PKS 2005-489 at VHE: four years of monitoring with HESS and simultaneous multi-wavelength observations

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Table 4:

Optical Monitor parameters and source fluxes for the three *XMM-Newton* observations.
Filter	$\lambda_{\rm e}$ ^a	$A_{\lambda_{\rm e}}/A_{\rm V}$ ^b	$F_{\rm conv}$ ^c	F_4/10^d	F_26/9^d	F_28/9^d
V	5430	1.016	$2.49 \times 10^{-16}$	11.84	14.51	14.42
B	4500	1.293	$1.29 \times 10^{-16}$	9.64	12.08	12.09
U	3440	1.634	$1.94 \times 10^{-16}$	7.48	9.79	9.78
UVW1	2910	1.870	$4.76 \times 10^{-16}$	6.12	8.27	8.14
UVM2	2310	2.827	$2.20 \times 10^{-15}$	5.57	7.74	7.71
UVW2	2120	3.167	$5.71 \times 10^{-15}$	-	-	7.08

Notes. ^(a) The effective wavelength of the filter in Å. ^(b) The ratio of $A_{\lambda_{\rm e}}$ , i.e. the extinction in magnitudes at the effective wavelength of the filter $\lambda_{\rm e}$ , to A_V (5500 Å) obtained from the interstellar reddening curve given by Cardelli et al. (1989) and updated by O'Donnell (1994). ^(c) The conversion factor from rate (Counts s^-1) to flux (erg cm^-2 s^-1Å^-1) from the OM in-orbit calibration (see SAS watch-out page). ^(d) The flux of PKS 2005-489, corrected for galactic extinction, measured in the three epochs (Oct. 4, 2005; Sept. 26 and 28, 2005). The units are mJy.

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