IMF), φ(m), and the CEL, z(t). These three functions can be changed to compute different synthetic CMDs and may be tested.

Once the three functions have been selected, the following process is used to build up a synthetic CMD.

  1. φ(m) and ψ(t) are used as distribution functions together with a Monte Carlo generator to obtain the mass and the age of a synthetic star. Then the metallicity is determined according to z(t).
  2. The stellar evolutionary models are used to determine whether a star of such a mass, age and metallicity is or is not alive. If it is, its evolutionary status is determined and a multidimensional interpolation is performed in the stellar evolutionary library to determine its luminosity and effective temperature.
  3. Finally, bolometric corrections are applied to obtain magnitudes in different filters.
This process is repeated several times until a synthetic CMD with the necessary amount of stars is obtained. The algorithm that our group is using is ZVAR, by Bertelli (unpublished). The result is a synthetic CMD for the input φ(m), ψ(t) and z(t) functions. But it is not yet comparable with the observational diagrams because it does not include the observational effects. Observational effects are produced mainly by three factors: crowding and blending of stars, signal to noise ratio limitations and defects in the detector. They modify the distribution of stars in the CMD in three ways: loss of stars (mainly faint); migration of stars in the CMD (affecting different stars differently) and dispersion of stars in the CMD (which is not a straightforward function of S/N). The space limitations of this paper prevent giving a further discussion of the observational effects and the way to simulate them in the synthetic CMD. Such a discussion can be found in Aparicio and Gallart (1995) and in Gallart et al. (1996b).

The final step of the process to determine the SFH of a galaxy is the comparison of the observed and synthetic CMDs. For this, the reader is referred to the papers by Gallart et al. (1998a and 1998b) about Leo I in this book (see also Aparicio et al. 1997a and 1997b).

3. Some results

Our group is working in the study of the SFH of nearby galaxies since several years. The objects we have analyzed are NGC 6822 (Gallart et al 1996a, 1996b and 1996c); Pegasus (Aparicio et al. 1997a); LGS 3 (Aparicio et al. 1997b) and Antlia (Aparicio et al. 1997c). We are currently working on Leo I (Gallart et al. 1998a, 1998b, 1998c); Phoenix (Martínez-Delgado et al. 1998c) and NGC 185 (Martínez-Delgado et al. 1998a, 1998b). Our main general results can be summarized as follow:

4. Some qualitative speculation using synthetic CMD

In this section I intend to give just a pretty, qualitative picture of what the synthetic CMD technique can produce for the SFH of galaxies if deep, high quality data are available. They do not intend to be concluding results and no detailed analysis of the CMDs has been done. Two galaxies have been chosen: Fornax and Carina. The reader is referred to Smecker-Hane et al. (1996) for the best CMD presently available for Carina and to Mighell (1997) and Hurley-Keller et al. (1998) for the two most detailed analysis of its SFH and to Stetson et al. (1998) for the best data and discussion on the stellar populations of Fornax (see Fig. 3). Figure 2 shows synthetic CMDs and the corresponding SFHs (here represented only by ψ(t) for simplicity) for Fornax and Carina.

[Click here to see Figs. 2 and 3!]

References


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First version: 15thAugust,1998
Last update: 25thSeptember,1998

Jochen M. Braun   &   Tom Richtler
 (E-Mail: jbraun|richtler@astro.uni-bonn.de)