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Wisconsin Ultraviolet Photo Polarimeter Experiment (WUPPE)
Astro2 WUPPE Halfwave Level 1 Data
Reduced Data: Flux & Polarimetry (Stokes Q & U, & Error) vs Wavelength
05 January 1999
by Marilyn Meade
o Description of the Instrument
The Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE) was one of three ultraviolet (UV) telescopes on the Astro-1 payload which flew aboard the space shuttle Columbia during a nine day mission in December 1990. It was reflown for 16 days in March 1995 on board Endeavour during the Astro-2 mission. WUPPE is a 0.5m f/10 Cassegrain telescope and spectropolarimeter. It obtained simultaneous spectra and polarization measurements, with a spectral resolution of about 16A, from 1450 to 3200A. A set of halfwave plates at 6 different angles provide spectropolarimetric modulation with 16A resolution on point sources through apertures from 6 to 40 arcsec. Calibrations of instrumental polarimetric efficiency, residual polarization, position angle registration, and flux sensitivity were performed by a combination of preflight laboratory measures and in-flight standard star observations. The data are corrected for telemetry errors, thermal background, cosmic ray hits, second order contamination, pointing errors, and instrumental polarization, which is roughly 0.05%.
A detailed description of the instrument is given in Nordsieck et al 1994, SPIE, 2010, 2. See also the WUPPE web site for more information:
http://www.sal.wisc.edu/WUPPE
o Astro-2 WUPPE Level 1 Halfwave Data
Astro-2 WUPPE Level 1 data products include calibrated spectra and polarizations. During the Astro-2 mission WUPPE took 369 observations of 254 objects; some objects have multiple pointings. 112 pointings of 79 targets were taken of WUPPE prime targets. WUPPE also observed the prime targets of the other two UV instruments which yielded good spectra in many cases but generally did not have sufficient signal-to-noise for useful polarization measurements. There were 149 pointings of 90 objects of Hopkins Ultraviolet Telescope (HUT) prime interest and 108 pointings of 85 objects of Ultraviolet Imaging Telescope (UIT) interest.
The data have been processed using methods developed for the ground- based spectropolarimetric data from the Pine Bluff Observatory (PBO) of the University of Wisconsin. This involves summation of equivalent readouts on a particular object, subtraction of background scans, division by the flat field calibration spectra, flux calibration using spectra of known bright stars, polarimetric calibration using data obtained during pre-launch and in-flight observations. For halfwave mode data, the filters are differenced and a Fourier analysis, pixel-by-pixel as a function of filter angle, is done to give Stokes parameters %Q and %U spectra along with an Error spectrum, all consisting of 1024 32-bit data points for each array from about 1450 to 3200A.
WUPPE data analysis and software development takes place at the Univer- sity of Wisconsin Space Astronomy Laboratory (SAL). Much of the WUPPE reduction software is based on a FORTRAN language generalized Reticon detector/spectropolarimeter package (REDUCE) developed at SAL to support ground-based (PBO) and rocket UV spectropolarimetric data. This software package was operating on UNIX based microVAXes for several years and is currently running on Silicon Graphics Indy machines running IRIX 6.3.
Of the 369 WUPPE observations taken during Astro-2, 150 pointings (115 objects) provided some useful polarimetric results and 47 additional pointings (43 objects) provided only flux information (no polarimetric result). The Stokes %Q and %U, and %Error spectra and flux calibrated (Flambda- ergs/cm**2/sec/A) data along with pertinent housekeeping data and data reduction information for the useful Astro-2 target halfwave mode pointings have been written to FITS files and are described in this document.
o WUPPE2 Halfwave Level 1 Data FITS file naming convention
WUPPE2_ObjectID_PointingID_HW.fits (e.g. WUPPE2_PHI-PER_220311_HW.fits)
where
ObjectID = The Mission Target List (MTL) name or the name of the object actually observed. The MTL names are common to the HUT, UIT and WUPPE instruments. For some pointings WUPPE offset from the HUT or UIT target or WUPPE co-pointed with HUT on a specific target in a large UIT field. The ObjectID for those cases is the object WUPPE actually observed as opposed to the MTL Target List name. Appropriate comments are included in the FITS header. See the table below for a list of these offset targets. The number of characters in ObjectID can vary from 3 to 8 characters and may be a mix of numbers and/or alphabetic information and may contain embedded '-'s.
PointingID = a 6 digit number representing the object identification number which was assigned during the mission. Each Astro-2 shuttle pointing had a unique PointingID number. (However, the PointingID number may not be unique for both Astro missions. A small number of PointingIDs used in the Astro-1 mission were also used in Astro-2.)
HW is the Halfwave polarimeter mode.
Note: Astro-2 Target Pointings with either a WUPPE offset from the HUT or UIT target or a co-pointing with HUT in a large UIT field:
Target Pointings with a Polarimetric Result:
Obj-ID PTG-ID MTL-Name P Sp V Comments -------- ------- -------- - -------- ---- ------------------- JUP/IO 1204-41 JUPITER H moon 2 fl pr JUP/IO 1204-51 JUPITER H moon SK-67174 2253-10 SK-67167 H O9II: 11.7 scat lgt >2100A SK-68135 2257-11 SK-68137 H B0Ia 11.3 scat lgt >2100A HD5980 2268-11 NGC346_4 H WR 10. 2 fl pr;scat lgt>2100A HD5980 2269-11 NGC346_6 H WR 10. scat lgt>2100A HD36402 4306-10 N51D U WC 11.4 scat lgt>2100A SK-69203 4416-10 SN1987A U B0.7Ia 12.3 HD68049 4804-10 FSGL_15 U B8/9III 9.7 2 fl pr HD177999 5109-11 NGC6752 U B9II-III 7.41 HD177999 5109-12 NGC6752 U B9II-III 7.41 2 fl pr HD177999 5109-14 NGC6752 U B9II-III 7.41 47-TUCBS 5201-12 47-TUC U B8-9 10.7 scat lgt>2100A BD36D367 5302-10 NGC0752 U A0III 9.7 scat lgt>2100A M67-F81 5311-11 M67 U B8 10.0 M67-F81 5311-12 M67 U B8 10.0 HD268653 5403-12 N4 U B3Iab 10.7 2 fl pr;scat lgt>2100A SK-69117 6198-10 LMC-BAR U OB 12.7 Pointings with Spectra Only, No Polarimetric Results: Obj-ID PTG-ID MTL-Name P Sp V Comments -------- ------- -------- - -------- ---- ------------------ JUP/IO 1204-20 JUPITER H moon HD5980 2250-10 NGC346_3 H WR 10. HD79548 5101-10 NGC2808 U A0 10.4 HD177999 5109-13 NGC6752 U B9II-III 7.41 HD116663 5116-10 OMG-CEN U B9V 8.80 BD+37426 5304-11 NGC0752 U F0III 9.87 scat lgt aff BD373423 5312-11 NGC6791 U K scat lgt aff AZV95 6112-10 SMC-B U O7.5III 13.9 scat lgt aff
o Example files and Description of the WUPPE2 Halfwave FITS files
Example FITS files for the Halfwave mode data:
WUPPE2_PHI-PER_220311_HW.fits
WUPPE2_GAM2VEL_220410_HW.fits (flux-only data)
The FITSIO package, version 4.14, written by William Pence at the Goddard Spaceflight Center, was used to generate the FITS files. They were written on a Silicon Graphics Indy running IRIX 6.3.
FITS files including the polarimetry are generally 34560 bytes in length. The flux-only FITS files are generally 11520 bytes.
A WUPPE2 Halfwave Level 1 FITS file looks like the following:
+-------------------+
| |
| Primary header |
| |
+-------------------+
+-------------------+
| Primary data |
| Flux (Flambda) |
| |
+-------------------+
+-------------------+
| |
| Extension Header |
| |
+-------------------+
+-----++----++----++----+
|Wavel|| %Q || %U ||%Err|
| || || || |
| || || || |
| || || || |
| || || || |
| || || || |
| || || || |
| || || || |
+-----++----++----++----+
The set of basic header information includes the primary array keywords and keywords describing the data arrays, target information, telescope engineering data relative to the observation, and calibration information. A set of comments giving the data reduction history is also included along with a "Special Comments" section. The exact headers of the 2 example files are given below. The primary array data consists of the Flux array (1024 data points-32 bits per data point) in units of ergs/cm**2/sec/A (Flambda). The binary tables extension includes headers and vectors for wavelength (Angstroms) and the Stokes parameters %Q & %U, and the %Error (also 1024 32-bit data points per array). There is no binary table extension for the flux-only FITS files.
For the fluxes, bad data have been zeroed out. For the polarization data, the bad data are when the %Error data have been zeroed out. The %Q and %U data remain (allowing inspection of those data) but should not be used.
o Astro-2 Level 1 WUPPE Halfwave FITS file header
FITS File header(flux & polarimetric data): WUPPE2_PHI-PER_220311_HW.fits
Primary FITS header:
SIMPLE = T / file does conform to FITS standard BITPIX = -32 / number of bits per data pixel NAXIS = 1 / number of data axes NAXIS1 = 1024 / length of data axis 1 EXTEND = T / FITS dataset may contain extensions COMMENT FITS (Flexible Image Transport System) format defined in Astronomy and COMMENT Astrophysics Supplement Series v44/p363, v44/p371, v73/p359, v73/p365. COMMENT Contact the NASA Science Office of Standards and Technology for the COMMENT FITS Definition document #100 and other FITS information. COMMENT FITSIO package v4.14 used CRVAL1 = 1354.00 / Wavelength in Angstroms of first pixel CDELT1 = 2.00 / Number of Angstroms/pixel CRPIX1 = 1.00 / Starting pixel number CTYPE1 = 'WAVELENGTH' / Wavelength in Angstroms CUNIT1 = 'angstrom' / Unit of Wavelength BUNIT = 'ERGS/CM**2/SEC/A' / Unit of Flux (FLAMBDA) ORIGIN = 'UW-Space Astronomy Lab' / Creator of FITS file DATE = '1998-12-09T17:11:57' / FITS file creation date DATE-OBS= '1995-03-05' / Date of Observation (GMT) ccyy-mm-dd OBSERVAT= 'ASTRO-2 ' / Observatory TELESCOP= 'WUPPE ' / Telescope INSTRUME= 'SPECTROPOLARIMETER' / Instrument Used MODE = 'HW ' / Halfwave Polarimeter Mode OBJECT = 'PHI-PER ' / Object Observed NAME2 = 'HD10516 ' / Alternate Target Name ID = '2203-11 ' / Target ID PRIME = 'WUPPE ' / Prime Instrument EQUINOX = 1950.00 / Equinox for coordinates RA = 25.13 / Right ascension in degrees DEC = 50.44 / Declination in degrees GMTSTART= '64/20:54' / GMT start time of observation (dd/hh:mm) METSTART= '03/14:16' / Mission Elapsed Time start time (dd/hh:mm) EXPOSURE= 997.0 / Useful Exposure Time (seconds) FRAMETIM= 0.2 / Frametime for each scan (seconds) SEQ-NUM = 106 / WUPPE Sequence Number HVPS = 3.70 / High Voltage Power Supply (volts) GAIN = 'High ' / Spectrometer Gain (High or Low) THERM = -33.10 / Instrument temperature (Centigrade) POSANGLE= 197.20 / Observatory Position Angle IMCSTATU= '-1 ' / Image Motion Compensation System status COMMENT IMCS:-1=man disab;0=auto disab;1=enab;2=out of limits DAYNIGHT= 'Day ' / Day-Night Status COMMENT Day-Night designations: "Night", "Day" (All Night or All Day) COMMENT "MostN", "MostD" (Mostly Night or Mostly Day), "N/D" or "D/N" COMMENT (Night into Day, Day into Night, roughly half the time in each). APERTURE= 8 / Aperture Used COMMENT Ap 8=6"x12";Ap 1=40" diam;Ap 2=4.2" diam FILTER = 6 / Starting Filter Number COMMENT Useful data generally are from 1450A-3200A with a spectral COMMENT resolution of 16A. HISTORY Data Reduction History HISTORY Wavelength calibration using Aluminum lines (created 4/25/95) HISTORY Filter mixing fixed for 0.2 sec frametime scans HISTORY Remove cosmic ray hits & telemetry errors & deviant scans HISTORY Remove offsets & thermal background & correct for thermal drift HISTORY Remove detector background (Astro-2 dtr bkg: created 5/22/95) HISTORY Apply noise reduction & 2nd order correction(created 3/13/96) HISTORY For each scan, correct for image motion in pitch & yaw HISTORY Apply flat field for Astro-2 point source (created 3/21/96) HISTORY Apply flux calibration: used HST standards & ptg correction HISTORY (created 4/1/97) HISTORY Apply Astro-2 high gain instrumental polarization calibration: HISTORY wuppe2i (created 5/16/96) COMMENT WUPPE Astro-2 flux calibration has a relative flux accuracy COMMENT of 5% between 1700A and 3000A and 10% outside this range. COMMENT Due to pointing instabilities, fluxes are not absolute. Binary extension header: XTENSION= 'BINTABLE' / binary table extension BITPIX = 8 / 8-bit bytes NAXIS = 2 / 2-dimensional binary table NAXIS1 = 16384 / width of table in bytes NAXIS2 = 1 / number of rows in table PCOUNT = 0 / size of special data area GCOUNT = 1 / one data group (required keyword) TFIELDS = 4 / number of fields in each row TTYPE1 = 'WAVELENGTH' / label for field 1 TFORM1 = '1024E ' / data format of the field: 4-byte REAL TUNIT1 = 'ANGSTROM' / physical unit of field TTYPE2 = 'Q ' / label for field 2 TFORM2 = '1024E ' / data format of the field: 4-byte REAL TUNIT2 = 'PERCENT ' / physical unit of field TTYPE3 = 'U ' / label for field 3 TFORM3 = '1024E ' / data format of the field: 4-byte REAL TUNIT3 = 'PERCENT ' / physical unit of field TTYPE4 = 'ERROR ' / label for field 4 TFORM4 = '1024E ' / data format of the field: 4-byte REAL TUNIT4 = 'PERCENT ' / physical unit of field EXTNAME = 'POLARIMETRY' / name of this binary table extension CALIBRAT= 'wuppe2i ' / Instrumental polarization calibration used AVE-POL = 0.436 / Mean %Pol over entire wavelength region AVE-ERRO= 0.004 / Mean %Error in %Pol AVE-PA = 49.4 / Mean Position Angle (degrees) COMMENT The errors given in the error array are the statistical errors COMMENT based on the residuals of the least squared fit to the 3 COMMENT filter-pair polarimetric data (see section 2.3 of Wolff, COMMENT Nordsieck & Nook 1996 AJ 111, 856). COMMENT The instrumental polarization stability of WUPPE is +/- 0.04% COMMENT and the polarization efficiency is Pol/20. COMMENT ***IMPORTANT NOTE*** COMMENT **The ERROR array is also being used as a QUALITY array. COMMENT **For bad/contaminated data, the errors have been set to zero COMMENT **but the %Q & %U arrays for those wavelengths remain unchanged COMMENT **to allow inspection of the bad data. COMMENT WUPPE Astro-2 instrumental polarization is Q=-0.04% and COMMENT U=-0.08% (which has been removed). COMMENT Special Comments COMMENT *2400A "Glitch"* COMMENT The data between about 2380A and 2420A are bad (& therefore the COMMENT error array has been set to zero) due to a detector flaw in COMMENT the "A" polarimetric array. ============================================================================ FITS File header (flux only data): WUPPE2_GAM2VEL_220410_HW.fits Primary FITS header: SIMPLE = T / file does conform to FITS standard BITPIX = -32 / number of bits per data pixel NAXIS = 1 / number of data axes NAXIS1 = 1024 / length of data axis 1 COMMENT FITS (Flexible Image Transport System) format defined in Astronomy and COMMENT Astrophysics Supplement Series v44/p363, v44/p371, v73/p359, v73/p365. COMMENT Contact the NASA Science Office of Standards and Technology for the COMMENT FITS Definition document #100 and other FITS information. COMMENT FITSIO package v4.14 used CRVAL1 = 1364.00 / Wavelength in Angstroms of first pixel CDELT1 = 2.00 / Number of Angstroms/pixel CRPIX1 = 1.00 / Starting pixel number CTYPE1 = 'WAVELENGTH' / Wavelength in Angstroms CUNIT1 = 'angstrom' / Unit of Wavelength BUNIT = 'ERGS/CM**2/SEC/A' / Unit of Flux (FLAMBDA) ORIGIN = 'UW-Space Astronomy Lab' / Creator of FITS file DATE = '1998-12-18T14:02:38' / FITS file creation date DATE-OBS= '1995-03-17' / Date of Observation (GMT) ccyy-mm-dd OBSERVAT= 'ASTRO-2 ' / Observatory TELESCOP= 'WUPPE ' / Telescope INSTRUME= 'SPECTROPOLARIMETER' / Instrument Used MODE = 'HW ' / Halfwave Polarimeter Mode OBJECT = 'GAM2VEL ' / Object Observed NAME2 = 'HD68273 ' / Alternate Target Name ID = '2204-10 ' / Target ID PRIME = 'WUPPE ' / Prime Instrument EQUINOX = 1950.00 / Equinox for coordinates RA = 122.01 / Right ascension in degrees DEC = -47.20 / Declination in degrees GMTSTART= '76/01:42' / GMT start time of observation (dd/hh:mm) METSTART= '14/19:30' / Mission Elapsed Time start time (dd/hh:mm) EXPOSURE= 214.0 / Useful Exposure Time (seconds) FRAMETIM= 0.2 / Frametime for each scan (seconds) SEQ-NUM = 433 / WUPPE Sequence Number HVPS = 3.10 / High Voltage Power Supply (volts) GAIN = 'Low ' / Spectrometer Gain (High or Low) THERM = -33.10 / Instrument temperature (Centigrade) POSANGLE= 161.70 / Observatory Position Angle IMCSTATU= '1 ' / Image Motion Compensation System status COMMENT IMCS:-1=man disab;0=auto disab;1=enab;2=out of limits DAYNIGHT= 'Night ' / Day-Night Status COMMENT Day-Night designations: "Night", "Day" (All Night or All Day) COMMENT "MostN", "MostD" (Mostly Night or Mostly Day), "N/D" or "D/N" COMMENT (Night into Day, Day into Night, roughly half the time in each). APERTURE= 8 / Aperture Used COMMENT Ap 8=6"x12";Ap 1=40" diam;Ap 2=4.2" diam FILTER = 6 / Starting Filter Number COMMENT Useful data generally are from 1450A-3175A with a spectral COMMENT resolution of 16A. HISTORY Data Reduction History HISTORY Wavelength calibration using Aluminum lines (created 4/25/95) HISTORY Filter mixing fixed for 0.2 sec frametime scans HISTORY Remove cosmic ray hits & telemetry errors & deviant scans HISTORY Remove offsets & thermal background & correct for thermal drift HISTORY Remove detector background (Astro-2 dtr bkg: created 5/22/95) HISTORY Apply noise reduction & 2nd order correction(created 3/13/96) HISTORY NO correction for image motion in pitch & yaw HISTORY Apply flat field for Astro-2 diffuse source (created 3/28/96) HISTORY Apply flux calibration: used HST standards & NO ptg correction HISTORY (created 4/1/97) COMMENT WUPPE Astro-2 flux calibration has a relative flux accuracy COMMENT of 5% between 1700A and 3000A and 10% outside this range. COMMENT Due to pointing instabilities, fluxes are not absolute. COMMENT No useful polarimetry was obtained from this observation. COMMENT Special Comments COMMENT Very bright object;Defocussed Image
o The WUPPE2 Target Halfwave Data Set
Polarimetric Results:
150 of 369 pointings (115 targets) have some useable polarization result. (See the Target Observation Log file below for more details on the observations.)
119 of these pointings (89 objects) resulted in polarization measured across the majority of UV wavelengths.
Eleven of these 119 pointings (ten objects) had only two filter pairs observed. During these observations, good data were obtained in only the first two sets of the three halfwave filter pairs. This prevents an independent estimate of the errors. The formal errors have been multiplied by three to give a more reasonable error estimate (this factor comes from empirical evidence by comparing the errors from three filter sets to those with only two filter sets).
Another three of the 119 pointings (three targets) had data where some "Droop" affects were seen. There are positions in Aperture 8 and especially Aperture 1 where part of the spectrum is projected off the edge of the A-array detector (the "Droop" area). Data >~2380A for Ap 1 and >~2800A for Ap 8 can be affected by Droop. "Droopy" scans were not used in the reduction in the affected wavelength regions. Only the B-array data (which are unaffected by Droop) were used for the flux data.
An additional six pointings (of the 119 pointings, five targets) gave very low signal/noise results and should be treated with caution. An additional 31 pointings (26 targets) have significant scattered daylight polarization contamination at wavelengths > 2100A. These data have the error array set to zero for those wavelengths denoting the poor polarization data. (Eight of these 31 pointings (6 objects) also were two filter pair observations.) Scattered light polarization affects were seen in observations of faint targets in the daytime with a sun angle < 90 degrees. See WUPPE2_SCATLGTF_000000_HW.fits for the mean estimated contribution of the scattered sunlight to the flux. It was found from daytime observations of blank sky that the scattered light polarization was about 50%(+-12%) at the solar position angle. Therefore even if the scattered light contribution to the flux is small, the potential contribution to the observed polarization can be significant (e.g. if the scattered light flux is only 1% of the observed flux, that translates into possibly a 0.5% contribution of scattered light polarization to the observed polarization).
Flux Only Results:
In some cases the observation was too short or data from at least two filter pairs were not collected to produce polarization results. The flux calibrated data are provided in these cases (47 of 369 pointings-43 targets). Of the 47 flux only pointings, 18 pointings (16 targets) have some amount of contamination due to scattered light flux. See WUPPE2_SCATLGTF_000000_HW.fits for the mean estimated contribution of the scattered light to the flux.
No Useful Results:
In 172 of the 369 target pointings (128 targets) the object was never in the aperture or was swamped by scattered sunlight or there were other problems. No data are provided in these cases.
Estimated Scattered Sunlight Flux:
This spectrum is the mean estimate of the scattered light flux which was detected by WUPPE when the sun angle was <90 degrees. It was created by coadding the flux from ten daytime targets where WUPPE offset from the target and three pointings where WUPPE observed blank sky during the day. The coadded data were divided into the WUPPE flux of the moon, smoothed, then multiplied by the lunar flux. The level of this flux can vary by about a factor of 2 (higher or lower). The FITS file for this mean estimated scattered light flux is named: WUPPE2_SCATLGTF_000000_HW.fits (where 000000 has been assigned as the PointingID for this data set).
See the WUPPE2 target observation log at the end of this document for more specific information on the target observations.
o Software
The programs polfitsread.f and fluxfitsread.f were written to verify the contents of the Astro-2 WUPPE Level1 FITS files. They also use the FITSIO v4.14 software package. These programs create the ASCII dump files described in the section below.
o Postscript Files
Postscript files have been provided in which the Flux (Flambda), binned percent Polarization and binned Position Angle have been plotted. Two sets of postscript files have been provided for each pointing. In one set, the polarization data are binned to a specific wavelength interval (e.g 100 Angstrom bins). In the other set, the polarization data are binned to a constant error (e.g. 0.05% error). The naming convention is the same as above except ".fits" has been replaced by "a.ps" or "e.ps", for angstrom binning or error binning respectively. For the daylight contaminated pointings, the flux plots include the the observed flux, the estimated scattered light flux (given in WUPPE2_SCATLGTF_000000_HW.fits), and the observed flux minus the mean estimated scattered light flux. (NOTE: The FITS files contain only the observed flux.)
e.g.
WUPPE2_ObjectID_PointingID_HWa.ps or WUPPE2_ObjectID_PointingID_HWe.ps
WUPPE2_PHI-PER_220311_HWa.ps (40A binning)
WUPPE2_PHI-PER_220311_HWe.ps (0.032% error binning)
For the flux only pointings 16 postscript files have been provided in which the flux of 47 pointings and the estimated scattered light flux have been plotted. The file names are:
Contains plots of:
PointingID Object Name
WUPPE2_HW_FLUX1.ps 0901-10 BET-CAS
2203-10 PHI-PER
2204-10 GAM2VEL
WUPPE2_HW_FLUX2.ps 3115-10 HD200775
4211-11 NGC7023
4211-12 NGC7023
WUPPE2_HW_FLUX3.ps 4511-10 SK66-19
4511-20 SK66-19
0000-00 SCATLGTF
WUPPE2_HW_FLUX6.ps 1204-20 Jupiter-Io
2250-10 HD5980
2828-10 HD57682
WUPPE2_HW_FLUX7.ps 2856-10 HD86466
2916-11 0839+399
3223-10 AM-Her
WUPPE2_HW_FLUX8.ps 4410-11 Vela-P1
4458-11 Vela-F
4460-10 Vela-H
WUPPE2_HW_FLUX9.ps 5101-10 HD79548
5109-13 HD177999
5116-10 HD116663
WUPPE2_HW_FLUX10.ps 6202-10 NGC2841
6246-10 NGC4736
6406-10 NGC4449
WUPPE2_HW_FLUX11.ps 7303-11 NGC3310
7305-10 NGC2903
7316-10 NGC5253
WUPPE2_HW_FLUX12.ps 7342-13 0833+652
8116-23 NGC4151
8202-21 NGC1068
Daylight contaminated pointings Plots include the observed flux, the mean estimated scattered light flux (given in WUPPE2_SCATLGTF_000000_HW.fits), and the observed flux minus the mean estimated scattered light flux. NOTE: The FITS files contain only the observed flux. (In some cases (e.g. 4413-12 CygLoopB), the mean scattered light flux estimate is too high. As stated earlier, the scattered light flux level can vary by a factor of 2.)
Contains plots of:
PointingID Object Name
WUPPE2_HW_FLUX4.ps 3270-11 NOVA-AQL
3401-10 EG-AND
3407-12 HM-SGE
WUPPE2_HW_FLUX5.ps 3411-11 V1329CYG
3430-11 BF-CYG
4593-11 SK67-90
WUPPE2_HW_FLUX13.ps 2251-11 SK80
2564-11 Wolf1346
5102-10 NGC0362
WUPPE2_HW_FLUX14.ps 4413-10 CygLoopB
4413-11 CygLoopB
4413-12 CygLoopB
WUPPE2_HW_FLUX15.ps 4442-10 CygLoopD
4470-11 CygLp-P8
4473-21 CygLp-11
WUPPE2_HW_FLUX16.ps 5304-11 BD+37 426
5312-11 BD+37 3423
6112-10 AZV95
o ASCII dumps of WUPPE2 Halfwave FITS files
ASCII dumps of each of the WUPPE target Halfwave FITS files have also been provided. Each ASCII dump file is named:
WUPPE2_ObjectID_PointingID_HW.dump (WUPPE2_PHI-PER_220311_HW.dump)
with the Object ID and Pointing ID as defined above. These files are the output of the programs polfitsread.f (for flux & polarimetric data fits files) and fluxfitsread.f (for flux only fits files).
o WUPPE Astro-2 Prime Target Observing Log
Field descriptions
Name ZET-TAU - Target Name (in Mission Target List)
ID 2209-10 - Target ID
Ref J22 - Publication Reference (J=Refereed Journal,
C=Conference Proceedings,A=AAS Abstract)
(see www.sal.wisc/edu/WUPPE/pubswuppe.html)
P W - Prime Instrument (H=HUT,U=UIT,W=WUPPE)
Sp B4IVe - Spectral Type
V 3.0 - V magnitude
Pol 0.629 - Mean %Polarization over approx. 1450-3200A
Error 0.002 - Mean Error in %Pol over approx. 1450-3200A
PA 31.1 - Mean Position Angle (degrees) over approx. 1450-3200A
Exp 1085 - Total Useable Exposure Time (secs)
RA 83.66 - Right Ascension in degrees
Dec 21.11 - Declination in degrees
JD 9785.05 - Julian Date - 2,440,000
MET 06/06:37 - MET start time of observation
GMT 67/13:15 - GMT start time of observation
D/N Night - Day/Night Status
Ap 8 - Observe Aperture (8=6"x12";1=40")
IMC 1 - IMC Status (-1=man.disab;0=auto-disab;1=enab;
2=out of limits)
Red-Comments low gain - Data Reduction Comments
==============================================================================
Summary of Astro-2 WUPPE Observations:
369 total WUPPE Astro2 pointings
119 pointings (89 objects) resulted in polarization measurement across
majority of UV wavelengths.
(11 of these ptgs (10 obj) had only 2 filter pairs observed; the
errors were multiplied by 3)
(3 of these ptgs (3 obj) had some DROOP affects >~2370A)
(6 pointings (5 obj) gave very low S/N results (error over entire
wavelength region >0.9%))
31 pointings (26 obj) have daylight contaminated data >~2100A
(8 of these ptgs (6 obj) had only 2 filter pairs observed; the
errors were multiplied by 3)
--
150 pointings (115 obj) with some polarization result
29 pointings (27 obj) were spectrum only
18 pointings (16 obj) were spectrum only & contaminated by scattered daylight
--
47 pointings (43 obj) with flux only result
172 pointings (128 obj) were scattered light only, object not in aperture,
or some other problem
(no useful result)
==============================================================================
The ASTRO-2 WUPPE OBSERVATION LOG has been extracted to a separate file for ease of access.
o WUPPE Reference List
see www.sal.wisc.edu/WUPPE/pubswuppe.html for the latest list of WUPPE references.
o Further Information
To request copies of relevant WUPPE documents, preprints/reprints, bibliography, or general questions, please contact Marilyn Meade at the UW Space Astronomy Laboratory, Chamberlin Hall, 1150 University Avenue, Madison, WI 53706, telephone (608) 263-4678, or by email at meade@sal.wisc.edu. See also the WUPPE Web site: http://www.sal.wisc.edu/WUPPE
This information was provided by Marilyn Meade of the WUPPE project.
Modifications as pertaining to MAST are italicized.
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