An absolute standard that depends on variables?
No, it doesn't depend on any variables.
stipe said:
Would not expansion make these readings change along with measured wavelengths?
Here's how I see it:
Star A has a blueshift value. A reading of 1 on an imaginary wavelength scale.
The constant is set at 2
Star B has a redshift value. 3 on the same scale.
Expansion occurs.
Star A now has a wavelength value of 30 times its original reading. 1x30=30.
The constant increases by the same amount (or potentially an exponentially higher amount). 2x30=60.
Star B will show a reading of 3x30=90.
Now both stars will still be blueshifted and redshifted just as before. What has changed is only the scale by which we measure their properties.
Does this make sense?
Ah, ok, thanks for the clarification. I understand where you're coming from now.
There's a misunderstanding as to how the "standard" is determined.
If we want to know how much the wavelength has shifted, we first have to know what the wavelength of light was when it was emitted, correct? The way we determine that is by using emission or absorption lines of certain elements. The reason these lines occur is not important to this discussion. Suffice it to say that when photons strike an element such as hydrogen, the electrons are excited and bumped to a higher energy level. When the electrons fall back to their original energy level, they emit a photon of a specific wavelength. These photons are called the hydrogen emission lines, and they occur at very specific wavelengths.
So to determine redshift, we look at the starlight from an incoming star or galaxy and find the hydrogen emission lines. The difference between the lines and the laboratory values of the lines is calculated. If the lines are shifted towards the red end of the spectrum, the light is called "redshifted", and vice versa. See
this image for a good illustration of redshifted lines. See how those lines are shifted towards the red?
So the standard is a value derived here and now. It is derived from a light source stationary with the measuring device. That's how we know what the wavelength of the light
should be. Then we compare incoming starlight to it and determine how much the light has been stretched or contracted as compared to the standard. It's like calibrating a scale. You have to "zero" the scale first with no weights on it. Likewise we have to "zero" the hydrogen emission lines with a stationary object. Only then can we measure how much the starlight's light has been shifted.
The wikipedia article on redshift is a worthwhile read if you're interested:
http://en.wikipedia.org/wiki/Redshift#Measurement.2C_characterization.2C_and_interpretation
So to use your illustration:
Star A has a blueshift value. A reading of 1 on an imaginary wavelength scale.
The constant is 2 (what we measured in the lab)
Star B has a redshift value. 3 on the same scale.
Expansion occurs.
Star A now has a wavelength value of 30 times its original reading. 1x30=30.
The constant is still 2.
Star B will show a reading of 3x30=90.
Now both stars will still be redshifted.