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IAUC 8301: 2004aq; IRAS 05436-0007

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                                                  Circular No. 8301
Central Bureau for Astronomical Telegrams
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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SUPERNOVA 2004aq IN NGC 4012
     Further to IAUC 8296, M. Armstrong reports his discovery of a
supernova located at R.A. = 11h58m27s.25, Decl. = +10o01'04".5,
which is 4".6 west and 12".8 south of the center of NGC 4012.
Available unfiltered-CCD magnitude estimates (by Armstrong, unless
noted otherwise):  2002 May 12 UT, [20.0; 2004 Mar. 2.128, 17.5;
7.080, 17.5; 8.848, 17.5 (D. Buczynski, Lancaster, U.K.).
     N. Elias-Rosa and S. Benetti, Osservatorio Astronomico di
Padova;, V. Stanishev and A. Goobar, Stockholm University; and A.
Jaervinen, Nordic Optical Telescope (NOT), on behalf of the 'ERTN'
(cf. IAUC 7987), report that inspection of a spectrum (range
320-910 nm, resolution 1.7 nm), obtained on Mar. 10.01 UT with the
NOT (+ ALFOSC) at La Palma, that SN 2004aq is a type-II supernova,
about 1 month after explosion.  The spectrum is dominated by P-Cyg
lines of H, Ca II, and Fe II overimposed on a relatively blue
continuum (T_bb about 8000 K).  The expansion velocities deduced
from the H_alpha and H_beta absorptions are about 7700 and 6500
km/s, respectively.

IRAS 05436-0007
     W. D. Vacca and M. C. Cushing, Ames Research Center, NASA; and
J. T. Rayner and T. Simon, University of Hawaii, report on a
medium-resolution 0.8-4.9-micron spectrum of the near-infrared
counterpart to IRAS 05436-0007 (cf. IAUC 8284), acquired on Mar.
8.25 UT using the NASA Infrared Telescope Facility (+ SpeX facility
spectrograph) on Mauna Kea.  The data show a broad absorption
feature centered at 3.1 microns due to water ice (which has an
optical depth of about 0.6) and a deep solid-state absorption at
4.7 microns of frozen CO.  Also present are a number of emission
lines in the Brackett and Paschen series of H I.  The strong
emission lines of Pa_delta and Pa_gamma exhibit prominent P-Cyg
components.  The CO overtone bands at 2.3 microns appear in
emission, as do the Ca II infrared triplet lines at 0.85 micron.
Lines of Mg I, Na I, Ca, and Fe are also seen in emission.  Several
He I lines present in absorption exhibit possible weak P-Cyg
structure.  The P-Cyg features, plus the appearance of the object
in the 2MASS survey at the position of a previously known IRAS and
millimeter-wave source (LMZ 12; cf. Lis et al. 1999, Ap.J. 527,
856), suggest that the current activity of the source may arise
from the onset of a strong outflow or the recent breakout of a
deeply embedded class-I object, rather than from an accretion
episode of a young FU-Ori star.

                      (C) Copyright 2004 CBAT
2004 March 10                  (8301)            Daniel W. E. Green

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