Nikhil · May 29, 2026, 12:22 AM
Rick Veregin · May 28, 2026, 11:59 PM
Regarding the question is a 3 nm filter better for narrowband?
If >= f6, assuming both filters have equal efficiency at the NB wavelength, generally a good assumption.
Contrast (NB signal/background) will always improve, inversely proportional to the bandwidth ratio. For example 7 to 3 nm, improves contrast about 7/3 = 2.3X
Iff also noise is background signal dominated, that is sqrt(background in e) » read noise, then S/N also improves by sqrt(7/3)=1.5X. This is true at 3 nm or greater bandwidth typically for 1 to 5 min subs, depending on the Bortle. For dark sites this requires a very low noise cameras and long subs typically. So for sure, 3 nm is more important for S/N improvement with more light pollution. If your noise is limited by read noise, there is no S/N improvement with 3 nm.
Note though, for NB targets in our galaxy all this is true, as well as galaxies in our local neighborhood, but as you go to 20 to 30 million light years for galaxies, the red shift will move NB wavelengths out of the optimum range at 3 nm, you will loose signal. For distant galaxies, 7 nm or more will be better for sure.
If < f6, at 3 nm the efficiency drops, especially at the edge of the field, so you will start to loose signal and any advantage of the 3 nm filter. This is due to the shift in wavelengths due to the higher incident angle.
For <= f4, you need to purchase special filters that are wavelength shifted to compensate, or just stay at 7 nm or higher for your NB filters, to accommodate the big wavelength shift.
Hope this helps
Rick
It does, thank you. This brand advertises that it is suitable to f >= 3, which is suitable for my setup.
On your note about contrast, I was figuring that all else being equal, S/N would scale as 1/sqrt(bandpass), since I’m at a dark site and I’m either photon-noise or background-noise limited, and I get a similar figure as yours. But I don’t know how this would look qualitatively, since I’ve only ever worked with 7 nm bandpass filters. I guess that would equivalently mean I would have to spend less time on a target if I got more advanced filters.
As far as cosmological implications for galaxies at larger distances, I think I would be limited to about 10 Mpc in Ha if I got the 3 nm filter, which is worth considering for some targets.
So maybe I should only upgrade the SII filter since it’s emission is so faint and I’m only going to use it for nearby nebulae.
Great that your filter is suitable for your setup.
Please note that contrast and S/N are not the same thing.
Contrast is just the the signal to background ratio. Since a NB filter reduces background, this scales as inverse bandwidth.
Signal to noise is either Signal/(Read noise+dark thermal noise) or Signal/sqrt(Background signal, which is the Poisson noise). Or if you are in between, the combination of the two. Not sure what you mean by photon noise, if you mean Poisson noise, then that is the signal/sqrt(background signal), where you are background limited for noise.
So again, either you are background limited or read noise limited for noise. If you are read noise limited, a narrow band filter does not affect that camera noise, you are limited by your camera. A filter only affects light coming in, not what your camera does to it. Mostly at dark sites you are likely read noise limited unless you are using exceptionally long exposures. So yes, you get a contrast benefit, but read noise limited means the filter will not help you at all for S/N, you are limited by your camera.
The SII channel is no different, if you are read noise limited in dark skies, 3 nm will not help S/N. You will get a contrast benefit though, which is important.
The basic message again is you will always get a contrast improvement as long as you filter efficiency at the NB wavelength is okay. But in dark skies, you likely will not get a S/N improvement.
Note, easy to determine if you are read noise or background sky noise limited. You know your read noise from your camera specs for your gain setting. Measure your background signal (or take the median signal over the whole frame, that is usually pretty close to the background signal), and convert to electrons.
Your read noise contribution in % is then: 100*Rn/[sqrt(Background +Rn²).
Rick