- Table 1:
Detection of novae within 2
of M31N 2004-11f.
- Table 2:
Log of archival Chandra observation to the M 31 center from July 2004 to February 2005.
- Table 3:
Log of archival XMM-Newton observation to the M 31 center in July 2004.
- Table 4:
Count rate conversion factors to un-absorbed 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
- Table 5:
Count rate conversion factors from Chandra HRC-I to the full energy band of
Chandra ACIS-I for different spectra derived for Chandra Cycle 6 using
PIMMS v3.7. For all spectra we assume a Galactic foreground
absorption of 6.66
cm-2. Model spectra include: power law
with photon index of 1.7 (PL), thermal bremsstrahlung with a
temperature of 1 keV (BR) and three black body spectra (BB) of
- Table 6:
XMM-Newton, Chandra and ROSAT measurements of M 31 optical nova
- Table 7:
X-ray detections and upper limits of M 31
optical nova candidates within about a year after outburst using Chandra and XMM-Newton
observations from July 2004 to February 2005.
- Table 8:
Observed and derived parameters of X-ray detected optical novae in
- Table B.1:
Nova positions of novae measured by Kamil Hornoch on discovery
images or on best images available at the time of announcement of discovery.
Eight additional positions for novae Nos. 24, 25, 32, 33, 37 to 39, and 41 were
measured on deep images with better signal to noise for novae and with better
resolution compared to announcement images. Discoverers and references for
the individual novae
are given under columns "Dis.'' and "Ref.''. For photometric data of individual novae see