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Observation

[nova] PNV J17335943-3606216: Nova Scorpii 2013

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We performed optical spectroscopic observations of of PNV J17335943-3606216
(= Nova Scorpii 2013;CBET 3542) on 2013 June 04.64UT by using LOSA/F2 spectrographmounted on the 1.3m-Araki telescope.
The obtained low-resolution spectrum (R is about 600 at H_alpha) of the nova shows prominent emission lines of H_alpha, Fe II(42,73,74), O I, N I and Ca II on a highly reddened continuum. The FWHM of H_alpha emission is about 2500 km/s. These features suggest that the object is an Fe II-type classical nova reddened by interstellar extinction.

[dwarf nova] PNV J06270375+3952504

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We performed low-dispersion optical spectroscopic observations
of a new optical transient (CBAT name is PNV J06270375+3952504) using
1.3m Araki telescope with LOSA/F2 (R~580 at H-alpha) on 2013 04 08.45 UT.
The figure shows our spectrum of the object.

The spectrum shows the Balmer series absorption in H-alpha, H-beta and
H-gamma on a bluish continuum emission. The H-alpha absorption seems
to be filled with its emission component. The FWHM of H-beta absorption line
is about 900 km/s.

These spectral features suggest that the object would be a dwarf nova
during its outburst.

PNV J17395600-2447420 : Possible Nova in Oph

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We performed low-dispersion optical spectroscopic observations of the possible nova in Oph (CBAT name is PNV J17395600-2447420 ) using 1.3m Araki telescope with LOSA/F2 (R~580 at H-alpha) on 2012 May 22.62 UT.

Their spectra of the object exhibits broad H-alpha(FWHM about 2800 km/s), H-beta , FeII multiplet and OI(777.4nm) emission lines on a reddened continuum emission. No P-Cygni profiles were detected in their spectrum.
These features suggest that the object would be a classical "Fe II"-type nova.

PNV J17260708-2551454 : Possible nova in Oph

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We obtained a low-resolution (R about 550) spectrum of this object using the 1.3m Araki telescope at the Koyama Astronomical Observatory on Mar. 27.74 UT.  Our spectra show prominent emission lines in H_alpha, Fe II and O I(777.4nm) with P-Cygni profiles on a highly reddened continuum.  The H_beta is also shown in our spectrum. The fwhm of the H_alpha is about 600 km/s.  These features suggest that the object is an Fe II-type classical nova. 

TCP J01495677+5335018 (=XMMSL1 J014956.7+533504)

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We obtained a low dispersion spectrum (R about 550) of TCP J01495677+5335018 (=XMMSL1 J014956.7+533504; ATel #3896)  on Jan. 31.46 UT using LOSA/F2.  The fgure shows our spectrum of the object. 

The Spectrum shows clearly a strong emisson of H-alpha, and absorptions of H-beta and H-ganmma on a blue continuum light.  The absorption component of the H-beta was filled with its emission. The He I at 667.1nm emission and the Na D absorption (E.W about 0.11 nm) were also detected. 

These features suggest that the current brightening of this object would be an outburst phnomenon in a dwarf nova.

[PNV J00422171+4112338] : PN in M31

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We performed optical low-dispersion spectroscopic observations of the possible nova in M31 ( PNV J00422171+4112338 ) on 2011 September 14.643UT using the 1.3m Araki telescope(+LOSA/F2). The total exposure time is 3600 sec.  The figure shows our spectrum of the object. The spectrum exhibits quite broad H-alpha and H-beta emission features. No other significant features are identified in our spectrum.  The FWHM of the H-alpha emission is about 4600 km/s ! This suggests that the object would be a very fast nova and a candidate of recurrent nova.  Such high expansion velocities are often observed in U Sco-type recurrent novae. The photometric observations are needed.

[dwarf nova] PNV J18422792+4837425

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We performed low-resolution optical spectroscopic observations of PNV J18422792+4837425 on 2011  September 6.55 at Koyama Astronomical Observatory. The spectrum shows Balmer series lines on a blue continuum light. The H-alpha line clearly shows a strong emission feature (E.W. about -300) in its absoption component. The H-beta and H-gamma were dominated by absorption components. These results indicates that the object would be a dwarf nova duirng its outburst.

[Possible Nova in M31] PNV J00444794+4138096

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We performed low-dispersion optical spectroscopic observations of a Possible Nova in M31  (CBAT name is PNV J00444794+4138096 ) usign 1.3m Araki telescope with LOSA/F2 (R~580@H-alpha) on 2011 August 07.6UT.  Our spectra of the object (the blue spectrum) exhibits broad H-alpha and H-beta emission lines with FWHM about 2000 km/s. Although other emission / absorption features are invisible in our spectra, such large expanding velocities suggest that the object would be a classical nova.  

[Possible Nova in M31] PNV J00414112+4120117

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We performed low-dispersion optical spectroscopic observations of Possible Nova in M31 (= PNV J00414112+4120117) using the 1.3m Araki telescope on 2011 August 03.7UT.

The red spectrum in the figure shows our preliminary spectrum of PNV J00414112+4120117. Our spectra of PNV J00424483+4118007 and V5588 Sgr are also shown. 

The spectrum exhibits the broad H-alpha, H-beta emissions (FWHM about 1600 km/s) and Fe II multiplet emission features, which suggest that the object is a Fe II-type classical nova after the maximum.

[Possible Nova in M31] PNV J00424483+4118007 is a Classical Nova

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We performed optical spectroscopic observations of PNV J00424483+4118007 using 1.3m Araki telescope with our low-dispersion optical spectrograph (LOSA/F2: R~580@6000) on July 29 and 30 UT at Koyama Astronomical Observatory, Kyoto Sangyo University, Japan.

The figure shows our preliminary specum on July 30.  We detected a broad H-alpha emission line with FWHM = 1800 (+/- 200) km/s in our preliminary spectra on both nights.  In spectra on July 30, H-beta and Fe II multiplet emissons were seen. Although this object is very faint (CCD~17), our spectrum shows a conitmuum light accompanied with a blue-trend. This means that the interstellar reddening toward to the object would be  small. These results suggest that PNV J00424483+4118007 is a 'Fe II'-type classical nova in M31. 

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