This document discusses insights into the morphology of planetary nebulae from 3D spectroscopy. It summarizes that planetary nebulae are expanding shells of material ejected from aging stars. Integral field spectroscopy is used to create spatially-resolved intensity, velocity, and chemical maps of planetary nebulae, revealing structures like toroidal shells and bipolar outflows. Examinations of nebulae like Th 2-A, M 2-42, and M 3-30 show complex non-spherical structures rather than simple round shells. Orientations of nebulae are also studied to understand formation mechanisms related to binary interactions or stellar magnetic fields.

1. In collaborations with: Quentin A. Parker (Macquarie/Hong Kong/AAO), Wolfgang Steffen (UNAM Mexico)
Insights to the Morphology of
Planetary Nebulae
from 3D Spectroscopy
Ashkbiz Danehkar
Harvard-Smithsonian Center for Astrophysics
ashkbiz.danehkar@cfa.harvard.edu

2. 20 November 2015 CfA Postdoc Symposium 2
Planetary Nebulae (PNe)
● Expanding shells of H-rich material ejected by AGB star
– Shell: Vexp ~ 10-40 km/s
– Density: Ne ~ 10- 105
cm-3
● Central stars left the AGB phase
– Progintor Mass: 1 M☉ < Minit < 8 M☉
– Current Stellar Mass: 0.5-0.9 M☉
● AGB star transited to PN phase
● UV radiations from stars ionize the shells
Herwig 2005
NGC 6543

3. 20 November 2015 CfA Postdoc Symposium 3
Morphology of Planetary Nebula

4. 20 November 2015 CfA Postdoc Symposium 4
Morphology of Planetary Nebula
●
Round (R) 22% of Galactic PNe
●
Elliptical (E) 49%
●
Bipolar/multi-polar/ring (B) 20%
●
point-symmetric 10%
Balick et al. 1987,AJ,94,1641
Low-Ionization Structures (LISs)
Fast, Low-Ionization Emission Regions (FLIERs)
– Velocity 50-200 km/s relative to the central star
– Density lower than the main shell

5. 20 November 2015 CfA Postdoc Symposium 5
Morphology of Planetary Nebula
● Rotating Stellar Winds + Strong Magnetic Fields
– Garcıa-Segura 1997; Garcıa-Segura&Lopez 2000; Frank&Blackman 2004
– single star may not supply enough angular momentum (Soker 2006)
● Binary System
– a. Direct Envelope Ejection (equatorial shell)
– b. Dynamo Driven Ejection (collimated outflows)
– c. Disk Driven Ejection (elliptical shell+ collimated outflows)
● At least 30% of bipolar PNe contain post-CE binaries (Miszalski et al. 2009)
● alignments between nebular shells and binary orbital inclinations
(e.g. Mitchell et al. 2007; Jones et al. 2010, 2012; Tyndall et al. 2012; Huckvale et al. 2013)
Balick et al. 1987,AJ,94,1641

6. 20 November 2015 CfA Postdoc Symposium 6
Morphology of Planetary Nebula
R
R
E
B
B
R
B
E
B
R
B
E
B
B
E
?
?
E
?
B
E
B
E
E
E
?
R

7. 20 November 2015 CfA Postdoc Symposium 7
Integral Field Spectroscopy
● Wide Field Spectrograph (WiFeS; Dopita 2007,2010)
– Image-Slicing Integral Field Unit (IFU)
– ANU 2.3-m Telescope, Siding Spring Observatory
– Field-of-view: 25” x 38”, spatial resolution: 1”
– spectral resolution: R ~ 7000 (~ 20 km/s)

8. 20 November 2015 CfA Postdoc Symposium 8
Integral Field Spectroscopy
ANU 2.3 WiFeS
Gemini 8.1 GMOS
● Wide Field Spectrograph (WiFeS; Dopita 2007,2010)
– Image-Slicing Integral Field Unit (IFU)
– ANU 2.3-m Telescope, Siding Spring Observatory
– Field-of-view: 25” x 38”, spatial resolution: 1”
– spectral resolution: R ~ 7000 (~ 20 km/s)

9. 20 November 2015 CfA Postdoc Symposium 9
Spatially-resolved Observations of PNe
● Spatial-resolved intensity and kinematic maps
● PN Th 2-A
– not round spherical morphology anymore!
– Torus with bipolar outflows
– i = −10° ± 5° (relative to the line of sight)
– Shell: ~ 40 ± 10 km/s
– Outflows: 70-110 km/s
Danehkar, ApJ, 2015, in press
HST F555W
Hα (Gornry et al 1999)
● Transition

10. 20 November 2015 CfA Postdoc Symposium 10
Spatially-resolved Observations of PNe
● Velocity-resolved channel maps
Danehkar, ApJ, 2015, in press
● PN Th 2-A
– not round spherical anymore! But, toroidal shell with collimated bipolar outflows

11. 20 November 2015 CfA Postdoc Symposium 11
Spatially-resolved Observations of PNe
● Spatially-resolved chemical ionic maps
● PN Th 2-A
Danehkar, PhD thesis, 2014

12. 20 November 2015 CfA Postdoc Symposium 12
Spatially-resolved Observations of PNe
● Velocity-resolved channel maps
● PN M 2-42
Bipolar Jets (Akras & Lopez,2012)
Asymmetric bipolar Jets & FLIERs
(Danehkar et al,2015, AJ, submitted)
Hα (Parker et al 2005)

13. 20 November 2015 CfA Postdoc Symposium 13
Spatially-resolved Observations of PNe
Danehkar et al, in preparation
● Spatially-resolved intensity and kinematic maps
● PN M 3-30
– Inclination i ~ 30° ± 5° (relative to the line of sight)
– Shell: ~ 30 ± 10 km/s
– Outflows: 50-70 km/s
Hα +[N II] (Schwarz et al. 1992)

14. 20 November 2015 CfA Postdoc Symposium 14
Spatially-resolved Observations of PNe
Danehkar & Parker, 2015, MNRAS, 449, L45
● Spatial orientations of compact objects
● Hen 3-1333 and Hen 2-113
– Compact objects ~3.5 arcsec
– Outer faint lobes (diameter 10 arcsec)
– Position Angles (PA)
PA = -15° (Hen3-1333), 65° (Hen 2-113)
in agreement with Chesneau et al 2006 and
Lagadec et al 2006
Hα +[N II] (Schwarz et al. 1992)

15. 20 November 2015 CfA Postdoc Symposium 15
Spatially-resolved Observations of PNe
Danehkar, PhD Thesis, 2014
● Spatial orientations of a large number of Galactic PNe
HST images
● NGC 6578
● NGC 6567
● NGC 6629

16. 20 November 2015 CfA Postdoc Symposium 16
Spatially-resolved Observations of PNe
● Spatial orientations of Galactic PNe toward Galactic Center
● Rees & Zijlstra,2013,MNRAS,435,975
– Hα HST images of 130 PNe
– Weak alignment with the Galactic Plane
Danehkar & Parker, 2015, IAU Symposium 312Rees & Zijlstra,2013,MNRAS,435,975

17. 20 November 2015 CfA Postdoc Symposium 17
Conclusions
● PN: Expanding H-rich material ejected by AGB star
● PN Typical Morphology: Elliptical and Bipolar
– Rotating Stellar Winds + Strong Magnetic Fields?
– Binary Systems?
– FLIERs: point-symmetric jets
● IFU Spectroscopy
– Intensity and Velocity maps
– Velocity channel maps
– Physical and chemical maps
● Spatially-resolved Kinematic Observations with WiFeS
– Pros: simple data analysis, more information than long-slit observation (PV diagram)
– Pros: good for large sample, overall image of the whole nebula
– Cons: Low kinematic resolution (20 km/s) & spatial resolution (1 arcsec), small details
– Cons: complicated data reduction, complex data extraction

18. 20 November 2015 CfA Postdoc Symposium 18
Thank you for your attention!Thank you for your attention!
●
Questions are welcome!Questions are welcome!