Transcript 2mm.ppt

COMPLETE 2MM SPECTRAL LINE SURVEY (130-170 GHZ)
OF
SGR B2N, SGR B2OH, IRC +10 216, ORION (KL), ORION-S,
W51M AND W3(IRS5)
Anthony J. Remijan
NRAO Assistant Scientist – ALMA Commissioning
Barry E. Turner – In Memoriam
NRAO Scientist
Diane P. Leigh (University of Virginia) &
Andrew J. Markwick-Kemper (University of Manchester)
63rd Ohio State University International Symposium on Molecular Spectroscopy
Columbus, OH
June 19, 2008
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
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Presentation Outline
http://www.cv.nrao.edu/~Turner2mmLineSurvey
http://arxiv.org/abs/0802.2273
• Survey Overview
– Dedication to Barry
– Scientific & Technical Justification
• Accessing the data
– Reduced data using SLiSE
• Initial Survey Results
– Composite spectra
– Orion KL molecule fits – uncovering new transitions?
– Sgr B2N molecule fits – re-confirming interstellar acetone?
• Future plans/disseminating the data to the community.
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Survey Overview
Until very recently, this project was entirely the work of Barry E. Turner. He wrote the
original proposal and did all of the observing.
B.E. Turner passed away on Saturday, May 10th after a long struggle with Parkinson's
Disease.
This presentation is a tribute to him and the work he performed on these data and to give
further information about the project and important information to the astronomical
community who will use these data.
We fully expect users of these data to give B.E. Turner
and this work the appropriate citation and credit.
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Survey Overview
Importance of a 2mm Line Survey:
At the time of the data collection, no published 2mm survey existed. In addition, highexcitation sources such as Orion the 2mm window will contain more detectable lines
(and hence more information) than the 3mm window, because of larger line
strengths on average, yet fewer lines than the 1.3mm window.
Sources of Interest: SGR B2N, SGR B2OH, IRC +10 216, ORION (KL), ORION-S, W51M
AND W3(IRS5)
From the forgoing, it is obvious that the astrochemistry most interesting regions are Orion
KL, Sgr B2N, W51M, and IRC +10 216, and the proposal focused primarily on these
regions, which occupy complementary positions in the sky.
At the time, the overwhelming body of astrochemical knowledge is based on only two
sources: Orion(core) and SgrB2(OH). How typical are these sources? However,
different positions within each of the sources reveal quite different chemical
abundances. Even greater differences appear to exist between entirely different star
forming regions such as SgrB2 and Orion. W51M appears to be quite different
again. Finally, IRC10216 serves to define the differences between circumstellar and
interstellar chemistry.
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Survey Overview
Observing Strategy:
The 2mm SIS junction receiver will be dual channel, and will cover the range
130-175 GHz with a hoped-for receiver noise temperature of typically < 75K
(DBS), with a worse case value of 100K DBS. The receiver is expected to be
tunable SSB.
The hybrid spectrometer will be used with a bandwidth of 600 MHz, and provide
768 channels for each of the two receivers. The spectral resolution is thus 0.781
MHz/channel or 1.3 km/s at 150 GHz.
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Initial Survey Results
Orion(KL):
The Orion(KL) spectra are very congested with lines leaving a low incidence of clean lines that
can be attributed to a single species. However, with about 1200 lines over the entire
frequency range, many species can be identified as undeniably present.
Therefore, though many of the lines are likely due to molecular transitions of two or more
different species, the shear volume of lines allows for the determination of some of the
physical properties of these molecules.
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Uncovering New Lines
CH3OCH3 : Trot= 75K
Nt= 6*1015cm-2
CH3CHO: Trot= 40K
Nt= 5*1013cm-2
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Initial Survey Results
Sgr B2N
NH2CHO: Trot= 75K
Nt= 5*1015cm-2
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Initial Survey Results
Sgr B2N
CH3OCHO: Trot= 150K
Nt= 3*1016cm-2
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Initial Survey Results
Sgr B2N
CH3CHO: Trot= 20K
Nt= 1.1*1015cm-2
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Initial Survey Results
Sgr B2N
CH3OCH3: Trot= 145K
Nt= 4.2*1016cm-2
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Initial Survey Results
Sgr B2N
CH3COCH3: Trot= 70K
Nt= 2.3*1015cm-2
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH
Accessing the Spectral Line Data
The data can be found in electronic form at: www.cv.nrao.edu/~Turner2mmLineSurvey
The data are distributed using the Spectral Line Search Engine (SLiSE). SLiSE is a data display tool that
contains all the fully reduced and calibrated archived data taken as part of this 2mm survey. The only
caveat is that SLiSE was built using Java 1.5. So an update to the user's java may be necessary. In
addition, SLiSE will work on a Mac running Safari, not Netscape.
Systematic errors in line frequencies and relative intensities are sure to exist based on the amount of
time over which these data were taken. However, we do not have access to all of B.E. Turner's
calibration and data reduction routines. We present the calibrated data using the SLiSE tool.
If you are interested in obtaining the raw data from the 12m during this time, we are working on making the
fits data available at that same web location through the NRAO single dish data archive. This is currently
a work in progress and subsequently may not be available until Fall 2008. Any data requests then should
be made to Anthony J. Remijan directly at: [email protected].
June 19, 2008
63rd OSU Meeting on Molecular Spectroscopy – Columbus, OH