The LOFT wide field monitor

Søren Brandt, M. Hernanz, L. Alvarez, P. Azzarello, D. Barret, E. Bozzo, Carl Budtz-Jørgensen, R. Campana, E. del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, J. L. Galvez Sanchez, D. Götz, F. Hansen, J. W. den Herder, R. Hudec, J. Huovelin, D. Karelin, S. KorpelaNiels Lund, P. Orleanski, M. Pohl, A. Rachevski, A. Santangelo, S. Schanne, C. Schmid, S. Suchy, C. Tenzer, A. Vacchi, J. Wilms, G. Zampa, N. Zampa, J. in't Zand, A. Zdziarski

    Research output: Contribution to journalConference articleResearchpeer-review

    Abstract

    LOFT (Large Observatory For x-ray Timing) is one of the four missions selected in 2011 for assessment study for the ESA M3 mission in the Cosmic Vision program, expected to be launched in 2024. The LOFT mission will carry two instruments with their prime sensitivity in the 2-30 keV range: a 10 m2 class large area detector (LAD) with a <1° collimated field of view and a wide field monitor (WFM) instrument based on the coded mask principle, providing
    coverage of more than 1/3 of the sky. The LAD will provide an effective area ~20 times larger than any previous mission and will by timing studies be able to address fundamental questions about strong gravity in the vicinity of black holes and the equation of state of nuclear matter in neutron stars. The prime goal of the WFM will be to detect transient sources to be observed by the LAD. However, with its wide field of view and good energy resolution of <300 eV, the WFM will be an excellent monitoring instrument to study long term variability of many classes of X-ray sources. The sensitivity of the WFM will be 2.1 mCrab in a one day observation, and 270 mCrab in 3s in observations of in the crowded field of the Galactic Center. The high duty cycle of the instrument will make it an ideal detector of fast transient phenomena, like X-ray bursters, soft gamma repeaters, terrestrial gamma flashes, and not least provide unique capabilities in the study of gamma ray bursts. A dedicated burst alert system will enable the distribution to the community of ~100 gamma ray burst positions per year with a ~1 arcmin location accuracy within 30 s of the burst. This paper provides an overview of the design, configuration, and capabilities of the LOFT WFM instrument.
    Original languageEnglish
    JournalProceedings of SPIE - The International Society for Optical Engineering
    Volume8443
    Issue numberPART 2
    Pages (from-to)84432G
    Number of pages14
    ISSN0277-786X
    DOIs
    Publication statusPublished - 2012
    EventSpace Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray - Amsterdam RAI Convention Ctr., Amsterdam, Netherlands
    Duration: 1 Jul 20126 Jul 2012
    Conference number: 8443

    Conference

    ConferenceSpace Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray
    Number8443
    LocationAmsterdam RAI Convention Ctr.
    Country/TerritoryNetherlands
    CityAmsterdam
    Period01/07/201206/07/2012

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