The IDS Home Page
The IDS Home Page
Much of the information provided here is also embedded in the IDS manual, however as a new Sparc-based control system, and data acquisition software have been released, the second half of this manual is now redundant. Useful links for more detailed optical information on the IDS are given below, and for a full discussion of the spectrographs optical design and construction the reader is referred to this IDS manual.
Observers are also referred to the General INT Help page which contains further information software and hardware changes in the INT, and reports of software problems and their solutions e.g. with the DAS
Quick links to related documents for those of you who know what you're looking for (for those who don't, the contents are briefly outlined in the FAQ below):
This page is designed to introduce potential users of the Intermediate Dispersion Spectrograph (IDS) on the INT to it's capabilities and specifications. It will help astronomers who are considering applying for time on the instrument to quickly assess whether their science can be carried out. It provides useful links for those of you who will be observing with IDS, and up-to-the minute advice on practical observing. The ING quality control results, which continually monitor the throughput and performance of the spectrograph and CCD configuration are also available for your perusal.
FaQ for applicants and observers:
Comming soon
Throughput measurements of
a flux standard
A number of flux standards were observed in 1998 with IDS to measure the throughput of the complete telescope+spectrograph+detector system. The figure below shows the results, which were consistent for each observed target. The Y-axis is the apparent AB magnitude of star observed at zenith which gives one detected photon per second per Angstrom. The lowest resolution grating (R150V) was used with a wide slit (10 arcsec), the conditions were photometric. The collimator used was Ag-Red. By comparison, data form the old EEV chip is shown from 1994. The large improvements are due to higher QE of the TEKs, cleaning of the reflecting surfaces within IDS in 1996 and aluminising of the primary mirror which took place the week before the TEK data were gathered.
We shall be monitoring the time-variation of the overall throughput, and new results will appear here. Data for the 500mm camera with TEK3 will also be presented soon, but as a rough guide Observers should consider the throughput of the 500mm to be similar to the 235mm. A quick method for calculating your count-rates under real observing (e.g. with a narrow slit, non-negligible airmass,different grating etc) can be found in the answers to the IDS FAQ.
Observing tips and setting
up the IDS
Click below for important information regarding observing with IDS and setting up, focusing and de-tilting the CCD detectors.
Reported optical problems,
and their investigations
This is a list of recently observed optical problems, which includes documented ghosts, vignetting and any other technical difficulties within the spectrograph itself. Each report will not necessarily include an explanation, but this is designed to be a database of previous problems which Support Astronomers and Observers can check if they are finding any unexplained characteristic of the spectrograph. The reader is also referred to the two paper folders in the INT control room labelled "IDS" for catalogues of older problems (pre-1997).
If, as an Observer or Support Astronomer, you come across any worrying or unexpected optical (or electronic) features within the IDS system, please mail details (including run numbers of the affected images) to the Instrument Specialist who will investigate and record the problem (bgarcia@ing.iac.es)
Last updated March 2000
Begoña García-Lorenzo (Instrument specialist)
bgarcia@ing.iac.es
Paolo García (Deputy)
pgarcia@ing.iac.es
