Thank you to everyone who replied to the Doodle poll!
Friday, 22 May, 15:00GMT – 16:30 GMT appears to be the best time slot for the most VMC School campaign participants, so let’s go with that. Go ahead and block that slot in your calendars (as will the MEX team). We’ll post details here in the blog later this week on how to join the #ESAHangout and how to post questions.
Mars Express Spacecraft Operations Engineer Simon Wood adds that, by Friday at 15:00GMT, the command stack that will trigger the VMC observations during ‘your’ three orbits next week should already be on board Mars Express!
The imaging plan with the overall target list for the VMC Schools Campaign is complete!
The MEX team have done a great job reconciling the proposed targets with all the conflicting requirements of the spacecraft, the mandated technical testing that MEX must do, the communication slots, pointing restrictions, etc.
Before you scroll down to the list below, please note several points:
For targets in the northern hemisphere and for equatorial targets (e.g. Tharisis, Valles Marineris, etc.), we will conduct imaging at (mostly) 8000-10 000km altitude.
For targets in the southern polar regions (Cavi Angusti, Phillips crater) we will be able to acquire images from much lower, at about 2000 km.
Irrespective of height, the proposals in green are the ones we believe we can do and get optimum results.
The ones in yellow are possible, but the VMC cannot be pointed directly at them and so the images won’t be centred on the target. While this is not ideal, it’s still pretty good. The green and yellow targets will be programmed into the Mars Express mission plan for the last week in May.
There are three requested observation targets that are, after a great deal of analysis, highly problematic or impossible.
North Pole: For the two observations proposed for imaging the North Pole, we will only see that area when it is about 90% in shadow, so you really wouldn’t see much. As an alternative – and if the proposers (HTBLA Kaindorf, Austria, and Aspiration Creation, USA, can accept) – we will be going over the South Pole under pretty good illumination conditions, and you could get images of that area. Just let us know!
Phobos: Imaging of Phobos (requested by School for Tomorrow, USA) will just not be possible – on the two occasions when Phobos crosses the disk of Mars (and so would be visible), we have an unavoidably higher-priority radio science pass.
The MEX team are now preparing a final mission plan, and we will have an animation and further details for you early next week.
We would also like to schedule a Google+ Hangout on 20, 21 or 22 May to provide interactive answers to as many of the teams as possible. We’ve set up a Doodle poll to determine which date/time is best for the most. PLEASE COMPLETE THE DOODLE HERE to let us know.
Today’s update compiled from inputs by several of the Mars Express team at ESOC. Thank you Simon, Andy and our Spacecraft Operations Manager Michel – Ed.
In the weeks since we announced which entries had made it through to the final round, we’ve been busy working out how many of the observations would be possible.
Even before we announced the VMC Schools Campaign, and assuming we might get, say, a handful of submissions, our original plan was to select as many of the requested targets as possible and then command Mars Express to turn and point VMC at each of them as it orbited the planet.
As you know, we ultimately received 25 excellent proposals (thank you!) and so the MEX team have been working hard to revise our strategy to accommodate this large number of requests.
The VMC webcam provides images of Mars having about the same quality as those provided by the ESA/NASA HUbble telescope. Image credit: ESA/Mars Express/VMC/ Humboldt Gymnasium, Vaterstetten
Mars Express was designed for performing steady observations and not rapidly turning to point at different science targets (we call these “pointings”).
And, as a safety feature, Mars Express is programmed to return to Earth-pointing between each science pointing (and it doesn’t slew, or rotate, very fast anyway – only about 10 degrees/min). Even a very short observation can take up to two hours, out of which 45 minutes are required for the move from Earth to the target pointing, and another 45 min to move back . As the spacecraft orbits Mars every seven hours, this restricts us to about three pointings per orbit.
Also, even though science will be turned off during the upcoming conjunction period, we must still allow time for communicating with Earth, which can take up to eight hours at a time. With the antenna and all the instruments rigidly fixed to the body of Mars Express, we cannot use communication periods for conducting observations with VMC. We also have other spacecraft tests that must be conducted in the week of 25-29 May.
All this reduces the number of orbits we have available for the VMC Campaign to four.
We also noticed that quite a few of the requested targets are close to each other. This causes a problem in that if we were to slew the spacecraft to point at any one first, by the time we have done this, then pointed back to Earth and then moved on to the next (nearby) target, it may well have moved out of view.
Together, these constraints mean that we might only observe about five of the proposed targets. Clearly, with so many excellent requests and so few discrete pointings available, we needed to devise Plan B.
When the cosmos hands you lemons, make lemonade
Of course, being Mars Express engineers, if we’re told that something is difficult or impossible, we take that as a personal challenge! We suspected that we could improve on this situation, and started working on ideas for a better plan.
First, note that, at 45 degrees, the field of view of the VMC camera is much larger than that of our main science camera. After a series of simulations, it became clear that by simply pointing VMC straight down and then flying the orbits, many of the requested targets would pass into view of the camera.
This wouldn’t be quite as good as performing individual pointings, but it would still be pretty good and remove the need for the time-consuming slews.
The trouble is, pointing VMC ‘straight down’ is not quite as simple as it may sound. What we actually do is called a ‘spot pointing’ in which Mars Express’ attitude control system aims an instrument at a specific point on Mars (such as Olympus Mons, for example) and then the spacecraft continuously adjusts its orientation to keep the instrument fixed on that spot.
In order to point down continuously, we would in fact need to conduct many of these spot pointings in a row – but then this means many slews and we’d be faced again with the multiple 45-minute slew delays!
That ‘a-ha’ moment
What we need is a single point on (or ‘in’) Mars that is ‘down’ no matter where we are over the surface; as it happens, there is such a point: The very centre of the planet.
The result is that VMC will continuously track the planet itself, keeping it in the camera’s field of view during the entire way around the orbit; by taking pictures at regular intervals we can then capture far more of the requested targets as they pass into view.
Indeed, at least one, or even, with some luck, several of the images thus acquired will be the closest to each of the requested targets. The MEX team at ESOC will download all the images, identify which picture(s) taken at which time(s) match the requested target, and parcel them out accordingly.
While this solution may seem obvious, remember that as the main instruments are only ever pointed at specific targets, this kind of observation was never catered for in the planning and control systems, and so we have had to do some deft programming to ‘fool’ the system (thanks for avoiding the word ‘hacking’ in our public blog posts – Ed.), but just by a little.
We think it’s an elegant solution to a perplexing problem and we think most if not all proposals can be met.
Making space movies
This solution, as hinted at the start of this post, uses the same technique we used for the Mars full orbit movies. The difference is that then, we collected a batch of images (about 600) during a single continuous orbit of seven hours.
This time, we will be performing the pointing in three segments for a total of 28 hours over a three-day period. This allows the best compromise between the requested VMC observations and the required communication periods and subsystem tests that we must do.
Reaction wheel on board Mars Express Credit: ESA
Currently, this plan is in the final stages of checking; our Flight Dynamics team are performing the required detailed calculations on the effects this will have on the spacecraft
For example, we cannot expose certain sides to the Sun for too long, nor can we allow our reaction wheels – the devices which turn the spacecraft to point in the desired direction – to build up too much speed.
The good news is that their analysis is almost complete and we expect the results shortly.
Once we have these, we can then use their output to generate a final simulation of the three-day observation period and can then give a final confirmation of which targets will be observed.