6dFGS Workshop, Epping

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The future of Schmidtery
at the AAO

• 6dFGS Workshop, Epping
• 11 July 2003
• Fred Watson (and the RAVErs)

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The future of Schmidtery
Overview What is RAVE? Science goalswhy are we
RAVEing? Instrumentation The RAVEs progress A
few other issues...
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What is RAVE?
RAdial Velocity Experiment International
collaboration22 scientists in 11 nations All-sky
survey of stellar velocities metallicities 50
million stars, complete to I15 (Biggest
EVER) Enables true galactic archaeology Spawned
from (now-defunct) space missions UK Schmidt
Telescope and a northern counterpart Completely
externally funded (A, , US, ?) Public
data-base VO compliant
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Science goals
Comparison with simulations of structure-growthwi
thin a CDM Universe (Steinmetz Navarro,
2002) Substructure in the halo (cold stellar
streams) Chemical signatures (?/Fe, Fe/H) to
identifycommon formation sites among
widely-separated stars Formation of bulges Origin
of the thick disk Dynamical state of the thin
disk and neighbouring spiral arms www.aip.de/RAVE
/
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RAVEthe first new-millennium survey
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Simulation of a galactic halo built up by
accretion of 100 satellite galaxies
The disrupted remnants can clearly be seen.
Same simulation plotted in phase space, revealing
the different orbits.
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More RAVEing
Phase I April 2003June 2005, using unallocated
UKST bright time during the 6dF Galaxy Survey 105
stars with Ilt13.5, B-Vlt0.8 Centred on Ca
triplet ?? 8498Å, 8542Å, 8662Å in the far red
region of the spectrum Currently measuring 700
stars per night Phase II 200610, all UKST time
once the Galaxy Survey is complete Will measure
22,000 stars per night
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The future of Schmidtery
Instrumentation for RAVEing
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Phase I instrumentation 6dF robot
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(with 100µm fibres)
6dF VPH Grating Parameters

• Grating Reciprocal Instrumental CCD Spectral di
  spersion resolution resolution range
  (Å/mm) (Å) (Å/pixel) (Å)
• 425R 169 6.6 2.20 5300-7600
• 580V 126 4.9 1.64 3900-5600
• 1201B 60 2.1 0.78 3600-4400
• 1700I 30 1.0 0.4 8415-8800
• (All in 1st order)

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Phase II instrumentation

• 6dF is too slow for 22,000 stars per night...
• Therefore adapt the 400-fibre positioner
  currently being developed by AAO for Subaru

Echidna Ball-Spine Array
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Moduleassembly

• Top bridge
• Fibre cover
• Middle bridge
• Fibre spines and piezo actuators
• Module PCB
• Module base

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Echidna complete design
Single module
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Echidna for RAVE

• 2250 spines (each with 15 arcmin patrol area)
• Covers full field area of 6 ? 6 deg2
• Feeds spectrograph with 3?750 banks of spectra
• Who builds the spectrograph?
• AAO has go-ahead for a UKidna design-study
• But UKidna will cost A2M
• How might it be funded?

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The MOMFOS story
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The future of Schmidtery
The RAVEs Progress
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Implementation plan
RAVE timeline 1.4.03 - 30.6.05 (2.25y) Phase
0/I (External staff required 2.0FTE by
31.12.03) 1.7.05 - 31.12.05 (0.5y) UKidna
installation/comm. 1.1.06 - 31.12.10 (5.0y)
Phase II (External staff required 6.0FTE by
1.7.05)
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6dF observations 03A
6dFGS RAVE N/S Total Exp 2003 (flds) (flds)
(flds) (flds) (hours) Jan/Feb
25 10 35 95.9 Feb/Mar 16 19 35 72.3 Mar/Apr
24 3 14 41 96.3 Apr/May 37 32 9 78 115.9 May/
Jun 33 12 8 53 84.9 Jun/Jul 37 21 2 60 80.5
Total 172 68 62 302 548.8 to 2003 July 8/9
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VO-compliance

• Data-format easy to make VO compliant (though
  AAO may adopt CADC format rather than VOtable)
• Metadata robot-generated data, etc. already
  written to data headers, but observer data is not
• Log6dF will allow additional metadata to be
  aatached (observing conditions, weather data,
  field alignment quality, observers name,
  observer comments, etc. etc.)

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RAVE spectrum?
A vs.
A vs.
A vs. US
A vs.