EGU General Assembly in Viena, Austria,7–12 April 201926th, 2018, including a broadband and a short-period seismometer (Seismic Experiment for Interior Structure,
SEIS). The seismic instrument package is specifically designed to record marsquakes and meteoritic impacts in
Martian conditions. Routine operations are split into two services: the Mars Structure Service (MSS) and the
Marsquake Service (MQS), which are responsible for defining structure models and seismicity catalogs, respectively.
The first “deliverable” of the MSS will be a model based on the events detected during the first 3 months of
seismic monitoring of the mission, for which only a few quakes might be expected based on current estimates of
Mars seismic activity. To test our approach of determining the interior model of Mars and to prepare the InSight
science team for data return, we made use of a “blind test” time series for which the Marsquake parameters (location,
depth, origin time, and moment tensor) and interior model were unknown to the group at large.
In preparation for the mission, the goal was to develop mature algorithms to handle the data as efficiency as possible.
Synthetic seismic waveforms were computed in a 1D mantle model with a 3D crust on top using AxiSEM
and Salvus. The time series were created by adding seismic noise that relies on pre-landing estimates of noise
generated by the sensors, electronic system, environment, and nearby lander.
To characterize what we could learn about Mars interior structure with only one station and with the first seismic
event, we performed inversions of a synthetic data following a blind test process, where the interior model was
unknown to all team members carrying out data analysis and inversion.
We detail and compare the results of this “blind test” using different methods including inversion of surface wave
dispersion data, body waves travel times, and the waveforms themselves.We have used mainly Bayesian techniques
to obtain robust probability density functions of interior structure parameters. The effects on the retrieved model
distributions of fixing mars quake location and origin time are investigated, as is the effect of using fixed Vs flexible
parameterizations. To allow for tighter constraints, we also test the use of priors based on thermodynamicallyconstrained
models together with seismic observations, as well as seismic confirmation/rejection of models purely
based on thermodynamical modelling. These techniques considered here form a large part of the planned modeling
of the MSS that will be ultimately employed with the first recording of a seismic event by InSight