Lpro Tool

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In SPEX, the lpro component (see Lpro: spatial broadening model) can be used to foldthe spectrum with a user defined broadening profile. This isparticularly useful for the analysis of extended sources with gratingspectrometers, like RGS aboard XMM-Newton. The rgsvprof program createsan input file (usually called vprof.dat) for the lpro component from aMOS1 detector image.

MOS1 detector image. In order to obtain a profile along thedispersion direction of RGS within the same field of view, theprogram asks for a MOS1 image of the source in detector coordinates(DETX,DETY) created by, for example, the XMM-Newton SAS taskevselect. Rgsvprof does not require a particular resolution for theimage, but a resolution of about 1/3 of the XMM-Newton PSF, i.e., is recommended. It is recommended toextract an image using events with energies falling in the RGS band:0.3-2.0 keV.

Cross-dispersion selection region. If the RGS spectrum is extractedfrom a certain area in the cross-dispersion direction, then providethe lower and upper boundary here in arcminutes with respect to thecentre of the field of view. The full RGS strip corresponds to arange between -2.5 and 2.5 arcminutes.

Source width in the dispersion direction. This parameter determinesthe boundaries of the resulting profile in wavelength space. Rgsvprofasks for the width of the source in arcmin centred on the peak of theemission. Choose this width to be somewhat larger than the actualwidth of the source to be sure that the brightest parts are includedin the profile. A width of 10 arcmin is typically enough,but a larger width will increase the size of the vprof.dat file andincrease processing times.

Rgsvprof creates an ASCII file with two columns. The left columnconsists of the grid of wavelengths that the profile is based upon andthe right column gives the normalised cumulative profile over this rangestarting with 0 and ending at 1. The profile will be centred on the peakof the emission.

Note: The cross-dispersion axis in RGS is parallel to the DETXcoordinate axis in MOS1 and has the same direction. This is particularlyhelpful when one extracts spatial regions in the cross-dispersiondirection of RGS.

This program works best for bright extended sources,where the background contribution is negligible. For sources with a lowsurface brightness, in principle a background subtracted image should beused. This program, however, cannot deal with negative values in theMOS1 image.

where is the spectral order, the wavelength, the grating spacing, the incidence angle of aphoton, and the diffracted angle. The wavelength shift due to an offset angle relative to the telescope boresight can be derived by differentiatingthe equation above with respect to, where isthe distance between the gratings (RGA) and the camera (RFC), the focal length of the telescope, and the incidenceangle corresponding to the telescope boresight. The resulting relationfor is:

Note that the value in Peterson et al. (2004) is notcorrect, because the factor was not applied. Thevalue in the above equation is used in rgsvprof to convert the spatialprofile from arcminute scales to wavelength scales.

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