Doppler redshift observed using parabolic reflector telescopes is an aberration, light with an angle of incidence produces parabolic caustic curves.
The majority of Light from a star or galaxy is not parallel or 'effectively parallel'.
While it is true that some light from a distance object is parallel, the amount of parallel light collected is the same as the diameter of the reflector. For a 1 meter reflector, only a 1 meter sample of the galaxy is being received as parallel light. It would be extremely difficult so isolate the small proportion of parallel light from the high proportion of incident light.
For similar sized objects:-
Angle of incidence is proportional to distance.
The caustic curve is proportional to angle of incidence.
Length of line produced by the intersection of the caustic curve and x=0 for the parabolic curve (x^2)/4 is directly proportional to the length of the spectrum observed.
The Collimating lens does not produce parallel light when incoming light has an angle of incidence.
All parabolic and spherical reflectors are designed using the (x^2)/4 parabolic curve, the aberration is constant no matter what the diameter of the reflector or the focal length.
The refraction of light to form a spectra, put simply, amplifies the divergent light produced by the caustic curve intersection with x=0.
As the parabolic curve (x^2)/4 is the function for parallel light, a decrease in the angle of incidence shifts all the light towards the ideal focal point of the parabolic curve. That is to say, parallel light will focus light to a point when reflected from the parabolic curve, closer objects focus to a series of points which form a line due to the caustic curve, which when intersected with x=0 produces a line with a length that increases as the distance to the object decreases.
Parallel light reflected from the parabolic curve to a single point, collimated and refracted, produces a spectra directly proportional to the refractive index of the instrument used. An ideal spectra.
Light that is not parallel, light with an angle of incidence, produces divergent light when any attempt is made to collimate it using an instrument designed for parallel light.
Refracted divergent light will produce a longer spectra, or more correctly a spectra longer than the ideal spectra.
The closer the object, the greater the angle of incidence, the greater the divergence, and the longer the spectra will be.
The distance, the angle of incidence, the caustic curve, the length of the intersection of the caustic curve with x=0, the divergent 'collimated' light and the refracted spectra are all proportional to each other.
Since red light is refracted less than blue light any absorption lines towards the blue end of the spectrum will be shifted closer or further from the ideal spectra depending on the angle of incidence.
The notion of an increase in redshift, proportional to an increase in distance, is an inverted logic.
There is an increase in blueshift the closer an object is, which is proportional to the angle of incidence and the resulting parabolic caustic curve.
The length of line produced by the intersection of the caustic curve and x=0 for the parabolic curve (x^2)/4 is extremely small, it is only when it is magnified using refraction that it is noticeable as a scaling of the spectra.
The majority of Light from a star or galaxy is not parallel or 'effectively parallel'.
While it is true that some light from a distance object is parallel, the amount of parallel light collected is the same as the diameter of the reflector. For a 1 meter reflector, only a 1 meter sample of the galaxy is being received as parallel light. It would be extremely difficult so isolate the small proportion of parallel light from the high proportion of incident light.
For similar sized objects:-
Angle of incidence is proportional to distance.
The caustic curve is proportional to angle of incidence.
Length of line produced by the intersection of the caustic curve and x=0 for the parabolic curve (x^2)/4 is directly proportional to the length of the spectrum observed.
The Collimating lens does not produce parallel light when incoming light has an angle of incidence.
All parabolic and spherical reflectors are designed using the (x^2)/4 parabolic curve, the aberration is constant no matter what the diameter of the reflector or the focal length.
The refraction of light to form a spectra, put simply, amplifies the divergent light produced by the caustic curve intersection with x=0.
As the parabolic curve (x^2)/4 is the function for parallel light, a decrease in the angle of incidence shifts all the light towards the ideal focal point of the parabolic curve. That is to say, parallel light will focus light to a point when reflected from the parabolic curve, closer objects focus to a series of points which form a line due to the caustic curve, which when intersected with x=0 produces a line with a length that increases as the distance to the object decreases.
Parallel light reflected from the parabolic curve to a single point, collimated and refracted, produces a spectra directly proportional to the refractive index of the instrument used. An ideal spectra.
Light that is not parallel, light with an angle of incidence, produces divergent light when any attempt is made to collimate it using an instrument designed for parallel light.
Refracted divergent light will produce a longer spectra, or more correctly a spectra longer than the ideal spectra.
The closer the object, the greater the angle of incidence, the greater the divergence, and the longer the spectra will be.
The distance, the angle of incidence, the caustic curve, the length of the intersection of the caustic curve with x=0, the divergent 'collimated' light and the refracted spectra are all proportional to each other.
Since red light is refracted less than blue light any absorption lines towards the blue end of the spectrum will be shifted closer or further from the ideal spectra depending on the angle of incidence.
The notion of an increase in redshift, proportional to an increase in distance, is an inverted logic.
There is an increase in blueshift the closer an object is, which is proportional to the angle of incidence and the resulting parabolic caustic curve.
The length of line produced by the intersection of the caustic curve and x=0 for the parabolic curve (x^2)/4 is extremely small, it is only when it is magnified using refraction that it is noticeable as a scaling of the spectra.
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