July 2005 Gdansk, Poland 1 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: MAS*H...

July 2005July 2005 Gdansk, PolandGdansk, Poland 11

The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: M*A*S*H

Q.A.ParkerQ.A.ParkerMacquarie University/AAOMacquarie University/AAO

A.Acker (Observatoire de Strasbourg, ULP)A.Acker (Observatoire de Strasbourg, ULP)A.E.J.Peyaud (MU/ULP), D.J.Frew (MU) & the A.E.J.Peyaud (MU/ULP), D.J.Frew (MU) & the

rest of the MASH teamrest of the MASH team


M*A*S*HM*A*S*H MMacquarie/acquarie/AAAO/AO/SStrasbourg trasbourg HHα Planetary Nebula Catalogue α Planetary Nebula Catalogue

(MASH)(MASH) of of ~1000 new Galactic Planetary Nebulae (PNe)~1000 new Galactic Planetary Nebulae (PNe) discovered from the AAO/UKST Hα survey of the southern discovered from the AAO/UKST Hα survey of the southern Galactic planeGalactic plane

MASH now complete (CDS catalogue release Aug/Sep 2005). MASH now complete (CDS catalogue release Aug/Sep 2005).

Combination of depth, resolution, uniformity and areal Combination of depth, resolution, uniformity and areal coverage of Hα survey permitted detection of large numbers of coverage of Hα survey permitted detection of large numbers of new PNe: new PNe: more evolved, larger angular extent, lower surface more evolved, larger angular extent, lower surface brightnessbrightness than in most other surveys. than in most other surveys.


STAMP COLLECTING…………STAMP COLLECTING………… Yes but:Yes but:

• I have a really nice album!I have a really nice album!• You are all interested in the stampsYou are all interested in the stamps• I have some very rare onesI have some very rare ones• They come from different regions with their varied and They come from different regions with their varied and

interesting designsinteresting designs• One can investigate their colours and composition of the One can investigate their colours and composition of the

inkink• One can test the glue on the back that hold them together One can test the glue on the back that hold them together

and that enables us to fix what they areand that enables us to fix what they are• I Like stampsI Like stamps


30arcmin

PFP1


Setting the scene:Setting the scene: The AAO/UKST HThe AAO/UKST Hαα survey survey

Survey completed in 2003 using a single-element interference Survey completed in 2003 using a single-element interference filter of exceptional quality (Parker et al, 2005, MNRAS filter of exceptional quality (Parker et al, 2005, MNRAS accepted: accepted: astro-ph/0506599astro-ph/0506599). ).

Filter aperture of 305mm is largest of its kind in astronomy Filter aperture of 305mm is largest of its kind in astronomy with fine-grained Tech Pan film detector with fine-grained Tech Pan film detector

Survey coverage Survey coverage (~4000sq.deg(~4000sq.deg) , resolution ) , resolution (~1arcsec(~1arcsec) and ) and sensitivity sensitivity (~5 Rayleighs(~5 Rayleighs) )

On-line as a digital data product of the WFAU of the ROE: On-line as a digital data product of the WFAU of the ROE: http://www-wfau.roe.ac.uk/sss/halpha/http://www-wfau.roe.ac.uk/sss/halpha/


The AAO/UKST H-alpha SurveyThe AAO/UKST H-alpha Survey

http://surveys.roe.ac.uk/ssa/hablock/hafull.html


Comparison between AAO/UKST H-alpha survey and the Comparison between AAO/UKST H-alpha survey and the SHASSA (CTIO)SHASSA (CTIO)

1.25deg1.25deg

This is still blocked x16 SCOS data!This is still blocked x16 SCOS data!


Full resolution 10um SCOS data



Culmination of an extensive programme of visual Culmination of an extensive programme of visual identification and identification and full confirmatory spectroscopyfull confirmatory spectroscopy (1998-2005) (1998-2005)• 2500 individual spectra obtained (many have multiple 2500 individual spectra obtained (many have multiple

spectra) from 30 observing missionsspectra) from 30 observing missions• Flux calibration for most (not easy with fibre spectroscopy)Flux calibration for most (not easy with fibre spectroscopy)

Entire sample derived from same, uniform observational data Entire sample derived from same, uniform observational data • yields the yields the largest, least biased and most homogeneouslargest, least biased and most homogeneous

sample of Galactic PNe yet created over the widest sample of Galactic PNe yet created over the widest evolutionary range.evolutionary range.

• Hα less affected by dust and so easier to detect than [OIII] imaging in more obscured regions of the Galactic Plane.

• almost almost doubling doubling of Galactic PNe of Galactic PNe • Hopefully significant impact on PNe research, especially at Hopefully significant impact on PNe research, especially at

extremes of PNe luminosity functionextremes of PNe luminosity function

New MASH Planetary NebulaeNew MASH Planetary Nebulae


MASH analysisMASH analysis

MASH will contribute to:MASH will contribute to:• late stellar evolution; mass-loss history of CSPNslate stellar evolution; mass-loss history of CSPNs

• PNe evolution and populationsPNe evolution and populations

• Rare typesRare types

• ISM interactionISM interaction

• Chemical enrichment of the ISM Chemical enrichment of the ISM

• Galactic abundance gradientsGalactic abundance gradients

• Bulge dynamicsBulge dynamics

• Birth rates, Galactic scale heightsBirth rates, Galactic scale heights

• Statistical correlationsStatistical correlations


Typical MASH PNe discovery

Hα- 3hours SR- 15mins Hα/SR

4x4arcminute


MASH PNe examples..MASH PNe examples..

The chromosome nebula

Hot lips!


Consecutive FLAIR spectroscopy of new PN candidatesConsecutive FLAIR spectroscopy of new PN candidates

Low dispersion data High dispersion (red) data


M*A*S*H CatalogueM*A*S*H Catalogue MASH completely updated from on-line SHS pixel-dataMASH completely updated from on-line SHS pixel-data

• Carefully checked previous identificationsCarefully checked previous identifications• Determined accurate estimates of PNe size & position (~1-2”)Determined accurate estimates of PNe size & position (~1-2”)• New morphological classifications assigned (ERBIAS)New morphological classifications assigned (ERBIAS)• Represents far more consistent and accurate description for MASH Represents far more consistent and accurate description for MASH

PNe compared to old version (CDROM 2001). PNe compared to old version (CDROM 2001). • Many contaminating HII regions removed and many new additional Many contaminating HII regions removed and many new additional

PNe added.PNe added. MASH PNe different to what is known in previous catalogues. MASH PNe different to what is known in previous catalogues.

• significant fraction represent some of the most senile stages of PNe significant fraction represent some of the most senile stages of PNe evolutionevolution

• Includes those interacting with the ISM (e.g. PFP1 in Pierce et al. Includes those interacting with the ISM (e.g. PFP1 in Pierce et al. 2004 and Frew and Parker, in preparation).2004 and Frew and Parker, in preparation).


MASH PNe propertiesMASH PNe properties

Currently < 10% of MASH PNe have obvious CSPN Currently < 10% of MASH PNe have obvious CSPN identified directly from the SHS images (too faint in red).identified directly from the SHS images (too faint in red).

Additional CSPN candidates found by examination of the Additional CSPN candidates found by examination of the SuperCOSMOS images for the matching B, R and I bandSuperCOSMOS images for the matching B, R and I band

Long term deep UBVR CCD photometry required to find most Long term deep UBVR CCD photometry required to find most MASH CSPNMASH CSPN

Average angular size is 51” with median of 27” but with Average angular size is 51” with median of 27” but with objects extending to several arcminutes (largest is ~30 arcmins objects extending to several arcminutes (largest is ~30 arcmins in size).in size).

Indicates that many are highly evolved where the central star Indicates that many are highly evolved where the central star has faded from easy optical detection and the nebula itself is has faded from easy optical detection and the nebula itself is dissipating/dissolving into the ambient ISM.dissipating/dissolving into the ambient ISM.


Better coverage of initial and terminal phases of PNe Better coverage of initial and terminal phases of PNe life by preferentially offering for study a factor of ~5 life by preferentially offering for study a factor of ~5 more large, highly evolved objects. more large, highly evolved objects.

Known PNe fall off near galactic latitude b=0◦ due to Known PNe fall off near galactic latitude b=0◦ due to extinction but new MASH PNe are found much extinction but new MASH PNe are found much closer to b=0◦ especially away from the heavily closer to b=0◦ especially away from the heavily obscured bulge region. obscured bulge region.

Improved low latitude coverage due to survey’s Improved low latitude coverage due to survey’s excellent sensitivity in Hexcellent sensitivity in Hαα band which is less affected band which is less affected by dust. by dust.


FromAcker catalogue:FromAcker catalogue:

~1100 PN N&S~1100 PN N&S

From new MASH sample:From new MASH sample:

includes 1021 New PNincludes 1021 New PN

Simple Acker vs MASH PN l,b plotSimple Acker vs MASH PN l,b plot


First M*A*S*H resultsFirst M*A*S*H results 20 new WR CSPN20 new WR CSPN (e.g. Morgan, Parker & Russeil, 2001, Parker & (e.g. Morgan, Parker & Russeil, 2001, Parker &

Morgan 2003) Morgan 2003) • Includes PM5, Includes PM5, only confirmed WN Wolf-Rayet star in the galaxyonly confirmed WN Wolf-Rayet star in the galaxy (Morgan, (Morgan,

Parker & Cohen 2003)Parker & Cohen 2003) A possible A possible new phase of PN evolutionnew phase of PN evolution by discovery of an OH IR strongly by discovery of an OH IR strongly

masing CPSN (Cohen, Parker & Chapman 2005)masing CPSN (Cohen, Parker & Chapman 2005) A large evolved PN caught in the first stages of interaction with the ISM A large evolved PN caught in the first stages of interaction with the ISM

(Pierce et al. 2004)(Pierce et al. 2004) Bipolar PNe (~13%): Bipolar PNe (~13%): Identification of two of the largest and closest bipolar Identification of two of the largest and closest bipolar

PNe (Frew, Parker & Russeil, 2005)PNe (Frew, Parker & Russeil, 2005) Discovery of a clear-cut bipolar Type I PNe in an intermediate age open Discovery of a clear-cut bipolar Type I PNe in an intermediate age open

cluster (Parker, Frew and Kcluster (Parker, Frew and Kööppen, in preparation)ppen, in preparation) New shells, ansae, lobes and halos around many known PNe: significant significant

implications for previous derived PNe properties such as distance and total implications for previous derived PNe properties such as distance and total ejecta mass (e.g. Parker, 2000 for NGC2899). ejecta mass (e.g. Parker, 2000 for NGC2899).


Type I bipolar PN in an open clusterType I bipolar PN in an open cluster

SR exposure H-alpha exposure

3.5’


The Galactic BulgeThe Galactic Bulge

About 500 MASH PN found in the Galactic Bulge region

Many found using sophisticated psf matching

Confirmed via FLAIR/6dF MOS spectroscopy on UKST or on 2m class telescopes (e.g. SAAO, MSSSO)


PSF match of H-alpha/SR new MASH PSF match of H-alpha/SR new MASH BULGE PNe + 6dF spectraBULGE PNe + 6dF spectra


Distribution of known and new MASHPNe in bulge region

Dust distributionFrom Schlegel 2003


<35”

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July 2005 Gdansk, Poland 1 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: M*A*S*H...

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July 2005 Gdansk, Poland 1 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: MAS*H...