The stellar initial mass function (IMF) is predicted to depend upon the temperature of gas in star-forming molecular clouds. introduction an additional parameter, $T_{IMF}$ , into photometric template fitting, allows galaxies be fit with a range IMFs. Three surprising new features appear: (1) most are best bottom-lighter IMF than Milky Way; (2) at fixed redshift very similar IMF; and (3) massiv...

Radial Basis Functions (RBFs) have been found to be widely successful for the interpolation of scattered data over the last several decades. The numerical solution of nonlinear Partial Differential Equations (PDEs) plays a prominent role in numerical weather forecasting, and many other areas of physics, engineering, and biology. In this paper, Differential Quadrature (DQ) method- based RBFs are...

The stellar initial mass function (IMF) is predicted to depend upon the temperature of gas in star-forming molecular clouds. introduction an additional parameter, $T_{IMF}$ , into photometric template fitting, suggest most galaxies obey IMF top-heavier than Galactic IMF. implications these revised fits on functions, quiescence and turnoff are discussed. At all redshifts highest become quiescent...

the rotation curves of a sample of 46 low- and high-surface brightness galaxies are considered in the context of milgrom's modi_ed dynamics (mond) to test a new interpolating function proposed by zhao et al. (2010) [1] and compare with the results of simple interpolating function. the predicted rotation curves are calculated from the total baryonic matter based on the b-band surface photometry,...

There is both theoretical and empirical evidence that the initial mass function (IMF) may be a function of the local star formation conditions. In particular, the IMF is predicted to flatten with increasing local luminosity density ρl, with the formation of massive stars being preferentially enhanced in brighter regions. In R136, the bright stellar cluster in 30 Doradus, the IMF gradient is ∂Γ/...

Deriving the Initial Mass Function and the Star Formation Rate (hereafter IMF and SFR) history of disc stars from local data implies assumptions concerning the vertical structure of the disc. Conversely, an accurate description of the vertical density of the stellar disc would require a precise knowledge of the stellar formation history. In this paper, the constraints available from local data ...

The stellar initial mass function (IMF) determines the relative number of stars born at a given mass. Despite the tremendous effort to establish a universal IMF, the astronomical literature offers a wealth of diverse evidence for IMF variations. This review was prepared for a controversial debate at the conference “Starbursts – Near and Far” at Ringberg Castle, 2000, and gives a one-sided portr...

There is both theoretical and empirical evidence that the initial mass function (IMF) may be a function of the local star formation conditions. In particular, the IMF is predicted to flatten with increasing local luminosity density ρl, with the formation of massive stars being preferentially enhanced in brighter regions. In R136, the bright stellar cluster in 30 Doradus, the IMF gradient is ∂Γ/...

We propose that the stellar initial mass function (IMF) is universal in the sense that its functional form arises as a consequence of the statistics of random supersonic flows. A model is developed for the origin of the stellar IMF, that contains a dependence on the average physical parameters (temperature, density, velocity dispersion) of the large scale site of star formation. The model is ba...

Among other things, we prove that multiquadric surface interpolation is always solvable, thereby settling a conjecture of R. Franke.