******************************************************** ** ** ** IIII NNN NN GGGGG ** ** II NNNN NN GG GG LA PALMA ** ** II NN NN NN GG ** ** II NN NN NN GG GGG INFORMATION ** ** II NN NNNN GG GG ** ** IIII NN NNN GGGGG BULLETIN ** ** ** ** ** ** DATE: 22 August 1997 ** ** NUMBER: 16 ** ** ** ******************************************************** >>>>> INTEGRAL FIELD SPECTROSCOPY ON THE WHT <<<<< Don Pollacco The INTEGRAL unit is situated at the GHRIL Nasmyth platform, mounted together with a newly built acquisition, guiding, and calibration units. INTEGRAL currently contains three science orientated fibre bundles (see below) any one of which can be easily and quickly positioned into the telescope beam. New fibre bundles can be easly mounted within INTEGRAL (provided they are equiped with the correct focal plane and WYFFOS mechanical interfaces). INTEGRAL was succesfully commissioned at the WHT during a six night period in July 1997 and will be offered during semester 98A on a shared risk basis (formal acceptance is due in October 1997). At the focal plane the fibres of each bundle are arranged in two groups, one forming a rectangle, and the other an outer ring which is intended for collecting background light. The physical characteristics of the bundles are given in the accompanying table below. Bundle 1 2 3 4 5 std #1 0.45 205 12.1x7.80 30 90 std #2 0.90 219 16.0x12.3 30 90 std #3 2.70 135 33.6x29.4 20 90 Key: 1 -- fibre core diameter (arcsec) 2 -- total number of fibres 3 -- spatial coverage of the central rectangle (arcsec x arcsec) 4 -- number of fibres in the outer ring 5 -- diameter of the outer ring (arcsec) A first estimation of the throughout gives a mean value of 1 count/A/s for a star of AB magnitude of 17 at 5000A. For further information contact Santiago Arribas (sam@iac.es), Evencio Mediavilla (emg@iac.es), Lewis Jones (lrj@ast.cam.ac.uk), or Don Pollacco, (dlp@ing.iac.es). >>>>> ESA-MUSICOS ON THE INT <<<<< John Telting Under an agreement between the ING and ESA, the new ESA-MUSICOS spectrograph is available for Semesters 98A and 98B. Developed as part of Multi-Site Continuous Spectroscopy (MUSICOS) project led by Claude Catala (Toulouse/OMP) and Bernard Foing (ESA Space Science Department), the spectrograph is now stationed at the INT. MUSICOS is a fiber fed cross-dispersed echelle spectrograph, with a resolution of about 30,000. It has two standard wavelength ranges, covering 3800 - 5900 Angstrom and 4700 - 8500 Angstrom. The spectrograph sits on an optical bench in a room next to the observing floor at constant temperature; this means that the spectrograph is extremely stable. It is fiber-fed from the Cassegrain focus, and uses the standard Cassegrain acquisition and guiding system of the INT. The spectrograph enables the study of line-profile variables at a longer time-base than generally possible at the WHT. With its power to collect a vast part of the visible spectrum in one exposure, the MUSICOS spectrograph offers excellent opportunities for abundance studies, and studies of the interstellar medium. The future of the spectrograph will partly be determined by the demand for observing time. For Semesters 98A and 98B one can apply for MUSICOS following the normal application route. For questions related to MUSICOS, contact Nic Walton (naw@ing.iac.es) or John Telting (jht@ing.iac.es). Information about MUSICOS is also available on the ING web pages (http://www.ing.iac.es/INGtech/musicos_apr96.html). Combined MUSICOS, INT and detector (TEK) throughput: lambda (nm) | S/N per resolution element (10 km/s) | in 40 minutes on a V=7 A0 star --------------+------------------------------------------------------ 400 | 200 500 | 450 600 | 540 700 | 510 800 | 440 >>>>> NEW CCDs <<<<< Rene' Rutten The last few months saw the delivery of three new CCDs: SIT1: a 2048 x 2048 pixel thinned device from STIe, with 24 micron pixels and RQE similar to the TEK CCDs. LOR1A and LOR2: 2048 x 2048 pixel thinned Loral devices, with 15 micron pixels. Excellent RQE, specially in the UV. The Loral CCDs have certain peculiarities which would require too much detail to explain in this Bulletin. For latest details on CCD performance, contact your support astronomer. >>>>> DETECTOR CHOICE <<<<< Rene' Rutten To date, observers had a virtually free choice of detectors on all instruments at ING. The consequence of this high level of flexibility was a large number of detector changes that had to be supported by the technical staff. The large number of detector changes also precluded reaching a stable configuration at the telescope which at times hampered achieving optimal performance of the detectors. In order to rationalize the number of detector changes on the different instruments we have defined for each focal station a default detector which will be offered to the observer. Observers will be informed in advance of the run what the default detector will be. If there is a compelling scientific reason to use another detector then we will certainly try to accommodate this, provided we are notified well in advance. Hence contact your support astronomer at the earlies possible occasion if you have a special detector request. >>>>> HIGHT-SPEED CCD READOUT MODE AT WHT <<<<< Rene' Rutten For high speed spectroscopy at the WHT a new CCD readout mode, called 'drift mode', has been installed. This readout mode is generally available on the WHT data acquisition system. This readout mode may be of interest when only small parts of the CCD are read out, and when speed of operation is crucial to the success of the observations. A manual is available on the ING web pages under http://www.ing.iac.es/~manuals/man_wht.html If after reading the manual you have further queries about this mode of operation then contact your support astronomer, or Rene' Rutten (rgmr@ing.iac.es). >>>>> STATUS OF WHIRCAM <<<<< Rene' Rutten Following the failure of the WHIRCAM array in December 1996, the array was repaired at the manufacturer and is now back in operation at the Nasmyth focus of the WHT. >>>>> THE ING FILTER DATABASE <<<<< John Telting The filters that can be used at the ING imaging stations and in Taurus and UES are all listed together in the ING filter database. Each of these filters has a unique sequence number, which makes it possible to request individual filters to be used for particular observations. Many of the filters are interchangable between different instruments. The ING filter database can be consulted on the WWW (http://www.ing.iac.es/~quality/filter/newfiltdoc.html). This page also holds the most up to date filter information, such as throughput curves of the newest filters. Questions about ING filters, or suggestions to expand our suite of filters, can be directed to John Telting (jht@ing.iac.es). >>>>> PATT-UK (only) ELECTRONIC SUBMISSION FOR SEMESTER 98A <<<<< Bill Martin, Vik Dhillon From Semester 98A the ING are introducing an alternative method of electronic submission, namely, the submission of a LaTeX file. Hence you may use either the usual FORMLOAD system (for 98A only) - see the ING web pages, at http://www.ast.cam.ac.uk/ING/ - or you can use the new LaTeX (stylefile) system, as described in the same web pages and below: [Note that this system is for PATT (UK) applicants only -ie NOT NL or CAT] We are indebted to Richard McMahon, who wrote the patt2.sty file and encouraged us to adopt this alternative system. The new LaTeX (stylefile) system -------------------------------- To use this, simply: 1. Use anonymous ftp to ftp.ast.cam.ac.uk. Login as anonymous and give your email address as password. Then: ftp> cd pub/lpinfo/stylefile and extract the three files: ftp> get patt2_example.tex, patt2_blank.tex, patt2.sty 2. You may also need the Starlink psfig or epsf style files if you want to embed figures in your text (note: we WILL accept embedded figures). These are available in the same ftp area: ftp> get psfig.sty, epsf.sty (you need only copy one of these, depending on whether you prefer to use psfig or epsf for embedding figures). An example of how to embed a figure in LaTeX using psfig is given in patt2_example.tex. If you would like to see how this looks, you must also copy over the file: ftp> get patt2_examplefig.ps 3. Edit/fill-in either the patt2_example.tex or patt2_blank.tex files with the information for your ING PATT proposal. Enter the information between the curly brackets. See the patt2_example.tex file for details. 4. Do not alter the font size from 11pt in the \documentstyle command at the top of the LaTeX file. Similarly, do not reduce the font in the abstract, scientific and technical justification sections by using LaTeX commands such as \small. The TAG members do not look favourably upon proposals written in small font sizes! 5. Ensure that the patt2.sty file is so named in your working directory. Do NOT edit this file. We will be processing your application with the version of patt2.sty appearing in the ftp directory so that any changes you make to your own version of patt2.sty will not be recognised by ours. 6. Ensure that the psfig.sty and epsf.sty files are so named in your working directory. For the same reasons as above, do NOT edit these files. You may embed figures in the LaTeX file using either psfig or epsf. An example of how to do this (using psfig) is given in the patt2_example.tex file. For further information on psfig and epsf, read the top of the psfig.sty and epsf.sty files (or ask your local LaTeX guru). 7. LaTeX your PATT proposal and ensure that it processes correctly. Print out or view your proposal to check all is well. In particular, ensure that your figures appear in the correct location on the form. 8. Send the completed proposal as a LaTeX file (i.e. the .tex file, NOT the .dvi or the .ps files) to: ingpatt@ast.cam.ac.uk. Do NOT send the patt2.sty (or the psfig.sty, epsf.sty) file back to us. 9. Also send any figures as PostScript files (i.e. .ps files). If you have embedded the figures in the text, please ensure that the correct name of the postscript file is given in the subject heading of your email. 10. PostScript figures greater than ~1MB in size should be left in an accessible location and the ftp address or URL provided in the scientific case of the proposal. 11. A reply to the email sender of the proposal will be sent within 2-3 days informing them whether the proposal was processed successfully or not, together with a reference number. If you do not hear anything after this period, please send us a message. 12. Please do NOT copy anything to Swindon! ingpatt@ast.cam.ac.uk is the only place you should send ING proposals to. NO paper proposals please! 13. We will continue to accept the FORMLOAD (.dat) files as before, but only expect to do this for semester 98A. 14. Please ask if you are not sure about anything by contacting: Bill Martin (wlm@ast.cam.ac.uk) or Vik Dhillon (vsd@ast.cam.ac.uk). >>>>> ASTRONOMY STAFF CHANGES <<<<< Rene' Rutten Phil Rudd will be leaving ING after having spend several years on the island, and many more years at the RGO. We wish him well in his further career. >>>>> WHO-IS-WHO FOR INSTRUMENT RESPONSIBILITIES ON SITE <<<<< Contact the following persons if you have queries about specific instruments (usernames@ing.iac.es are given in brackets): WHT - Chris Benn (crb) / Don Pollacco (dlp) INT - Nic Walton (naw) / John Telting (jht) JKT - John Telting (jht) / Nic Walton (naw) JKT imaging - John Telting (jht) / David Sprayberry (dspray) WHT imaging - David Sprayberry (dspray) / Don Pollacco (dlp) INT imaging - David Sprayberry (dspray) / Don Pollacco (dlp) ISIS/FOS2 - Rene' Rutten (rgmr) / Steve Smartt (sjst) AUTOFIB - Don Pollacco (dlp) / Rene' Rutten (rgmr) WYFFOS - Don Pollacco (dlp) / Rene' Rutten (rgmr) UES - Nic Walton (naw) / John Telting (jht) TAURUS - Nic Walton (naw) LDSS - John Telting (jht) / Rene' Rutten (rgmr) IDS/FOS1 - Steve Smartt (sjst) / Don Pollacco (dlp) WHIRCAM - Chris Benn (crb) GHRIL - Chris Benn (crb) ING contacts at RGO-Cambridge: Bill Martin (wlm@ast.cam.ac.uk) Vik Dhillon (vsd@ast.cam.ac.uk) >>>>> SERVICE NIGHTS COMING UP <<<<< Part or all of the following nights are available for the PATT (UK and NL) and CAT Service Scheme on the ING telescopes, subject to schedule changes: D means dark; G, grey and B, bright nights. WHT: ISIS/ Oct 2(D),18(B),Nov 9(B),13-14(B),19(B),21(G),30(D) Aux Port Dec 4(G),7(G),14(B),26(D),Jan 4(G),7(B) (Imaging)/ Jan 27(D) or UES LDSS/UES Aug 19(B) TAURUS/UES Jan 14(B),17(B) Prime Focus Aug 25-26(G), 9-10(G) (Imaging) WYFFOS/AF2 Dec 20-21(G) INT: IDS Aug 21-22(B),Sep 4(D),14(B),24(G), Oct 1(D),9(G),12(B),Nov 5(G),11(B), Jan 5-8(B),11(B), Prime Focus Oct 23(G),Nov 24(G),Dec 18(B),Jan 19(G) (Imaging) JKT: CCD Imaging Aug 25(G),Sep 2(D),26(G),Oct 17(B) Nov 26(D),Dec 3(D),10(B),23(G),30(D) Jan 7(B),24(D) Service requests should be for NOT more than 3 hours, including calibration. For more information on the new service scheme see ING Information Bulletin No. 14, or the announcement in Spectrum No. 12 (Dec. 1996). Use the new html fill-in form on the World-Wide Web at: http://www.ing.iac.es/service/nserviceform.html >>>>> NEXT PATT APPLICATION DEADLINE <<<<< September 30, 1997 for Semester 98A [Feb. 1 to Jul. 31, 1998]. March 31, 1998 for Semester 98B [Aug. 1 1998 to Feb. 1 1999]. >>>>> CONTACTING La Palma <<<<< La Palma can best be reached through INTERNET address: user@ing.iac.es On the WWW look for us at http:/www.ing.iac.es/ ============================================================================== This information bulletin was prepared at the Isaac Newton Group of Telescopes. Distribution is by e-mail only. For free subscriptions send your Internet address to: >>>>>>>>>>>>> bulletin@ing.iac.es <<<<<<<<<<<<<<<< Suggestions regarding content are appreciated. ==============================================================================