[IAUC] CBET 2796: 20110828 : PR LUPI = NOVA LUPI 2011 = PNV J14542000-5505030

quai en eps.harvard.edu quai en eps.harvard.edu
Mie Sep 14 16:18:41 ART 2011


                                                  Electronic Telegram No. 2796
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
CBAT Director:  Daniel W. E. Green; Hoffman Lab 209; Harvard University;
 20 Oxford St.; Cambridge, MA  02138; U.S.A.
e-mail:  cbatiau en eps.harvard.edu (alternate cbat en iau.org)
URL http://www.cbat.eps.harvard.edu/index.html
Prepared using the Tamkin Foundation Computer Network


PR LUPI = NOVA LUPI 2011 = PNV J14542000-5505030
     Nicholas J. Brown, Two Rocks, Western Australia, reports his discovery of
a possible nova (mag 10.2) on two TMax 400 films taken on Aug. 4.73 UT using a
135-mm-f.l. f/2 Canon camera lens.  Brown's approximate position for the
variable is R.A. = 14h54m20s, Decl. = -55d05'03" (equinox 2000.0); he notes
that nothing brighter than mag 11.7 appears on a film that he took on July
5.85.  The variable was designated PNV J14542000-5505030 when it was posted
on the Central Bureau's TOCP webpage, and based on the spectroscopic reports
confirming the object as a nova (see below), it has been assigned the
permanent GCVS designation PR Lup by N. N. Samus.  Ernesto Guido, Nick Howes,
and Giovanni Sostero report that a CCD image taken of PR Lup remotely through
the 2.0-m f/10 Ritchey-Chretien "Faulkes Telescope South" (+ Bessel R filter)
on Aug. 13.5 shows it at mag 8.4 and at position R.A. = 14h54m23s.09, Decl.
= -55d05'11".2 (equinox 2000.0; USNO-B1.0 catalogue reference stars).  Guido
et al. have posted a color image at website URL http://bit.ly/onysAh, and
a comparison of their image with a Digitized Sky Survey R plate from 1999
is posted at http://bit.ly/pUq8jd.
     Additional magnitudes for PR Lup (visual unless otherwise noted):  July
20.042 UT, [11.5 (W. Liller, Vina del Mar, Chile; 85-mm-f.l. Nikon lens +
Tech Pan film + orange filter); July 25.989, 11.1 (Liller); Aug. 1.008, 10.4
(Liller); Aug. 8.040, 10.3 (A. Amorim, Florianopolis, Brazil; moonlight);
Aug. 8.066, 10.3 (Gonzalo Vargas Beltran, Cochabamba, Bolivia; via E. Waagen,
AAVSO); Aug. 8.375, 10.3 (R. Stubbings, Tetoora Road, Victoria, Australia;
via Waagen); Aug. 12.443, 9.6 (Joseph Brimacombe, Cairns, Australia; remotely
using a 40-cm RCOS telescope + U9000 CCD camera at Macedon Ranges Observatory,
Melbourne, Australia; position end figures 23s.06, 11".2; image posted at
website URL http://www.flickr.com/photos/43846774@N02/6041126507/);
Aug. 13.988, 8.5 (Liller).

     F. M. Walter, Stony Brook University, reports that Brown's suspected
nova is indeed an "Fe II"-type nova.  Photometric and spectroscopic
observations were obtained using the SMARTS/Cerro Tololo facilities, starting
on Aug. 9 UT.  Photometry with the 1.3-m telescope (+ ANDICAM dual-channel
photometer) shows maximum light (V = 9.1, K = 6.2) on Aug. 13.02 (+1/-2 days).
By Aug. 23.0, the nova had faded to V = 11.2 and K = 8.1.  Optical
spectroscopy with the 1.5-m telescope (+ RC specrograph) at a variety of
resolutions between Aug. 9.0 and 22.0 shows the spectrum of a classical
"Fe II"-type nova near maximum light.  Near photometric maximum, on Aug. 12.0,
the blue spectrum (range 365-540 nm; 0.43-nm resolution) showed strong
emission, with P-Cyg absorption, in the Balmer series H-beta through H_11, Ca
II K, and the Fe II multiplets 42 and 49.  At this resolution, a single
absorption component is seen, at a velocity of about -1100 km/s.  On Aug.
13.98, H-alpha had an emission equivalent-width of -17.0 nm, with P-Cyg
absorption at -1100 km/s.  Low-dispersion (1.7-nm resolution) spectra covering
the full optical range on Aug. 16.97 and 22.04 show strong emission from O I
630.0-, 777.4-, and 844.6-nm; C II 732.5-nm; and the Ca infrared triplet.
As of Aug. 22.0, no helium lines were obvious, and no high-temperature lines
had appeared.

     H. L. Malasan, J. Suherli, and E. Wiyando, Bosscha Observatory, Institut
Teknologi Bandung, Indonesia; and A. Arai and H. Kawakita, Koyama Astronomical
Observatory, Kyoto Sangyo University, Japan, report on optical spectroscopic
observations (R about 400) of PNV J14542000-5505030 = PR Lup on Aug. 16.6 UT
at Bosscha Observatory using a 20-cm Schmidt-Cassegrain telescope (+ SBIG DSS7
spectrograph).  The spectra exhibit strong H-alpha, H-beta, and Fe II multiplet
emissions, suggesting that the variable is a "Fe II"-type classical nova.
P-Cygni profiles are absent, and the FWHM of the H-alpha emission is about
1700 km/s.


NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
      superseded by text appearing later in the printed IAU Circulars.

                         (C) Copyright 2011 CBAT
2011 August 28                   (CBET 2796)              Daniel W. E. Green



Más información sobre la lista de distribución Iauc