improve phase coherence on a stereo track wavelab

#IMPROVE PHASE COHERENCE ON A STEREO TRACK WAVELAB UPDATE#
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We then provide estimates of the expected signal to noise ratios. We then describe the instrument concept which will also act as a framework for the more detailed sections in the rest of the paper. We begin by describing the top level scientific objectives of CaSSIS. The two Russian experiments, ACS and FREND, are described in Korablev et al.

#IMPROVE PHASE COHERENCE ON A STEREO TRACK WAVELAB UPDATE#

( 2015) have described the other European-led instrument on TGO, Nadir and Occultation for Mars Discovery (NOMAD) with an update in Vandaele et al. This paper describes CaSSIS in detail to act as a future instrument reference. Many aspects of CaSSIS are derived from the HiSCI concept, but although similar in concept and scope, CaSSIS has several important differences forced by the need to meet a highly accelerated schedule and reduced mass and volume allocations.

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The full payload is described in Vago et al. The Colour and Stereo Scientific Imaging System (CaSSIS) became the main imaging system on the spacecraft replacing the HiSCI instrument. The schedule for TGO was maintained with a payload of 4 instruments (2 Russian led, 2 European led) and an entry, descent, and landing demonstrator (subsequently called Schiaparelli). However, following the loss of the attempted collaboration with NASA in ExoMars, both the programme and the payload were reconfigured in 2012 as a joint ESA-Roscosmos endeavour. A joint US-European team successfully responded to this AO with an instrument called HiSCI (McEwen et al. A total mass of 25 kg was allocated and an average power of 15 W. This report foresaw that the HRCSC would provide ∼1 m/pixel, near-simultaneous stereo, colour discrimination of water ice, and dust and surface variations incorporating imaging of potential trace gas sources and detection of surface changes. An Announcement of Opportunity (AO) was issued in 2010 calling for payload based on the JIDT report. The orbiter spacecraft was named the ExoMars Trace Gas Orbiter (TGO) and a commitment was made to launch in the 2016 window. The definition team focused on a High Resolution Colour Stereo Camera (HRCSC) concept that would provide geological characterisation of trace gas sources. 2011) suggested provision of very high spatial resolution imaging or mapping instruments (e.g., cameras and/or multi-beam active lasers) to provide geological context and location of small-area sources of trace gases should they exist (e.g., a volcanic vent, rift or crater). A NASA-ESA Joint Instrument Definition Team (JIDT) report (see Zurek et al. 2015 and references therein) and work to place these results into context (e.g. We note in passing the on-going work connected to the detection and variability of Martian atmospheric methane and other trace species (e.g. 2009) led to the concept of providing the orbiter with the capability to detect trace gases. The orbiter element was to provide communications while the rover was specifically targeted at investigating the sub-surface where primitive lifeforms might have survived having been protected from the harmful UV and ionising radiation present at the surface.Īlthough the orbiter was primarily foreseen as communication infrastructure for the rover element, the possibility to place payload on the orbiter was attractive and the detection of methane in the atmosphere of Mars (Formisano et al. The first element, an orbiter, was to be followed by a rover, 26 months later. The programme underwent a number of configuration changes in the subsequent decade but in 2009 the scenario became based around a two-step programme combining instrumentation from both NASA and ESA.

This programme was aimed at performing an in situ search for extinct or extant life on Mars. 1999) which eventually led to the setting up of the ExoMars mission as part of ESA’s optional programme. Outputs from these studies included a detailed report (ESA 1999) and associated papers (e.g.

#IMPROVE PHASE COHERENCE ON A STEREO TRACK WAVELAB SERIES#

In the 1990s, the European Space Agency (ESA) set up a series of study teams to establish the scientific aims and objectives for a mission focused on the search for past or present extra-terrestrial life.

Improve phase coherence on a stereo track wavelab