An evolutionary disc model of the edge-on galaxy NGC 5907
Astronomisches Rechen-Institut am ZAH, Mönchhofstraße 12-14, 69120 Heidelberg, Germany e-mail: firstname.lastname@example.org
2 Landessternwarte am ZAH, Königsstuhl 12, 69117 Heidelberg, Germany
Accepted: 2 August 2006
Context.We present an evolutionary disc model of the edge-on galaxy NGC 5907 based on a continuous star formation history and a continuous dynamical heating of the stellar subpopulations.
Aims.This model explains the disparate two observational facts: 1) the exponential vertical disc structure in the optical and NIR of the non-obscured part of the stellar disc and 2) the FIR/submm luminosity enhanced by about a factor of four near the obscured mid-plane, which requires additional dust and also stellar light to heat the dust component.
Methods.We use multi-band photometry in U, B, V, R, and I-band combined with radiative transfer through a dust component to simultaneously fit the vertical surface-brightness and colour index profiles in all bands adopting a reasonable star formation history and dynamical heating function. The vertical distribution of the stellar subpopulations are calculated self-consistently in dynamical equilibrium and the intrinsic stellar emissivity is calculated by stellar population synthesis.
Results.The final disc model reproduces the surface-brightness profiles in all bands with a moderately declining star formation rate and a slowly starting heating function for young stars. The total dust mass is as required from the FIR/submm measurements. Without a recent star burst we find in the midplane an excess of 5.2-, 4.0-, and 3.0-times more stellar light in the U-, B-, and V-band, respectively. The corresponding stellar mass-to-light ratios are 0.91 in V- and 1.0 in R-band. The central face-on optical depth in V-band is and the radial scale length of the dust is 40% larger than that of the stellar disc.
Conclusions.Evolutionary disc models are a powerful method to understand the vertical structure of edge-on galaxies. Insights into the star formation history and the dynamical evolution of stellar discs can be gained. FIR/submm observations are necessary to restrict the parameter space for the models.
Key words: stellar dynamics / galaxies: kinematics and dynamics / galaxies: evolution / galaxies: stellar content / galaxies: structure
© ESO, 2006