Brightness Temperature Analysis of Mare Marginis Based on CE-2 CELMS Data

Mare Marginis (13.3 °N, 86.1 °E) is situated on the lunar nearside with rich geological diversity. This letter analyzes the brightness temperature (
$T_{B}$
) features of Mare Marginis through the normalized brightness temperature (
$\text{n}T_{B}$
) performances and brightness temperature difference (
$\text{d}T_{B}$
) using data from the Chang’E-2 Lunar Microwave Sounder (CELMS), in combination with slope, rock abundance (RA), and (FeO + TiO2) abundance (FTA). The results are as follows. First, the
$\text{n}T_{B}$
of Mare Marginis is relatively high at both daytime and nighttime. The daytime
$\text{n}T_{B}$
shows consistency with FTA distribution. Second, the
$\text{d}T_{B}$
of Mare Marginis is basically consistent with the FTA distribution, the consistency decreases as the frequency increases. Third, the correlation analysis shows that slope and FTA are the main factors influencing
$\text{n}T_{B}$
. In addition, the high substrate temperature is identified as the primary factor responsible for nighttime
$\text{n}T_{B}$
anomalies of Mare Marginis, whereas the high RA accounts for the emergence of the cold spot phenomenon at Goddard A crater.