(cba:news) Probable nova Eri 2009: the spectrum

[Joe Patterson]

i haven't studied the spectrum yet, but this reported spectrum is much 
more suggestive of a nova, not a dwarf nova (the DN usually show just 
broad Balmer absorption, with some weak emission cores).  Plus Tom 
Krajci's light curve from NM showed only weak variability at best.

The star still has some serious 'splainin' to do; even as a nova, it's 
pretty odd, and possibly a good campaign target for us some day. 
Probably not now, though, unless new spectral evidence emerges, or rapid 
light variations.  Maybe one of the southerners can be the Nova Eri 
sentry...

joe

-------- Original Message --------
Subject: [vsnet-alert 11694] Re: Bright eruptive object in Eridanus
Date: Fri, 27 Nov 2009 00:55:49 +0900
From: Hiroyuki Maehara <maehara at kwasan.kyoto-u.ac.jp>
To: vsnet-alert at ooruri.kusastro.kyoto-u.ac.jp, 
vsnet-campaign-nova at ooruri.kusastro.kyoto-u.ac.jp, 
vsnet-outburst at ooruri.kusastro.kyoto-u.ac.jp
References: <E1NDWnl-0005AE-OZ at mars.kusastro.kyoto-u.ac.jp>

  M. Fujii (Okayama, Japan) obtained a low-resolution spectrum
of the object. He reports that the spectrum shows the Balmer
(FWHM of H_alpha emission is 3200 km/s), He I (447.1, 501.6,
587.6, 667.8, 706.5 nm), N III (464.0 nm), Na I D (589.2 nm),
O I(777.3, 844.6 nm), and Mg II (823.2 nm) emission lines.

http://otobs.org/FBO/fko/nova/pn_eri_20091126.gif


  I also obtained a spectrum of the object which shows broad Balmer,
He I, and N III emission lines. The FWHM of H_alpha emission is 3400km/s.

http://www.kwasan.kyoto-u.ac.jp/~maehara/novae/ERInova2009_20091126.gif


  These features suggest that this object is a He/N nova.

On Thu, Nov 26, 2009 at 02:21:57PM +0900, Taichi Kato wrote:
>    According to CBET 2050, Itagaki-san has discovered a bright (8.1 mag)
> eruptive object in Eridanus (position 044754.21 -101043.1).
> Although this object has been suggested to be a possible nova,
> the object might also be a WZ Sge-type dwarf nova.
> Spectroscopic and time-resolved photometric observations are urged.