Star counts in the Galaxy. Simulating from very deep to very shallow photometric surveys with the TRILEGAL code

TL;DR

TRILEGAL is a versatile stellar population synthesis code that accurately simulates star counts across various surveys and Galactic components, aiding in the analysis of deep and shallow photometric data.

Contribution

The paper introduces improvements to the TRILEGAL code, enabling it to better match diverse observational datasets and handle extensive input libraries for Galactic star count modeling.

Findings

The model reproduces star counts from deep to shallow surveys.

Calibration successfully matches data from multiple surveys including 2MASS and Hipparcos.

Deviations occur near the Galactic Center and Plane.

Abstract

We describe TRILEGAL, a new populations synthesis code for simulating the stellar photometry of any Galaxy field. The code attempts to improve upon several technical aspects of star count models, by: dealing with very complete input libraries of evolutionary tracks; using a stellar spectral library to simulate the photometry in any broad-band system; being very versatile allowing easy changes in the input libraries and in the description of all of its ingredients -- like the SFR, AMR, IMF, and geometry of Galaxy components. In a previous paper (Groenewegen et al. 2002), the code was first applied to describe the very deep star counts of the CDFS stellar catalogue. Here, we briefly describe its initial calibration using EIS-deep and DMS star counts, which are adequate samples to probe both the halo and the disc components of largest scale heights (oldest ages). We then present the changes in the calibration that were necessary to cope with some improvements in the model input data, and the use of more extensive photometry datasets: the relatively shallower 2MASS catalogue, which probes mostly the disc at intermediate ages, and the immediate solar neighbourhood as sampled by Hipparcos, which contains a somewhat larger fraction of younger stars than deeper surveys. Remarkably, the same model calibration can reproduce well the star counts in all the above-mentioned data sets, that span from the very deep magnitudes of CDFS (16<R<23) to the very shallow ones of Hipparcos (V<8). Significant deviations are found just for fields close to the Galactic Center and Plane, and for a single set of South Galactic Pole data. The TRILEGAL code is ready to use for the variety of wide-angle surveys in the optical/infrared that will become available in the coming years.