An Initial Mass Function for Individual Stars in Galactic Disks: I. Constraining the Shape of the IMF

Abstract

We derive a semi-empirical galactic initial mass function (IMF) from observational constraints. We assume that the star formation rate in a galaxy can be expressed as the product of the IMF, $\psi (m)$, which is a smooth function of mass $m$ (in units of \msun), and a time- and space-dependent total rate of star formation per unit area of galactic disk. The mass dependence of the proposed IMF is determined by five parameters: the low-mass slope $\gamma$, the high-mass slope $-\Gamma$, the characteristic mass $m_{ch}$ (which is close to the mass $m_{\mathrm{peak}}$ at which the IMF turns over), and the lower and upper limits on the mass, $m_l$ (taken to be 0.004) and $m_u$ (taken to be 120). The star formation rate in terms of number of stars per unit area of galactic disk per unit logarithmic mass interval, is proportional to $m^{-\Gamma }\left\{1-\exp \left[-(m/m_{ch}{)}^{\gamma +\Gamma }\right]\right\}$, where ${\mathcal{N}}_{\ast }$ is the number of stars, $m_l<m<m_u$ is the range of stellar masses. The values of $\gamma$ and $\emch$ are derived from two integral constraints: i) the ratio of the number density of stars in the range $m=0.1-0.6$ to that in the range $m=0.6-0.8$ as inferred from the mass distribution of field stars in the local neighborhood, and ii) the ratio of the number of stars in the range $m=0.08-1$ to the number of brown dwarfs in the range $m=0.03-0.08$ in young clusters. The IMF satisfying the above constraints is characterized by the parameters $\gamma =0.51$ and $\emch=0.35$ (which corresponds to $m_{\mathrm{peak}}=0.27$). This IMF agrees quite well with the Chabrier (2005) IMF for the entire mass range over which we have compared with data, but predicts significantly more stars with masses $<0.03M_{\odot }$; we also compare with other IMFs in current use.

46 pages, 8 figures, submitted to ApJ

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