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-rw-r--r--fg21sim/extragalactic/clusters/emission.py8
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)