dust and molecules in spiral galaxies as seen with the jcmt
DESCRIPTION
F.P. Israel, Sterrewacht Leiden. DUST AND MOLECULES IN SPIRAL GALAXIES as seen with the JCMT. ATOMS and MOLECULES. ... AND DUST. SCUBA 850 mu. M51 Line and Continuum. M51 J=3-2 CO depleted in center, enhanced in arms. ISM in Spiral Galaxies. Atomic gas avoids center - PowerPoint PPT PresentationTRANSCRIPT
DUST AND MOLECULES IN SPIRAL GALAXIES
as seen with the JCMT
F.P. Israel, Sterrewacht Leiden
ATOMS and MOLECULES ...
... AND DUST
SCUBA 850 mu
M51 Line and Continuum
M51 J=3-2 COdepleted in center, enhanced in arms
ISM in Spiral Galaxies
Atomic gas avoids center Molecular gas often concentrated in
center Dust emission follows total gas Metallicity & excitation gradients
Center: exclusively molecular Inner disk: molecules dominant
Outer disk: atoms dominant
Nuclear CO concentrationsdisk, torus or spiral?
12CO degeneracy resolved by 13co
Molecules in galaxy centers
Concentrated within R = 0.5 kpc High contrast with disk CO CO pollutes broadband continuum! Physical parameters only from several
line transitions! At least two components:
Lukewarm and dense Hot and tenuous
Hot and tenuous gas >50% of mass
Dust in galaxy centers
heating/cooling depends on: dust grain composition
dust grain size (distribution) Radiation, shocks, turbulence
Size distribution and other properties affected radiatively and dynamically active circumnuclear environment
The AGN in CENA
M83
NGC 6946, NGC 891 1
Origin of Subm/FIR emission: NGC 6822
Israel, Bontekoe & Kester, 1996 IRAS 60 microns
I
Dust-to-gas ratios
Dependent on metallicity, but how ?
log [O]/[H] = α log Mdust / Mgas + cst
Issa et al. 1990 α = 0.85
Schmidt & Boller 1993 α = 0.63
Lisenfeld & Ferrara 1998 α = 0.52
Dwek 1998 (model) α = 0.77
Interpretation of SEDs
SED reflects:
Big Grains 5-250 nm (MRN, thermal)
Very Small Grains (nonthermal)
Polycyclic Aromatic Hydrocarbons (PAHs)
at various temperatures
with potentially varying size distributions
NGC 1569: ISO & SCUBA
Cold dust?
Lisenfeld et al. 2002, 2005
Same observations, different views
Galliano et al. 2003
dust cold 5-7 K
most dust in small clumps
gas/dust ratio 320-680
(740-1600)
Lisenfeld et al. 2002/2005
dust warm 35 K
processed dust
VSG enhanced 7-12 times
gas/dust ratio 1500-2900
Evidence for dust processing
Spitzer: PAHs depleted in BCDGs weak relation radiation field hardness
strong relation energy density
Wu et al. 2006, Rosenberg et al 2006, Higdon et al 2006
IRAS: PAH depletion sequence f25 / f12:
Im 4.5 Sm 2.9 Sc 1.8 Melisse & Israel 1994a, b
ANS-UV: behaviour 2175A bumps
H2 from FIR or submmindependent from CO measurements
FIR or subm maps tracing dust column densities
Flux ratios tracing dust temperatures HI maps tracing atomic gas
Assumption dust-to-gas ratio
proportional to metallicity (!)
X-factor as function of metallicity
Filled symbols: large beam
Open symbols: resolved
log X = -α log [O]/[H] + c
α = -2.3 (+/-0.3)
Israel 1997, 2000
Molecular gas in galaxy centers
(Much) less H2 than expected from CO strength
Yet molecular gas is >90% of the total gas mass
On same curve as metal-poor galaxies?
What next?
JCMT Legacy Survey Physical Processes in Galaxies in the Local Universe
299 galaxies randomly selected from an HI-flux-limited sample, plus 32 remaining
SINGS galaxies, using HARP-B and SCUBA2 (2007-2009)
Christine Wilson (Canada)Stephen Serjeant (UK)
Frank Israel (NL)(coordinators) and many others
JCMT LEGACY SURVEY
Physical properties of dust
Molecular gas and gas-to-dust ratios
Effects of galaxy morphology Low-metallicity
Cluster environment Haloes, superwinds, and AGN
Luminosity and dust mass functions of galaxies