Table 1: Count rate conversion factors to unabsorbed fluxes (ECF) into the 0.2-1 keV band for black body models with temperatures of 40 eV and 50 eV for different instruments and filters, including a Galactic foreground absorption of 6.66 $\times$ 10²⁰ cm^-2.
Detector Filter 40 eV 50 eV

(10^-11 erg cm^-2 ct^-1)

EPIC PN thin 1.77 1.04

medium 2.15 1.22

EPIC MOS1 thin 9.66 5.14

medium 11.4 5.94

EPIC MOS2 thin 9.23 5.00

medium 11.1 5.78

Chandra ACIS S 7.25 5.10

Chandra HRC I 9.17 6.76

ROSAT HRI 29.9 24.9

ROSAT PSPC 6.42 6.55

**Table 1:** Count rate conversion factors to unabsorbed fluxes (ECF) into the 0.2-1 keV band for black body models with temperatures of 40 eV and 50 eV for different instruments and filters, including a Galactic foreground absorption of 6.66 $\times$ 10²⁰ cm^-2.
Detector	Filter	40 eV	50 eV
		(10^-11 erg cm^-2 ct^-1)
EPIC PN	thin	1.77	1.04
	medium	2.15	1.22
EPIC MOS1	thin	9.66	5.14
	medium	11.4	5.94
EPIC MOS2	thin	9.23	5.00
	medium	11.1	5.78
Chandra ACIS S		7.25	5.10
Chandra HRC I		9.17	6.76
ROSAT HRI		29.9	24.9
ROSAT PSPC		6.42	6.55

Source LaTeX | All tables | In the text

	1 Introduction
	2 M 31 optical nova catalogue
	3 M 31 and M 33 optical novae detected with XMM-Newton, Chandra and ROSAT
	4 Discussion
	5 Summary and conclusions
	References