11

Do post-common Do post-common envelope objects form envelope objects form

a distinct subset of a distinct subset of PNe?PNe?

David J. FrewDavid J. FrewPerth Observatory & Macquarie UniversityPerth Observatory & Macquarie University

Q.A. Parker and the MASH CollaborationQ.A. Parker and the MASH Collaboration

Asymmetrical Planetary Nebulae IVAsymmetrical Planetary Nebulae IV

La Palma, 21 June 2007La Palma, 21 June 2007

22

The Solar Neighbourhood The Solar Neighbourhood Sample…Sample…

Database of ‘potentially nearby’ PNe

Improved integrated fluxes in H and [OIII]

Combination of literature and new spectroscopic data, kinematic data, and CSPN photometry

Using revised/new distances, define a volume-limited sample within 1.0 kpc (presently, n = 53)

Extending sample volume to 1.5 kpc and 2.0 kpc (in progress)

33

FP 1824-0321FP 1824-0321 (Frew et al., in prep.)(Frew et al., in prep.)

30' 30'

PFP 1PFP 1(Pierce et al. 2004)(Pierce et al. 2004)

RCW 24RCW 24(Frew et al. 2006)(Frew et al. 2006)

FP 0905-3033FP 0905-3033(Frew et al., in prep.)(Frew et al., in prep.)

30’

New giant PNe in the solar neighbourhoodNew giant PNe in the solar neighbourhood

44

Planetary nebula or ionized ambient Planetary nebula or ionized ambient ISM…ISM…

Sh 2-174, DeHt 5, RE 1738+665, Sh 2-68, HDW 5… Sh 2-174, DeHt 5, RE 1738+665, Sh 2-68, HDW 5… PG 0108+101, PG 0109+111, KPD 0005+5106, PG 0108+101, PG 0109+111, KPD 0005+5106,

Hewett 1…Hewett 1… PHL 932, EGB 5… PHL 932, EGB 5… … … are not bona fide PNeare not bona fide PNe, but simply ionized , but simply ionized

‘Str‘Ströömgren spheres’ in ambient ISMmgren spheres’ in ambient ISM

Can conclude that Can conclude that nono DO white dwarf is physically DO white dwarf is physically associated with a PNassociated with a PN

NoNo sdB/sdOB (AGB-manqu sdB/sdOB (AGB-manquéé) star has an associated ) star has an associated ejecta nebula or ‘PN’ejecta nebula or ‘PN’

55

HH SB – radius relation SB – radius relationAll calibrators (All calibrators (nn = 114) = 114)

log S(H)= -3.42(±0.21)log R – 5.23(±0.16)

66

High-excitation PNe (High-excitation PNe (nn = 16) = 16)Close-binary PNe (Close-binary PNe (nn = 11) = 11)

HE PNe: squaresCE PNe: trianglesOthers: crosses

Incr

easi

ng

ma

ss

M

S(H

)½

‘Large high-excitation PNe’ (Kaler 1981)

• Round, elliptical, or amorphous (filled-centre) morphologies

• Large expansion velocities

• RT instabilities often seen

• Very high excitation: HeII 4686 ≥ 0.75 H and very weak or absent [O II], [N II] and [S II] emission

• CS is hot (Teff > 100 kK), and luminous relative to nebular flux

• Large scale height, |z| = 340 pc

• Low ionized masses ≤ 0.25 M

88

The post-common envelope PN The post-common envelope PN samplesample

23 close-binary PNe from De Marco 23 close-binary PNe from De Marco (2006, IAU (2006, IAU Symp. 234)Symp. 234)

Removed Abell 35, NGC 6302 and Sh 2-71Removed Abell 35, NGC 6302 and Sh 2-71 LoTr 5 and NGC 1514 are included, but have LoTr 5 and NGC 1514 are included, but have

unknown orbital periodsunknown orbital periods Also added NGC 1360 Also added NGC 1360 (Bond & Afsar 2005)(Bond & Afsar 2005)

Sample of 21 objectsSample of 21 objects Selected 11 PNe with reliable distances and Selected 11 PNe with reliable distances and

flux data, as calibrating objectsflux data, as calibrating objects

99

Sh 2-71 does not have a close binary Sh 2-71 does not have a close binary nucleus…nucleus…The true CS has been misidentified in the The true CS has been misidentified in the literatureliterature

The true CS (mB ≈ 19) is directly at centre (arrowed)

Credit: Adam Block / KPNO

1010

Calibrating post-common envelope PNe

PNPN Distance Distance (kpc)(kpc)

MethodMethod MassMass (M(M))

HFG 1 HFG 1 # 0.6 ± 0.30.6 ± 0.3 spectroscopic parallaxspectroscopic parallax 0.5:0.5:

NGC 1514NGC 1514 0.37 ± 0.100.37 ± 0.10 spect. parallaxspect. parallax 0.030.03

NGC 2346NGC 2346 0.9 ± 0.20.9 ± 0.2 spect. parallax, spect. parallax, extinctionextinction

0.060.06

LoTr 5LoTr 5 0.5 ± 0.20.5 ± 0.2 spect. par., Wilson-Bappu, spect. par., Wilson-Bappu, trig.trig.

0.130.13

SBS SBS 1150+599A1150+599A

18 ± 518 ± 5 gravity methodgravity method 0.170.17

SuWt 2SuWt 2 1.6 ± 0.41.6 ± 0.4 spect. parallaxspect. parallax 0.060.06

DS 1 DS 1 # 0.73 ± 0.070.73 ± 0.07 reflection effectreflection effect 0.260.26

BE UMa BE UMa # 2.0 ± 0.42.0 ± 0.4 reflection effectreflection effect 0.2:0.2:

Abell 46Abell 46 1.7 ± 0.61.7 ± 0.6 eclipsing binaryeclipsing binary 0.140.14

Abell 63Abell 63 2.4 ± 0.42.4 ± 0.4 eclipsing binaryeclipsing binary 0.080.08

NGC 1360 NGC 1360 # ** 0.38 ± 0.20.38 ± 0.2 Gravity, trig. parallaxGravity, trig. parallax 0.130.13# High excitation * Inferred close binary (Afsar & Bond 2005)

1111

Post-CE PNe: MorphologiesPost-CE PNe: Morphologies

‘Filled-centre’ ellipticalsBipolar and toroidal rings, …but no double-shell ellipticals

NGC 2346 PHR 1818-1526 NGC 1360 NGC 6578

NGC 5979Abell 65SuWt 2Shapley 1

DSS.

Credit: H. Bond / HST/ NASAAAO/UKST Survey

Credit: ESA/ESO/NASAAAO/UKST Survey

?

1212

Post-CE PNe: PropertiesPost-CE PNe: Properties

SB(HSB(H) = –2.5 to –6.0 erg cm) = –2.5 to –6.0 erg cm-2-2 s s-1-1 sr sr-1 -1 (+0.2 to –6.7) (+0.2 to –6.7)

Average ionized mass (Average ionized mass (post-CE PNepost-CE PNe) = 0.17 ± 0.13 ) = 0.17 ± 0.13 MM

Average ionized mass (Average ionized mass (post-CE PNe,post-CE PNe, excluding HFG excluding HFG 11) = 0.13 ± 0.08 ) = 0.13 ± 0.08 MM

Average ionized mass = 0.64 ± 0.5 Average ionized mass = 0.64 ± 0.5 MM ((non post-CE non post-CE local PNe, restricted range of SBlocal PNe, restricted range of SB))

Post-CE PNe have low ionized massesPost-CE PNe have low ionized masses. Extends . Extends conclusion of Bell et al. (1994) re Abell 63conclusion of Bell et al. (1994) re Abell 63

1313

Binarity of CSPN: Binarity of CSPN: optical/near-optical/near-IR colours (2MASS and/or DENIS)IR colours (2MASS and/or DENIS)

• ~53 PNe in solar neighbourhood (d ≤ 1.0 kpc)• ~7 wide binaries, e.g. Ciardullo et al. 1999 (6/6 with

2MASS data show excess at J, H and/or K)• ~7 close binaries (4 have periods; 5/6 in 2MASS show

excess at J, H and/or K)• 3 more CSPN have excess at J, H and/or K• 16 show no IR excess• 21 PNe have no observational data

Of the 32 PNe with optical/near IR colours,• total binary fraction ≈ 53% (agrees with Duquennoy &

Mayor)• total close-binary fraction ≈ 13 − 31%

1414

Selection bias?Selection bias?

2MASS photometry limit at J ≈ 16, K2MASS photometry limit at J ≈ 16, Kss ≈ 15 ≈ 15 Detection limit for CS companion is M0V – M8V, Detection limit for CS companion is M0V – M8V,

depending on luminosity of CSPNdepending on luminosity of CSPN Alternatively, CS may have brown dwarf or Alternatively, CS may have brown dwarf or cool WDcool WD

companion, or be a merger product ...companion, or be a merger product ...

… … but recall the but recall the Brown Dwarf DesertBrown Dwarf Desert (e.g. Marcy & (e.g. Marcy & Butler 2000, Armitage & Bonnell 2002, Grether & Lineweaver Butler 2000, Armitage & Bonnell 2002, Grether & Lineweaver 2006).2006).

Solar-type stars (i.e. PN progenitors) have an almost Solar-type stars (i.e. PN progenitors) have an almost total absence of brown dwarf companions within 5 total absence of brown dwarf companions within 5 AU !!AU !!

1515

Figure from Grether & Lineweaver (2006)Figure from Grether & Lineweaver (2006)

The Brown Dwarf Desert

1616

Conclusions & future work:Conclusions & future work:

Close binary (post-CE) PNe Close binary (post-CE) PNe have a distinct trend in SB-r have a distinct trend in SB-r spacespace, shared by optically-thin, low mass, high-excitation , shared by optically-thin, low mass, high-excitation PNe. PNe.

Post-CE PNe have low ionized masses and distinctive filled-Post-CE PNe have low ionized masses and distinctive filled-centre, bipolar or toroidal morphologies.centre, bipolar or toroidal morphologies.

Post-CE PNe Post-CE PNe comprise a minority of PNecomprise a minority of PNe. Should they be . Should they be called ‘true PNe’?called ‘true PNe’?

Need to continue search for close-binary nuclei via time-Need to continue search for close-binary nuclei via time-series photometry and RV monitoringseries photometry and RV monitoring

Need Need deepdeep BVRIJHKBVRIJHK photometry of photometry of all CSPNall CSPN in local in local volume-limited PN samplevolume-limited PN sample. Utilise UKIDSS, VHS data… . Utilise UKIDSS, VHS data… SPITZERSPITZER……

Single stars can do it !!Single stars can do it !!