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IAUC 8358: COMET C/2001 Q4 (NEAT); C/2003 Y11-Y15; 2004ci

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                                                  Circular No. 8358
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)

COMET C/2001 Q4 (NEAT)
     Further to IAUC 8351, W. J. Carpenter (University of
Cincinnati), M. L. Sitko, R. W. Russell, and D. L. Kim report
additional 3-13-micron spectrophotometry of C/2001 Q4, obtained on
June 17.2 UT at Mt. Lemmon (integration time 45 min; reference star
alpha Boo):  "A smooth comet continuum was seen to rise from 3.5 to
8.4 microns, beyond which a moderate silicate emission band was
observed.  An underlying blackbody continuum with a temperature of
about 305 +/- 5 K was fit to the continuum flux at 5, 8.4, and 12
microns.  This grain temperature is about 16 +/- 2 percent higher
than that of an equilibrium blackbody at the heliocentric distance
of the comet.  The silicate-feature-to-continuum ratio was about
1.26 +/- 0.02 -- lower than the values of 1.65 reported on May 14.2
(IAUC 8342) and 1.43 reported for May 31.2 (IAUC 8351).  During the
period of observation, the strength of the silicate feature above
the continuum was unchanged.  The crystalline olivine feature at
11.2 microns continues to be present with approximately the same
contrast as orginally seen.  With our aperture, the comet has the
following narrowband (about 0.25 micron) magnitudes and combined
random errors: [3.7 microns] = 7.75 +0.45/-0.33, [4.7 microns] =
5.68 +0.20/-0.17, [5 microns] = 5.61 +0.23/-0.18, [8 microns] =
1.96 +/- 0.10, [10.5 microns] = 0.43 +/- 0.03, [12 microns] = 0.15
+/- 0.02."

COMETS C/2003 Y11-Y15 (SOHO)
     Further to IAUC 8357, measurements have been reported by K.
Battams (C/2003 Y11) and K. McGleam (remainder) of additional
Kreutz sungrazing comets found on SOHO website images by M. Oates
(C/2003 Y11), R. Matson (2003 Y12, Y14, Y15), and X.-m. Zhou
(C/2003 Y13).  C/2003 Y13 and Y15 were observed in C3 images, while
C/2003 Y11-Y14 were all visible on C2 images.  The reductions by R.
Kisala and orbital elements by B. G. Marsden appear on the MPECs
cited below.

  Comet         2003 UT          R.A. (2000) Decl.       MPEC
  C/2003 Y11    Dec. 26.314      18 24.2   -24 51       2004-L67
  C/2003 Y12         27.333      18 28.4   -24 46       2004-L68
  C/2003 Y13         27.351      18 36.5   -29 21       2004-L68
  C/2003 Y14         27.375      18 29.1   -24 44       2004-L68
  C/2003 Y15         31.870      18 53.8   -25 06       2004-L68

SUPERNOVA 2004ci IN NGC 5980
The report by Park and Foley on IAUC 8357 was an independent

                      (C) Copyright 2004 CBAT
2004 June 18                   (8358)            Daniel W. E. Green

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