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[vsnet-preprint 83] V2540 Oph paper
V2540 Oph paper
The following paper will appear as IBVS No. 5309.
The figures are available at:
http://vsnet.kusastro.kyoto-u.ac.jp/pub/vsnet/preprints/V2540_Oph/
Regards,
Taichi Kato
===
\documentstyle[twoside,epsf]{article}
\input{ibvs2.sty}
\begin{document}
\IBVShead{5309}{xx xxx 2002}
\IBVStitletl{V2540 O\lowercase{ph} (N\lowercase{ova} O\lowercase{ph} 2002):
Large-Amplitude Slow Nova}\
{with Strong Post-Outburst Oscillations}
\IBVSauth{Kato,~Taichi$^1$; Yamaoka,~Hitoshi$^2$; Ishioka,~Ryoko$^1$}
\vskip 5mm
\IBVSinst{Dept. of Astronomy, Kyoto University, Kyoto 606-8502, Japan, \\
e-mail: (tkato,ishioka)@kusastro.kyoto-u.ac.jp}
\IBVSinst{Faculty of Science, Kyushu University, Fukuoka 810-8560, Japan,
e-mail: yamaoka@rc.kyushu-u.ac.jp}
\IBVSobj{V2540 Oph}
\IBVStyp{N}
\IBVSkey{nova, astrometry, identification, classification}
\begintext
V2540 Oph (Nova Oph 2002) was independently discovered by Katsumi Haseda
and Yuji Nakamura at magnitude 9.0 on 2002 January 24
(Haseda et~al. 2002). Retter et~al. (2002)
detected emission lines of hydrogen and Fe II, indicating that the object
is an Fe II class nova caught in the early decline stage. Later examination
of photographs revealed that the nova was already at magnitude 8.9
on 2002 January 19 (Seki et~al. 2002).
Since the detection of the outburst, the nova has been intensively
monitored by a number of observers.
Figure 1 shows the light curve constructed from visual, CCD $V$-band and
photovisual observations reported to the VSNET Collaboration.\footnote{
http://vsnet.kusastro.kyoto-u.ac.jp/vsnet/} The nova showed
strong post-maximum oscillations up to 1 mag. The large-amplitude
early stage oscillations resemble those observed in V1178 Sco =
Nova Sco 2001 and V4361 Sgr = Nova Sgr 1996 (Kato, Fujii 2001).
The light curve of V2540 Oph also resembles that of V2214 Oph =
Nova Oph 1988 (Lynch et~al. 1989), which has been later suggested to be
a magnetic nova (Baptista et~al. 1993).
Superimposed on these oscillations, the nova showed a steady fade
at 0.033 mag d$^{-1}$. [This rate was determined using
the data between 2452294 and 2452341, during which the general trend
of the fading can be approximated by a single decline rate. The last part
of the light curve, when the nova underwent a long-lasting brightening,
was not used in this analysis. If we incorporate the last part of the
light curve, the average decline rate becomes 0.013 mag d$^{-1}$, which
may more severely constrain the following discussion].
By applying the recently calibrated relation
(Downes, Duerbeck 2000) of absolute maximum magnitude vs
rate-of-decline (MMRD) in classical novae, we obtain the expected
absolute $V$-band maximum magnitude of $M_{\rm V}$=$-$6.8$\pm$0.6.
We performed the accurate astrometry with the images obtained by
Kyoto 0.30-m telescope taken on Mar. 8.23 UT, which revealed the
position of the nova as: R.A. = 17$^{\rm h}$ 37$^{\rm m}$
34$^{\rm s}$.385 $\pm$ 0$^{\rm s}$.017, Decl. = $-$16$^\circ$
23$^\prime$ 18$^{\prime\prime}$.19 $\pm$ 0$^{\prime\prime}$.18
(equinox 2000.0, using 59 UCAC1 reference stars). This position is
marginally consistent of the reported position by K. Kadota, who
measured Haseda's discovery films (Haseda et~al. 2002).
No corresponding object was found on
DSS and 2MASS scans within 2$^{\prime\prime}$.5 of the nova, setting
an upper limit of the prenova magnitude of $\sim$21 (Figure 2; a wider
field map together with the outburst image is shown in Figure 3).
\IBVSfig{9cm}{v2540-fig1.eps}{
Light curve of V2540 Oph (Nova Oph 2002) constructed from visual,
CCD $V$-band and photovisual observations reported to the VSNET
Collaboration.
}
\IBVSfig{10cm}{v2540-fig2.eps}{
The position of V2540 Oph (square) on DSS2 red image. No prenova
can be found to the image limit (mag $\sim$21). The north is up, and
the east is left.
}
\refstepcounter{figure}
\begin{figure}[hpt]
\normalsize
\vskip 3mm plus 1mm minus 1mm
\centerline{\epsfysize=8.0cm \epsffile{v2540-fig3a.eps} \hskip 2mm
\epsfysize=8.0cm \epsffile{v2540-fig3b.eps}}
\vskip 2mm plus 1mm minus 1mm
\begin{center}
{\figfon Figure \thefigure .}
\figcap Field map of V2540 Oph. Each panel shows 5 arcminutes square,
north is up, east is left. (Left) DSS image. A thick small square
with a hair shows the position of V2540 Oph (see Fig. 2), and a thin box
shows the field of Fig. 2. (Right) Kyoto image taken on 2002 Mar 8.23.
\large
\end{center}
\end{figure}
\vskip 4mm plus 1mm minus 1mm
This indicates that the lower limit of
the outburst amplitude is $\sim$12.5 (by adopting the observed maximum
magnitude of 8.5), which is unusually large for a slow nova
with a decay rate of 0.033 mag d$^{-1}$.
By using the above expected absolute $V$-band maximum magnitude, we can
set an upper limit of $M_{\rm V}$$\sim$5.7 for the nova progenitor.
This magnitude is extremely faint for known prenova magnitudes and other
novalike cataclysmic variables (Warner 1986, 1987).
[Available observations suggest that the true maximum of the
nova msut have been missed. By considering this, both the decline rate
and the outburst amplitude could be larger than the values in this
discussion. However, we consider this effect will not severely affect
the conclusion, because 1) the MMRD-relation
(della Valle, Livio 1995, Downes, Duerbeck 2000)
is known to be relatively flat (i.e. little depends on the decline rate)
around the decline rate in question; a brighter maximum will therefore
tend to pose a more stringent upper limit for the prenova), and 2)
the reported spectrum (Retter et~al. 2002) suggests that the object
was caught during an early decay stage.]
Such a faint prenova magnitude would require a small mass-transfer
rate, a small dimension of the disk, or a high inclination. Because
V2540 Oph is a slow nova, the low mass-transfer rate is a rather
unlikely explanation. We propose that the nova should have either
a short orbital period or a high inclination. Among the well-observed
classical novae, V2540 Oph most resembles the presumed magnetic nova
V2214 Oph in many aspects: large outburst amplitude,
slow rate of decline, and the presence of prominent oscillations.
Since the characteristic double-wave orbital modulations were already
present during the decay stage of V2214 Oph (Baptista et~al. 1993),
we strongly encourage observers to detect orbital signatures in V2540 Oph.
\vskip 3mm
We are grateful to all observers who reported vital observations to VSNET.
This work is partly supported by a grant-in aid [13640239 (TK),
14740131 (HY)] from the
Japanese Ministry of Education, Culture, Sports, Science and Technology.
This research has made use of the 2MASS scan at NASA/IPAC Infrared Science
Archive, the Digitized Sky Survey producted by STScI, and the VizieR
catalogue access tool.
\references
Baptista, R., Jablonski, F.~J., Cieslinski, D., \& Steiner, J.~E.\ 1993,
{\it ApJ}, {\bf 406}, L67
della Valle, M., \& Livio, M.\ 1995, {\it ApJ}, {\bf 452}, 704
Downes, R.~A., \& Duerbeck, H.~W.\ 2000, {\it AJ}, {\bf 120}, 2007
Haseda, K., Nakamura, Y., Soma, M., Kadota, K., West, D., \& Pearce, A.\
2002, {\it IAUC}, No. 7808
Kato, T., \& Fujii, M.\ 2001, {\it IBVS}, No. 5150
Lynch, D.~K., Rudy, R.~J., Rossano, G.~S., Erwin, P., \& Puetter, R.~C.\
1989, {\it AJ}, {\bf 98}, 1682
Retter, A., O'Toole, S., Stathakis, R., Pogson, J., \& Naylor, T.\ 2002,
{\it IAUC}, No. 7809
Seki, T., Sato, H., Kato, T., Nishimura, H., Muraoka, Y., Garcia, J.,
Linnolt, M., \& Pearce, A.\ 2002, {\it IAUC}, No. 7809
Warner, B.\ 1986, {\it MNRAS}, {\bf 222}, 11
Warner, B.\ 1987, {\it MNRAS}, {\bf 227}, 23
\endreferences
\end{document}
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