Extinction correction (photometry)

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SUMMARY

The discussion centers on the concept of extinction correction in photometry, specifically addressing the relationship between uncorrected and corrected instrumental magnitudes. It is established that if the uncorrected extinction instrumental magnitude is ##v^A_V = 9.00##, the corrected magnitude will always be less than 9.00. This is due to the nature of extinction, which absorbs light and results in fainter observed magnitudes. Consequently, the corrected magnitude reflects a brighter object, confirming that corrected magnitudes are always smaller than their uncorrected counterparts.

PREREQUISITES
  • Understanding of photometric magnitudes
  • Knowledge of extinction effects in astronomy
  • Familiarity with instrumental magnitude measurements
  • Basic grasp of light absorption principles
NEXT STEPS
  • Research the mathematical formulas for extinction correction in photometry
  • Explore the impact of different extinction coefficients on magnitude calculations
  • Learn about the tools used for measuring instrumental magnitudes in astronomical observations
  • Investigate case studies on extinction correction in various astronomical surveys
USEFUL FOR

Astronomers, astrophysicists, and students studying photometry who seek to understand the effects of extinction on magnitude measurements and how to apply corrections in their analyses.

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Homework Statement
I am learning photometry and I am wondering is the uncorrected extinction instrumental magnitude always less than the corrected extinction instrumental magnitude when applying transformation coefficients?
Relevant Equations
##m_{\lambda}^A=m_{\lambda}+[\kappa_0+\kappa_1 (B-V)]X##
For example suppose the uncorrected extinction instrumental magnitude is ##v^A_V = 9.00##, will the corrected extinction instrumental magnitude always be greater than ##9##?
 
Physics news on Phys.org
Extinction causes an object to be fainter, because some of the light coming from the object is absorbed. So the corrected magnitude should always be brighter than the uncorrected magnitude. So the corrected magnitude will always be less than the uncorrected magnitude, since brighter objects have smaller magnitudes.
 

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