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WUPPE Search Output Columns
This document defines the catalog entries describing
the WUPPE Data Archive as delivered to STScI by NSSDC.
The documentation below was obtained primarily from Marilyn Meade
from the WUPPE project at the University of Wisconsin,
as well as from the online documentation available
from the
ADF at Goddard Space Flight Center, and the
WUPPE home page
at the University of Wisconsin.
Archive Background:
The Wisconsin Ultraviolet Photo-Polarimeter Experiment
(WUPPE)
was flown as part of the ASTRO-1 mission
on the space shuttle Columbia in December, 1990,
and again with the ASTRO-2 mission in March, 1995
on the space shuttle Endeavor.
Altogether, WUPPE made 183 polarization measurements of 121 objects, and
obtained 89 spectra for 75 objects.
Clicking on this box will mark the entry for retrieval.
To Retrieve:
The selected datasets will be downloaded in a single file.
You may select the file type: .tar, .tar.gz, .tar.Z, and .zip.
After selecting the file type, click on the "Download selected files" button
and the selected files will be downloaded to your disk.
To Coplot:
After selecting up to 15 observations to be plotted, click on the "Plot marked spectra" button
to coplot the selected observations.
The spectra that you selected will be automatically scaled to the full range of wavelengths and
nearly the full range of fluxes (i.e., y axis plot scale runs from 0 (or .25 * the minimum flux
for spectra with negative fluxes) to the 10th highest flux). Each spectrum is automatically
assigned a color, up to a maximum of 15. The spectra are labelled by their dataset names, with a
summary of the datasets plotted given below the plot. After inspecting the plot, you may wish to
change the selection of datasets which are displayed. Use your browser "Back" button to do this.
Plot range Adjust the minimum and maximum wavelengths (in \305ngstroms) and minimum and maximum fluxes (in erg
/cm2/sec/\305) to select the spectral region of interest and to exclude noisy data.
Plot dimensions Adjust the X size and Y size in pixels to create the size of plot desired. The maximum dimensions ar
e 850 by 640 pixels.
Redraw plot Use this button to replot the spectra when you have changed the plot range or plot dimensions.
Object's Right Ascension in J2000 coordinates specified
in hours, minutes, and seconds. (Note the original coordinates
provided by the project were B1950.) For moving targets,
the coordinates refer to the position of the target in the sky
at the start of the observation.
Object's declination in J2000 coordinates specified in
degrees, minutes, and seconds. (Note the original coordinates
provided by the project were B1950.) For moving targets,
the coordinates refer to the position of the target in the sky
at the start of the observation.
The mean polarization position angle in degrees
averaged over approximately 1450-3200 Å.
This describes how the polarization is oriented in the
sky as measured from the direction of the North Celestial pole and
increasing to the East.
This is the GMT time of the
start of the observation (Note, although stored in the database to the
nearest second, the default print format truncates the date to the minute.)
The total useable exposure times in seconds.
Note these times were corrected to compensate for pointing
problems. In many cases, the target did not stay centered
in the aperture.
These are broad categories assigned by the WUPPE project
using a classification system adopted by the ASTRO mission.
The entire list of ASTRO science classes (as obtained from the Astrophysics
Data Facility at Goddard Space Flight Center) is listed below.
Note that the WUPPE search page lists only those categories for
which WUPPE observations were obtained.
Astro Science Classes:
0 Calibration
0.0 HUT Camera Sensitivity Targets
0.1 HUT Spectrometer Focus Targets
0.2 HUT
0.3 UIT Flat Field Sources
0.4 UIT
0.5 WUPPE Aperture Position Calibrators
0.6 WUPPE Unpolarized & Polarized Standards
0.7 BBXRT Calibration Sources
0.8 BBXRT
0.9 Joint Focus and Alignment Targets
1 Solar System Objects
1.1 Comets
1.2 Planets
1.3 Asteroids, etc.
2 Individual Stars
2.1 Supergiants
2.2 Oe/Be Stars
2.3 Wolf-Rayet Stars
2.4 Rapid Rotators
2.5 Normal White Dwarfs
2.6 Magnetic/Pulsating W.D.'s
2.7 Planetary Nebula Nuclei
2.8 Normal Stars A0 & Later
3 Variable and Binary Stars
3.1 Pre-Main Sequence Stars
3.2 Cataclysmic Variables
3.3 Interacting Binaries
3.4 Symbiotic Stars
3.5 Active Chromospheres
3.6 Pulsating Variables
3.7 Low Mass X-Ray Binaries
3.8 High Mass X-Ray Binaries
3.9 X-Ray Transients
4 ISM & Nebulae
4.1 Planetary Nebulae
4.2 Reflection Nebulae
4.3 H II Regions
4.4 Super Nova Remnants
4.5 I.S. Polarization Probes
4.6 I.S. Absorption Probes (Nearby & Hot)
4.7 Herbig-Haro Objects
4.8 Dark Clouds
4.9 Diffuse Galactic X-Ray Emission Regions
5 Star Clusters
5.1 Metal Poor Globulars
5.2 Metal Rich Globulars
5.3 Open (Galactic) Clusters
5.4 O/B Associations
6 Normal Galaxies
6.1 Nearby Galaxies
6.2 Spirals
6.3 Ellipticals
6.4 Irregulars
6.5 Dwarfs
6.6 Edge On Systems
7 Abnormal Galaxies
7.1 Interacting Galaxies
7.2 Amorphous Galaxies
7.3 Rapid Star Formation
7.4 W/Circumgalactic Matter
7.5 E/S0 with I.S. Matter
7 X-Ray Miscellany
7.6 X-Ray Background
7.7 Unidentified X-Ray Sources
8 Active Extragalactic
8.1 Seyfert I Galaxies
8.2 Seyfert II Galaxies
8.3 Radio Galaxies
8.4 Radio Loud Quasistellar Objects
8.5 Radio Quiet Quasistellar Objects
8.6 BL Lacertae Objects
8.7 LINERs
8.8 Optically Violent Variable (OVV) Quasars
9 Clusters of Galaxies
9.1 Spiral Poor Clusters
9.2 Spiral Rich Clusters
9.3 X-Ray Selected Clusters
9.4 Deep Survey Fields
9.5 Cooling Flow Clusters
9 Spacecraft Specific
9.7 TAPS Tests
9.8 Gyros/IMC/IPS
9.9 Waterdumps/Handovers
A pointer to papers in which data from the specific observation
was published. The field entry includes a letter
followed by a sequential number where the letter is defined as follows:.
J=refereed paper, C=conference proceeding, A=AAS Abstract.
Describes whether the observation occurred during the day or
night. Vaild entries include: D=Day, N=Night, DN=target observed
during day and night, and ND=target observed night and day.
Type of polarization filter used. Valid entries include:
HW=halfwave filter, L2=Lyot filter, medium
resolution, L4=Lyot filter, low resolution.
(Note cuurently only halfwave data is available.)
A measure of the polarization data quality for halfwave data
based on signal/noise estimates.
The valid entries include: G=good, F=fair, P=poor, N=none.
Indicates the status of the image motion compensation system which
corrected pointing errors at the secondary mirror.
The valid entries include: -1=manually disabled, 0=automatically disabled,
1=enabled, 2= out of limits.
The WUPPE entry_id uniquely defines each WUPPE observation. The name
is of the form MISSION-OBJECTID-nnnnnn
where
MISSION = either WUPPE1 or WUPPE2
OBJECTID = object name (e.g., GAM-GEM or NGC4151),
identical to the entries under "Target Name",
nnnnnn = a unique six-digit number (also known as the
PointingID), based on the
2-digit ASTRO Science Class, a 2-digit preassigned target number for a given
science class (although some targets have more than one target number),
and a 2-digit pointing number (i.e., jotfid) for a particular target.
The first digit of the pointing number is a sequential number indicating the
nth observation at a particular roll angle, and the second digit is the
nth exposure at that roll angle.
As an example, entry_id WUPPE1_HD5980_226911 designates an observation
of HD5980,
which is in science class 22, was the 69th selected target in class
22, the first observation at a given roll angle, and the first
observation at that roll angle. Within the ASTRO project, the number
226911 would be referred to as the PointingID and the jotfid is 11.
Note that for each observation, several data sets may be produced representing
different stages of processing.