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?. Tijana Prodanović, University of Novi Sad Gary Steigman , Ohio State University Brian D. Fields, University of Illinois at Urbana Champaign. The (Un)True Deuterium Abundance in the Galactic Disk. Only created in Big Bang ( Boesgaard & Steigman 1985) - PowerPoint PPT Presentation
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Tijana Prodanović, University of Novi SadTijana Prodanović, University of Novi SadGary Steigman, Ohio State UniversityBrian D. Fields, University of Illinois at Urbana Champaign
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
1
?
Only created in Big Bang (Boesgaard & Steigman 1985)
All other processes destroy it (Epstein et al. 1976, Prodanović & Fields 2003)
Should (?) decrease monotonically from high to low z Deuterium – a powerful tool in cosmology!
Cosmic baryometer! BBN success story WMAP & BBN (blue) and high-z obs. (yellow) – a match!
Deuterium – a powerful tool in chemical evolution! Probes virgin ISM fraction!
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe, November 9th 2009
2
Cyburt et al. (2008)
20.019.0
5
82.2
10/
Dp
D
y
HDy
Large variations of D in local ISM over different lines of sight!
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe, November 9th 2009
3
2.25.0 DyData from Linsky at al. (2006)
Deuterium preferentially (compared to H) depleted onto dust! (Jura 1982, Draine 2004, 2006)
Measure lower bound on the “true” D “True” ISM D abundance (Linsky at al. 2006)
“True” ISM D = 82% of PRIMORDIAL!
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe, November 9th 2009
4
24.031.2, dustISMDy
Deuterium destroyed through stellar cycling Astration factor (Steigman et al. 2007)
But new FUSE high ISM D Most gas still unprocessed? Gas observations say ~20% of present baryonic
mass in ISM But D observations say ~80% initial gas
unprocessed! Thus GCE says INFALL NEEDED
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
5
15.022.1 Df
8.1/4.1 DISMDpD yyf
Assume infall rate ~ star form. rate
D vs. gas fraction Shaded = observations Allowed infall rate
Almost balances out star-formation!
Still tension with GCE Is ISM D really so high?
Prodanovic & Fields 2008
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe, November 9th 2009
6
15.0
Linsky et al. 2006
Try something different – make (almost) no assumptions
Bayesian analysis (introduced by Hogan et al. 1997)
Use all available LOS Assume only a possible (dust) depletion Find 2-parameter maximum likelihood
- Max. D abundance consistent with observations; a lower limit to true ISM D
- Depletion parameter
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
7
min,max, DD yyw
wyD ,max,
max,DyISMDD yy ,max,
Prodanovic, Steigman & Fields (2009)arXiv:0910.4961
Know nothing about (dust) depletion distribution
Make as little assumptions1) Top hat – all levels of depletion
equally probable2) Negative bias – favors large
depletion3) Positive bias – favors low
depletion
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
8
Local Bubble very different from non-Local Bubble
LB – blue Uniform
nLB – red Large scatter
First treat separately
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
9
Prodanovic, Steigman & Fields (2009)arXiv:0910.4961
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
10
Prodanovic, Steigman & Fields (2009)arXiv:0910.4961
Top-hat depletion distribution
21 Local Bubble LOS
25 non-Local Bubble LOS
All 46 LOS
3.1 6.1 1.2 ,, nLBDnLBD fwy
4.1 3.1 0.2 max,max, DD fwy
8.1 0 5.1 ,, LBDLBD fwy
Use all 46 LOS Top-hat depletion distribution – highest max
likelihood value
Marginally consistent with
Releases tension with GCE models
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
11
1.00.2max,, DISMD yy
1.04.1 Df
24.031.2, dustISMDy
Linsky et al. (2006)
If Local ISM D abundance close to primordial – problems with most GCE models
Bayesian analysis following Hogan et al. (1997) Assume all variations due to (dust) depletion Analyze all LOS Tested 3 simple depletion distributions
Top-hat gives max likelihood value “True” ISM D abundance new estimate:
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe, November 9th 2009
12
5max 10)1.00.2()/()/( HDHD ISM
Prodanovic, Steigman & Fields (2009)arXiv:0910.4961
Uniform LB D abundance vs. large scatter in nLB? LB - no depletion? nLB – large depletion?
Is LB uniformily depleted? Is nLB enriched with unmixed infall? How do we discriminate? Is Fe really a good depletion indicator for D? Steigman & Prodanović (2009/10) in preparation
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe November 9th 2009
13
6.1 1.2, wy nLBD
0 5.1, wy LBD
Tijana Prodanović [email protected]
IAU Symposium 268: Light Elements in the Universe, November 9th 2009
14