Transcript Columbus05_DIBs.ppt

Correlations among
Diffuse Interstellar Bands,
Atoms, and Small Molecules
Ben McCall
Department of Chemistry and Department of Astronomy
University of Illinois at Urbana-Champaign
APO DIB Collaboration:
Máté Ádámkovics (Berkeley), Tom Fishman (Chicago), Scott Friedman (STScI), Lew Hobbs (Yerkes),
Ben McCall (UIUC), Takeshi Oka (Chicago), Brian Rachford (Carleton), Ted Snow (Colorado),
Paule Sonnentrucker (JHU), Julie Thorburn (Yerkes), Dan Welty (Chicago), Don York (Chicago)
Discovery of the DIBs
• 5780, 5797 seen as unidentified lines
–  Per,  Leo (Mary Lea Heger, Lick, 1919)
• Six bands confirmed as “detached” lines
– Merrill & Wilson, Mt. Wilson, 1938
• Broad (“diffuse”)
B. J. McCall, in preparation
Merrill & Wilson, ApJ 87, 9 (1938)
What are the DIBs?
• Reasonable correlation with dust extinction
– but “level off” at high AV → diffuse clouds only?
– for a long time, solid state carriers favored
• Several characteristics argue against dust:
– constancy of 
– lack of emission
– fine structure!
• Present consensus:
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gas-phase molecules
probably large
likely carbon-based
reservoir of organic material
Sarre et al., MNRAS 277, L41 (1995)
• Greatest unsolved mystery in spectroscopy!
The APO DIB Survey
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Apache Point Observatory 3.5-meter
3,600–10,200 Å ; / ~ 37,500 (8 km/s)
119 nights, from Jan 1999 to Jan 2003
S/N (@ 5780Å) > 500 for 160 stars (115 reddened)
Measurements & analysis still very much underway
The “C2 DIBs”
• First set of DIBs known to be correlated with a
known species!
Tuairisg atlas
1.5
1.4
Relative Intensity
N(C 2) (10
1.3
12
HD 183143
<3
HD 167971
<4
HD 179406
73
HD 206267
93
HD 34078
-2
EB-V
cm )
1.27
1.08
0.33
0.53
110
0.52
1.2
HD 147889
210
HD 172028
1.1
1.07
270
0.79
HD 204827
1.0
430
1.11
0.9
4960
4965
4970
4975
4980
4985
5170
Wavelength (Å)
5180
5540
5550
Thorburn et al, ApJ 584, 339 (2003)
C2 DIBs toward HD 62542
• Unusual sightline with only diffuse cloud “core”
– outer layers stripped away by shock (?)
– DIBs undetected [Snow et al. ApJ 573, 670 (2002)]
• Recent Keck observations (higher S/N)
– Classical DIBs (e.g. λ5780) very weak
– C2 DIBs among the few DIBs observed
• C2 DIBs evidently form in denser regions
Ádámkovics, Blake, & McCall ApJ 625, 857 (2005)
λ5780 and N(H)
well correlated with H
no correlation with H2
[a la Herbig ApJ 407, 142 (1993)]
r=0.944
(linear fit,
w/o outliers)
York et al., in preparation
r=0.589
(linear fit)
N(CH) and N(H2)
reasonable correlation
[a la Federman et al. ApJ 287, 219 (1984)]
r=0.886
(linear fit,
w/o outliers)
Visible spectroscopy can pinch-hit for UV spectroscopy?
Search for a Common Carrier
• Assumptions:
– gas phase molecules
– DIBs are vibronic bands
– low temperature
• carriers all in v=0
– relative intensities fixed
A
v=0
• Franck-Condon factors
• independent of T, n
• Method:
– look for DIBs with tight
correlations in intensity
• Prospect:
– identify vibronic spectrum of
single carrier
– spacings may suggest ID
X
v=0
DIB Correlations
r=0.55
r=0.985
“C7- bands”
measurement errors
could be causing deviations?
Still much work to do, especially on weaker bands!
Statistics of Correlations
• 1218 pairs of DIBs
observed in >40 stars
• 58 DIBs included
• Histogram of r
• Few very good
correlations
– 19 with r > 0.95
• Most strong DIBs
have distinct carriers
Decorrelation Bias from Error
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Observed r=0.986
Assume perfection
Add Gaussian noise
1000 M.C. trials
Double the noise
1000 M.C. trials
Statistically OK if we
underestimated errors
r=0.985
r=0.996
Measurement Errors
• Is doubling the error estimate reasonable?
• Error sources include:
– finite S/N
– unexpected structure
• Agreement not
always perfect!
– interfering DIBs?
– continuum placement
HD 281159
– CH+ A-X band
• Hard to say; but
it’s certainly a
very good
correlation!
r=0.985
The Road to a Solution
• Laboratory spectroscopy is essential
• Blind laboratory searches unlikely to work
~107 organic molecules known on Earth
~10200 stable molecules of weight < 750
containing only C, H, N, O, S
• Observational constraints & progress are
also essential!
• Computational chemistry will play an
important role
• Close collaborations needed!
Acknowledgments
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NASA Laboratory Astrophysics
NSF CAREER Award
Dreyfus New Faculty Award
ACS PRF Starter Grant
University of Illinois
McCall Group