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IAUC 8630: 2005kd, 2005ke, 2005kf; (2006)

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                                                  Circular No. 8630
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)

SUPERNOVAE 2005kd, 2005ke, 2005kf
     Three apparent supernovae have been reported:  2005kd by T.
Puckett and A. Pelloni (via the 0.35-m automated supernova patrol
telescope; cf. IAUC 8629), and 2005ke and 2005kf by M. Baek, R. R.
Prasad, and W. Li (via LOSS/KAIT; cf. IAUC 8628).

SN      2005 UT      R.A.  (2000.0)  Decl.    Mag.     Offset
2005kd  Nov. 12.22   4 03 16.88  +71 43 18.9  17.0  0".1 W, 5".0 N
2005ke  Nov. 13.33   3 35 04.35  -24 56 38.8  17.2  40" E, 40" S
2005kf  Nov. 11.53   7 47 26.51  +26 55 32.4  17.2  0".8 E, 0".6 S

Additional approximate magnitudes for 2005kd in PGC 14370:  Sept.
18 and Nov. 9, [20.0; Nov. 13.02 UT, 16.7.  Additional approximate
magnitudes for 2005ke in NGC 1371:  Oct. 24.32, [19.5; Nov. 14.35,
16.3.  Additional approximate magnitudes for 2005kf, which is in a
galaxy located 82" east and 16".5 south of the center of NGC 2449:
Apr. 5.20, [19.5; Oct. 14.52, 17.0; 20.53, 16.5; 31.50, 16.7; Nov.
16.52, 17.5.
     SN 2005kd has been found by an Ohio State University group (J.
Eastman et al., communicated by J. Prieto; cf. CBET 290) to be a
young type-IIn supernova from a spectrogram (range 390-730 nm)
taken on Nov. 13.3 UT with the MDM 2.4-m telescope (+ CCDS); the
spectrum shows a blue continuum and strong hydrogen Balmer (H_alpha,
H_beta, H_gamma, and H_delta) and He I lines in emission at central
wavelengths fully consistent with the recession velocity of PGC

    D. Pray, Greene, RI; P. Pravec and P. Kusnirak, Ondrejov
Observatory; and W. Cooney, J. Gross and D. Terrell, Sonoita
Research Observatory, report that observations obtained during Nov.
1-13 show that the minor planet (2006) consists of a pair of bodies
orbiting each other with a period of 19.15 +/- 0.02 hr and
producing mutual eclipse/occultation events 0.06-mag deep.  There
are present two rotational lightcurves with periods of 3.1183 +/-
0.0002 and 6.656 +/- 0.001 hr, with amplitudes of 0.08 and 0.06 mag,
respectively, that persist during the mutual events.  This suggests
that either the system is binary with both bodies rotating non-
synchronously with the orbital motion or there is a third body
producing the additional period.  A lower limit on the mean-
diameter ratio of the eclipsing pair is 0.22.  Further observations
are needed to fully resolve the system.

                      (C) Copyright 2005 CBAT
2005 November 16               (8630)            Daniel W. E. Green

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