diff options
| -rw-r--r-- | fg21sim/extragalactic/clusters/emission.py | 8 |
1 files changed, 4 insertions, 4 deletions
diff --git a/fg21sim/extragalactic/clusters/emission.py b/fg21sim/extragalactic/clusters/emission.py index a798470..24d8d2f 100644 --- a/fg21sim/extragalactic/clusters/emission.py +++ b/fg21sim/extragalactic/clusters/emission.py @@ -355,12 +355,12 @@ class HaloEmission: specific luminosity (Lν) because the redshifted object is emitting flux in a different band than that in which you are observing. And the k-correction depends on the spectrum of the object in - question. For any other spectrum (i.e., vLv != const.), the flux + question. For any other spectrum (i.e., νLν != const.), the flux density Sv is related to the specific luminosity Lv by: - Sv = (1+z) L_v(1+z) / (4π DL^2), + Sν = (1+z) Lν(1+z) / (4π DL^2), where - * L_v(1+z) is the specific luminosity emitting at frequency v(1+z), - * DL is the luminosity distance to the object at redshift z. + * Lν(1+z): specific luminosity emitting at frequency ν(1+z), + * DL: luminosity distance to the object at redshift z. Reference: Ref.[hogg1999],Eq.(22) |