the role of cold gas in the chemical evolution of nearby ... · in the chemical evolution of nearby...
TRANSCRIPT
The role of cold gas
in the chemical evolution
of nearby galaxies
Tom Hughes Luca Cortese (Swinburne), Alessandro Boselli (LAM),
Guiseppe Gavazzi (Milan), Jonathan Davies (Cardiff), Veronique Buat (LAM)
The Role of Hydrogen in the Evolution of Galaxies
Kuching, 17th September 2014
Metals from stellar nucleosynthesis Expulsion of metals & unprocessed gas
Gas cools in the ISM, aided by dust Stars form in collapsing gas clouds
Dust forms in
cooling metal
rich gas
INT
ER
GA
LA
CT
IC
ME
DIU
M
The baryonic matter cycle
Lequeaux et al. 1979 Tremonti et al. 2004
•
•
Stellar mass – metallicity
>53,000 SDSS galaxies
Ma
ss
Metallicity
Stellar mass
Ox
yg
en
ab
un
da
nc
e
Some open questions
Da
ve
et
al.
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11
Constant
No wind Slow
Conserved
• Shape
- galactic scale winds
- variable SF efficiency
- variable IMF
•
•
Some open questions
Mass Surface density
Concentration Inclination
Ha EW Colour
Tre
mo
nti
et
al.
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04
• Shape
- galactic scale winds
- variable SF efficiency
- variable IMF
• Scatter
- most galaxy properties
do not correlate with
metallicity residuals
•
Some open questions
Mo
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cin
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t a
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• Shape
- galactic scale winds
- variable SF efficiency
- variable IMF
• Scatter
- most galaxy properties
do not correlate with
metallicity residuals
• Environment
- weak/strong dependence (see e.g. Cooper et al 2008)
- no statistical dependence
(see e.g. Ellison et al 2008)
Sk
illm
an
et
al.
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96
Local density Local density
Hubble Type VCirc B magnitude
Role of gas content
Infer:
K-S Law (Tremonti et al. 2004),
HI Scaling relations (Zhang et al. 2009).
Sk
illm
an
et
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96
Predict: decreasing Z with increasing gas fraction μ: Z = y ln (1 / μ) (Edmunds 2001)
Observe:
in Virgo
.
Herschel Reference Survey
Sample selection criteria:
• 15 - 25 Mpc volume limit
• 2MASS KsTot ≤ 12 mag
• Galactic latitude > +55º
• Extinction AB < 0.2
Ancillary data is complete for:
• H, B & V photometry ~ stellar mass
• NUV GALEX imaging ~ SFR
• HI 21cm ~ HI gas mass
• Drift-scan spectra ~ metallicity
- magnitude- and volume-limited sample covering 323 nearby galaxies in a
range of environments, from isolated systems to Virgo cluster members
(Boselli et al. 2010).
Herschel Reference Survey
Sample selection criteria:
• 15 - 25 Mpc volume limit
• 2MASS KsTot ≤ 12 mag
• Galactic latitude > +55º
• Extinction AB < 0.2
Ancillary data is complete for:
• H, B & V photometry ~ stellar mass
• NUV GALEX imaging ~ SFR
• HI 21cm ~ HI gas mass
• Drift-scan spectra ~ metallicity
- magnitude- and volume-limited sample covering 323 nearby galaxies in a
range of environments, from isolated systems to Virgo cluster members
(Boselli et al. 2010).
Error-weighted mean oxygen abundance from combination of
strong-line metallicity calibrations and base conversions from
Kewley & Ellison (2008).
HI deficiency is:
the difference between the observed HI mass and that expected for an isolated galaxy of similar size and type.
Blue circles –
Galaxies with normal gas content
Red circles –
Gas deficient objects, i.e.
galaxies missing up to 70% of their gas compared to healthy isolated systems.
Log stellar mass Gas fraction
Oxygen a
bundance
Resid
ual abundance
(Gas-poor Gas-rich)
Scatter in M-Z relation
correlates with gas fraction.
Gas-deficient objects
typically more metal-rich.
Hu
gh
es
et
al.
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13
Observed role of hydrogen
No significant environmental dependence,
consistent with Ellison et al. 2009 + Mouhcine et al. 2007
Log stellar mass Gas fraction
Oxygen a
bundance
Resid
ual abundance
Log stellar mass Log stellar mass
Hu
gh
es
et
al.
20
13
Effects of environment
Log stellar mass
Oxygen a
bundance
Resid
ual abundance
Log stellar mass Log stellar mass
HI-deficient select systems most perturbed by environment,
also consistent with Skillman et al. 1996, Gavazzi et al 2004.
Hu
gh
es
et
al.
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Effects of environment
Hu
gh
es
et
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NGC 4254
metallicity profile (Skillman et al. 1996)
Ch
un
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Drift –scan spectroscopy only probes metallicity across observable HII regions…
Degeneracy only broken using IFU spectroscopy (e.g. SAMI, CALIFA, MaNGA)
An observational bias…?
• Does SFR govern scatter?
- a fundamental M-Z-SFR
(see e.g. Lara-Lopez et al. 2010,
Mannucci et al. 2010)
•
•
Log Mass
Oxygen a
bundance
Ma
nn
uc
ci
et
al.
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10
Oxygen a
bundance
M-Z-SFR relation
• Does SFR govern scatter?
- a fundamental M-Z-SFR
(see e.g. Lara-Lopez et al. 2010,
Mannucci et al. 2010)
• CALIFA results
- correlation between SFR
and scatter only found when
simulating SDSS apertures (Sanzhez et al. 2013)
•
Log SFR
Log SFR Log μSFR
Resid
ual abundance
R
esid
ual abundance
Integrated HII regions
Simulated SDSS apertures
Sa
nc
he
z e
t a
l. 2
01
3
M-Z-SFR relation
• Does SFR govern scatter?
- a fundamental M-Z-SFR
(see e.g. Lara-Lopez et al. 2010,
Mannucci et al. 2010)
• CALIFA results
- correlation between SFR
and scatter only found when
simulating SDSS apertures (Sanzhez et al. 2013)
• Independent studies
- HI content drives scatter (see e.g. our work; Bothwell et al. 2013)
- SFR a proxy for gas content
(see e.g. Kahid et al. 2014)
Log SFR
Log SFR Log μSFR
Resid
ual abundance
R
esid
ual abundance
Integrated HII regions
Simulated SDSS apertures
Sa
nc
he
z e
t a
l. 2
01
3
M-Z-SFR relation
See Hughes, Cortese et al., 2013, A&A, 550, 115H
Boselli, Hughes et al., 2013, A&A, 550, 114B
• First time combined direct gas information with
metallicities from drift-scan optical spectroscopy
using new calibration techniques.
• Gas content related to scatter of M-Z relation,
environment of secondary importance.
• Future work must examine the spatially-resolved
observations to avoid potential aperture biases.
Summary