Extinction correction (photometry)

In summary, extinction correction in photometry is the process of correcting for the effects of dust and gas in the line of sight on astronomical measurements. It is important because it allows for more accurate and reliable measurements of celestial objects. This correction is typically performed by comparing the target object's magnitudes to those of a reference star with negligible extinction. Extinction correction can be applied to all wavelengths of light, but may vary in amount. However, it has limitations, such as assuming a uniform distribution of dust and gas and not accounting for intrinsic variations in the object's brightness or color.
  • #1
learningastronomy
15
3
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
  • #2
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.
 

1. What is extinction correction in photometry?

Extinction correction in photometry is a method used to correct for the loss of light due to the Earth's atmosphere. This loss of light, known as extinction, can affect the accuracy of measurements taken by telescopes and other instruments.

2. Why is extinction correction necessary in photometry?

Extinction correction is necessary in photometry because the Earth's atmosphere absorbs and scatters light, causing a decrease in the amount of light reaching the telescope. This can lead to inaccurate measurements and must be corrected for in order to obtain reliable data.

3. How is extinction correction calculated in photometry?

Extinction correction is calculated by comparing the observed brightness of a celestial object to its expected brightness based on its known properties. The difference between these two values is then used to determine the amount of extinction and the appropriate correction factor.

4. What factors can affect the amount of extinction correction needed in photometry?

The amount of extinction correction needed in photometry can be affected by various factors, including the altitude of the observing site, the amount of water vapor and dust in the atmosphere, and the wavelength of light being observed. These factors can vary depending on the location and time of observation.

5. How does extinction correction impact the accuracy of photometric measurements?

Extinction correction is crucial for obtaining accurate photometric measurements. Without correcting for the loss of light due to the Earth's atmosphere, the measured values may be significantly lower than the actual values. This can lead to incorrect conclusions and interpretations of astronomical data.

Similar threads

  • Introductory Physics Homework Help
Replies
3
Views
751
  • Introductory Physics Homework Help
Replies
1
Views
892
  • Introductory Physics Homework Help
Replies
4
Views
797
  • Biology and Medical
Replies
5
Views
1K
  • Introductory Physics Homework Help
Replies
2
Views
955
  • Advanced Physics Homework Help
Replies
6
Views
2K
  • Astronomy and Astrophysics
Replies
1
Views
1K
  • Cosmology
Replies
1
Views
974
Replies
7
Views
2K
  • Astronomy and Astrophysics
Replies
3
Views
2K
Back
Top