|- The Camera|
|- The Spectrographs|
|Early Data Release|
|Details of the Data|
The SDSS survey collects data with modern, digital detectors. An enormous array of CCD detectors takes images, and a pair of spectrographs, fed by optical fibers, collects spectra.
The CCD Camera
The inner sanctum of the Sky Survey telescope contains what may be the most complex camera ever built. The camera includes 30 electronic light sensors called charge-coupled devices, or CCDs like the one at left, each two inches square. The CCDs are arranged five to a column, and scientists encase each column in a vacuum-sealed chamber. To enhance sensitivity, liquid nitrogen cools each chamber to -80 degrees Celsius.
Each CCD is made up of more than four million picture elements (pixels) that release
electrons when they absorb light. The electrons are then amplified into
electronic signals that can be digitized, recorded on tape and ultimately
fed into a computer. Each of the five rows of CCDs receives light through
a different colored filter, so each row records the brightness of objects in a
different color. A night of observing will produce up to 200 gigabytes of
data on a dozen tapes.
The drawing to the right shows a schematic view of the camera. Unlike a typical camera, this one doesn't snap a still picture. Instead, the telescope is parked in a given position, and as the earth rotates, the sky moves over the camera, from top to bottom. The electrons released by the incoming light are moved (or clocked) along the CCDs at the same rate that the sky moves over the camera, ensuring that the signal is always gathered from the same objects. When a moving electron hits the edge of a CCD, it is read out through amplifiers. This readout is done continuously, resulting in long, skinny strips of sky imaged in one observation. Because the CCDs have spaces between them, to make a full picture, the telescope must be moved a little bit, and a second, slightly offset strip is imaged. A pair of strips is then combined into a single stripe, which has no empty areas.
A spectrograph, a prism like device that disperses light into many colors, measures
how much light objects emit at different wavelengths. This information, called
a "spectrum," can be used to analyze the distance, composition and age of
each celestial object. SDSS astronomers drill 640 holes in an aluminum plate, with
each hole corresponding to the position of a selected star, galaxy, or quasar.
Scientists plug the holes with optical fiber cables (right). The fibers
capture light from the 640 objects simultaneously and send it into the
two spectrographs. The spectrographs split the light form each object into
composite colors, and the resulting spectra are recorded using CCDs. Each
spectrum is measured from 3800Å (blue) to 9200Å (near infrared)
[One Å=10-10 meters] on 2048 x 2048 CCDs.
To increase the resolution of the spectrographs' data,
light from each object is split into a blue half and a red half and the spectrum
from each is recorded on a separate CCD. The splitting is done by
a beamsplitter with a special coating. The coating reflects the
blue half of the spectrum while allowing the red half to be transmitted.
Because the light is split, four images are created for each spectroscopic
observation: both a red and blue image for spectrograph #1 and also
for spectrograph #2. The plug plates are placed at the focal plane of
the telescope, just like the CCD camera. On a good night, SDSS astronomers will use six
to nine plates, obtaining spectra for up to 5,000 objects!
The spectrograph will observe all galaxies seen by the imaging survey at magnitude
17.8 or brighter. The survey plans to obtain over a million galaxy spectra - thirty times
more than any presently available galaxy redshift survey. In addition to obtaining
galaxy spectra, the SDSS plans to target 100,000 quasar candidates (selected based on
their colors), tens of thousands of stars, and many other objects, such as
X-ray and radio sources.