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Astron. Astrophys. 315, L64-L70 (1996)

ISOPHOT - capabilities and performance

D. Lemke1, U. Klaas1,12, J. Abolins2, P. Ábrahám1,15, J. Acosta-Pulido1,3,12, S. Bogun1, H. Castañeda1,3,12, L. Cornwall2,12, L. Drury4, C. Gabriel12, F. Garzón3, H.P. Gemünd5, U. Grözinger1, E. Grün6, M. Haas1, C. Hajduk1, G. Hall2, I. Heinrichsen6,12, U. Herbstmeier1, G. Hirth1, R. Joseph7, U. Kinkel1,12, S. Kirches1, C. Kömpe8, W. Krätschmer6, E. Kreysa5, H. Krüger1, M. Kunkel1, R. Laureijs12, P. Lützow-Wentzky1, K. Mattila9, T. Müller1, T. Pacher1, G. Pelz1,12, E. Popow10, I. Rasmussen11, J. Rodríguez Espinosa3, P. Richards2, S. Russell4, H. Schnopper11, J. Schubert1, B. Schulz12, C. Telesco13, C. Tilgner1, R. Tuffs6, H. Völk6, H. Walker2, M. Wells14, and J. Wolf1 *,**

1 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
2 Rutherford Appleton Laboratory, Chilton, Didcot, OX11 0QX, UK
3 Instituto de Astrofisica de Canarias, E-38200 La Laguna, Tenerife, Spain
4 Dublin Institute for Advanced Studies, School of Cosmic Physics, 5 Merrion Square, Ireland
5 Max-Planck-Institut für Radioastronomie, Postfach 2024, D-53010 Bonn, Germany
6 Max-Planck-Institut für Kernphysik, Saupfercheckweg, D-69117 Heidelberg, Germany
7 University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, Hawaii 96822, USA
8 Universitäts-Sternwarte, Schillergässchen 2, D-07745 Jena, Germany
9 Observatory, P.O. Box 14, FIN-00014 University of Helsinki, Finland
10 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
11 Danish Space Research Institute, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
12 ISO Science Operations Center, Astrophysics Division of ESA, Villafranca, Spain
13 Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
14 University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, Scotland
15 Konkoly Observatory of the Hungarian Academy of Sciences, P.O. Box 67, Budapest H-1525, Hungary

Received 2 August 1996 / Accepted 30 August 1996

Abstract. ISOPHOT covers the largest wavelength range on ISO from 2.5 to 240 img2.gifm. Its scientific capabilities include multi-filter and multi-aperture photometry, polarimetry, imaging and spectrophotometry. All modes can optionally include a focal plane chopper. The backbone of the photometric calibration are internal standard sources checked against celestial primary standards. The instrument is in excellent condition with all components functioning properly. There is increased detector noise due to the ionizing cosmic radiation affecting the detectability of the faintest sources. All lessons learnt from operating the instrument in space are continously being implemented in the standard data reduction software packages available to every observer. Particular strengths of the instrument include the detectability of very cold sources, high resolution mapping and fast spectrophotometry.The far infrared serendipity sky survey performed during slews of the satellite has successfully started.

Key words: instrumentation: detectors, photometers - infrared: general

* several co-authors have changed the above given affiliation since their involvement in ISO
** ISO is an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA.

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