Physics Stack Exchange is a question and answer site for active researchers, academics and students of physics. It's 100% free.

Sign up
Here's how it works:
  1. Anybody can ask a question
  2. Anybody can answer
  3. The best answers are voted up and rise to the top

I have observed magnitudes and fluxes for an object in different wavelengths from optical to mm. Now I need a tool, routine or something like that to fit a spectral energy distribution (SED) and derive some physical parameters from the fit.

I'm looking for a ready tool which can be run remotely or installed locally.

Mind you, I'm aware of this:

share|cite|improve this question

closed as off topic by Chris White, Manishearth Jan 24 '13 at 11:48

Questions on Physics Stack Exchange are expected to relate to physics within the scope defined by the community. Consider editing the question or leaving comments for improvement if you believe the question can be reworded to fit within the scope. Read more about reopening questions here.If this question can be reworded to fit the rules in the help center, please edit the question.

@Peter Mortensen: Thanks for the edit, it reads much better:) – Tigran Khanzadyan Jul 9 '11 at 13:00
up vote 2 down vote accepted

There certainly are, but it depends on what the object is?

For example, I have used the `flared disk' model of Dullemond Dominik & Natta (2001) to model the SED of hot dust around a sgB[e] star

where at optical wavelengths emission is dominated by a ~25kK stellar source but at 10 microns it is due to hot dust (~1000K) that forms in a equatorial disk around the central B[e] star and a cold dust component (~100K) that dominates the long-wavelength emission. CMFGEN will also model the SED for hot stars, LBVs, Wolf-Rayets etc., but the underlying physical conditions are very different, while a QSO would be very different again - and it's really the geometry, distribution and composition of material that affect the SED of an object, so different objects require different models. Short of the basic approach of fitting one or more Black Body models, I don't think there's a one-size-fits-all approach.

share|cite|improve this answer
This is a great suggestion. The objects that I'm dealing with are Young Stellar Objects, particularly Class 0/I and maybe Class II. I could in principle test the model for some of my TTau candidates where I expect conditions are "right" for the specific case. – Tigran Khanzadyan Aug 2 '11 at 15:52