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AAVSO Special Notice #183: Update on Nova Eri 2009 AAVSO HOME > publications > special notice

AAVSO Special Notice #183

Update on Nova Eri 2009
November 29, 2009

Contrary to my expectations, this transient object appears to
be a true nova.

H. Maehara, Kwasan Observatory, Kyoto University, reported in
CBET 2053 that a low-resolution spectrum shows Halpha in emission
with FWHM of 3400km/s.  M. Fujii reported on another spectrum
that gives an Halpha FWHM of 3200 km/s, and other emission lines
that suggest He/N nova classification; this classification was
also suggested by Rudy et al., CBET 2055, from NIR spectra.

In addition, Kasia Malek of the "Pi of the Sky" consortium,
reported in [vsnet-alert 11695,11696] that their system obtained
photometry of the nova from 2009/11/13 through 2009/11/26UT,
with the object reaching a peak Cousins-R magnitude of
Rc=5.60 on 2009/11/14.  This gives an outburst amplitude of
about 9 magnitudes, reasonable for a nova.

Bright Star Monitor photometry on 2009/11/28 gave rough colors
and magnitude of V=8.38, (B-V) = -0.18, (V-Rc) = 0.63,
(Rc-Ic) = 0.028, (V-Ic) = 0.67, showing the influence of
the bright Halpha line.  This probably also influences the
Pi-of-the-Sky magnitudes.

These factors taken together strongly suggest that this is
a classical He/N nova, about two weeks after maximum.  Being
bright and in a good observing location for the next few
months, this nova should be followed extensively until the
end of the season.  CCD observers should use filters,
preferably V and B; visual observers should be alert for any
flaring activity.  As suggested by R. Huziak, many meteor
observers acquiring images of the Leonid meteor shower may
have early photometry, which will be especially valuable if
the images were taken in RAW mode on DSLRs.  Since this nova
has a bright progenitor, you may also have images from earlier
periods, and there may be existing published photometry that
can be data-mined.

Charts with comparison stars can be generated with VSP, and
observations can be submitted with names 000-BJR-847,
VSX J044754.2-101043, or N Eri 2009.  We will be updating
the comparison stars to give more accurate photometry and
Rc/Ic bandpasses as soon as the weather improves in the
Southwestern U.S.

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