J/A+A/543/A86 Nova V1280 Sco BVRcIcy light curves (Naito+, 2012)
Five-year optical and near-infrared observations of the extremely slow nova
V1280 Scorpii.
Naito H., Mizoguchi S., Arai A., Tajitsu A., Narusawa S., Yamanaka M.,
Fujii M., Iijima T., Kinugasa K., Kurita M., Nagayama T., Yamaoka H.,
Sadakane K.
<Astron. Astrophys. 543, A86 (2012)>
=2012A&A...543A..86N 2012A&A...543A..86N
ADC_Keywords: Novae ; Binaries, cataclysmic ; Photometry, CCD
Keywords: stars: individual: V1280 Sco - novae, cataclysmic variables -
stars: abundances - stars: distances
Abstract:
We present optical (B, V, Rc, Ic and y) and near-infrared (J, H, and
Ks) photometric and spectroscopic observations of a classical nova
V1280 Scorpii for five years from 2007 to 2011. Our photometric
observations show a declining event in optical bands shortly after the
maximum light, which took about 250 days to recover. This event was
most probably caused by dust formation. The event was accompanied by a
short (∼30 days) re-brightening episode (∼2.5mag in V), which suggests
that there had been some re-ignition of the surface nuclear burning.
After 2008, the y band observations show a very long plateau at around
y=10.5 for more than 1000 days until April 2011 (∼1500 days after the
maximum light). The nova had taken a very long time (∼50 months) to
enter the nebular phase, according to a clear detection of both [OIII]
4959 and 5007 and is still continuing to generate the wind caused by
H-burning. This finding suggests that historically V1280 Sco is
evolving at its slowest ever measured rate. The interval from the
maximum light (2007 February 16) to the beginning of the nebular phase
is longer than any previously known slow novae: V723 Cas (18 months),
RR Pic (10 months), or HR Del (8 months). It suggests that the mass of
a white dwarf in the V1280 Sco system might be 0.6M☉ or lower.
The distance, based on our measurements of the expansion velocity
combined with the directly measured size of the dust shell, is
estimated to be 1.1±0.5kpc.
Description:
B, V, Rc, Ic, and y magnitudes of V1280 Scorpii observed with the
0.51-m reflector and a CCD camera at Osaka Kyoiku University from
February 2007 to April 2011 are presented. The APPHOT package in IRAF
was used in performing aperture photometry. HD 152819 (B4 IV) was used
as a comparison star to obtain differential magnitudes. The y
magnitudes were measured by comparing with the V magnitude of the
comparison star. Magnitudes of HD 152819 (B=9.951, V=9.935, Rc=9.878,
and Ic=9.847) were taken from Henden & Munari (2007IBVS.5771....1H 2007IBVS.5771....1H).
Objects:
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RA (2000) DE Designation(s)
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16 57 40.91 -32 20 36.4 V1280 Sco = NOVA Sco 2007 a
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
v1280sco.dat 62 133 BVRcIcy magnitudes of V1280 Sco from 2007 to 2011
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Byte-by-byte Description of file: v1280sco.dat
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Bytes Format Units Label Explanations
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1- 7 I7 --- JD Julian date
9- 13 F5.2 mag Bmag ? Johnson B magnitude
15- 18 F4.2 mag e_Bmag ? rms uncertainty on Bmag
20- 24 F5.2 mag Vmag ? Johnson V magnitude
26- 29 F4.2 mag e_Vmag ? rms uncertainty on Vmag
31- 35 F5.2 mag Rcmag ? Cousins R magnitude
37- 40 F4.2 mag e_Rcmag ? rms uncertainty on Rcma
42- 46 F5.2 mag Icmag ? Cousins I magnitude
48- 51 F4.2 mag e_Icmag ? rms uncertainty on Icma
53- 57 F5.2 mag ymag ? Stroemgren y magnitude
59- 62 F4.2 mag e_ymag ? rms uncertainty on yma
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Acknowledgements:
Hiroyuki Naito, naito(at)stelab.nagoya-u.ac.jp
(End) Hiroyuki Naito [Nagoya Univ., Japan], Patricia Vannier [CDS] 14-May-2012