More information on Spitzer operations

It might seem, if you're just using Spitzer data (as opposed to planning observations), that you don't need to know much about Spitzer operations. But, it turns out that you do need to know a little bit about how Spitzer works in order to understand why the data look the way they do.

Spitzer is a robot

Spitzer is a robot, designed to operate autonomously for 12-24 hours at a time. We at the SSC prepare schedules for the telescope, and this is done for a whole week at once. We then upload the schedule (in whole or in part) up to the spacecraft. The telescope then goes about taking data all by itself. Every 12 or 24 hours (whatever we've told it to do), it "calls home", downloads the data and gets any new instructions. We use the Deep Space Network (DSN) to communicate with Spitzer; pretty much every other spacecraft not in Earth orbit is also competing for this limited resource. We have to plan out well in advance when we will be able to use certain radio dishes that are part of the DSN. For example, when there is a special event, such as an "orbital insertion" (when a spacecraft goes into orbit around another planet), then that event takes priority over all others, that spacecraft gets whatever antennas it needs, and we have to rearrange our uplink/downlink times accordingly.

This operational constraint is why we can't drop everything and make an observation of whatever you want right this second. This also means that there is NOT someone sitting with a joystick (or joystick-like-thing) at the SSC or at JPL, commanding the spacecraft in real time. All of the observations have to be planned in great detail at least 2 months in advance, usually more in advance than that. This is one way that observing from space is very different than observing from the ground.

Spitzer sees (in) donuts

Spitzer is more or less cylindrical in shape. (For pictures of the spacecraft and its components, visit this online gallery.) Its solar panels cover essentially one whole side of the cylinder, and that side must always face the Sun, not only because it is good to keep the spacecraft powered, but because the solar panels help keep the telescope shaded from the Sun, and we need a cold telescope to be able to observe. So the only way in which Spitzer can move is to rotate in a circle with that side of the cylinder always facing the Sun. In this fashion, Spitzer can see a circle, or torus, or donut, of the sky at any one time. (This cartoon is meant to show this torus.) As Spitzer continues in its orbit around the Sun, it can see the sky directly above and below the orbital plane (the north and south ecliptic poles) all the time, but it can only see objects in the ecliptic plane (the plane of the Solar System - not necessarily just things in the Solar System, but things behind that plane) for a little while - two periods of about 40 days in duration each year. So, over 6 months, Spitzer can see any part of the entire sky. But it can't just point anywhere at any time.

Spitzer has many instruments

Spitzer has three different science instruments: IRAC, the InfraRed Array Camera, IRS, the InfraRed Spectrograph, and MIPS, the Multiband Imaging Photometer for Spitzer. (Here is the scientist-focused overview page with a high-level summary of each of the instruments.)

IRAC has four cameras inside that image using 4 broad-band filters, centered at 3.6, 4.5, 5.8, and 8 microns.

MIPS has three cameras inside that image using 3 broad-band filters, centered at 24, 70, and 160 microns.

IRS is primarily designed to take spectra, and it has two modules inside that take low-resolution (lambda/delta lambda ~64-128) spectra over two wavelength ranges (5.2-14.7 microns and 14.3-35.1 microns), and two more modules that take high-resolution (lambda/delta lambda~600) spectra over two other wavelength ranges (9.9-19.5 microns and 18.9-37.0 microns). In order to help it center on the source of interest, it also has two small cameras, centered roughly on 15 and 24 microns.

Spitzer (sort of) does only one thing at a time

Only one of the instruments is on at a time, so that means that you can't do simultaneous observations with, say, MIPS and IRAC. However, when one of them is on, for the most part, all pieces of it are on at the same time, and you can't turn a piece off. This still doesn't mean that you can do simultaneous observations using different pieces of a given instrument, for the following reason.

There is only one moving part on the whole spacecraft (and that is the MIPS scan mirror). We do not have, as might be found on ground-based telescopes, a single field of view with, say, a pick-off mirror that rotates to feed light to different instruments. Instead, for a given pointing of the spacecraft, each camera within each instrument sees a slightly different piece of the sky. This figure has a picture of Spitzer's focal plane, e.g., all those fields of view projected onto the sky.

So, what does this mean in practice? Let's walk through an IRAC observation. IRAC has four cameras, and two fields of view (the two large blue squares in the figure linked above). Each one of IRAC's fields of view has a special kind of optics component called a beamsplitter, which reflects some wavelengths of light and allows other wavelengths to pass through. One IRAC field of view is shared by the 3.6 micron and 5.8 micron cameras (IRAC channels 1 and 3) -- the beamsplitter sends the 3.6 micron photons one way and the 5.8 micron photons another way. The other IRAC field of view is shared by the 4.5 and 8 micron cameras (IRAC channels 2 and 4). If you construct an observation that asks the spacecraft to observe a certain target in just 3.6 microns, then the telescope will slew to center that target in the 3.6 micron field of view. Because you can't turn off the other three IRAC cameras, you will also get data in those other three channels "for free." The 5.8 image will also be centered on the target you asked for, because it sees the same target as the 3.6 micron camera. The 4.5 and 8 micron cameras both see a different field of view, offset from the target you asked for. The edges of the two IRAC fields of view are separated by about 1.5 arcminutes.

For more advanced readers: The direction of the offset of the second IRAC field of view is set by the time and location (in the sky) of the observation -- for the reasons given above ("Spitzer sees (in) donuts"), the focal plane rotates on the sky. This rotation is about a degree a day on the ecliptic poles, and there is no (or very little) rotation on the ecliptic plane. So you can't obtain just any angle at just any time. If you want to be sure a certain region is covered in all four IRAC bands, you need to make a small map that ensures that the region you want to be covered is covered by both IRAC fields of view, regardless of when the data are taken (regardless of rotation angle). Spot helps you do this.