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July 2005 Gdansk, Poland 1 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: M*A*S*H Q.A.Parker Macquarie University/AAO A.Acker (Observatoire.

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Presentation on theme: "July 2005 Gdansk, Poland 1 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: M*A*S*H Q.A.Parker Macquarie University/AAO A.Acker (Observatoire."— Presentation transcript:

1 July 2005 Gdansk, Poland 1 The Macquarie/AAO/Strasbourg H-alpha Planetary Nebulae Project: M*A*S*H Q.A.Parker Macquarie University/AAO A.Acker (Observatoire de Strasbourg, ULP) A.E.J.Peyaud (MU/ULP), D.J.Frew (MU) & the rest of the MASH team

2 July 2005 Gdansk, Poland 2 M*A*S*H Macquarie/AAO/Strasbourg Hα Planetary Nebula Catalogue (MASH) of ~1000 new Galactic Planetary Nebulae (PNe) discovered from the AAO/UKST Hα survey of the southern Galactic plane Macquarie/AAO/Strasbourg Hα Planetary Nebula Catalogue (MASH) of ~1000 new Galactic Planetary Nebulae (PNe) discovered from the AAO/UKST Hα survey of the southern Galactic 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 coverage of Hα survey permitted detection of large numbers of new PNe: more evolved, larger angular extent, lower surface brightness than in most other surveys. Combination of depth, resolution, uniformity and areal coverage of Hα survey permitted detection of large numbers of new PNe: more evolved, larger angular extent, lower surface brightness than in most other surveys.

3 July 2005 Gdansk, Poland 3 STAMP COLLECTING………… Yes but: Yes but: I have a really nice album! I have a really nice album! You are all interested in the stamps You are all interested in the stamps I have some very rare ones I have some very rare ones They come from different regions with their varied and interesting designs They come from different regions with their varied and interesting designs One can investigate their colours and composition of the ink One can investigate their colours and composition of the ink One can test the glue on the back that hold them together and that enables us to fix what they are One can test the glue on the back that hold them together and that enables us to fix what they are I Like stamps I Like stamps

4 July 2005 Gdansk, Poland 4 30arcmin PFP1

5 July 2005 Gdansk, Poland 5 Setting the scene: The AAO/UKST Hα survey Survey completed in 2003 using a single-element interference filter of exceptional quality (Parker et al, 2005, MNRAS accepted: astro-ph/ ). Survey completed in 2003 using a single-element interference filter of exceptional quality (Parker et al, 2005, MNRAS accepted: astro-ph/ ). Filter aperture of 305mm is largest of its kind in astronomy with fine-grained Tech Pan film detector Filter aperture of 305mm is largest of its kind in astronomy with fine-grained Tech Pan film detector Survey coverage (~4000sq.deg), resolution (~1arcsec) and sensitivity (~5 Rayleighs) Survey coverage (~4000sq.deg), resolution (~1arcsec) and sensitivity (~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:

6 July 2005 Gdansk, Poland 6 The AAO/UKST H-alpha Survey

7 July 2005 Gdansk, Poland 7 Comparison between AAO/UKST H-alpha survey and the SHASSA (CTIO) 1.25deg This is still blocked x16 SCOS data!

8 July 2005 Gdansk, Poland 8 Full resolution 10um SCOS data

9 July 2005 Gdansk, Poland 9

10 July 2005 Gdansk, Poland 10 Culmination of an extensive programme of visual identification and full confirmatory spectroscopy ( ) Culmination of an extensive programme of visual identification and full confirmatory spectroscopy ( ) 2500 individual spectra obtained (many have multiple spectra) from 30 observing missions 2500 individual spectra obtained (many have multiple spectra) 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 largest, least biased and most homogeneous sample of Galactic PNe yet created over the widest evolutionary range. yields the largest, least biased and most homogeneous sample of Galactic PNe yet created over the widest evolutionary range. Hα less affected by dust and so easier to detect than [OIII] imaging in more obscured regions of the Galactic Plane. almost doubling of Galactic PNe almost doubling of Galactic PNe Hopefully significant impact on PNe research, especially at extremes of PNe luminosity function Hopefully significant impact on PNe research, especially at extremes of PNe luminosity function New MASH Planetary Nebulae

11 July 2005 Gdansk, Poland 11 MASH analysis MASH will contribute to: MASH will contribute to: late stellar evolution; mass-loss history of CSPNs late stellar evolution; mass-loss history of CSPNs PNe evolution and populations PNe evolution and populations Rare types Rare types ISM interaction ISM interaction Chemical enrichment of the ISM Chemical enrichment of the ISM Galactic abundance gradients Galactic abundance gradients Bulge dynamics Bulge dynamics Birth rates, Galactic scale heights Birth rates, Galactic scale heights Statistical correlations Statistical correlations

12 July 2005 Gdansk, Poland 12 Typical MASH PNe discovery Hα- 3hoursSR- 15mins Hα/SR 4x4arcminute

13 July 2005 Gdansk, Poland 13 MASH PNe examples.. The chromosome nebula Hot lips!

14 July 2005 Gdansk, Poland 14 Consecutive FLAIR spectroscopy of new PN candidates Low dispersion data High dispersion (red) data

15 July 2005 Gdansk, Poland 15 M*A*S*H Catalogue M*A*S*H Catalogue MASH completely updated from on-line SHS pixel-data MASH completely updated from on-line SHS pixel-data Carefully checked previous identifications Carefully 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 PNe compared to old version (CDROM 2001). Represents far more consistent and accurate description for MASH PNe compared to old version (CDROM 2001). Many contaminating HII regions removed and many new additional PNe added. Many contaminating HII regions removed and many new additional 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 evolution significant fraction represent some of the most senile stages of PNe evolution Includes those interacting with the ISM (e.g. PFP1 in Pierce et al and Frew and Parker, in preparation). Includes those interacting with the ISM (e.g. PFP1 in Pierce et al and Frew and Parker, in preparation).

16 July 2005 Gdansk, Poland 16 MASH PNe properties Currently < 10% of MASH PNe have obvious CSPN identified directly from the SHS images (too faint in red). Currently < 10% of MASH PNe have obvious CSPN identified directly from the SHS images (too faint in red). Additional CSPN candidates found by examination of the SuperCOSMOS images for the matching B, R and I band Additional CSPN candidates found by examination of the SuperCOSMOS images for the matching B, R and I band Long term deep UBVR CCD photometry required to find most MASH CSPN Long term deep UBVR CCD photometry required to find most MASH CSPN Average angular size is 51” with median of 27” but with objects extending to several arcminutes (largest is ~30 arcmins in size). Average angular size is 51” with median of 27” but with objects extending to several arcminutes (largest is ~30 arcmins in size). Indicates that many are highly evolved where the central star has faded from easy optical detection and the nebula itself is dissipating/dissolving into the ambient ISM. Indicates that many are highly evolved where the central star has faded from easy optical detection and the nebula itself is dissipating/dissolving into the ambient ISM.

17 July 2005 Gdansk, Poland 17 Better coverage of initial and terminal phases of PNe life by preferentially offering for study a factor of ~5 more large, highly evolved objects. Better coverage of initial and terminal phases of PNe life by preferentially offering for study a factor of ~5 more large, highly evolved objects. Known PNe fall off near galactic latitude b=0◦ due to extinction but new MASH PNe are found much closer to b=0◦ especially away from the heavily obscured bulge region. Known PNe fall off near galactic latitude b=0◦ due to extinction but new MASH PNe are found much closer to b=0◦ especially away from the heavily obscured bulge region. Improved low latitude coverage due to survey’s excellent sensitivity in Hα band which is less affected by dust. Improved low latitude coverage due to survey’s excellent sensitivity in Hα band which is less affected by dust.

18 July 2005 Gdansk, Poland 18 FromAcker catalogue: ~1100 PN N&S From new MASH sample: includes 1021 New PN Simple Acker vs MASH PN l,b plot

19 July 2005 Gdansk, Poland 19 First M*A*S*H results 20 new WR CSPN (e.g. Morgan, Parker & Russeil, 2001, Parker & Morgan 2003) 20 new WR CSPN (e.g. Morgan, Parker & Russeil, 2001, Parker & Morgan 2003) Includes PM5, only confirmed WN Wolf-Rayet star in the galaxy (Morgan, Parker & Cohen 2003) Includes PM5, only confirmed WN Wolf-Rayet star in the galaxy (Morgan, Parker & Cohen 2003) A possible new phase of PN evolution by discovery of an OH IR strongly masing CPSN (Cohen, Parker & Chapman 2005) A possible new phase of PN evolution by discovery of an OH IR strongly masing CPSN (Cohen, Parker & Chapman 2005) A large evolved PN caught in the first stages of interaction with the ISM (Pierce et al. 2004) A large evolved PN caught in the first stages of interaction with the ISM (Pierce et al. 2004) Bipolar PNe (~13%): Identification of two of the largest and closest bipolar PNe (Frew, Parker & Russeil, 2005) Bipolar PNe (~13%): Identification of two of the largest and closest bipolar PNe (Frew, Parker & Russeil, 2005) Discovery of a clear-cut bipolar Type I PNe in an intermediate age open cluster (Parker, Frew and Köppen, in preparation) Discovery of a clear-cut bipolar Type I PNe in an intermediate age open cluster (Parker, Frew and Köppen, in preparation) significant implications for previous derived PNe properties such as distance and total ejecta mass (e.g. Parker, 2000 for NGC2899). New shells, ansae, lobes and halos around many known PNe: significant implications for previous derived PNe properties such as distance and total ejecta mass (e.g. Parker, 2000 for NGC2899).

20 July 2005 Gdansk, Poland 20 Type I bipolar PN in an open cluster SR exposure H-alpha exposure 3.5’

21 July 2005 Gdansk, Poland 21 The 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)

22 July 2005 Gdansk, Poland 22 PSF match of H-alpha/SR new MASH BULGE PNe + 6dF spectra

23 July 2005 Gdansk, Poland 23 Distribution of known and new MASH PNe in bulge region Dust distribution From Schlegel 2003

24 July 2005 Gdansk, Poland 24 <35”


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