Let's say I have a galaxy SED like this:
from synphot import SourceSpectrum
from synphot.models import BlackBodyNorm1D
sp = SourceSpectrum(BlackBodyNorm1D, temperature=6170.4796)
wave = sp.waveset
flux = sp(wave) #Photlam
flux_flam = flux.to(u.erg / u.s /...
The bandwidth of the H-alpha filter is 30 A or 3 nm. I need the wavelength dependent quantity because I will compute the counts (electrons/sec) from the object. The general formula being: Flux/PhotonEnergy(λ) * Filter_bandwidth (nm) * Aperture (m^2) * QE * PlateScale^2(arcsec^2). For broadband...
I think I made some progress.
The article for the Vizier data base is here: https://academic.oup.com/mnras/article/431/1/2/1036908
On pg. 12 in the pdf "
with the exception of McCullough et al. (2001) who
determined a flux for Abell 36 of F(Hα) = 2.8 × 10−11 erg cm−2 s−1,
which is 28 per cent...
I have a vizier catalog with H-alpha fluxes as logF(Haplha) in units as mW/m^2. See sample data here: http://vizier.cds.unistra.fr/viz-bin/VizieR-3?-source=J/MNRAS/431/2/fluxes How do I convert mW/m^2 to W/m^2/nm or erg/s/cm^2/A? The first entry is logF(Halpha) = -12.03 mW/m^2
Signal - help I did found a help file for an older calculator.
So, for extended objects the electron counts are multiplied by the area of a pixel in arc seconds. For this we use the plate scale, that determines the size of the pixel in arc seconds. If my plate scale is 0.5 arc seconds per pixel...
I am trying to compute the exposure time needed for an extended object (galaxy), in python.
I have found the following formulas:
Exposure time app # press the help button at the bottom of the calculator for the formulas used
Exposure time calc
Let's take for example the M33 galaxy. It has...
I am trying to replicate the space time plot (the 2nd plot with Proper distance vs Time) as in this thread: space-time
I wrote everything in python using the astropy cosmology package.
Everything went smooth, but I am stuck at plotting the light path on the 'purple path', as per the above...