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IAUC 6522: 1996by; 2S 0114+650; 81P

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                                                  Circular No. 6522
Central Bureau for Astronomical Telegrams
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
Phone 617-495-7244/7440/7444 (for emergency use only)

SUPERNOVA 1996by in UGC 3379
     Weidong Li, Qiran Qiao, Yulei Qiu, and Jingyao Hu, Beijing
Astronomical Observatory (BAO), on behalf of the BAO Supernova
Survey, report their discovery of a supernova located 7".2 west and
27".9 south of the nucleus of UGC 3379 (R.A. = 5h58m26s, Decl. =
+68o27'.6, equinox 2000.0).  Unfiltered CCD images taken on Dec. 14
and 15 with the BAO 0.60-m reflector show the object at mag 16.5
and 16.1, respectively.  CCD images of the same field taken on Dec.
7 and 8 (limiting mag approximately 19.0) and on Dec. 11 (limiting
mag approximately 18.0) show no star at the position of SN 1996by.
A low-resolution, high-quality spectrogram (0.48 nm/pixel, range
400-800 nm), taken with the BAO 2.16-m telescope by W. Li, J. Wei,
L. Cao, and Q. Qiao on Dec. 15.75 UT shows that this is a type-Ia
supernova prior to optical maximum.  There is strong Si II 635.5-nm
absorption at 607 nm.  Strong lines of S II, Fe III, and Ca II are
also present, with minima measured at 574.0, 538.6, 481.4, 423.5,
and 393.6 nm.  The photospheric expansion velocity, measured from
the minimum of the Si II doublet, is approximately 14 600 km/s.

2S 0114+650
     R. Corbet, Goddard Space Flight Center (GSFC) and Universities
Space Research Association, for the RXTE ASM team at GSFC and the
Massachusetts Institute of Technology; and J. P. Finley, Purdue
University, report:  "RXTE ASM observations of 2S 0114+650 obtained
between 1996 Jan. 5 and Dec. 5 show the presence of a modulation at
a period of 2.7388 +/- 0.0006 hr and a peak-to-peak amplitude of
approximately 60 percent.  We identify this with the 2.78-hr (+/-
0.01 hr) period reported by Finley et al. (1992, A.Ap. 262, L25),
showing that this is a persistent coherent property of the source.
In addition, the ASM data indicate a modulation at a period of 11.7
+/- 0.2 days (amplitude approximately 60 percent), consistent with
the 11.6-day optical period (Crampton et al. 1985, Ap.J. 299, 839).
These results can be interpreted in terms of a neutron star
rotating with a 2.7-hr period in an 11.6-day eccentric orbit around
its early-type companion."

     Total (visual) magnitude estimates:  Nov. 6.80 UT, 14.4 (A.
Nakamura, Kuma, Ehime, Japan, 0.60-m reflector + unfiltered CCD);
22.14, 13.5: (K. Hornoch, Lelekovice, Czech Republic, 0.35-m
reflector); Dec. 4.33, 12.5 (A. Hale, Cloudcroft, NM, 0.41-m

                      (C) Copyright 1996 CBAT
1996 December 15               (6522)            Daniel W. E. Green

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