Red and Blue shift

  • Thread starter Bjarne
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How accurate is it possible to measure the EM spectre ?
 

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  • #2
It depends on your tool...
 
  • #3
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It depends on your tool...
When the best possible is used
 
  • #4
russ_watters
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You're asking about the red and blue shift of stars and galaxies? Very accurately, since you have spectral absorption lines to compare with a reference.
 
  • #5
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You're asking about the red and blue shift of stars and galaxies? Very accurately, since you have spectral absorption lines to compare with a reference.
Yes - Red and blue shift of stars and galaxies.
What is "very accurate" ?
1 millionth of a meter?
Which devise is the best ?
 
  • #6
russ_watters
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What about absorbed photons, is it only these that has very certain frequencies that are absorbed?
For example here http://www.astro.ucla.edu/~wright/doppler.htm is mentioned that those at 393 nm are absorbed.
My question is; - how accurate is that?
Is it only these that have the exact wavelength 393nm that are absorbed
What when one is 394 nm or 392nm , - will noting happen ?
If so it must be possible to measure much more accurate as 0.1% to 1%.
I mean the difference between 393nm and 392 nm is not much.
 
  • #8
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The spectrograph gives you signal over a range of wavelengths, so you should see characteristic peaks on a graph.

393 nm/392 nm = 0.26% which seems nicely in the range 0.1-1%.
 
  • #9
Janus
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What about absorbed photons, is it only these that has very certain frequencies that are absorbed?
For example here http://www.astro.ucla.edu/~wright/doppler.htm is mentioned that those at 393 nm are absorbed.
My question is; - how accurate is that?
Is it only these that have the exact wavelength 393nm that are absorbed
What when one is 394 nm or 392nm , - will noting happen ?
If so it must be possible to measure much more accurate as 0.1% to 1%.
I mean the difference between 393nm and 392 nm is not much.
There are a number of factors that determine the frequency range over which you will measure a spectral line:

http://www-star.st-and.ac.uk/~kw25/teaching/nebulae/lecture08_linewidths.pdf
 
  • #10
Drakkith
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What about absorbed photons, is it only these that has very certain frequencies that are absorbed?
For example here http://www.astro.ucla.edu/~wright/doppler.htm is mentioned that those at 393 nm are absorbed.
My question is; - how accurate is that?
Is it only these that have the exact wavelength 393nm that are absorbed
What when one is 394 nm or 392nm , - will noting happen ?
If so it must be possible to measure much more accurate as 0.1% to 1%.
I mean the difference between 393nm and 392 nm is not much.
Those spectrographs are looking at light that was emitted from an object. The spectral lines are absorbed at the SOURCE, not the instrument. In other words, the line at 393 nm absorbed by calcium is a result of actual calcium in the star or galaxy absorbing the light, not calcium here on Earth. The light that is at 392 nm is NOT being absorbed by calcium, the line is wider than 1 nm because of several different effects, such as the rotation of the star. (Part of the star is moving away and part is moving towards us, so the line is wider than it would be otherwise) When we look at the patterns of lines in the spectrum and compare it with our own lines here on Earth we see a difference where the lines are shifted to the red end, aka redshifted. Measuring the difference between the lines we observe from the object and our comparison here in the lab we can tell how fast something is moving away from or towards us.
 
  • #11
Dotini
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...spectrographs are looking at light that was emitted from an object. The spectral lines are absorbed at the SOURCE, not the instrument.
As a minor curiosity, an isolated lab test has apparently demonstrated that electron density (of intervening media?) may play some role in the story of spectral line shift phenomena.
http://www.sciencedirect.com/science/article/pii/S0030402608000089

Respectfully submitted,
Steve
 
  • #12
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The light that is at 392 nm is NOT being absorbed by calcium, the line is wider than 1 nm because of several different effects, such as the rotation of the star.
This would imply a velocity of ~1/400c or about 1000km/s, which is equivalent to a rotational period of about an hour for a sun-sized star. As comparison: The sun's surface needs 25-30 days for a rotation (depends on the latitude), and 1/400c is much more than the escape velocity of stars.


There is no theoretic limit on the precision, and the technical limits depend on the instruments, measurement time and brightness of the source. Exoplanet searches can measure the radial velocity of nearby stars with a precision of ~1m/s which is equivalent to a relative precision of ~3*10^(-9). The key point here: While the actual lines are broader than this, the center of those lines can be measured with a precision better than the line widths.
 

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