Deep Impact Observations with MIRO 

19th SWTM for the
International ROSETTA Mission
ESOC
Darmstadt, Germany
September 2, 2005
Samuel Gulkis





Deep Impact Workshop * Hilo, Hawaii * 28-29 July 2005 

Submillimeter Observations of Tempel 1with the MIRO Spectrometer on ROSETTAduring the encounter of DEEP IMPACT 

Samuel Gulkis1, Mark Allen1, Charles Backus1, Gerard
Beaudin2, Dominique Bockelee-Morvan2, Nicolas Biver2,
Jacques Crovisier2, Didier Despois3, Pierre Encrenaz2,
Therese Encrenaz2, Margaret Frerking1, Mark Hofstadter1,
Paul Hartogh4, Wing Ip5, Mike Janssen1, Lucas Kamp1,
Emmanuel Lellouch2, Ingrid Mann6, Duane Muhleman7,
Heike Rauer8, Peter Schloerb9, and Thomas Spilker1


1. Jet Propulsion Laboratory, Cal. Inst. of Tech. , 2. Obs. de Paris, 3. Obs. de Bordeaux, 4. Max Planck Inst. SolarSystem Research, 5. National Central University, Taiwan, 6. University Wilhelm, Germany, 7. Cal. Inst. Of Tech. , 
8. DLR, Germnay, 9. Univ. of Mass. 



(Note comment sgulkis
8/26/05 12:42 PM
Unmarked set by sgulkis)
* 
Figure provided by Biver 
(Text Box comment ROSETTA
ORBIT
)



Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005- 4 
Instrument Description 
30 cm aperture telescope (7.6 arc min at 560 GHz) 
2 uncooled, heterodyne mixers (190 GHz and 560 GHz) with phase lock 
loop and Ultra Stable Oscillator on 560 GHz receiver 
2 Continuum channels 
Submillimeter (560 GHz) mixer feeds 4096 channel, high resolution (44 
kHz /23 m/s) chirp transform spectrometer (CTS) 
- Fixed tuned to transitions of 
* H2O16 (556.936 GHz) 
* H2O17 (552.021 GHz) 
* H2O18 (547.676) 
* CH3OH (3 TRANSITIONS) (553.146, 568.566, 579.151 GHz) 
* NH3 (572. 498 GHz) 
* CO (576.268 GHz) 
Thermal line width of 560 GHz water line at 10 K is 300 kHz 
LO is frequency switched +/- 5 MHz every 5 seconds and alternate 
spectra are subtracted to produce frequency switched spectrum 
Subject of this presentation is MIRO observations of the ground state 
rotational transition of water at 556.936 GHz



Ideal Frequency Switched Spectrum 

FREQUENCY SWITCHED SPECTRUM


AMPLITUDE OF SIGNAL 

0.08 

0.06 

0.04 

0.02 

0 

-0.02 

-0.04 

-0.06 

-0.08 

010020030040050060070080010 MHz between lobes 
BIN NUMBER 

Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-5 




Tempel 1 Observations with MIRO 


Pre-Impact Observations June 29, 2005 (02 hr) to July 4, 2005(05hr45m) [20051800200 to 20051850545] 
Post-Impact Observations July 4, 2005(06hr) to July 8, 2005(09hr58m) [20051850600 to 20051890958] 
Observations divided into on source (Tempel 1) and off sourcepositions. 
There is an automatic calibration every 30 minutes-movablemirror directs beam to warm calibration target, cold calibrationtarget, and then to sky 
Spectrum is recorded every 30 seconds following the sequencof local oscillator (LO) settings [-5 MHz, +5MHz, -5MHz, +5MHz, 
5MHz, + 5MHz] -each LO position is held for 5 seconds.
Recorded spectrum is difference between two local oscillatorsettings 
Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-6 




Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005- 7 
UNBINNED AND SMOOTHED SPECTRA 
POST IMPACT (4Jul-0600/8Jul-0958)2005 
-0.8 
-0.6 
-0.4 
-0.2
0 
0.2 
0.4 
0.6 
0.8
3300 3400 3500 3600 3700 3800 3900 4000 4100 
-0.15 
-0.1 
-0.05
0 
0.05 
0.1 
0.15
3300 3400 3500 3600 3700 3800 3900 4000 4100 
.044 MHz /bin 
26.4 MHz



Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005- 8 
UNBINNED AND SMOOTHED DATA WITH 
SUPERIMPOSED MODEL - POST IMPACT 
-0.8 
-0.6 
-0.4 
-0.2
0 
0.2 
0.4 
0.6 
0.8
3300 3400 3500 3600 3700 3800 3900 4000 4100 
BIN NUMBER (1 BIN = 44 kHz) 
SSB ANTENNA TEMPERATURE, K 
-0.15 
-0.1 
-0.05
0 
0.05 
0.1 
0.15
3300 3400 3500 3600 3700 3800 3900 4000 4100 
BIN NUMBER (1 BIN = 44 kHz) 
SSB ANTENNA TEMPERATURE, K



LEAST SQUARE FIT LINE PARAMETERS 

DATA LINE 
AMPLITUDE 
LINE WIDTH UNSWITCHED 
LINE POSITION 
UNBINNED 
(IDL ) 
0.095 +/- 0.021 K 85.2 +/- 24 BINS 
3.75 MHz +/- 1.0 MHz 
2 Km/s+/- 0.54 km/s 
Bin 3689.5 +/- 16 
Red shift 53.0 +/- 
16 bins = 2.33 
MHz +/- 0.7 MHz 
=1.25 km/s +/- 0.4 
km/s 
SMOOTHED 
(EXCELSOLVER) 
0.11 +/- 0.028 K 70 Bins 
3.1 MHz 
1.65 Km/s 
Deconvolved 
(2.50 MHz/1.34 km/s) 
Bin 3682 
Redshift 45.4 
bins = 2.0 MHz 
=1.07 km/s 

Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-9 




PRE-IMPACT OBSERVATIONS 


DATA FROM 29JUNE02HR TO 4JUL05HR45MIN 2005
[20051800200 TO 20051850545]
32 BIN DATA HAS RMS OF .030 K 
NO SIGNAL WAS DETECTED 
ASSUMING A 3 SIGMA UPPER LIMIT, WE ESTIMATE AN UPPER 
LIMIT SIGNAL AMPLITUDE OF .090 K 
ANALYSIS IS STILL UNDERWAY 
Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-10 




Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005- 11 
UNBINNED & SMOOTHED PRE-IMPACT DATA WITH 
SUPERIMPOSED 3 SIGMA UPPER LIMIT MODEL 
-0.6 
-0.4 
-0.2
0 
0.2 
0.4 
0.6 
0.8
3300 3400 3500 3600 3700 3800 3900 4000 4100 
-0.1 
-0.08 
-0.06 
-0.04 
-0.02
0 
0.02 
0.04 
0.06 
0.08 
0.1
3300 3400 3500 3600 3700 3800 3900 4000 4100 
UPPER LIMIT AMPLITUDE 
=0.090 K (3 SIGMA)



PRODUCTION RATES 


NO DETAILED ANALYSIS HAVE BEEN PERFORMED AT THIS TIME
PRIOR TO THESE OBSERVATIONS, BIVER ESTIMATED (MIRO TEAMMEETING, UNPUBLISHED) THAT WATER PRODUCTION RATE OF1E(28) MOLECULES/SEC WOULD LEAD TO A PEAK ANTENNATEMPERATURE OF 0.125 K. 
SCALING FROM BIVER'S ESTIMATE, UNBINNED LEAST SQUARE FIT 
OF POST-IMPACT DATAT YIELDS PRODUCTION RATE OF 7.6E(27) +/- 
1.6E(27) MOLEC /S 
PRE-IMPACT 3 SIGMA UPPER LIMIT YIELDS MAXIMUM PRODUCTION 
RATE CONSISTENT WITH POST IMPACT DETECTION PRODUCTION 
RATE 
BOCKELEE-MORVAN ESTIMATES QH2O - 6.3E(27) to
9.7E(27)(preferred value)
Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-12 




PRE- AND POST-IMPACT ANTENNA 
TEMPERATURE LIMITS 

0 
0.02 
0.04 
0.06 
0.08 
0.1 
0.12 
0.14 
0.16 
0.18 
Antenna Temperature, K3 SIGMA UPPER LIMIT 
PRE-IMPACT 
3 SIGMA LIMIT 
POST-IMPACT 
DETECTION 
178 180 182 184 186 188 

DOY 2005 

Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-13 




Conclusions 


The ground state rotational transition of water at 556.936 GHzwas detected by the MIRO instrument in the post-impacphase of the observations. (0.204 K km/s) The estimated 
production rate of water is 7.6E(27) +/- 1.6E(27) MOLEC /S
THIS IS A PROVISIONAL NUMBER. 


The detection of water required long integration times. Thesignal to noise was too low to detect variability in the waterproduction rate in the post-impact phase 
No water was detected in the pre-impact phase. Assuming a3 sigma upper limit, we cannot conclude if the waterproduction rate changed(increased or decreased) after the DIimpact 
The MIRO results suggest a red shift gas velocity of 1.25km/s after removing the comet -S/C doppler velocity 
Spectroscopic Observations of Tempel 1 with MIRO Deep Impact Workshop - Hilo * 27-28 July 2005-14