How do they define luminosity function in astrophysics?

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Luminosity in astrophysics refers to the total integrated flux of an object, defined as the total radiated power across all wavelengths, typically measured in Watts or Solar luminosities. A luminosity function describes the distribution of luminosities among a group of astronomical objects, providing insights into their formation and evolution. The term "luminosity interval" is not widely recognized, but it may relate to specific ranges of luminosity used in studies. The Present Day Mass Function (PDMF) is relevant in the context of compact bodies like white dwarfs and neutron stars, indicating the mass distribution of these objects at the present time. Understanding these concepts is crucial for analyzing stellar populations and their characteristics.
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hi, please explain me how to define a luminosity function? what is meant by luminosity interval? and the last one , what is meant by Present Day Mass Function (PDMF)?

reagrds
 
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The luminosity in astrophysics is usually the total integrated flux of an astrophysical object. In other words, it usually defined as the total radiated power over all wavelengths (energy per unit time, and in SI units measured in Watts, but often measured in Solar luminosities for a star in astrophysical situations) of an astrophysical object. The Sun, for example, has a luminosity of order 4*10^26 Watts.

I have not heard of the terms "luminosity interval" or "PDMF", could you provide some context on where they were used?
 
they are used in compact bodies studies..like white dwarf, neutron star etc
 

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