Download Competitive advantage

Competitive advantage
Highly Successful Existing Centre
2014 Mid-term review:
ü  “excellent scientific achievements”
ü  “exceptional level of collaboration”
ü  “outstanding and supportive environment for students and
postdoctoral researchers”
ü  “outstanding gender equity program”
ü  “highly effective and efficient Centre administration
ü  “highly successful and innovative outreach program”
“The Centre management, including the Board, is encouraged to
strategically focus on a vision for the future beyond 2017”
CAASTRO Opportunities
2017-2024: A New Era
of Australian Facilities
SKA Pathfinder Murchison Widefield Array AAT HERMES AAT SAMI / Hector Giant Magellan Telescope Square Kilometre Array Intrinsically
3-D
Facilities
Science Themes
The Ionized Universe: Epoch of Reionization
The Massive Universe: Growth of mass and angular momentum
The Chemical Universe: How the building blocks of life evolved
Themes chosen where
Australia will lead
internationally in 2017-2024.
Requires combination of
Optical, Radio and Theory
The Ionized Universe
What are the sources of reioniza0on? How were the sources distributed? How did the ionizing sources evolve across space and cosmic 0me? MWA
The Ionized Universe
What are the sources of reioniza0on? When did reioniza0on begin and end? How did the ionizing sources evolve across space and cosmic 0me? First Stars
Skymapper
Discovering the
Oldest stars
First Galaxies
James Webb
Space Telescope
Galaxy
Evolution
Keck, AAT
Redshift space covered
6
The Massive Universe
How did mass and angular momentum build across the universe? Early Universe: Gravitational Lensing
Cluster
magnifies
galaxy light
10-30x
Keck
The Massive Universe
How did mass and angular momentum build across the universe? Nearby Universe: ASKAP + SAMI & Hector
Image Slice
at a given
wavelength
3-D picture of a
galaxy and its motion
Spectrum
at a given
pixel
The Massive Universe
9
The Chemical Universe
How did the building blocks of life proliferate across the universe? Carbon, Nitrogen, Oxygen Efficiency:
Same Observations
First Galaxies
Give chemical data
James Webb
First Stars
Space Telescope
Skymapper
Keck
Oldest star
discovered: 13.6 Gyr
Galaxy
Evolution
Keck, AAT
The Chemical Universe
How did the building blocks of life proliferate across the universe? Carbon, Nitrogen, Oxygen GAIA
Galactic Archeology
Chemical
elements
reveal the
history of
our
Milky Way
AAT HERMES
Redshift range covered
12
National Benefit
Building the research capacity and technical exper0se to fully exploit Australia’s $480M investment in future Astronomy Infrastructure. CAASTRO-3D
2017
2018
2019
Giant Magellan Telescope
2020
2021
2022
2023
2024
2025
Square Kilometre Array
CAASTRO-3D and HECTOR
›  HECTOR will address all three science themes for the local
universe:
1.  Ionization mapping
2.  Chemical abundance mapping
3.  Mass and angular momentum build-up
How do these quantities change as a function of environment
and mass?
14
HECTOR specs
To measure metallicities and ionization parameters we must:
1.  Separate star formation from AGN per spaxel
2.  Separate star formation from shocks per spaxel
For accurate angular momentum estimates, we need:
1.  Reliable stellar velocity maps
2.  HI maps
15
Star formation vs AGN
Composite spaxels form
a clean ring of mixed
Starburst-AGN activity
Davies, Rich, Kewley & Dopita
(2014, MNRAS, 439, 3835)
Starburst vs AGN fraction
Davies, Kewley & Dopita (2014), MNRAS,444, 3961
Starburst vs AGN
Fits from data cube of ESO 137−G34
25
Rblue = 3000
Rblue = 2000
Median H −[O III] flux deviation (%)
20
15
10
H
[O III]
5
0
7000
6000
5000
4000
Rred
3000
5000
18
Star formation vs AGN
Fits from data cube of ESO 137−G34
0.08
Rblue = 3000
Rblue = 2000
Median line ratio deviation (dex)
0.06
[O III]/H
0.04
0.02
[S II]/H
[N II]/H
0.00
7000
6000
5000
4000
Rred
3000
5000
19
Star formation vs Shocks
Narrow
Component
IC 1623
flux
Broad component
20
Isolating Shocks: Velocity Dispersion
R=7000
Rich et al. 2011 (ApJ, 734, 87)
IC 1623
NGC 3256
log([NII]/Hα)
log([SII]/Hα)
log([OI]/Hα)
Isolating Shocks
Rich et al. 2011 (ApJ, 734, 87)
SAMI Shocks
HII
Three velocity
dispersion peaks
??
Shocks
Ho et al. 2015, MNRAS, 3894, 910
Star formation vs shocks
SAMI R1750 in blue
SAMI R4500 in red
WiFeS R7000
WiFeS R7000
Star formation vs shocks
Ho et al. 2015, MNRAS, 3894, 910
SAMI R4500
WiFeS R7000
SAMI vs WiFeS
Ho et al. 2015, MNRAS, 3894, 910
Electron density & shocks
Ho et al. 2015, MNRAS, 3894, 910
HECTOR: Bottom Line
›  Spectral resolution is extremely important for this science.
›  Ideal: R=7000 both red (i.e. @ 6500A) and blue (i.e. @ 4500A)
›  Minimal: R=5000 in Red and R=3000 in blue: Red line in Robert’s 4x 2kx 2k
resolution vs λ plot would work, among others.
›  Wavelength coverage:
›  Require [OII] 3727 to [OIII] 5007 in blue
›  Require [NII] 6548 to [SII] 6731 in red
›  i.e. for λ<7500, require z<0.1 for a HECTOR survey
›  Gaps between red and blue are OK
›  Spatial coverage:
›  > 2 Re ideal – we do need larger bundles than SAMI
›  Resolution of individual SF regions ideal 10-100 pc
HECTOR on
an 8-10m?
Nodes and CIs
Prof. Lisa Kewley (CAASTRO-­‐3D Director) Prof. Ma>hew Colless (RSAA Director) Prof. Mar@n Asplund (Laureate Fellow) AAO
CSIRO
Prof. Joss Bland-­‐Hawthorn (Laureate Fellow) Prof. Elaine Sadler (current CAASTRO director) Prof. Sco> Croom (Future Fellow) Prof. Stuart Wyithe (Laureate Fellow) Prof. Rachel Webster Prof. Michele Tren@ Prof. Karl Glazebrook (Director) Prof. Darren Croton (QEII Fellow) Dr Emma Ryan-­‐Weber Prof. Steven Tingay (Director) Dr. Cath Tro> Prof. Lister Staveley-­‐Smith (Director) Prof. Simon Driver Prof. Chris Power (Future Fellow) Governance
Advisory Board
Director
Executive
Science Management Committee