Galactic extinction as a function of distance I am looking at several galactic sources in the $I$, $R$ and $V$ bands and I want to calculate their absolute magnitudes. I can get the apparent magnitude and I know the distance so I just need to account for extinction to acquire the absolute magnitude. I first used the NED Coordinate Transformation &amp; Galactic Extinction Calculator but the calculated extinction values are too high. I figured that this is probably due to the fact that my sources are relatively close ($\sim 100\,\text{pc}$) and I am thus only looking through a fraction of the dust that these coefficients were calculated for.

If I lower the extinction coefficients to a certain fraction of NED's value (say 60% in a particular case) then I get the expected answer but I'm looking for an accurate way to choose this fraction. I've looked for a method to calculate the extinction coefficients as a function of distance but haven't been able to find anything. Does there exist a map of extinction as a function of distance (and galactic coordinates) in the galaxy from which I can extrapolate the information required? Is there a way to calculate the extinction coefficients ($A_I$, $A_R$ and $A_V$) for an object in the galaxy a known distance away? I found IPHAS which seems to be the right idea but I'm not sure if I can use it to get what I want (or how).
If your sources are within 100pc then the best thing to do is assume the extinction is zero, unless you are looking for absolute magnitudes that are a lot more precise than say +/- 0.1 mag. I think you would be very unfortunate if the extinction was any more than about ~0.1 mag in the V-band (and less than that at R and I). 

Beyond that you are really struggling because the structure of the ISM is very non-uniform, so you would have to go with the kinds of maps that are produced (for example) using IPHAS - but these are only in the galactic plane. But even if you could find some general map covering all positions it would be unlikely to give you an accurate answer out to 100pc, because there isn't enough extinction to give an effect that is big enough to be measured with any precision (i.e. the uncertainty might be bigger than the value).

If you have spectral types for your objects then you could always compare the V-I colour with what you expect for a star of that spectral type. This gives you the reddening $E(V-I)$ and then (roughly speaking) $A_V \simeq 2E(V-I)$.