The subduction of the Nazca Plate beneath the South American Plate along Chile has produced some of the largest earthquakes recorded on modern seismic instrumentation. These include the 1960 M 9.5 Valdivia, 2010 M 8.8 Maule, 2014 M 8.1 Iquique, and more recently the 2015 M 8.3 Illapel earthquakes. Slip heterogeneity in the 2010 Maule earthquake has been noted in various studies, with bilateral slip and peak slip of ~15 m north of the epicenter. For other great subduction zone earthquakes, such as the 2004 M 9.1 Sumatra, 2010 M 8.8 Maule, and 2011 M 9.0 Tohoku, there was an increase in normal-faulting earthquakes in regions of high slip. In order to understand aftershock behavior of the 2010 Maule event, we are expanding the catalog of small magnitude earthquakes using a template-matching algorithm to find other small earthquakes in the rupture area. We use a starting earthquake catalog (magnitudes between 2.5-4.0) developed from regional and local array seismic data; these comprise our template catalog from Jan. - Dec. 2012 that we use to search through seismic waveforms recorded by a 2012 temporary seismic array in Malargüe, Argentina located ~300 km east of the Maule rupture area. We use waveform cross correlation techniques in order to detect new events, and then we use HYPOINVERSE2000 (Klein, 2002) and a velocity model designed for the south-central Chilean region (Haberland et al., 2006) to locate new detections. We also determine focal mechanisms to further analyze aftershock behavior for the region. To date, over 2400 unique detections have been found, of which we have located 133 events with an RMS <1. Many of these events are located in the region of greatest coseismic slip, north of the 2010 epicenter, whereas catalog events are located north and south of the epicenter, along the regions of bilateral slip. Focal mechanisms for the new locations will also be presented. Authors @en

The internal structure of the Moon has been investigated over many years using a variety of seismic methods, such as travel time analysis, receiver functions, and tomography. Here we propose to apply body-wave seismic interferometry to deep moonquakes in order to retrieve zero-offset reflection responses (and thus images) beneath the Apollo stations on the nearside of the Moon from virtual sources colocated with the stations. This method is called deep-moonquake seismic interferometry (DMSI). Our results show a laterally coherent acoustic boundary around 50 km depth beneath all four Apollo stations. We interpret this boundary as the lunar seismic Moho. This depth agrees with Japan Aerospace Exploration Agency's (JAXA) SELenological and Engineering Explorer (SELENE) result and previous travel time analysis at the Apollo 12/14 sites. The deeper part of the image we obtain from DMSI shows laterally incoherent structures. Such lateral inhomogeneity we interpret as representing a zone characterized by strong scattering and constant apparent seismic velocity at our resolution scale (0.2–2.0 Hz).@en