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Subj: Non-detection of Fragment B

We are observing at Palomar with the 200-inch Hale telescope, using
a 7.9 micron imaging spectrometer in imaging mode and a 256x256
InSb at 2.35 microns. We began observing with the imaging spectrometer
at around 02:35 UT and with the InSb camera at around 03:05 UT. We
have not seen anything as of 03:55 UT.

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Subj: Negative observations of B impact from ESO La Silla

Continuing observations with TIMMI at 9um on the 3.5m telescope
and IRAC 2B at 2.2um on the 2.2m at ESO La Silla show that nothing
was seen over the predicted impact site B up to 3:35UT, 17 July.
Conditions were not ideal but this is a strong indication of
differences between the A and B impacts.

Richard West & Richard Hook, ESO Garching

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Subj: Nondetection of B impact

We obtained a sequence of images every 10 seconds from 2:44 to about
3:25 UT, of Jupiter at 1.7 microns (till 3:12) and 2.3 microns
(thereafter), and saw nothing unusual at all on Jupiter's limb.
Predicted impact time was 2:54. Clouds rolled in after 3:25.

John Spencer, Darren DePoy, OSIRIS, CTIO 4-meter.

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Subj: Persistance of A and Lack of B

Observations using a NICMOS2 array and a NICMOS3 spectrometer were obtained
at approx. 0hr U.T. of the A impact site which was clearly visible at 2.2um. A spectrum
of the impact site from 2.0-2.4um at R=1600 was obtained with the impact site clearly
distinguishable from the remainder of the impact latitude. Observations from 02:40 U.T.
through 03:30 U.T. showed nothing from the B impact site in either 2um images or
spectroscopically. In other data we have acquired after the A impact but before B we
observed the H2 auroral emission to be much weaker than in March at the same system III
longitude.
George and Marcia Rieke, Milagros Ruiz, Chad Engebracht, Pat Frawley, Dave Wittman
Steward Observatory 90-inch, Kitt Peak

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Subj: No B Detection

We observed Jupiter from 02:35 to 4:02 UT with 2
narrow band filters centered at 2.22 and 2.36 microns
with a 1 - 2.5 imaging camera on the Apache Point
Observatory 3.5 m telescope. We see no evidence
of any consequence of the B impact. This instrument
is the second generation of the SPIREX camera at
the South Pole which reported a positive detection
of A in the same filter.

Nancy Chanover
Mark Marley
New Mexico State

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Subj: Detection of B plume at 3 micron

Report from W. M. Keck Observatory, Mauna Kea, Hawaii: Impact B.

We observed impact B in a narrow band L band (3.27-3.44 micron); the
plume was faint, but clearly detected at the expected position,
starting at 02:56, fading at around 3:13.

Imke de Pater, James Graham, Garrett Jernigan and collaborators.

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Monitoring the H3+ ionospheric lines at 3.5 microns with CGS4 echelle
spectrometer on UKIRT, Mauna Kea, Hawaii, we saw a fivefold
brightening of the emission around the time of impact of fragment B
(around 2:50 UT) on the east limb of Jupiter. The spectrometer slit
was approximately aligned on the nominal impact latitude. This faded
over 90 minutes.

Steve Miller
Mary-Frances Jagod
Tom Geballe
Tim Brooke

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Subj: IRTF detection of C fragment impact site

Beginning at 1994 Jul 17 7:15 UT, the NASA/Infrared Telescope Facility
observed the development of a bright spot on Jupiter associated with
the impact of fragment C. The NSFCAM near-infrared camera took
0.9-sec integrations every 3.6 seconds at a wavelength of 2.248 +/-
0.011 microns. Starting at 6:51 UT, the camera recorded Io and
Europa, searching for a flash; no flash was obvious but the data are
yet to be photometrically reduced. At 7:15 the telescope moved to
Jupiter, and detected both the remnant of the A impact, with a surface
brightness similar to that of the south polar hood at this wavelength,
and a dim spot from fragment C. By 7:18, site C was considerably
brighter than site A, but by 7:28 site C had faded to about site A's
brightness, and continued to fade until about 7:40, when it was
considerably fainter.

NASA/IRTF Comet Collision Science Team

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Subj: SPIREX detects fragment C impact site

SPIREX detected a fragment C impact site at 07:19 UT at
a wavelength of 2.36 microns. The impact site has also been
monitored at 2.20 microns.

SPIREX will continue to monitor further impacts in these bands.

Mark Hereld, Hien Nguyen, Bernard J. Rauscher, Scott A. Severson
Astronomy & Astrophysics Center, University of Chicago

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Subj: Detection of HCN following impact C

16th July

Detection of HCN 4-3 in emission following impact of fragment C:
---------------------------------------------------------------

We observed the HCN 4-3 line at 354.505 GHz using Receiver B3i on the
JCMT with a beamwidth of 14" FWHM. We tracked on the position of fragment
B for over 1 hour, but did not detect anything to an rms noise of 0.2 K
antenna temperature. Observations of the location of the fragment C
impact point over a 30-minute period as it rotated into view produced a
detection of an approx. 1-K line at the correct velocity (19 km/s). The
line half-width is about 10 km/s. Subsequent observations did not result
in a confirmation of the detection, but Jupiter was setting and the system
temperature rapidly increasing. We are therefore not able to say whether
or not the effect was short-lived.

Matt Griffin, Andre Marten, David Naylor, Gary Davis, Greg Tompkins

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Subj: UKIRT/CGS4 observations of the impact of fragment C

CGS4 (with echelle at about 20 km/s resolution) on UKIRT detected dramatic
changes in the spectrum near 3.5um at the location where the C fragment struck
Jupiter. In addition to a bright continuum (where there previously was
essentially none), the relative strengths of pre-existing emission lines of H3+
changed and many new lines appeared, very few of which are identified by us at
present. In particular, at the wavelength of a previously undetectable "hot
band" transition of H3+, a bright line appeared whose strength surpassed that
of all other pre-existing H3+ lines. A second line, unidentified at present,
succeeded in saturating its central pixel in a ten second exposure. Some of the
lines seem considerably (Doppler) broadened, but, due to the high density of
spectral features, confirmation will have to wait until after the observers get
some sleep. The emission faded with a 1/e time of roughly 15 minutes.

Tom Geballe
Mary-Frances Jagod
Steve Miller
Tim Brooke

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Subj: Japanese Observation of C & D

First report from Okayama Astrophysical Observatory.

We observed the plumes of C and D with Near-IR camera attached to
188cm telescope at Okayama Astrophysical Observatory,
National Astronomical Observatory of Japan.

Thermal plume of C appeared 07:17 UT on July 17 on 2.36 micron images.
It was the brightest around 07:21. The decay phase was observed
over one hour.
Thermal plume of D appeared 12:01 UT on July 17, but it is fainter
than that of C.

J. Watanabe, T. Yamashita, H. Hasegawa, S. Takeuchi, M. Abe,
Y. Hirota, E. Nishihara, A. Mori, S. Okumura,

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Subj: Fragment D - No flash

CCD imaging at Perth observatory of Io, Europa, and the limb of Jupiter
with a duty cycle of only about 30% did not reveal any obvious flashes
associated with the impact of fragment D. Photometric analysis will be
required to remove large scintillation effects.
Mike A'Hearn
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First report from Okayama Astrophysical Observatory.

We observed the plumes of C and D with Near-IR camera attached to
188cm telescope at Okayama Astrophysical Observatory,
National Astronomical Observatory of Japan.

Thermal plume of C appeared 07:17 UT on July 17 on 2.36 micron images.
It was the brightest around 07:21. The decay phase was observed
over one hour.
Thermal plume of D appeared 12:01 UT on July 17, but it is fainter
than that of C.

J. Watanabe, T. Yamashita, H. Hasegawa, S. Takeuchi, M. Abe,
Y. Hirota, E. Nishihara, A. Mori, S. Okumura,


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Subj: Impact e seen at 10 microns with CAMIRAS at NOT

Impact E has been seen at 10 microns with the CAMIRAS camera mounted on the
Nordic Optical telescope at about 15h17min . UT. It was fainter than impact A
seen yesterday.
French-Swedish-Spanish team

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Calar Alto reports the detection of the fireball from fragment E with
the 3.5m telescope at the 2.3 um band. The event was first noted at
15:17:30 and rapidly increased to more than 30 times the brightness of
Europa. By 15:23, the fireball has dimmed to less than Europa's
brightness.

The Calor Alto Observing Team
Max Planck Institut fuer Astronomie (Heidelberg, Germany)
Tom Herbst
Kurt Birkle
Ulrich Thiele

Max Planck Institut fuer Kernphysik (Heidelberg, Germany)
Doug Hamilton

Universitaets-Sternwarte Muenchen (Muenchen, Germany)
Hermann Boehnhardt
Alex Fiedler
Karl-Heinz Mantel

Instituto de Astrofisica de Andalucia (CSIC Granada, Spain)
Jose Luis Ortiz

Astrophysical Institute Arcetri (Florence, Italy)
Giovanni Calamai
Andrea Rickicki

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Subj: Fragment E - No Optical Flashes

Fragment E (predicted at 1505 UT)
CCD imaging at Perth Observatory July 17 1450-1530 UT.
Broad CH4 filter at 893nm, 2-sec exposures of limb of
Jupiter (rest of Jupiter occulted by mask) with 60-70%
duty cycle. No flashes or plumes were obvious in the
raw data. Flashes greater than 25% of a square arcsec
of Jupiter should have been seen in the raw data.
Mike A'Hearn