Legacies of the MacquarieAAOStrasbourg Planetary Nebula project: MASH

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Legacies of the Macquarie/AAO/Strasbourg
Planetary Nebula project MASH

• Q.A.Parker
• Macquarie University/AAO
• A.Acker (ULP, Strasbourg) D.J.Frew (MQ/Perth),
  Brent Miszalksi (MQ/Strasbourg), Warren Reid
  (MQ), Martin Cohen (UC Berkeley) Anna Kovacevic
  (MQ), Kyle de Pew (MQ), Ivan Bojicic (MQ), Alan
  Peyaud (MQ/Strasbourg), Anne Green (U.Syd), Rhys
  Morris (Bristol), Malcolm Hartley (AAO) the
  greater MASH team

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The AAO/UKST Ha survey MASH project as a
conveyor-belt for HDR students, publications
more

• To my knowledge 14 HDR students have been
  supported so far from the AAO/UKST Ha survey
  with 9 of these from MQ of whom 5 have graduated
  since September 2005 (Pierce, Peyaud, Stupar,
  Reid, Frew)
• Currently 4 MQ postdocs associated Reid, Stupar,
  Frew (from march 2009), Peyaud (from April 2009)
• Establishment of MQ Concentration Of Research
  Excellence (CORE) ? new faculty, postdocs and PhD
  students!
• New faculty De Marco (from March 2009) Zucker
  (from Jan 2009)
• Currently 5 HDR students Miszalski, Bojicic,
  Kovacevic, DePew, Baxter 4 MQRES PhDs to
  advertise (DeMarco, Zucker)
• Total MQ/AAO astronomy group size now 30!
• 50 publications in last 5yrs
• MUCH of the above is down to MASH.

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What is a Planetary Nebula?We will discuss this
in detail laterbut

• Is a shell (or torus) of ionised gas around a hot
  (Teff 30,000 100,000K) central star (CS).
• PN formed as a low- to intermediate-mass star
  (1-8Msun) evolves from the asymptotic giant
  branch (AGB) to the white dwarf state.
• The PN represents the outer atmosphere of the
  former red giant, swept up and snow-plowed by
  the strong stellar wind of the hot CS which then
  ionises the ejected shroud.
• PNe show a wide variety of morphologies, ranging
  from spherical and elliptical, to bipolar and
  multi-polar forms.
• They show a rich, emission-line spectrum
  dominated by Hydrogen recombination lines, He
  lines, and strong forbidden lines of O, N, Ne, S,
  and Ar, plus a weak continuum.

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Galactic PNe catalogues

• Galactic PNe catalogues represent an extremely
  heterogeneous collection!
• They have arisen from over 85 years of diverse
  searches undertaken with a host of different
  telescopes and detection techniques over both
  hemispheres
• They are primarily listed as compilations in
• The ESO/Strasbourg Galactic PNe catalogues (Acker
  et al. 1992, 1996) which contain 1385 true and
  probable PNe and 489 possible PNe
• The independent, but essentially equivalent,
  compilations of 1510 Galactic PNe by Kohoutek
  (e.g. Kohoutek 2001)
• Additional Galactic PNe in relatively small
  numbers since then until the advent of MASH in
  the South and now IPHAS in the North (Corradi and
  Zijlstra talks later)

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However..

• PNe become rapidly unobservable.
• The typical expansion velocity of 25km/s, the
  decreasing low density of the gas and the
  declining luminosity of the central star as it
  descends into the white dwarf cooling track,
  causes a gradual decrease in emission measure.
• These effects yield an average PN lifetime of
  10,000yrs (eg Zijlstra Pottasch, 1991) before
  dissipation and invisibility.
• It is hence important in search techniques to
  highlight the faintest of detections, else there
  is a risk of bias in the known populations of
  highly evolved and PNe.
• Conversely, young PNe may also be very compact
  and difficult to distinguish from stars in direct
  imaging a known problem with MASH prior to
  MASH-II

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We all know why we survey for PNe ?

• PNe are among the most complex, beautiful and
  fascinating of celestial phenomena.
• PNe hold the key to determining the physics and
  time-scales of mass loss and evolution for low to
  intermediate mass stars (Iben 1995).
• They are also vital probes of
• nucleosynthesis processes
• abundance gradients
• chemical enrichment of the interstellar medium
  (PN are a key source off pre-biotic carbon)
• PNe also act powerful tracers of our Galaxys
  star-forming history and are useful kinematical
  probes visible to large Galactic distances due to
  their rich emission line spectrum.
• Can be used as powerful standard candles in
  external galaxies due to apparent constancy of
  the bright-end cut-off of the PNLF
• These scientific drivers and others motivate the
  search for and study of the PNe diaspora in our
  galaxy.

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The MASH Galactic Planetary Nebulae Catalogues

• Sadly, the MASH PNe discovery phase is drawing to
  a close ?
• Culmination of an extensive 10 year programme of
  visual identification, multi-wavelength
  comparison and spectroscopy (1998-2008)
• Obtained gt3000 individual spectra!
• Used for for confirmation, kinematics and
  abundances
• Obtained using a variety of 2m, 4m and 8m
  telescopes
• e.g. SAAO 1.9m, MSSSO 2.3m, UKST 6DF/FLAIR, AAT
  AAOmega, SPIRAL, Gemini GMOS and ESO VLT
  IFU/FLAMES
• Supplemented by radio study using ATCA (Bojicic
  talking later)

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Some MASH spectroscopic observing
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pre observing SAAOwe did observe later that
night!
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Consecutive FLAIR spectroscopy of new PN
candidates

• Low dispersion data

• High dispersion (red) data

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The MASH Galactic Planetary Nebulae Catalogues

• 1250 new Galactic PNe uncovered so far Parker
  et al., 2006 Miszalski et al., 2008 and see
• http//www.vizier.u-strasbg.fr/vizier/MASH
• Entire sample derived from same, uniform
  observational data.
• This is a significant advantage and was essential
  to yield
• the largest, least biased and most homogeneous
  sample of Galactic PNe yet created over a wide
  evolutionary range
• Uncovered PNe are not simply the same as found in
  previous catalogues
• MASH PNe sample the more extremes of PNe
  evolution
• They are are often more obscured, more extended
  and of lower surface brightness

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Setting the scene It is the AAO/UKST Ha survey
that has enabled MASH!

• Survey completed in 2003 using a single-element
  interference filter of exceptional quality
  (Parker et al, 2005, MNRAS, 362, 689).
• Filter aperture of 305mm is largest of its kind
  in astronomy
• Fine-grained Tech Pan film detector, 70Angstrom
  FWHM filter
• Survey coverage (4000sq.deg) , resolution
  (1arcsec) and sensitivity (5 Rayleighs)
• FULLY on-line as a digital data product of the
  WFAU of the ROE http//www-wfau.roe.ac.uk/sss/hal
  pha/

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SuperCosmos H-alpha Survey (SHS)http//www-wfau.
roe.ac.uk/sss/halpha
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Comparison with other surveys
Even with the advent of VPHAS no other Ha survey
will have the same Galactic plane coverage in
terms of resolution and sensitivity apart from
perhaps a future SkyMapper survey (details later
if there is time)
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In the IPHAS/SHS overlap region SHS comparable
depth to IPHAS for extended emission (R.Morriss)
SHS
IPHAS
IPHAS
IPHAS
IPHAS
SHS
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SHS Flux calibration it is possible!

• Extensive testing and comparison has been
  performed between SCOS and SHASSA data (Pierce,
  Frew, Parker, Gunawardhena)
• The SHASSA data has been directly calibrated to a
  Rayleigh scale and is reliable
• The SHS data is generally very well behaved
  though each survey field does need to be
  calibrated separately

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The SHS can be flux calibrated over 2.5dex
Gunawardhena Parker, 2009, PASA
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MASH analysis

• MASH will contribute to
• late stellar evolution mass-loss history of
  CSPNs
• PNe evolution and populations ? access to more
  representative samples
• Rare types ? adds to debate as to what is a PNe?
• ISM interaction ? increase examples for study
• Chemical enrichment of the ISM
• Galactic abundance gradients ? ESO VLT/2.3m data
• Bulge dynamics ? accurate radial velocities
  available
• Birth rates, Galactic scale heights ? from local
  volume
• Statistical correlations, PNLF structure ? sheer
  statistics

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Highlights from MASH

• Doubling known PNe numbers in the Galaxy and
  tripling those in the LMC (Parker et al 2006,
  Miszalski et al 2008, Reid Parker, 2006ab)!
• Finding more extreme examples of PNe evolution
  and ISM interactions eg. PFP1 (Pierce et al.,
  2004), RCW24 (Frew Parker 2006)
• Improved techniques for eliminating contaminants
  (Parker et al. 2007, Frew 2008, Frew Parker in
  prep)
• Clean local volume census of PNe within 2Kpc
  (Frew thesis 2008)
• New estimates for PNe Galactic population,
  scale-height and birth rate (Frew thesis 2008,
  Frew et al in prep)
• New surface-brightness radius relation for
  improved PNe distance estimates (Frew thesis,
  2008)
• New local volume, Bulge and LMC PNLFs (Frew,
  Kovacevic, Reid theses)

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The importance of sensitivity and narrow-band
imaging
30 or 3pc PFP1
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MASH IIPlanetary Nebulae REDUX
MPA1644-4002
SuWt3
(Brent Miszalski), Quentin Parker, Agnes Acker,
Martin Cohen David Frew, Anna Kovacevic, Jayne
Birkby and the MASH team
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New data processing techniques

• A selection of carefully written scripts (Brent
  Miszalski) allowed efficient data download, for
  use in analysing potential candidates from the
  blocked down quotient data.
• By combining the 3hr Ha and short red (SR)
  exposures with the corresponding UKST/blue Bj
  band image, RGB images for each candidate were
  created at full resolution.
• This provided a vital means of distinguishing
  between true candidates and PN mimics.
• Matching 2MASS J, H and K band images provided
  another means for eliminating non-PN contaminants
  in the selection, particularly dust shrouded IR
  bright stars.
• FULL details will follow in Brents talk ?

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Examples of New Large MASH-II PNe
BMP1808-1406 Diameter 470 arcsec High NII/Ha
ratio Blue Central Star
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Reid Parker (2006ab)
NOAO/AURA/NSF C.Smith
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Colour combination of Red and H? Stack Images


Red Stack
H? Stack


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Images and Spectra
PR 23
RP 25
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Two evolved bipolar PNe Frew, Parker Russeil
(2006, MNRAS, 372, 1081)

• Bran 147 A/B ? RCW24
  RCW 69
• originally identified as two HII regions

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RCW24 - this object got David Frew and I
together..? when I was still at the ROE in 2001
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Multi-wavelength Comparisons and access to
federated data-sets

• Ideal to combine multi-wavelength NIR, MIR,
  optical and radio imaging (including in narrow
  optical bands) with large spectral wavelength
  coverage in (UV)/Optical/NIR to provide more
  complete picture of the PNe phenemenon
• Previously difficult to achieve in most cases
  without detailed individual follow-up
• Advent of major wide-area surveys and their
  accessibility in the last few years has improved
  the situation considerably (SHS, SHASSA, IPHAS,
  MOST, NVSS, MSX, 2MASS, UKIDSS, GLIMPSE)!
• These offer unprecedented opportunities for
  discovery and permit investigation of
  relationships between measured and derived
  parameters with unrivalled precision and to
  eliminate contaminants (Frews talk later today).
• Frew has used these techniques to eliminate 20
  of known PNe from his local volume sample as
  not being bona-fide (see later)

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Spot the difference.

• Compact MASH-II PN candidates left to right
  colour Ha/SR/Bj
• Composite, Ha/Sr quotient and 2MASS JHK
  composite. The lack of a JHK counterpart bodes
  well for the PN identification.

More compact MASH-II candidates. Note that here
there is a bright 2MASS point source coincident
with the putative PN indicating that it is far
more likely to be a stellar source.
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Removing impostorsImproved techniques for
removing imposters are based on multi-wavelength
photometry, spectral diagnostics, environment,
kinematics etc

• Nebular morphology (does it look like a PN?)
• Emission line ratios (are they appropriate?)
• Ionization structure (including the consistency
  of any ISM interaction with PM vector of central
  star, if known)
• Systemic velocity of nebula (does it differ from
  star?)
• Line width of nebular gas (is the gas moving at
  sensible speeds?)
• Properties of central star, including
  evolutionary age
• NIR/MIR properties (e.g. use 2MASS, MSX, GLIMPSE
  data)
• No one criterion is generally enough to
  define the status of an object so we use the
  "overall body of evidence to make a choice.

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Importance of multi-wavelength comparison
2arcmin
Was a PN candidate but MSX form spectroscopy
indicated a HII region
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Fresh insights into multi-wavelength PNe
properties. MIR/radio flux ratio evolution of
Pne (Cohens talk)

• Typical MASH-I PN (203") is larger more
  evolved than typical ESO PN (125") x1.67
• As PN expands MOST beamgtPN diameter, radio flux
  unchanged FUV to sustain the PDR drops x1.672
  ?x2.8
• PAHs in PDRs emit 8?m so MIR/ratio falls as
  fewer UV photons pump PAHs into IR fluorescence
  12/2.84.3
• HII regions show little change in MIR/radio,
  unlike PNe
• MASH-II PNe fainter than MASH-I PNe either much
  more compact (hard to see) or much larger (very
  faint)
• Suggest ESO12?MASH-I5 ?MASH-II2?

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A GLIMPSE at some MASH PNe
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Towards a new Census of Local PNeDavid Frew
(PhD, 2008)

• Remove impostors!
• Use new census to estimate number density and
  scale height of PNe
• Give new estimates of PN birth rate and total
  number of Galactic PNe.
• Derive a more complete PNLF for local sample
• Compare with new LMC PNLF (Reid Parker, 2009)

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The Solar Neighbourhood (1 kpc) Censussome
numbers(Frews thesis, 2008)

• PN column density 26 3 kpc-2
• PN scale height 195 30 pc
• Galactic PN population 28 000 4000
• Galactic production rate 0.4 yr-1
• PN formation rate 0.9 0.3 x 10-12 pc-3 yr-1
• WD formation rate 0.75 0.25 x 10-12 pc-3 yr-1
  (Vennes et al. 2002)
• WD formation rate 1.0 0.25 x 10-12 pc-3 yr-1
  (Liebert et al. 2005)

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The Ha surface-brightness radius (SB-r) relation

• We have recently developed an innovative, Ha
  surface-brightness radius (SB-r) relation that
  can provide more accurate distance estimates.
  This runs over a factor of 10 million in surface
  brightness (Frew Parker 2007, Frew 2008) see
  Fig.1.
• Such a relation could only be derived with the
  advent of homogeneous Ha surveys, eg. Gaustad et
  al. (2001), Parker et al. (2005) and Drew et al.
  (2005).
• The SB-r relation is built via observational
  parameters for 118 critically evaluated PN
  calibrators with reliable distances from primary
  techniques over a broad range of excitation and
  brightness.
• Our advantage over previous efforts in this
  direction lies in the surveys dynamic range, in
  our ability to remove contaminants and in
  intelligent use of the very best data.
• For the first time, we can now construct
  accurate volume-limited PN samples (for further
  details refer to Frews second talk).

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Highlights continued

• Discovery of 3 eclipsing binary CSPN (Miszalski
  et al., 2008)
• Discovery of 20 binary CSPN using OGLE-III and
  new estimate for CSPN binary fraction (Miszalksi
  et al., 2009, Miszalski thesis 2009)
• Discovery of several halo PN with velocities
  gt300km/s towards the Galactic Centre, discovery
  of likely Sagittarius dwarf PN
• Discovery of a PN in an old open cluster (Parker
  et al., 2009, in prep).
• Finding additional shells, ansae and lobes around
  many known Pne
• An unseen phase of PN evolution Discovery of
  PN around OH IR star V1018 Sco (Cohen et al.,
  2005, 2006)
• New shape to excitation class distribution for
  MASH and LMC PNe cf. previous known sample
• Discovery of 20 Wolf-Rayet CSPN of MASH PN
  including PM5 the only known WN (Parker et al.,
  2003, Cohen et al., 2005, De Pew thesis)

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Of 21 binary CSPN found 12 are from
MASHMiszalski et al., 2009, in press
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A new bipolar PN in an intermediate-age open
cluster
3.5
SR exposure
Ha exposure
Blue region
Red region
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The faint old open cluster, ESO 96-SC04

• Cluster has a core diameter of 1.0'. PN is
  within cluster core and has a similar radial
  velocity!
• Estimated age is 7 x 108 years (Carraro et al.,
  1995).
• Estimated distance 11.8 kpc one of the most
  remote open clusters.
• PN optical diameter is 20 arcsec, which gives a
  physical diameter of 1pc for the PN if it is a
  cluster member.
• Is the only PN found within 4 square degrees of
  the cluster.
• Is a Type I PN, with enhanced N and He
  abundances. This suggests a progenitor star mass
  of gt 2.3 solar masses, in agreement with the
  turnoff mass of the cluster.
• New CTIO 4-m mosaic camera photometry and AAOmega
  spectroscopy of cluster stars
• Paper in prep (Parker, Frew et al., 2009).

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Bi-polar PN in an open cluster AL1 (ES096-SC04)!
3.5
SR exposure
H-alpha exposure
Red region
Blue region
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NGC2899 discovery of faint outer lobes
NW lobe
14arcmins
SE lobe
28arcmins
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Close-up of two lobes
SE lobe
NW lobe
Each image is 3.2arcmins across
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FLAIR spectra of central PN and SE lobe
NII
SII
Central PNE red spectrum
SE lobe red spectrum
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Examples of known PN with newly identified
external features
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An unseen phase of PN evolution V1018Sco

• The only PN detected around a star still
  pulsating on the AGB!
• 1500d period still pulsating regularly
• Faint, almost circular ionized nebula
• Ha, NII and SII typical of PN spectra
• With ATCA sought diffuse continuum across PN
• Found 2 strongly non-thermal synchrotron sources
• Previously unobserved phase of stellar evolution?
• 4M? AGB star just started to form a PN
• Fast wind from the central star has recently
  turned on
• Ploughs into the slow AGB wind creating shocks,
  non-thermal emission and a compressed shell which
  is visible

Cohen, Parker, Chapman 2005, MNRAS, 357,
1189 Cohen, Chapman, Deacon, Sault, Parker, Green
2006, MNRAS, 369, 189
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V1018 Sco, OH354.88-0.54 the masers the nebula
LI
IRAS
OH 1612 MHz

RI
1612 MHz lightcurve
MSX

Ha/SR quotient image of the PN with variable PSF
matching before dividing Ha and SR pixel data.
Transient H2O maser
RI post-AGB LI intermediate mass ?4M? AGB
stars. V1018 Sco is LI.
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PNe excitation class
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Images spectra of first new Wolf-Rayet CSPN
discovered in MASH
WO4 PMR1
WC9/WC10 PMR2
4.6arcmin
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Serendipity
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But what of the future???

• MASH exploitation will continue for some years
  yet..
• However, MQ and growing MASH group keen to remain
  involved and to participate more directly in
• IPHAS B group activities and exploitation
• Can offer co-tutelle PhDs joint supervision,
  extended visits, AAO links
• Access to 2.3m/AAOmega
• SkyMapper through links with ANU (Keller/Bessell)
• VPHAS can offer manpower (data analysis,
  follow-up etc)

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But we are still discovering new PNe SNRs!
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.
SkyMapper and prospects for narrow-band Imaging
surveys of the Southern Galactic plane

• Quentin Parker (AAO/MQ)
• on behalf of
• Stefan Keller, Brian Schmidt and Mike Bessell
  (ANU)

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Rapid survey era is emerging
Ha
2.4
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Proposed Ha filter
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Skymapper!
early 2009
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Narrow band SkyMapper filters

• Originally planned to re-use the AAO/UKST
  monolithic Ha filter (worth 46K in todays
  money)
• Unfortunately re-designs to filter wheel meant
  that the AAO/UKST filter would no longer fit into
  the required enclosure
• New Ha filter will be required and various
  options have been discussed (Mike Bessell)
• Decision made in March 2009 but will come from
  ANU funds with possible addition from MQ
• Additional narrow-band filters such as OIII and
  SII will be the subject of a LIEF bid led in
  May 2009 by ANU but with MQ/VPHAS participation
  (and possibly others)

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Possible Ha survey(s)

• Approximately 75 of the time on SkyMapper will
  be initially dedicated to the Southern Sky
  Survey.
• This leaves 25 for other projects including a Ha
  survey that can make effective use of BoM.
• Proposed 120sec Ha exposures with 25sec readout
  and 5.7sq.deg/exposure ? 1296 sq/deg/night.
• SkyMapper has 1.174 LGP of UKST.
• Entire 4000sq.deg of SHS covered in 3.1 nights
  but 1mag shallower or 24 nights to same depth
  with 15min exposures
• SkyMapper pixel size 0.5arcsec (cf SCOS
  0.67arcsec)

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Tangible community benefits

• The H-alpha filter will be available to any user
  of the SkyMapper telescope.
• This will allow a wider range of science to be
  conducted by the telescope, thereby increasing
  its user-base and scientific impact.
• The analysis of H-alpha data will be incorporated
  into a program to provide research experience for
  undergraduates.
• This program will assist in the retention of
  students to higher degree programs by engaging
  them in cutting edge science.
• The H-alpha filter will expedite the PhD thesis
  of Mr. Simon Murphy and form the basis of
  numerous theses in the future. It will facilitate
  Australian (Prof. Q. Parker, Macquarie
  University, Dr. M. Filopovic, Univ. Wollongong,
  Prof. A. Green, Univ. Sydney) and international
  (Prof. J. Drew, Imperial UK) collaborations with
  RSAA academics.

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Skymapper H-alpha data

• The SkyMapper H-alpha filter will adds an
  additional dimension to the current SkyMapper
  program
• it opens up the study of the gas phase building
  on the success of the AAO/UKST H-alpha survey in
  the South
• The H-alpha data obtained together with the
  SkyMapper survey data
• It is intended to make the H-alpha data available
  to the world via the web after data validation
  and perhaps some preliminary exploitation (TBC)
• This develops an additional powerful data
  resource of benefit to the national and
  international communities