![Page 1: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/1.jpg)
FUSE results on deuterium abundances;FUSE results on deuterium abundances;
What can we learn from D/O and D/N ratios?What can we learn from D/O and D/N ratios?
Guillaume HGuillaume HÉBRARDÉBRARDInstitut d’Astrophysique de Paris
LoLa-GE meeting
International Space Science Institute, BernFebruary 24rd, 2004
Guillaume Hébrard
Institut d’Astrophysique de Paris
98bis, boulevard Arago
F-75014 Paris
phone: (33 1) 44 32 80 78
fax: (33 1) 44 32 80 01
email: [email protected]
Current address:
Guillaume Hébrard
The Johns Hopkins University
Department of Physics & Astronomy
Bloomberg, room 144B
3400 North Charles Street
Baltimore, MD 21218
USA
phone: 410 516 7496
fax: 410 516 5494
email: [email protected]
![Page 2: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/2.jpg)
Hébrard & Moos (2003): ApJ 599, 311Hébrard & Moos (2003): ApJ 599, 311This paper includes most of the references quoted in this talk
![Page 3: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/3.jpg)
Three kinds of abundance measurements:
– Primordial (14 x 109 year)
– Proto-solar (4.5 x 109 year)
– Interstellar (present epoch)
Deuterium: tracer of chemical evolution
![Page 4: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/4.jpg)
Rogerson & York (1973)
Copernicusβ Cen
![Page 5: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/5.jpg)
D/H measurements (70’, 80’, 90’): spatial variations or not?
Ferlet et al. (1995)
(Linsky et al. 1995)
![Page 6: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/6.jpg)
FUSEFUSEFFar ar UUltraviolet ltraviolet SSpectroscopic pectroscopic EExplorerxplorer
Wavelength (Å)
Nu
mb
er
of
line
s
(pe
r 1
00
Å in
terv
al)
Photons energy (eV)
Ground
June 24th, 1999
HD
H2
Atoms & Ions
![Page 7: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/7.jpg)
FUSE in few words
Total cost: ~250 106 US$
Duration: 3 + 2 years (+ 2 years)
Cycles 1, 2 & 3 (PI + GI): 1999 → 2003
Cycle 4 (GI): April 2003 → March 2004
Cycle 5 (GI): Begins in April 2004(80 programs selected)
Cycle 6 (GI): July 2004(deadline: Sept. 17th, 2004)
FUSE Science Conference Victoria (Canada)August 2-6, 2004
Web: http://fuse.pha.jhu.eduhttp://fuse.pha.jhu.edu
About 3500 observations already performed (2700 public)
![Page 8: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/8.jpg)
![Page 9: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/9.jpg)
Equivalent widths measurements
→ curves of growth
Friedman et al. (2002)
![Page 10: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/10.jpg)
Profile fitting
Wood et al. (2002)
![Page 11: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/11.jpg)
Example of a line fit
Wavelength (Å)
Flu
x
WD 2211-495
FUSE MDRS SiC2A
D I
Hébrard et al. (2002)
![Page 12: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/12.jpg)
Profile fitting (Voigt) with Owens.f (M. Lemoine)
Ly
Ly
Ly
Ly
Ly
Ly
Ly
Ly
Ly
Ly
Ly
Ly
Ly
DI
DI
DIDI
DIDI
DIDI
DIDI
DI
DI
DI
DI
DI
DIDI
DIDI
OI
OIOIOIOI
OI
OIOI
OI OI OI OI OI OI
OI
OI DIOI
OIOIOIOI
OI
OIOI
OIOIOIOIOI
O ID I
Hébrard et al. (2002)
![Page 13: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/13.jpg)
Results toward 24 targets
Overview:
Hébrard & Moos (2003)
ApJ 599, 297-311.
Moos et al. (2002)Friedman et al. (2002)
Hébrard et al. (2002)
Kruk et al. (2002)
Lemoine et al. (2002)
Lehner et al. (2002)
Sonneborn et al. (2002)
Wood et al. (2002)
Hoopes et al. (2003)
Oliveira et al. (2003)
![Page 14: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/14.jpg)
White dwarf
Most local ISM
Subdwarf
More distant ISM
![Page 15: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/15.jpg)
D/O
Hébrard & Moos (2003)
![Page 16: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/16.jpg)
D/N
Hébrard & Moos (2003)
![Page 17: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/17.jpg)
D/O vs. D/N
Hébrard & Moos (2003)
2 = 8.4 for 13 d.o.f.
d.o.f. = degrees of freedom
2 = 117.9 for 23 d.o.f.
2 = 189.9 for 23 d.o.f.
D/OD/O
D/ND/N2 = 37.3 for 13 d.o.f.
![Page 18: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/18.jpg)
Hébrard & Moos (2003)
![Page 19: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/19.jpg)
Local Bubble
D/O = ( 3.84 ± 0.16 ) x 10-2 • Moos et al. (2002)
5 targets in LB →
D/O = ( 3.76 ± 0.20 ) x 10-2
• Oliveira et al. (2003)
8 targets in LB →
D/O = ( 3.87 ± 0.18 ) x 10-2
• Hébrard & Moos (2003)
14 targets in LB →
D/O = ( 3.84 ± 0.16 ) x 10-2
D/O
Hébrard & Moos (2003) log N(HI) = 19.3 – 19.4
→ Local Bubble wall (Sfeir et al. 1999)
![Page 20: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/20.jpg)
D/O
If D/H = 1.5 0.1 x 10-5 (Linsky 1998)
or D/H = 1.52 0.08 x 10-5 (Moos et al. 2002),
with O/H = 3.43 0.15 x 10-4
D/O = 4.4 0.3 x 10-2
If D/O = 3.84 0.16 x 10-2,
with O/H = 3.43 0.15 x 10-4 (Meyer 2001)
D/H = 1.32 0.08 x 10-5
D/O = (D/H) / (O/H)
If D/O is homogeneous in the LB
D/H and O/H homogeneous in the LB
Hébrard & Moos (2003)
D/O in the Local Bubble
D/H
O/H
![Page 21: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/21.jpg)
D/O
Hébrard & Moos (2003)
Local Bubble
Which value for D/O is representative of the present epoch?
![Page 22: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/22.jpg)
D/O
Hébrard & Moos (2003)
Local Bubble
D/O = ( 3.96 ± 0.15 ) x 10-2
2 = 12.5 for 15 d.o.f.
![Page 23: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/23.jpg)
Hébrard & Moos (2003)
![Page 24: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/24.jpg)
D/O
Hébrard & Moos (2003)
![Page 25: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/25.jpg)
D/O vs. D/N
Hébrard & Moos (2003)
![Page 26: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/26.jpg)
Local Bubble
D/O = (1.50 ± 0.25) x10-2
→ D/H = (5.2 ± 0.9) x10-6
D/O
Hébrard & Moos (2003)
HD191877 (Hoopes et al. 2003)
HD195965 (Hoopes et al. 2003)
LSS1274 (Hébrard & Moos 2003)
![Page 27: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/27.jpg)
Local Bubble
D/N = (1.15 ± 0.16) x10-1
D/N
Hébrard & Moos (2003)
→ D/H = (8.6 ± 1.3) x10-6
HD191877 (Hoopes et al. 2003)
HD195965 (Hoopes et al. 2003)
LSS1274 (Hébrard & Moos 2003)
![Page 28: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/28.jpg)
2 high values (D/H > 2 x10-5):
2 Vel (Sonneborn et al. 2000): → D/H = (2.18 ± 0.20) x10-5
– Feige 110 (Friedman et al. 2002): → D/H = (2.14 ± 0.41) x10-5
5 low values (D/H < 1 x10-5):
Ori A (Laurent et al. 1979; Jenkins et al. 1999): → D/H = (0.74 ± 0.11) x10-5
Sco (York 1983): → D/H = (0.76 ± 0.25) x10-5
Car (Allen et al. 1992): → D/H = (0.50 ± 0.16) x10-5
– HD191877 (Hoopes et al. 2003): → D/H = (0.78 ± 0.20) x10-5
– HD195965 (Hoopes et al. 2003): → D/H = (0.85 ± 0.15) x10-5
2 extra low values in Orion (ISO, HD molecule):
– Orion molecular outflow (Bertoldi et al. 1999): → D/H = (0.76 ± 0.29) x10-5
– Orion Bar (Wright et al. 1999): → D/H = (1.0 ± 0.3) x10-5
Previous distant D/H measurements
Hébrard & Moos (2003)
![Page 29: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/29.jpg)
Hébrard & Moos (2003)
Galactocentric gradient?
![Page 30: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/30.jpg)
Chiappini, Renda, & Matteucci (2002)
d log (D/N) / dR
0.14 dex / kpc
d log (D/O) / dR
0.13 dex / kpc
t = 14 Gyr
t = 14 Gyr
![Page 31: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/31.jpg)
Hébrard & Moos (2003)
5.2
2.8 2.8
2.0
1.1 1.1
![Page 32: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/32.jpg)
O/H: depletion
André et al. (2003)Meyer et al. (1998)
![Page 33: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/33.jpg)
Chiappini, Renda, & Matteucci (2002)
t = 14 Gyr
D/O 4.0 x 10-2
D/O 2.5 x 10-2
R (kpc)
• QSO 0105+1619 : D/O = (280 ± 30) x10-2 (O’Meara et al. 2001)• QSO 0347-3819 : D/O = (37 ± 3) x10-2 (Levshakov et al. 2002)
= (21 ± 4) x10-2 (D’Oddorico et al. 2001)• QSO 1243+3047 : D/O = (3000 ± 300) x10-2 (Kirkman et al. 2003)
• Complex C : D/O = (28 ± 12) x10-2 (Sembach et al. 2004)
QSOQSO
D/O = (1.50 ± 0.25) x 10-2
![Page 34: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/34.jpg)
HD/H2
Dense clouds:
HD/H2 = 2 x D/H
Ferlet et al. (2000)
More than 100 HD
detections with FUSE
Future work
![Page 35: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/35.jpg)
D H (105)
Hébrard et al. (2000)
Deuterium Balmer seriesDeuterium Balmer series
Future work
A&A 354, L79 and A&A 364, L31
![Page 36: FUSE results on deuterium abundances; What can we learn from D/O and D/N ratios?](https://reader035.vdocuments.us/reader035/viewer/2022062423/56814336550346895dafa8df/html5/thumbnails/36.jpg)
– D/O and D/N are less sensitive to systematic errors than D/H;
– D/H is homogeneous within the Local Bubble (~100pc) and is 1.5 x 10-5 (direct measurement) or 1.3 x 10-5 (measurement via D/O);
– This local value IS NOT the canonical value of (D/H)ISM, characteristic of material at the present epoch;
– The (D/H)ISM ratio characteristic of the present epoch is likely to be significantly lower than the local value.
Conclusions:
FUSE
Hébrard & Moos (2003)