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Mouse: A Mini Observatory for UV Space Exploration of the Galactic Poles and Equator

Published online by Cambridge University Press:  26 July 2016

R. Ragazzoni ,
L. Buson ,
M. Turatto ,
A. Bianchini ,
E. Cappellaro ,
M. Cecconi ,
F. La Franca ,
U. Munari ,
S. Ortolani  and
I. Porro
...Show all authors
R. Ragazzoni
Affiliation:
Astronomical Observatory of Padova, Italy
L. Buson
Affiliation:
Astronomical Observatory of Padova, Italy
M. Turatto
Affiliation:
Astronomical Observatory of Padova, Italy
A. Bianchini
Affiliation:
Department of Astronomy, University of Padova, Italy
E. Cappellaro
Affiliation:
Astronomical Observatory of Padova, Italy European Southern Observatory, La Silla, Chile
M. Cecconi
Affiliation:
Center of Studies and Activities for Space ‘G. Colombo’, University of Padova, Italy
F. La Franca
Affiliation:
Department of Astronomy, University of Padova, Italy
U. Munari
Affiliation:
Astronomical Observatory of Padova, Italy
S. Ortolani
Affiliation:
Department of Astronomy, University of Padova, Italy
I. Porro
Affiliation:
Center of Studies and Activities for Space ‘G. Colombo’, University of Padova, Italy
P. Rafanelli
Affiliation:
Department of Astronomy, University of Padova, Italy Center of Studies and Activities for Space ‘G. Colombo’, University of Padova, Italy
R. Stagni
Affiliation:
Department of Astronomy, University of Padova, Italy Center of Studies and Activities for Space ‘G. Colombo’, University of Padova, Italy
F. Bertola
Affiliation:
Department of Astronomy, University of Padova, Italy Center of Studies and Activities for Space ‘G. Colombo’, University of Padova, Italy
P.L. Bernacca
Affiliation:
Department of Astronomy, University of Padova, Italy Center of Studies and Activities for Space ‘G. Colombo’, University of Padova, Italy

Abstract

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The small orbiting observatory MOUSE is described in its essential features. Insights in the optical solution (a 2 mirrors 3 reflections telescope using pure hyperbolical surfaces, no aspherics) are given which fit such type of optical layout to scientific requirements. An in-flight recentering of the photons collected by a solar-blind photon counter device will allow for an equivalent angular resolution of 2–3 arcsec over a field-of-view exceeding one square degree. The capabilities of the proposed satellite (imaging, low resolution grisms, polarizers) are described. The choice of the selected sky areas (the two Galactic Poles, the galactic equator and some Bulge Windows) is justified in terms of forefront astrophysical scientific objectives requiring imaging in UV over large fields. The science comprises UV analysis of a complete sample of QSOs, stellar population in galaxies, White Dwarfs, Globular and Open Clusters and OB Associations. In addition a plan for the early UV detection of Supernova events is described.

Type
Part One: Wide-Field Sky Surveys and Patrols
Information
Symposium - International Astronomical Union , Volume 161: Astronomy from Wide-Field Imaging , 1994 , pp. 52 - 54
Copyright
Copyright © Kluwer 1994