Output Table Description

For help on a specific output column, you may click on its link in the output table heading, repeated after every 15th row of table output (HTML format only).

The Previous Page and Next Page buttons at the foot of the output form (HTML, ASCII, CSV and TSV formats) enable you to navigate incrementally between output pages when the total number of records returned by a query exceeds the page size as set by the parameter Show in the Query Form. For HTML output, it is generally more efficient to page large queries into several small pages (Show set to 50 or 100 records) than into fewer large pages (250 or 500 records).

The Query Form button returns you to the default query form, and the arrow icon returns you to the top of the output form.

Note: Grey-shaded columns of the output form refer to data stored at the Principal Centre and its mirror (HTML format only).


The camera names and wavelength ranges are:

Image Number

The sequential image number which, combined with the camera name, gives the image identification.


The dispersion mode of the observation:


The aperture used for the exposure:

Observation Date

The U.T. date of the start of the exposure

Observation Time

The U.T. of the start of the exposure

Object Name

The Homogeneous Object Identifier (HOI) for the target. This field has been defined only for output purposes. It is one of the names of the object given by SIMBAD, or following the IAU Minor Planet Center recommendations in the case of comets and asteroids. If the observation has an optional complementary identification (e.g. specifying the exact pointing position within an extended object), it is also displayed.

IUE specific observations have the prefix IUE. Solar System objects have the prefix ZZ. Objects in the Magellanic Clouds have the prefix MC. Exception to these rules are Novae and Supernovae, for which the HOI is always "Nova" and "Supernova", respectively, even if they are not located in the Galaxy. Objects which do not have an individual entry in the CDS are labeled with the prefix AOO (Any Other Object), e.g. AOO FSSW 5

Whenever the query has been made by object name or by a list of objects, the output screen will show the number of names resolved (e.g. the query string 'V*UMi' will result in five different objects: V* alf UMi, V* RR UMi, V* gam UMi, V* SS UMi and V* eps UMi).

More details about the INES Name Resolver can be found here.

Right Ascension

The Homogeneous Right Ascension of the object for equinox B1950.


The Homogeneous Declination of the object for equinox B1950.

Target Name

The target name as provided by the Guest Observer.

Target Right Ascension

The target Right Ascension for equinox B1950 as provided by the Guest Observer.

Target Declination

The target Declination for equinox B1950 as provided by the Guest Observer.

IUE Object Class

The IUE Object Classification code for the target:
Object Classes 00-29
00 Sun 10 WC 20 B0-B2 V-IV
01 Earth 11 WN 21 B3-B5 V-IV
02 Moon 12 Main Sequence O 22 B6-B9.5 V-IV
03 Planet 13 Supergiant O 23 B0-B2 III-I
04 Planetary satellite 14 Oe 24 B3-B5 III-I
05 Minor planet 15 Of 25 B6-B9.5 III-I
06 Comet 16 SD O 26 Be
07 Interplanetary medium 17 WD O 27 Bp
08 Giant red spot 18 28 sd B
09 19 Other UV-strong sources 29 WDB
Object Classes 30-59
30 A0-A3 V-IV 40 F0-F2 50 R, N or S Types
31 A4-A9 V-IV 41 F3-F9 51 Long Period Variable Stars
32 A0-A3 III-I 42 Fp 52 Irregular Variables
33 A4-A9 III-I 43 Late-Type Degenerate Stars 53 Regular Variables
34 Ae 44 G IV-V 54 Dwarf Novae
35 Am 45 G III-I 55 Classical Novae
36 Ap 46 K V-IV 56 Supernovae
37 WDA 47 K III-I 57 Symbiotic Stars
38 Horizontal Branch Stars 48 M V-IV 58 T Tauri
39 Composite Spectral Type 49 M III-I 59 X-ray
Object Classes 60-89
60 Shell Star 70 Planetary Nebula+Central Star 80 Spiral Galaxy
61 ETA Carinae 71 Planetary Nebula-Central Star 81 Elliptical Galaxy
62 Pulsar 72 H II Region 82 Irregular Galaxy
63 Nova-like 73 Reflection Nebula 83 Globular Cluster
64 Other Stellar Objects 74 Dark Cloud (absorption spectrum) 84 Seyfert Galaxy
65 Misidentified Targets 75 Supernova Remnant 85 Quasar
66 Interacting Binaries 76 Ring Nebula (shock ionised) 86 Radio Galaxy
67 77 87 BL Lacertae Object
68 78 88 Emission Line Galaxy (non-Seyfert)
69 Herbig-Haro Objects 79 89
Object Classes 90-99
90 Intergalactic Medium 94 97
91 95 98 Wavelength Calibration Lamp
92,93 96 99 NULLS and Flat Fields

Exposure Classification Code

The exposure classification code for continuum, emission lines and background, derived from the raw image immediately after read-down, and ranging from 0 (weakest) to 9 (heavily saturated) for each category. Before mid-1979 the ECC referred only to continuum and emission lines.

The meaning of the codes for continuum and emission lines is as follows (raw pixels value range from DN=0 to DN=255):
Code Description
0 not applicable
1 no spectrum visible
2 very faint spectrum: max DN < 20 above background
3 underexposed spectrum: max DN < 100 above background
4 weak spectrum: 100 < max DN < 150 above background
5 good: no saturation but max DN over 150 above background
6 a bit strong: a few pixels saturated
7 saturated for less than half the spectrum
8 mostly saturated but some parts usable
9 completely saturated
The meaning of the code for background, implemented on 1 Sep. 1979, is:
Code Description
0 DN < 20
1 21 < DN < 30
2 31 < DN < 40
3 41 < DN < 50
4 51 < DN < 60
5 61 < DN < 70
6 71 < DN < 80
7 81 < DN < 90
8 91 < DN < 100
9 DN > 101
X saturated
Note: Goddard images used the letter X to refer to saturation.

Abnormality Code

This column holds any abnormality flags for the observation. If abnormality codes are present it is advisable to check carefully the COMMENTS section of the FITS primary header. The meaning of the characters in the abnormality code are:
Code Description
T Track lost during exposure
U UVC voltage other than -5kV
R Remnant of previous spectrum visible
Z Contamination by solar spectrum or extended source
A Abnormal read
B Bad scan in the LWP camera
N Non-standard image acquisition
S Serendipity exposure
P Partial read
H History playback
C Data corrupted (DMU anomaly)
W LWR heater warm-up
8 Cross-correlation < 80%
M Missing temperature
O Offset from centre or nucleus

Exposure Mode

A 3-character code indicating whether the exposure was multiple, segmented or trailed. For multiple, X and Y indicate multiple spectra offset along the FES X-axis and Y-axis respectively, and A and O indicate multiple spectra offset along the aperture and another non-standard method respectively, and N indicates not multiple. For segmented, Y and N indicate segmented and not segmented respectively. For trailed, X and Y indicate trailing along the FES X-axis and Y-axis respectively, and N indicates not trailed.

Exposure Time

The effective exposure time in seconds, i.e. the commanded exposure time corrected for camera rise time and exposure quantization, and for aperture length and trail rate quantization for trailed exposures.

Heliocentric Julian Date

The heliocentric Julian date of mid-exposure.

Position Angle

The position angle of the large aperture during the observation.

FES Counts and Mode

The FES counts and mode during acquisition of the target. (F,S) denote fast or slow track, and (U,O) denote underlap or overlap mode. The mode and counts give an estimate of the visual brightness of the target in a S-20 photocathode bandpass.


The number of publications which have used the corresponding observation. By clicking the link, the reference to each publication and links to its abstract in the ADS Astronomy Abstract Service are obtained (HTML format only).

Browse Plot

To generate a browse plot of a spectrum (i.e. quality flags not indicated), click on the corresponding link in the output table column Plot (HTML format only). A panel summarising the spectrum is listed next to the plot, and the full FITS headers may be listed by clicking on the panel title, Summary. For a high resolution observation, the initial browse plot is of the rebinned spectrum; zoom plots of 30Å regions of the parent concatenated, high resolution spectrum may be generated subsequently.

HiRes Zoom Plot

For a high resolution observation, a zoom plot (quality flags not indicated) of a 30Å region of the concatenated, high resolution spectrum may be generated on the Principal Centre/Mirror server by entering the desired central wavelength in Ångstroms in the grey-shaded panel adjacent to the rebinned spectrum plot, and either pressing Enter/Return or clicking Plot Zoom.

A new viewport, centred on the input wavelength rounded to the nearest Ångstrom, is created for the high resolution zoom; you therefore have an overview of the entire spectrum in the rebinned plot, and a simultaneous detailed view of a 30Å region of the parent concatenated, high resolution spectrum. The viewport is automatically refreshed for subsequent zooms (on the same or a new spectrum). Clicking Reset Panel clears, and returns focus to, the wavelength input box.

Note:You may encounter a problem creating zoom plots with Internet Explorer 4.0/4.01 under Windows 95 or Windows NT 4.0. If so, it is easily rectified.

Save Plot

To save a copy of a browse or zoom plot on your local computer, place the mouse cursor over the plot, click mouse button three (rightmost), and select "Save Image As..." [Source] in Netscape, or "Save Picture As..." [GIF] in Internet Explorer. The resultant disk file can then be re-plotted and printed with an image display utility such as xv. The default GIF file-naming convention is consistent with the FITS file-naming convention:

FITS Headers

To list the FITS primary and binary table headers of a low resolution or rebinned high resolution spectrum, click on the corresponding link in the Header column of the query output table (HTML format only). The FITS headers may also be listed for a particular spectrum by clicking on Summary in its browse plot window.

Fetch and Mark

A detailed description of data retrieval options and compression schemes available in the HTML-format output form is given here.

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Last update: June 22, 2000.