HD 204827, the C 2, C 3 rich sightline. The C 2 Diffuse Interstellar Bands Takeshi Oka Department of Astronomy and Astrophysics And Department of Chemistry.

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Presentation transcript:

HD , the C 2, C 3 rich sightline

The C 2 Diffuse Interstellar Bands Takeshi Oka Department of Astronomy and Astrophysics And Department of Chemistry The Enrico Fermi Institute, University of Chicago J. A. Thorburn, L. M. Hobbs, T. Oka, D. E. Welty, D. G. York B. J. McCall, S. D. Friedman, P. Sonnentrucker, T. P. Snow ApJ 584, (2003) Carbon in space, Lago di Como, May 23, 2006 T. Oka, Thorburn, J. A., McCall, B. J., S. D. Friedman, L. M. Hobbs, P.Sonnentrucker, D. E. Welty, D. G. York ApJ 582, (2003)

HD , the C 2, C 3 rich sightline

William Huggins, Comet Tebbutt, Alex Douglas C IVR The Douglas effect 1975 HCCCCCN, HCCCCCCCN, HCCCCCCCCCN Origin of diffuse interstellar lines Nature, (1977) Alex Douglas CnCn Proc. R. Soc. London, A. 34, 148 (1881) 4050 Å

J. A. Thorburn, L. M. Hobbs, T. Oka, D. E. Welty, D. G. York, B. J. McCall, S. D. Friedman, P. Sonnentrucker, T. P. Snow Apache Point Observatory 3.5-meter 3,800–10,000 Å ; /  ~ 38,000 (8 km/s) 53 stars, at 5780 Å Systematic observations of DIBs

HD versus HD E(B-V)= C 2 C 3 N(C 2 ) < 6  cm -2 = 440  cm -2 High discrimination N(CH) = 50  cm -2 = 80  cm -2 Poor discrimination C 2 richC 2 poor

C 2 rich C 2 poor C 2 DIBs Minority Weak and sharp Diffuse Interstellar Bands

W(DIB) versus N(C 2 ) Å r = Å r = C 2 DIBsNon-C 2 DIBs Å r = Å r = 0.416

C 2 DIBs λ(Å)Δλ(Å)r(C 2 )r(C 3 )Note cm cm cm cm cm -1

Doublet Lines

The Doublets cm cm cm cm cm -1 Π Π Π Σ HC 3 HC 5 HC 6 HC 7 HC 8 C 3 - C 7 - A (cm -1 ) λ (Å) Δ T ex 22 K 34 K 26 K Π←Σ 3  10 6 s I s / I w A HD HD HD Or inverted

C 2 -rich HD Hot HD T = 301 K T = 40.6 K

C 2 rich C 2 poor C 2 DIBs Minority Weak ans sharp

Keck Adamkovics, Blake and McCall B = 365 MHz for T = 100 K 182 MHz 200 K 122 MHx 300 K B = MHz HC 7 N MHz HC 9 N MHz HC 11 N 2.60 cm -1

Summary DIBs which correlate well with C 2 and C 3 C 2 DIB HD , Minority, Weak and sharp Doublet structure suggests spin-orbit splitting Linear carbon chain molecule Relatively high density ? DIBs for high temperature medium HD Rotational structure  B n  8 – 12? Big question: C 2, C 3  C 2 DIB or C 2 DIB  C 2, C 3 ?

HD T = 301 K HD T = 40.6 K C3C3 Adamkovics, Blake, McCall RA 06 The high temperature sightline HD R head