The following forms are included in this appendix:
Additional copies of these as well as all other forms are available on request from the observatory.
The information submitted on the Observation Specification Form is used for scheduling Observatory operations and for estimating the exposure times required for each object. One full-size Observation Specification Form should be returned with a regular episode proposal. For added targets and the initial requests for discretionary time, a copy of the reduced size form contained in this appendix is acceptable. Upon approval of a discretionary time program, the proposer will be asked to complete a full size form if he/she has not already done so. Full size forms are available on request from the observatory. An attempt has been made to provide an information format flexible enough to satisfy each user's observing needs, and every attempt will be made to schedule in accordance with the information given.
The IUE Project expects to be experimenting with increasingly automated scheduling routines in preparation for future episodes and IUE observational "windows" restricted by spacecraft constraints that worsen as the spacecraft ages. To ensure that your high priority objects receive greater consideration in scheduling, the importance of each target to your program should be noted in the target priority (RANK) columns of the Observation Specification Form. See the end of this section for detailed instructions on completing the form and specifying priority. Examples which show how the Observation Specification Form should be filled out for various types of objects are included.
Target coordinates are to be specified in 1950 epoch, giving right ascension to a tenth of a second of time and declination to one second of arc. Valid coordinates are necessary because the accuracy of a spacecraft maneuver depends upon the positional accuracy of both the desired target and the previously observed object. The necessity of having an accurate position is not reduced by any presumed "ease" of identifying the target. Furthermore, these coordinates are used to verify that requested (post-peer-review) additions to one program do not duplicate targets on another approved program.
When filling out the forms please note the following:
|Integer running from l to N, where N is the total number of entries.|
The preferred catalog source is the HD.
|Eight alpha-numeric characters, right justified.|
|Coordinates (1950 epoch only)|
|RIGHT ASCENSION: HOURS||HR||I2||14-15|
|TENTHS OF SECONDS||SEC/10||I1||23|
Spectral types are used to derive exposure times.
A single digit from 1 to 9 given as follows. If not specified, a default value
of 5 will be assumed.
|Brightness Mode Indicator||E/F||A1||40|
|Indicates the type of information specified in the next two
(blank) means VIS MAG and B-V.
E means VIS MAG and E(B-V).
|Visual Magnitude||VIS MAG||F6.2||42-47|
|For BRIGHTNESS MODE E or blank, specify visual magnitude, right justified.|
|Color or Wavelength||B-V/E(B-V)||F6.2||49-54|
|If BRIGHTNESS MODE is blank, specify B-V. If omitted, the target is treated as unreddened. For BRIGHTNESS MODE E, specify E(B-V). If omitted, the target is treated as unreddened. Should be right justified.|
|To assist the Observatory in scheduling programs, targets should be ranked by priority, with RANK=1 being the highest. Targets of equal priority can be given equal ranking and rankings need not be sequential. Backup targets, for instance, can be given much lower ranking than the primary targets. If all targets have equal priority and no preferences exist, all targets should be assigned RANK=1. Right justify.|
|Day of Observation||DAY||F7.3||70-76|
|Day of year for the desired time of observation if the date and/or time of observation is scientifically critical beyond the normal beta-angle requirements. This may be specified with a time resolution of up to 0.001 days, and should be right justified. The year is implied by the approximate dates of the observing episode (12 months in length) beginning in June. In order to ensure that requests for specific dates and/or times are considered by the Observatory's scheduler, the Principal Investigator should communicate the program's requirements in writing to the Observatory immediately following program approval.|
|Object Class||OBJ CLASS||A3||78-80|
|Classify each target according to the codes (01 through 99) supplied on the enclosed description of Object Classification. Right justify.|
The following examples should clarify any questions regarding the application of the coding form parameters.
EXAMPLE 1 HD 30614 is to be observed at high resolution (R=1), both long and short wavelength (W=3). Visual magnitudes and B-V are specified (E/F = blank). It is a backup for high radiation shifts and has been given a low (relative) priority (RANK = 10).
EXAMPLE 2 HD 36512 is to be observed at low resolution (R=2), long wavelength (W=1). Visual magnitude and E(B-V) are specified (E/F=E). It too is given a RANK = 10.
EXAMPLE 3 C 273 is to be observed at low resolution (R=2), short wavelength (W=2). An approximate visual magnitude is given. A spectral type entry is not appropriate and so it is omitted.
EXAMPLE 4 AND 5 NGC 4472 is to be observed at low resolution (R=2) and both long and short wavelength (W=3). The short wavelength exposure, as well as those planned for target 7, are the highest priority observations to be made and are assigned RANK = 1. The long wavelength exposure is often a lower, but still important, priority (RANK = 2).
EXAMPLE 6 Jupiter is to be observed on July 29, when it is in a region which will not cause heating of the on-board computer (beta angle=47 degrees). The observer should check the position of the Moon before requesting a specific date or time.
EXAMPLE 7 The subdwarf O star BD+28 4211 is the desired target.
EXAMPLE 8 RU Peg is a variable star, an example of an "OTHER" Catalog Source.
EXAMPLE 9 PKS 2216-038 is the target. Even if the observer does not care about the exposure time (an 8-hour exposure is not expected to overexpose the spectrum of this source), he should still provide as much information as possible, for example the visual magnitude and (B-V), so that it can be included in the observatory log.
|00||Sun||50||R, N, or S Type Star|
|01||Earth||51||Long-Period Variable Stars|
|04||Planetary Satellite||54||Dwarf Novae|
|05||Minor Planet||55||Classical Novae|
|07||Interplanetary Medium and Sky Background||57||Symbiotic Stars|
|08||Great Red Spot||58||T Tauri stars|
|12||Main Sequence O||62||Pulsar|
|16||O sub-dwarf||66||Interacting Binary Stars|
|19||Other Strong UV Sources||69||Herbig-Haro Objects|
|20||B0-B2 V-IV||70||Planetary Nebula + Central Star|
|21||B3-B5 V-IV||71||Planetary Nebula - Central Star|
|22||B6-B9.5 V-IV||72||H II Region|
|23||B0-B2 III-I||73||Reflection, Nebula|
|24||B3-85 III-I||74||Dark Cloud (Absorption Spectrum)|
|25||B6-B9.5 III-I||75||Supernova Remnant|
|26||Be||76||Ring Nebula (Shock Ionized)|
|30||A0-A3 V-IV||80||Spiral Galaxy|
|31||A4-A9 V-IV||81||Elliptical Galaxy|
|32||A0-A3 III-I||82||Irregular Galaxy|
|33||A4-A9 III-I||83||Globular Cluster|
|37||WDA||87||BL Lacertae Object|
|38||Horizontal Branch Stars||88||Emission Line Galaxy (Non-Seyfert)|
|39||Composite Spectral Types||89|
|48||M V-IV||98||Wavelength Calibration Lamp|
|49||M III-I||99||Nulls and Flat Fields|