Explanation of the DIRBE Point Source Photometry Tool
This interactive service permits measurement of photometry from DIRBE time-ordered data for sources much smaller than the 0.7 x 0.7 degree DIRBE beam. As described in section 5.6.6 of the DIRBE Explanatory Supplement, time-ordered data must be used to obtain the most accurate point source photometry. Measurement of point source photometry from a DIRBE skymap underestimates source fluxes. The error is on the order of 10%, and varies considerably from source to source and from band to band depending on factors such as the beam shape, the distribution of scan position angles at which the source was observed, and the location of the source relative to the DIRBE pixel boundaries. (The DIRBE spectral energy distribution browser can be used to obtain quick estimates of the flux of a point source and the dispersion of sky intensities at nearby reference positions from skymap data.) The point source photometry tool makes use of the DIRBE Calibrated Individual Observations (CIO) files, which contain the calibrated individual 1/8-second data samples taken in science-survey mode during each day of the cryogenic mission (11 December 1989 - 21 September 1990). The user specifies the source position, time interval in days, and DIRBE wavelength band. For each source scan, the software returns the source flux in Jy after baseline subtraction and beam profile correction, an error estimate for the source flux, and the background intensity determined from the baseline fit. The tool does not have the capability of tracking a moving object; fluxes for planets and asteroids detected in the DIRBE time-ordered data are available in the Solar System Object Dataset.
DIRBE Characteristics Relevant for Point Source Observations Nominal Delta_lambda/ Sensitivity RMS Short-term RMS Long-term RMS Absolute Beam Band Wavelength lambda per 1/8 second Gain Variation Gain Variation Calibration Solid Angle (microns) (Jy) (%) (%) Error (%) (sr) ____ __________ _____________ ______________ ______________ ______________ ____________ ___________ 1A 1.25 0.26 2.5 0.14 0.3 3.1 1.208e-4 2A 2.2 0.17 3.4 0.08 0.3 3.1 1.408e-4 3A 3.5 0.27 2.9 0.09 0.4 3.0 1.290e-4 4 4.9 0.14 4.2 0.08 0.4 3.0 1.466e-4 5 12 0.67 17 0.16 0.6 3.1 1.422e-4 6 25 0.36 32 0.20 0.5 14.6 1.478e-4 7 60 0.46 56 0.44 0.8 10.0 1.506e-4 8 100 0.31 60 0.54 1.3 12.8 1.442e-4 9 140 0.25 4100 0.13 1.5 10.1 1.362e-4 10 240 0.42 2300 0.18 1.8 10.1 1.332e-4 Notes: Detector sensitivity is given for a typical sky brightness at solar elongation of 90 degrees. Short-term gain variations pertain to timescales shorter than 1 day. Long-term gain variations were measured over timescales from ~5 to ~50 days; peak long-term gain variations are about 1% for bands 1A-4, and 2-3% for bands 5-10.
Option 1: Source Visibility
Option 1 produces a visibility chart showing the weeks of the cryogenic mission during which the specified source position was observed by DIRBE. The DIRBE line of sight pointed 30 degrees from the spacecraft spin axis, and the combined spinning and orbital motion of the spacecraft caused DIRBE to trace out a helical pattern on the sky within a viewing swath between about 64 degrees and 124 degrees in solar elongation angle. Over the course of the COBE mission, sources near the ecliptic plane would be located within the viewing swath for 2 months, and then be unobservable for 4 months before coming back into view. Sources within about 25 degrees of one of the ecliptic poles were continuously in the viewing swath. Sample plots from option 1 are available for a source in the ecliptic plane and for a source at 45 degrees ecliptic latitude. Weeks during which the source was visible are shown shaded in green. A given week of the mission is shaded if the source was viewed at any time during that week.
Option 2: Source Photometry for One Day
Option 2 selects CIO data for scans that pass within about 0.3 degrees of the source position during a single day. The number of available scans can range from zero to more than 20, and generally increases with decreasing distance between the source and the edge of the DIRBE viewing swath. See, for example, the weekly sky coverage plot in Figure 3.1-1 of the DIRBE Explanatory Supplement. For each selected scan, a time string is extracted that consists of 15 consecutive data samples centered on the sample taken closest to the source position. Two plots are produced. The first plot shows the source position and the pointing positions for the time strings in ecliptic coordinates. An arrow at the end of each time string shows the scan direction. The second plot shows the observed intensity as a function of along-scan position for each of the time strings. (Along-scan position is the along-scan component of the angular distance of the source from the pointing direction, defined as positive toward the scan direction, so time increases from right to left for this plot.) Sample output from option 2 is available for Sirius at 3.5 microns. Sirius contributes to the observed signal for the three central data samples of each time string, and the appearance of these data samples in the photometry plot is determined by the source flux and by the DIRBE beam response at the along-scan, cross-scan position of each data sample. The DIRBE beam profiles are normalized to a peak response of unity. Occasional bad data samples (mostly due to cosmic ray hits or detector hysteresis immediately following the passage of a very bright source through the field of view) are sentinelized at large negative intensity values in the CIO data, and appear as nearly vertical lines extending off scale from the neighboring good data samples in the time string. The sample photometry plot for Sirius includes one such data sample.
Option 2 also produces a table of source photometry and other parameters for
each source scan. Entries in the table are as follows.
1990 Day Number -- Average time of the central data sample (the sample taken closest to the source position) in the time string. 1990 Day Number = 1.0 at 1990 January 1 00:00:00 UTC, and day numbers less than 1 refer to dates in 1989.
If there is more than one source scan, the source photometry table is followed by a list of summary statistics. This includes a mean source flux averaged over the different scans with weighting by 1/(estimated error)2, the standard deviation of the individual source flux values, the standard error of the mean, and the mean background intensity. The standard error of the mean provides an appropriate error estimate for the mean flux if the errors for the individual source flux values are random and the source is not variable. If confusion errors are important, the standard deviation of the individual source flux values may be more appropriate.
Option 3: Source Photometry for Many Days
Option 3 allows batch mode processing for time periods longer than one day. It sends an email message to the user containing a table of source photometry for each source scan within the specified period, followed by a list of summary statistics. The content is the same as that of the option 2 output. Some sample light curves have been constructed from option 3 results. A light curve for Sirius at 3.5 microns illustrates the stability of DIRBE photometry for a nonvariable source that is much brighter than nearby sky confusion noise. Sample light curves can also be viewed for Mira, a long period variable with a period of 332 days. Light curves constructed from option 3 results occasionally show individual outlying data points with small error bars, such as the low data point on day 177 in the Mira 4.9 micron light curve. Such an outlier can be caused by a cosmic ray hit that was not identified by the glitch detection algorithm in the data processing software, or can be caused by an unusually large error in the spacecraft attitude determination. Thus, an occasional single outlying data point (either above or below neighboring points in the light curve) should not necessarily be attributed to intrinsic source variability.
Option 4: DIRBE Map Centered on Source position
Option 4 allows the user to view a 4 x 4 degree DIRBE map centered on the source position, in order to assess the source strength relative to nearby confusion. The image is from the Zodiacal Subtract Mission-Average (ZMSA) data at the wavelength specified by the user. Currently, the image can only be displayed in ecliptic coordinates, with an intensity scale ranging from the minimum to the maximum pixel value. The 41 x 41 image is pixel-replicated 5 times to create the 205 x 205 image on the display.