Central Bureau for Astronomical Telegrams

Central Bureau for Astronomical Telegrams -- Image credits

IAUC 7559: V445 Pup; C/1999 T1

The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which circulars are made available on our WWW site).

Read IAUC 7558  SEARCH Read IAUC 7560

View IAUC 7559 in .dvi or .ps format.
IAUC number

                                                  Circular No. 7559
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions)
URL http://cfa-www.harvard.edu/iau/cbat.html  ISSN 0081-0304
Phone 617-495-7440/7244/7444 (for emergency use only)

     N. N. Samus, Sternberg Astronomical Institute, Moscow, informs
us that the designation V445 Pup has been given to the possible
nova reported on IAUC 7552 and 7556.
     N. M. Ashok and D. P. K. Banerjee, Physical Research
Laboratory, Ahmedabad, report 1.1-2.3-micron spectroscopy of V445
Pup, with the Mt. Abu 1.2-m telescope (+ PRL Near-Infrared Imaging
Spectrometer + HgCdTe NICMOS3 detector array) on Jan. 2.875 UT:
"The J- and H-band (1.08-1.78 microns) spectra are dominated by
emission features arising from C I, C III, and C IV (the prominent
ones being at 1.167, 1.177, 1.259, 1.371, and 1.691 microns).  A
fairly strong unidentified emission feature is seen at 1.132
microns.  The Brackett-series lines of H I in the K and H bands and
the Paschen-beta line are not present.  However, an emission
feature at 1.095 microns, coinciding with the Paschen-gamma line,
is likely due to He II.  A weak emission line with a P-Cyg profile
at 2.062 microns is attributable to He I.  A discernible rise in
the continuum is seen redward from 1.60 microns, indicating the
presence of a cooler component."
     T. Kato, Kyoto University, reports that a 14-min Tri-X
exposure taken by Y. Nakamura (Suzuka, Mie, Japan, 200-mm f/4
camera lens) on 2000 Sept. 26.78 UT shows no object to mag 12.0 at
the location of V445 Pup.
     Photometry by A. C. Gilmore with the 0.6-m f/16 reflector at
the University of Canterbury's Mt. John Observatory, Lake Tekapo,
New Zealand (reference star Cousins E352; uncertainties about 0.01
mag):  Jan. 6.58 UT, V = 9.05, U-B = -0.44, B-V = +0.62, V-R =
+0.40, V-I = +1.04.

     N. Biver, D. Bockelee-Morvan, and J. Crovisier, Observatoire
de Paris-Meudon; D. C. Lis, California Institute of Technology; and
H. Weaver, Johns Hopkins University, report:  "The CO J(3-2) line
at 345.8 GHz has been detected on Jan. 5.7 UT at the Caltech
Submillimeter Observatory (CSO) with a line area of 0.17 +/- 0.03 K
km/s in main-beam brightness temperature.  During Jan. 5-7 at CSO,
we also detected the HCN J(3-2) line (0.19 +/-0.01 K km/s) and
CH_3OH lines at 307.2 (0.23 +/- 0.02), 304.2 (0.16 +/- 0.02), and
241.79 GHz (0.17 +/- 0.03 K km/s).  The average production rates
relative to water, using the water-production rate from Schleicher
et al. (cf. IAUC 7558), are:  CO, 40 percent; CH_3OH, 5 percent;
HCN, 0.11 percent.  This is until now the highest mixing ratio of
CO observed in a comet that is relatively close to the sun."

                      (C) Copyright 2001 CBAT
2001 January 11                (7559)            Daniel W. E. Green

Read IAUC 7558  SEARCH Read IAUC 7560

View IAUC 7559 in .dvi or .ps format.

Our Web policy. Index to the CBAT/MPC/ICQ pages.

Valid HTML 4.01!