PROBA2 SCIENCE CENTER

Submitted SWAP papers

adegroof — 2011-05-02T09:16:51Z

The following SWAP papers are submitted but not yet published, or not available through ADS. SWAP papers under review YearJournal or ProceedingsTitleAuthorsStatus 2011 Astronomy & Astrophysics (peer-reviewed) Temperature response of EUV imagers on SOHO, STEREO, SDO and PROBA-2 Raftery, Bloomfield, Gallagher, Seaton, Berghmans, De Groof Submitted 2011 Space Weather Space Climate (peer-reviewed) Variations in EUV irradiance, comparison between LYRA and SWAP integrated flux Yalim, (...) - Publications

SWAP performance evolution

David — 2011-01-20T14:10:27Z

Every two weeks, typically on Tuesdays, a SWAP calibration sequence is run consisting of several LED and dark images. The results are processed by Jean-Philippe Halain (CSL) and are summarized in this article. In addition, the temperature evolution of the SWAP and LYRA detectors is shown and commented upon. The graph below shows the evolution of the SWAP response as measured by the bi-weekly LED and dark image sequences (last update on Sep 1st 2011). The decrease in response is not just (...) - 20. Instrument guide

Level 1 calibration steps

adegroof — 2010-05-04T14:38:09Z

The level1 data are generated by applying different calibration steps to level0 data (most of them still in beta version). Below we give an overview of the calibration procedures which are implemented at present. All the calibration steps below leave a trace in the HISTORY keyword of the level1 FITS file. In this way it is always clear which processing steps have been performed on a particular image. P2SW_HDRCHK: Checks critical keywords like detector temperature in the level0 header. (...) - 20. SWAP analysis manual

Progress of SWAP commissioning

David — 2010-02-03T20:24:11Z

PROBA2 was launched on November 2, 2009 and SWAP opened its door on December 14. From then on, to March 2010, we were in the so-called commissioning phase in which every subsystem of the telescope, its electronics and its software is critically tested. Meanwhile thousands of images have been brought to the ground and handled by the PROBA2 Science Center. In this article we give a brief overview of all the fun we had in the first 7 weeks of commissioning. During the first two weeks (...) - About SWAP

Acknowledgements

David — 2010-02-02T14:23:01Z

The SWAP team is proud to share its data according to an open data policy, provided adequate reference is made to the origin of the SWAP data and instrument. The data rights of the SWAP observations are those of on an open data policy: The use of SWAP data is free for analysis and can be used in oral and written presentations, on the conditions stated below: (1) A reference to the SWAP instrument paper must be mentioned, as well as an explicit mention of the version of the used (...) - Publications

Data products: Description of the FITS files headers

sarpy — 2010-01-15T15:43:38Z

SWAP data are stored in FITS files, each with a keyword header containing all the information about the image. All lines in the header contain a keyword and its value, and a short comment concerning the keyword definition. There are two levels of SWAP FITS files: Level Zero (LV0) and level 1 (LV1). A SWAP LV0 FITS file contains all information that is required to analyze any particular image (contains image data in digital numbers (DN)), but at the same time to restrict this information (...) - 20. SWAP analysis manual

Electronics

sarpy — 2010-01-08T12:01:58Z

Detector and Focal Plane Assembly The detector is a technologically advanced CMOS (Complementary Metal Oxide Semiconductor) device coated with a scintillator layer to improve sensitivity in the EUV range. It has 1024 by 1024 pixels, each pixel having a 18 µm x 18 µm size. This particular type of detector, called “High Accuracy Startracker” (HAS), is a radiation hardened, active pixel sensor (APS) detector. The detector will be passively cooled with an external radiator viewing cold space to (...) - 20. Instrument guide

Optical design

sarpy — 2009-12-01T13:00:57Z

SWAP will image a square field of view of 54 arcmin on 1024x1024 pixels, using an off-axis telescope derived from a Ritchey-Chretien system. An elliptical primary mirror combined with a spherical secondary mirror used in quasi-normal incidence will focus the solar light on a technologically advanced CMOS detector, implemented in a focal plane assembly. A set of optical planar baffles will avoid unwanted stray light onto the detector. General overview of the SWAP optical path The overall (...) - 20. Instrument guide

ADS papers: PROBA2

David — 2009-11-10T14:02:18Z

The astrophysics Data System (ADS) is an online catalogue of publications. Below we show the result for the search term "PROBA2". Some PROBA2 papers are not available via ADS, but are considered as interesting overview papers: YearJournalTitleAuthorsLink 2010 ESA bulletin 144 BIG YEAR FOR SMALL SATELLITE - ESA's second in-orbit technology demonstration mission: Proba-2 Gantois, Santandrea, Teston, Strauch, Zender, Tilmans, Gerrits PDF file The result of the ADS search on keyword (...) - Publications

Optical path

David — 2009-11-10T14:01:55Z

TBW - Telescope body

Spectral response

David — 2009-11-10T14:01:15Z

TBW - Telescope body

SWAP Team Members

Dan — 2009-10-22T14:28:11Z

SWAP was developed by the Centre Spatial de Liège (CSL) and the Royal Observatory of Belgium (ROB). However various international partners participated in the realization of SWAP and continue to contribute in the scientific exploitation of the instrument. Royal Observatory of Belgium (ROB) David Berghmans SWAP Science PI Dan Seaton Bogdan Nicula Andrew Stanger Elke D'Huys Carlos Cabanas Parada Christophe Marque Centre Spatial de Liège (CSL) Jean-Marc Defise SWAP Development PI (...) - About SWAP

SWAP Science Goals

Dan — 2009-10-22T13:40:32Z

SWAP will serve as the successor to the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO), a joint ESA-NASA mission that has provided uninterrupted observations of the sun since its 1996 launch. Specifically, EIT monitors activity and dynamics in the low solar corona in four carefully-selected EUV bandpasses; in its nominal 'CME watch' program, an image is taken in its 19.5 nm bandpass every 12 min. The EIT instrument has proved to be (...) - Science outcome

Data analysis software

David — 2009-10-21T18:57:22Z

How to download and read SWAP FITS files? How to process them? Peter Gallagher and his co-workers at Trinity College Dublin have developed a PROBA2/SWAP subtree for the SolarSoft software library. If you would like to add this subtree to your Solarsoft installation do IDL> ssw_upgrade, /swap, /spawn In order to use the SWAP tools, you also need to add SWAP to your instrument list. One of the most powerful tools for SWAP is the SWAP Object, developed by the TCD group. A full tutorial is (...) - 20. SWAP analysis manual

On-Board Operations

Dan — 2009-10-21T14:02:38Z

SWAP data will benefit from series of innovations that have been implemented during the development of the instrument and platform flight software. Most of them can be considered as demonstrators for future space missions. PROBA2 will fly with the new 100 MHz AT697 LEON II microprocessor. It will be the first satellite mission to fly ESA's new high performance, radiation hardened processor which is expected to be used for many other ESA missions such as Solar Orbiter. The extra computing (...) - 20. Instrument guide

ADS papers: SWAP

Boris Giordanengo — 2009-10-14T16:12:15Z

The astrophysics Data System (ADS) is an online catalogue of publications. Below we show the result for the search term "SWAP". Papers which are submitted but not yet available through ADS are listed under the tab "Submitted SWAP papers" (see left menu). - Publications

In two words ...

Boris Giordanengo, Dan — 2009-10-11T01:31:49Z

The SWAP telescope (Sun Watcher using Active Pixel System detector and Image Processing) has been developed as part of the PROBA2 payload. SWAP is directly derived from the concept of the EIT telescope that we developed in the '90s for the SOHO mission. SWAP provides images of the solar corona at a temperature of roughly 1 million degrees, with a cadence of 1 image per 1-2 minutes, and field of view (FOV) of 54 arcmin. Several major innovations have been introduced in the design of the (...) - 20. SWAP