Image of the raw Spectra for a spectral line map of W3.
The horizontal axis is frequency (in channels) for 1024 channels
in a 20 MHz band centered on 334 MHz.
The vertical axis is time, where each spectrum is from a 10 second
The white horizontal stripes show times when the telescope was observing
the brightest parts of W3. The dark orange data show times when the
telescope was pointed at the edges of W3.
The verticle purple lines show frequencies where RFI was flagged.
The two horizontal purple lines show time ranges where broadband RFI was
Image of a 4 by 4 degree region containing W3.
This image shows one channel of the spectral line cube produced from an
average of 5 channels of data from the spectra at left.
The center frequency 334 MHz and the bandwidth was 100 KHz.
The image is produced using the high cal noise diode assuming an
effective temperature of 1 K. The actual noise diode temperature was 29.3
K, so the image intensity should be scaled by a factor of 29.3.
The spectra were obtained in 10 second integrations while continuously
slewing the telescope over the region at a rate of 2 degrees/minute.
The colored dots show the average intensity for the 10 second integration,
but the data were taken continuously while the 17 two minute scans