This document defines the catalog entries describing
the HUT Data Archive as delivered to STScI by NSSDC.
Most of the documentation below was obtained from the
project, and the online documentation available
ADF at Goddard Space Flight Center.
The Hopkins Ultraviolet Telescope (HUT) was one
of three instruments which comprised the ASTRO observatory.
ASTRO-1 was flown on the space shuttle Columbia in December, 1990,
and ASTRO-2 was flown in March, 1995 on the space shuttle Endeavor.
General Results Options
Most mission search results pages have the following general
features/options. (Note that the sorting, paging and VOPlot
and the interactive plotting option uses HTML5 which is not
supported in Internet Explorer before version 9.)
Clicking on the column headings at the TOP of the
results table will sort the returned results based on the selected
field. Clicking the column heading a second time will sort the
results in descending order. As of August, 2014 sorting is now
possible with RA and Dec coordinates in sexigesimal notation,
and the previous bugs
whereby exponents are ignored in numbers using exponential notation
(e.g., 6.3E-3 is sorted as if it were 6.3), and signs were
ignored in floating point numbers have both been corrected.
that the sort functions (like many interactive features)
Alternatively, selecting the sort options in the initial query
and will sort the entire search result, not just the displayed
Clicking one of the column headings
at the END of the results table (or clicking the
"columns help" link at the top of the page) will display
help information about the search results page and the displayed
columns (i.e., this page).
By default, results are shown with 500 entries per page, with links
to additional pages if more than 500 entries were returned. The number of
rows per page can be modified using the "Records per Page" form element
on the search form. The total number
of entries returned is set by the "Maximum Records" value from the search page.
One numerical column can be plotted versus another using VOPlot
although see the Help page regarding issues
with the latest version of Java.
For some missions, thumbnail images of the returned entries
can be displayed by clicking the link listed just below the VOPlot link.
The mark column, as described below, can be used to plot spectra
and download files. Plots are now interactive with added features.
Clicking on this box will mark the entry for retrieval or for coplotting.
The data will be downloaded to your computer in a single .tar, .tar.gz, tar.Z or .zip file. Choose the file type you desire. Then click on the "Download selected datasets" button.
After selecting up to 15 datasets to be plotted, click on the "Plot marked spectra" button.
This will bring up a menu of files for the selected datasets.
Choose the files you wish plotted and click the plot marked spectra" button.
This option allows you to choose day or night spectra from the dataset.
he 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.
Adjust the minimum and maximum wavelengths (in Angstroms) and
minimum and maximum fluxes (in erg/cm2/sec/\3 05) to select
the spectral region of interest and to exclude noisy data.
Adjust the X size and Y size in pixels to create the size of plot desired.
The maximum dimensions are 850 by 64 0 pixels.
Use this button to replot the spectra when you have changed the plot range
or plot dimensions.
The HUT data ID uniquely defines each set of HUT observations.
The name is of the form
objectid = object name, and
nnn = a three-digit number describing the Mission
Elapsed Time (MET) in hours.
As an example, data ID HD45677-184 designates a HUT-1 observation
of HD 45677 taken 184 hours into the mission.
Note that for each observation, several data sets may be produced representing
different stages of processing.
Clicking on an "Data ID" entry will display the HUT preview file. This
page contains a plot of calibrated flux vs. wavelength as well as links to display
the FITS header, download a tar file of gzipped FITS files, download
an ASCII file of fluxes and wavelengths, and display
online ADS papers referencing the specific data ID.
Specifies the number of currently known papers
referencing the listed HUT data ID. A blank
indicates there are currently no known papers
listed data ID (although the database may not
yet be complete).
Clicking on a "Ref" entry (other than a "-") will
display the list of known papers with links to the online
These are broad categories assigned by the HUT 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 HUT search page lists only those categories for
which HUT observations were obtained.
Astro Science Classes:
0.0 HUT Camera Sensitivity Targets
0.1 HUT Spectrometer Focus Targets
0.3 UIT Flat Field Sources
0.5 WUPPE Aperture Position Calibrators
0.6 WUPPE Unpolarized & Polarized Standards
0.7 BBXRT Calibration Sources
0.9 Joint Focus and Alignment Targets
1 Solar System Objects
1.3 Asteroids, etc.
2 Individual Stars
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
6.6 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
8.8 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
HUT-1 data includes a comment which usually refers to the
quality of the signal-to-noise ratio. (Not available for HUT-2 data.)
When searching on the comments field, you may want to use wild card such as *S/N* .
Use all caps when entering comments as a search criteria. Remember that only
data acquired during the first ASTRO mission includes comments.
To observe brighter stars, the HUT telescope aperture
could be reduced by closing one or two semi-circular shutter doors
(full aperture size was 5120 cm2), and by opening either of two
small apertures (although
the 1 cm2 aperture was not employed during either mission).
Changes made in HUT-2 software allowed 2 additional
modes in which the shutter doors were partially closed.
All the possible values are shown below:
1 cm2 small aperture
1 cm2 small aperture
50 cm2 small aperture
50 cm2 small aperture
partial aperture 3.9% of full aperture
partial aperture 14.6% of full aperture
Note that door 4 was never used.
Valid search qualifications are 1,2,3,5,6,7
Used to describe one of 8 aperture sizes and/or filters
combinations as shown in the table below
. The Al filter was used
to reject first order FUV light
and provide a pure EUV bandpass (i.e., 415-700 Å), while
the CaF2 filter excluded Lyman-alpha and all wavelengths
below 1250 Å. Note the
aperture selection was revised for HUT-2, so the values in the
database table have different meanings depending on which
mission is referenced.
30" Al filter
32" diameter Al filter
18"x116" CaF2 filter
the qualification 2*,3* and all objects classeNote that slit options 3 and 4 were not used. Valid search qualification values
ID code assigned by the ASTRO missions that identifies each shuttle pointing
includes the jotfid which identifies each target
The Point Id is a character field. The first two characters in the field are codes for
the category of the target. The last two characters identify the specific target.
Where know, the number of the pointing follows a -. The first four characters are
also known at the JOT ID.
The first character is a broad category
(e.g. 2 is the broad category for Individual Stars and 3 is the broad category for
Variable and Binary Stars). The second character is a more specific category
(e.g. 21 would be Supergiants). See the category help to see
how they are broken down.
With this knowledge you can use this field for a more general search on
category. For instance if you are interested in all stars you could enter
2*,3* and all objects classified as stars by the ASTRO project would be found.
See the category to see
ID assigned to each astronomical target name by ASTRO missions.
The JOT ID is a numeric field. It is the numeric version of the first four characters of the point ID column.
Like the Point ID field, you could use it
it to find all of one category. To find all the stars you could enter
2000..4000 and all objects classified as stars by the ASTRO project would be found.
For more information see information on the
Point ID and Category.