Molecular Gas in Nearby Dwarf Galaxies:
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Transcript Molecular Gas in Nearby Dwarf Galaxies:
Molecular Gas and Star
Formation in Dwarf Galaxies
Alberto Bolatto
Research Astronomer
UC Berkeley
• Adam Leroy*
• Josh Simon*
• Leo Blitz
* Hard working grad students
Why should you care?
“…Extreme properties are often sought for in Astronomy as one
way to sharpen our understanding of fundamental concepts…”
Dwarf galaxies:
are the first structures to form in bottomup ΛCDM cosmologies
have low heavy element abundances, just
like primordial systems
are the simplest systems
Local dwarfs are windows onto the
high-z Universe
A single-dish/interferometric survey
MIDGet
A CO survey of IRAS-detected,
compact, nearby, northern
dwarf galaxies out to VLSR=1000
km s-1, with rotational velocities
under ~100 km s-1
Observed 121 central pointings
with the Kitt Peak 12m
Follow up of 30+ galaxies
mapped using BIMA
Fabian Walter’s OVRO sample
UASO 12m
BIMA
Two questions:
What global properties distinguish
galaxies with and without CO?
Some of the best molecular gas predictors
are surprising: LK, Mdyn/LK, B-K (B-V)
Are there any differences between large
and dwarf galaxies in their molecular
gas/star formation properties?
Remarkably very few, even where some
where expected
Distributions of detections/nondetections
Best
predictors
of CO: LK,
LB, Hubble
Type,…
1/5 Z
Distributions of detections/nondetections
Best
predictors
of CO: LK,
LB, Hubble
Type, FIR
luminosity,
B-K color,
K-band
mass to
light ratio
One of the best predictors of CO in the survey…
M/L ~ 3 (B-band) and ~ 2 (K-band)
But the correlation is much tighter at the low
end in B light… CO nondetections are
systematically fainter in K-band!
M
M
LFIR, LK, LB, B-K,
Hubble Type, Z,
are all correlated
Can we identify
a driving
parameter?
Normalizing by
LK removes
trends and
minimizes
dispersion
M
M
What is the driving relationship?
What is the driving relationship?
LFIR, LK, LB, B-K,
Hubble Type, Z,
are all correlated
Can we identify
a driving
parameter?
Normalizing by
LK removes
trends and
minimizes
dispersion
Mmol/LK is the
tightest
correlation.
Across all galaxy
sizes
Mmol/LK~0.075
What does it mean?
Facts:
Tightest Mmol correlation is with LK, a proxy for M*
and Σ*
Correlations with Mgas (HI) or Mdyn are
considerably weaker
Taken together, suggest that what matters in the HIH2 conversion
is the amount of matter in the disk (Σ*), not just the amount of
“stuff”
Correlations with B-K could arise from enhanced
photodissociation/less dust in bluer systems…
…but systems with no CO tend to be
underluminous (for their mass) in K-band, not
overluminous in B-band
Suggests that photodissociation plays only a secondary role in
setting the global amount of H2
This is indirect evidence in support of the
local density (pressure) controlling HIH2
Are large and dwarf
galaxies different in their
molecular gas/star
formation properties?
The SFR vs. H2 relationship…
1.4 GHz flux traces star formation
(e.g., Condon et al.
2002, Murgia et al. 2002; SFSNCRsynchrotron?)
The SFR vs. H2 relationship…
1.4 GHz flux traces star formation
MIDGet and large galaxies fall on the same SFRH2 correlation
(e.g., Condon et al.
2002, Murgia et al. 2002; SFSNCRsynchrotron?)
ΣSFR=10-3.4±0.1ΣH21.3±0.1
ΣSFR=10-3.4±0.2ΣH21.4±0.2
The SFR vs. H2 relationship… is independent of Z!
1.4 GHz flux traces star formation
MIDGet and large galaxies fall on the same SFRH2 correlation using the Galactic Xco!
(e.g., Condon et al.
2002, Murgia et al. 2002; SFSNCRsynchrotron?)
Attempts to correct CO-H2 for metallicity fail
There is no segregation by inferred metallicity
Richer & McCall 1995)
(using
Attempts to correct CO-H2 for metallicity fail
There is no segregation by inferred metallicity
Richer & McCall 1995)
Corrections destroy the agreement!
(using
Ways out of a constant Xco…
Size-dependent
corrections to
RC-SFR (e.g.
Bell 2003)?
Even then large
changes in Xco
are out of the
question
A different SFRH2 regime for
dwarf galaxies?
The sweet spot for star formation efficiency…
A maximum
star formation
efficiency at
1010 M?
To a first
approximation
galaxy-size /
metallicity
corrections to
LFIR and Xco
cancel
A large Xco(Z)
makes the
maximum
more
pronounced
Summary
Mmol correlates very well with LK, not
with MHI or Mdyn
Indirect support for a local
density/pressure controlled HIH2
transition
Same SFR-H2 relationship for dwarfs
and large galaxies, suggesting constant
CO-H2 for star forming gas despite
changing metallicity
A minimum H2 depletion time /
maximum SF efficiency at 1010 M?
CARMA is moving forward