Multiwavelength studies of Planetary Nebulae

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Multiwavelength studies of Planetary Nebulae
Martin Cohen University of California/Berkeley M
ASH Legacies Workshop 17 February 2009
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In collaboration with the following

• Quentin Parker, Warren Reid, Brent Miszalski,
  David Frew
• Anne Green, Tara Murphy, Ron Ekers
• Jessica Chapman, Indra Bains, Rachel Deacon
• Jim Caswell, Lister Staveley-Smith, Naomi
  McClure-Griffiths, Dick Manchester, Mark
  Calabretta
• Joss Bland-Hawthorn, Mark Wardle, Russell Cannon,
  Peter Tuthill
• Peter Wood, Mike Dopita, Miroslav Filipovic
• Vince Mcintyre, Sean Amy, Nathan Pope
• Bairbel Koribalski, Robert Braun
• The GLIMPSE Legacy Team (Ed Churchwell U
  Wisconsin)
• The SAGE Legacy Team (Margaret Meixner, Joe Hora)

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Outline

• Mid-IR emission in thermal radio regions, SST
  GLIMPSE Legacy, contaminants in PN search
• The search for PNe solely using MIR criteria
• MIR false-colours of PNe and excitation class
• The AT20G survey Planck calibrators and PNe
• The MIR/radio flux ratio evolution of PNe
• Two distinctly unique planetary nebulae
• Magellanic Cloud PNe IR PNLFs AGB halos
• 1100 PNe in the Galactic Bulge optical, MIR,
  radio study for PNLFS and halo

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GLIMPSE Benjamin et al. 2003 PASP, 115, 953
45"
1983
1996
2004
19"
1.7"
b1.1
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Thermal radio regions in the l312? field

• Matched-resolution (MOST) 843MHz (MSX) 8.3?m
  Galactic Plane images
• Radio - ionized gas MIR - PAHs in PDRs
• What is the relationship betweenMIR/radio?
• Field chosen for its diverse inventory of thermal
  and nonthermal regions 1?
• Cohen Green ratio F?(8.3?m)/S?(843MHz)
• Thermal radio emission median 255

Whiteoak, Cram, Large 1994, MNRAS, 269, 294 Cohen
Green 2001, MNRAS, 325, 531 Cohen et al. 2007,
MNRAS, 374, 979
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How are MIR and radio related?
Radio (black) ionized gas IR (white) hydrocarbon
molecules in the PDR
Mid-IR MSX 8.3?m
Far-IR emission from dust heated by the star
Radio MOST 843MHz
Radio
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MIR morphology of HII regions 4.5 5.8 8.0?m 234
Compact
Ultra-compact
Cometary
Compact
HII
Compact
Compact
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HII regions as contaminants for PNe
d H
H
H
dH
CHII central star deep silicate absorption
diffuse regions have different IR spectra.
Diffuse emission in IRAC must be absolutely
recalibrated for aperture correction issue.
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Planetary Nebulae MASH-I and GLIMPSE
PHR1457-5812
PM5 WN
PHR1246-6324
234
234
234
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Tools for matching MASH PNe PHR18570207
H?
3.6?m
5.8?m
H? greyscale image
4.5?m
8.0?m
234
Cohen et al. 2007 (ApJ, 669, 343) studied 54
MASH-I PNe in H?, radio MIR
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The value of IRAC false-colour images 21
MASH-I PNe stand out against their surroundings
by their IRAC false colours 3 are orange 8 are
red 10 are violet
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MIR false-colour a proxy for excitation class
(65486584 NII)/H?

• 26 MASH-I PNe show 3 distinct false colours
• 29 MASH-II PNe show the same false colours
• Combine both samples compare NII/H?
• 16 Orange PNe have 3.60.6
• 17 Red PNe have 2.00.4
• 13 Violet PNe have 1.00.4
• Control group of 49 ESO PNe in GLIMPSE

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Samples of the AT20G UCHII regions
1.Almost no MIR UC 2. PNe look nothing like
UCHII regions
From a blind search for sources of S20200 mJy
0.843-20GHz index 0.1 Murphy et al., 2008, in
prep. MIR/Radio 42
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PNe found among the AT20G HII regions
Serendipitous PNe with same criteria of radio
flux spectral index as our AT20G subset
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MIR/radio 8?m/843MHz ratio for PNe

• ? 18/33 ESO 122 Cohen Green 2001, MNRAS, 325,
  531
• ?18/58 MASH-I 3.61.4 Cohen et al. 2007, MNRAS,
  374, 979
• ? 15/29 MASH-II PNe 5.0 1.3 Cohen et al. 2009,
  in prep.
• 33/87 MASH-I/II 4.21.3
• 82/135 MASHESO 6.01.7
• PNe FOUND in AT20G survey of all ratios from 160
  (optically thick at 843Mz), ratios of 1-2 for
  PNe in Galactic Bulge Murphy et al. 2009, in
  prep.

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MIR/radio flux ratio evolution of PNe

• ESO12?MASH-I4.6 ? MASH-II GB2
• Typical MASH-I PN (203") is larger more
  evolved than typical ESO PN (125") x1.67
• As PN expands MOST beamPN diameter, radio flux
  unchanged FUV to sustain the PDR drops x1.672
  ?x2.8
• PAHs in PDRs emit 8?m so MIR/radio falls as
  fewer UV photons pump PAHs into IR fluorescence
  12/2.84.3
• HII regions MIR/radio (U)C, 42 diffuse, 25
• MASH-II PNe fainter than MASH-I PNe either much
  more compact (hard to see) or much larger (very
  faint)

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IRAC color-color plots for 135 PNe
dH
H
P
H
P
dH
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The third IRAC color-color plane
Query 49 million GLIMPSE point sources for
PNe Using all 6 IRAC colors (1-2,1-3,1-4,2-3,2-4,3
-4)
dH
H
P
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PNG313.300.3 Cohen et al. 2005, ApJ, 627, 446
Ionized FS hi-exc
PAHs or H2
CSPN
13cm
20cm
13cm
4.5?m
13cm
8.0?m
234
ATCA discovery, refound by Spitzer. Undetected
in optical and by 2MASS. In Scutum-Crux spiral
arm at 6.6 kpc, AV 36m. Central star detected
at 13, 20cm, 3.6, 4.5?m suggests a very hot
emission-line object. Might it be a young SNR?
Parkes hunt for pulsar
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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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A rare phase of PN evolution

• Phase of stellar evolution previously called
  OHPNE by Zijlstra et al. (1989)
• The faintest PN detected around a still pulsating
  AGB star
• 1500d period still pulsating regularly
• Faint almost circular ionized nebula
• Ha, NII and SII typical of PN
• With ATCA sought diffuse continuum across PN
• Found 2 strongly nonthermal synchrotron sources
• 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

, Zijlstra, te Lintel Hekkert, Pottasch, Caswell
, Ratag, Habing AA,217,157 Cohen, Parker,
Chapman 2005, MNRAS, 357, 1189 Cohen, Chapman,
Deacon, Sault, Parker, Green 2006, MNRAS, 369, 189
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ATCA continuum observations
Source A curves, concentric with PN
3cm
H? image 6cm contours
13cm
20cm
A and B have same spectral index within errors ?
-0.8 synchrotron
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LMC PNe Spitzer IR Luminosity Functions and AGB
Halos (Cohen, Hora, Parker Reid IAU Symp. 256,
UK)
Data bins 0.75mag dashed vertical lines -
completeness limits. Solid curves are scaled
universal functions with least squares cut-offs.
Too few PNe detected at 70µm to analyze its LF.
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Attributes of the IR PNLFs
Spitzer SAGE Legacy IR data and 2MASS enable
study of LMC PNe at 9 wavelengths from 1.2 to
70µm. Of the 700 PNe known largely from recent
discoveries by Reid Parker (2006) and observed
by SAGE, 523 are detected by 2MASS, IRAC/MIPS. We
display IR PNLFs in 8 bands. Compare with the
new OIII LF presented by Reid Parker at IAU
Symp. 256 based on 583 PNe.
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Objects exceeding cut-off mags
Our large PN sample (?700) reveals 12 different
objects past the cut-offs of which only 7 exceed
the cut-off magnitude in more than one band.
Table 2 lists these candidates and gives their
bolometric luminosities assessed from 1.2 to 24
or 70µm. Only two survive as true PNe after
removing objects contaminated by nearby stars or
found to be late-type, symbiotic Mira, or
post-AGB stars, or VLE nebulae. Further study of
these two PNe continues.
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SAGE detects AGB halo in the LMC

SMP27 PN RP105 and its large
optical and IR halo
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Well-defined MIR colours of LMC PNe
RP Reid-Parker
L Leisy
Search SAGE database for PN-coloured point sources
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With grateful thanks to Quentin for making it
possible for me to attend this workshop
My participation in non-conference MASH
activities over the years was enabled by NASA
through LTSA grant NAG5-7936 and ADP grants
NNG04GD43G and NNX08AJ29G.