From bf7dcc7ea87e0ae13562bb9a6bd6187d394fb18b Mon Sep 17 00:00:00 2001
From: Aaron LI <aly@aaronly.me>
Date: Sun, 21 Jan 2018 00:04:46 +0800
Subject: clusters/emission: improve description symbols :-)
---
fg21sim/extragalactic/clusters/emission.py | 8 ++++----
1 file changed, 4 insertions(+), 4 deletions(-)
(limited to 'fg21sim/extragalactic/clusters')
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)
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