XMM-Newton Users Handbook

3.5.3.1 OM operating modes

The OM can operate in the two modes listed in Table 15. These allow either imaging or fast photometry or both simultaneously.

Table 15: The science data acquisition modes of OM

Mode$^1$	Special feature
Imaging	Mosaic of 2-D imaging windows with long exposure times ($>800$ s)
Fast	High time resolution, providing 2-D time-sliced images over small areas.

Notes to Table 15:
1) Both modes can be used simultaneously, as long as total memory capacity and telemetry bandwidth are not exceeded.

• Imaging mode

  The Image Mode emphasises spatial coverage at the expense of timing information. Images can be taken at the full sampling of the instrument or binned by a factor of 2 to yield a resolution element on the sky of approximately 0.5 or 1.0 seconds of arc. The maximum total size of the science windows is determined by the memory available in the Data Processing Unit DPU. A single Image Mode window binned by a factor 2$\times$2 can be up to 976$\times$960 detector pixels, which results in a 488$\times$480 binned pixel image being stored in the DPU. At full sampling (with no binning) the window can be up to 652$\times$652 pixels. The trade off is that the images with unbinned pixels take more memory and therefore more telemetry when downloading the data.

  The maximum allowed integration time for an OM imaging mode exposure is 5 ks. Since the OM in its imaging mode produces accumulated images, there is no timing information attached to individual incoming photons.

  Any drift in the pointing direction of the spacecraft is corrected in the image by tracking guide stars.

  There are three different Imaging Modes: - "EPIC/RGS Image Mode" default combination of 5 exposures in predefined windows. - "Full Frame Low/High resolution Mode" single image covering the OM field of view with or without rebinning. - "Science User Defined Mode" flexible combination of imaging and fast windows of variable sizes and resolutions.

• Fast mode

  The Fast Mode emphasises timing information at the expense of spatial coverage. In its Fast Mode, the OM does not produce accumulated two-dimensional images, but instead produces event lists like the X-ray instruments. This mode is useful for monitoring rapidly variable sources, for example Blazars or accreting binaries. Two small windows can be assigned, each of a maximum of 512 pixels only. Thus the maximum size of an approximately square window would be 22$\times$23 pixels (= 506 total). There is no binning within a Fast Mode window. The pixel locations of individual photons within the window are recorded and assigned a time tag, which has a user-specified integration time of between 500 ms and the tracking frame duration (10-20 s). No tracking correction is applied to Fast Mode data. This can be applied on the ground, from the drift history supplied by the OM. The data are obtained by default in 0.5 s time slices, each preserving the pixel information. Shorter times are in principle possible, but at the risk of overloading the DPU (e.g. when two Fast Mode windows are operated), and are therefore discouraged.

  The maximum allowed integration time for an exposure with one Fast mode window is 4.4 ks, and 2.2 ks if two Fast mode windows are used simultaneously.

  For critical time coverage, it has to be taken into account that during ground station handovers OM exposures are interrupted for 1800 sec.

  Fast mode data can be acquired at the same time as image mode data. The default configuration for fast mode includes a large image window, in which the fast mode one is embedded. In case of User Defined windows, it is recommended to include an image mode window of bigger size than the fast mode one that includes the later.

Each mode has a specific overhead, i.e., time needed for the instrument set-up, before the actual science exposure can start. For both the above OM modes this overhead includes also the reference frame exposure. In addition, about 1000 s are needed before starting the OM exposures for the field acquisition of the satellite star tracker. The reader is referred to § 4.5.2 for a general discussion of the impact of instrumental overheads on the planning of an XMM-Newton observation, and to the XRPS User's Manual for a detailed description of the OM overheads. An interactive web tool is available at the MSSL web page:
http://www.mssl.ucl.ac.uk/www_astro/xmm/om/om_tool_current.html, which may help the user to better handle and understand OM windows and operational overheads.