RESIK & Diogeness NEWS



(Week 14, 2003, 31 Mar. - 6 Apr.)

In the display above (click to enlarge), the solar X-ray fluence seen by RESIK (black points)  is plotted atop GOES red line. Only periods with good spectral measurements are indicated. The total number of good spectral measurements is given in the title line.


Operation mode:

2 s DGI has been used, except for the interval between
Apr. 04, 22:46:05 UT and Apr. 05, 00:45:56
UT when we tested
1
s DGI with data compression.

'3rd order reflections' (ORD3) is used as stand-by mode.
3rd order
measurements are indicated (green boxes) on  the main 
catalogue page
http://www.cbk.pan.wroc.pl/resik_catalogue.htm .

 


Calibrations made:

No calibrations made

 

ADS Settings:

Since Apr. 05, 00:47:05 UT, new values are used (see Table below).
This new settings are introduced in order to optimize operation of detectors
with the backup power supply.

 

(ORD1) HV: Det. A - 1450 V, Det. B - 1419 V.  (ORD3) HV: Det. A - 1389 V, Det. B - 1328 V.

Channel

l Band

ADS

 Channel

l Band

ADS

#1 #2 3.37 - 3.88 Å 45 - 120 #1 #2 1.16 - 1.29 Å 110 - 230
#2 #0 3.82 - 4.33 Å 75 - 170 #2 #0 1.27 - 1.44 Å 110 - 230
 #3 #3 4.31 - 4.89 Å 105 - 170 #3 #3 1.44 - 1.63 Å 110 - 230
 #4 #1 4.96 - 6.09 Å 145 - 205 #4 #1 1.65 - 2.03 Å 140 - 230
 

      software indexes

      software indexes

       spectroscopic notation (papers)

        spectroscopic notation (papers)


Data gaps due to missing telemetry: ~ 10 h.


Note, that the link to the catalogue page  is now: http://www.cbk.pan.wroc.pl/resik_catalogue.htm.


 

RESIK Effective Areas – First Order Reflection

 

For quantitative analysis of the observed spectra it is of basic importance to know the response function of the spectrometer. This response function is conveniently represented as so-called effective area S, expressed in [cm2].

Known effective areas allow to convert the rates [cts/s/bin] observed in each RESIK spectral bin into „absolute” fluxes [photons/cm2/s]. Determination of wavelength (energy) dependence of effective area is a primary objective of the instrument ground and in-flight calibration and involves detailed knowledge of the instrument construction details.

We present below version_1.0 of  effective area dependence on the wavelength S(λ) calculated according to the following formula (based on Jim Lang’s RAL notice, 1995):

In this formula, parameters have the following meaning:

TBa  - transmission of the detector strengthening bars (probability)
Tf (λ) - transmission of the thermal filter (probability)
Tw(λ) - transmission of the detector window (probability)
ED (λ   - probability of absorption in the detector gas
RC (λ - total reflection coefficient from the monocrystal [radians]
WD    - width of the detector [cm]
- bent radius of (convex) crystal [cm]
2d  - crystal constant (doubled spacing) [Å]
λ - wavelength [Å]

Dependence of individual factors on wavelength has been calculated according to the following equations:

where κ (λ), p, d,  are mass absorption coefficient, density and effective width of Kapton (index k) and aluminium layers of the thermal filter.

Similar quantities for detector’s  beryllium window: 

Probability of absorption in the detector gas mixture of Ar, Xe and CO2, dd - is the detector depth for absorption:

In the calculations, we have used κ(λ) from Tabulations from webpage http://www-cxro.lbl.gov/optical_constants/. The values of other parameters used are given in the Table.

Values of the total reflection coefficient RC have been taken from interpolation of theoretical „ideal”, single crystal calculations performed using Cowan & Brennan Code (Brennan S. and Cowan P.L.: 1992, Rev. Sci. Instr., 63, 850). Uncertainties have been estimated based on comparison with respective data for double crystal reflectivities from Figures 26 and 27 given by Anthony Burek (Space Sci. Instrumentation, 2, 53 – 104, 1976)

 

Table 1. Values of parameters used in calculations of RESIK effective areas.

 

 

In the plot below we present calculated dependence of S(λ) for all channels. It should be noted that the values calculated represent the FIRST ORDER approach only as we have made a number of assumptions, which will be relaxed one by one as further progress in laboratory calibration is reached. The assumptions to be relaxed are:

  • constant dispersion along the crystal length (now dispersion is determined based on the apparent bin position of known spectral lines),
  • - constant (along the crystal length) radius of curvature R (now values of technical specifications are used),
  • - normal incidence of crystal „reflected” radiation on the detector (actually, it slightly changes along the detector aperture),
  • - central location of the source with respect to the solar disk.
  •  

    Figure 1. Wavelength dependence of the RESIK effective area for the first order reflection.



    Prepared by: Marek Siarkowski ms@cbk.pan.wroc.pl, Janusz Sylwester js@cbk.pan.wroc.pl, Stefan Plocieniak sp@cbk.pan.wroc.pl  and Barbara Sylwester bs@cbk.pan.wroc.pl.

    The report presented  has been done in "real time" and so it may contain jargon, blunders, or trivialities. We do not have also an English native speaker in our Wroclaw group! We would be happy to discuss problems mentioned above in more details  if necessary. 


    RESIK data are in the open public domain and can be requested from: http://surfwww.mssl.ucl.ac.uk/surf/data_request.html.

     

    Previous RESIK_weekly notes are in the archive: http://www.cbk.pan.wroc.pl/resik_archive.htm
     


    Page made on 11 April 2003 by:  Anna Kepa ak@cbk.pan.wroc.pl and Jarek Bakala jb@cbk.pan.wroc.pl

     

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