Serendipitous XMMNewton Survey of Planetary Nebulae

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Serendipitous XMM-Newton Survey of Planetary
Nebulae
Rodolfo Montez Jr.
and
Joel H. Kastner
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Outline

• X-rays from PNe (brief overview)
• Serendipitous Survey Details
• Some Survey Results

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A Brief Overview of X-rays from PNe
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X-rays from PNe
All Methods of PNe Formation Predicted Gas
Shocked to X-ray Emitting Temperatures (ISW,
CFW, Jets) High Resolution X-ray Missions
Definitively Resolved These Sources (BD30, NGC
7027, etc.)
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X-rays from PNe
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X-rays from PNe
As observations caught-up to theory, we uncovered
discrepancies. (Low TX, Many Non-Detections) As
these trends emerged, the theory quickly evolved
in an attempt to resolve the discrepancies. (IJW,
Thermal Conduction, Slower Post-AGB Winds)
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X-rays from PNe
With so few sources to test the theories, new
sources are a valuable commodity. Hence, our
search for serendipitously observed PNe in the
vast XMM-Newton data archive.
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Serendipitous Survey Details
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Survey Details

• EPIC detectors (pn, MOS1, MOS2)
• Sensitive from 0.2 to 12.0 keV
• Imaging Spectrometry
• Large Field of View (d 30 arcmin)
• Observing for nine years!

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Survey Details

• GSFC/SAO HEASARC
• Reprocess Data Files
• Generate Filtered Images
• Define Extraction Regions
• Extract Spectrum
• Merge Event Lists

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Some Survey Results
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PN H 1-36
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PN H 1-36
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PN H 1-36
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PN H 1-36
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PN H 1-36
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H 1-36 is a D-type symbiotic system with a
high-excitation emission-line spectrum. Angeloni
et al. 2007 analyzed available data across a
broad range of the EM spectrum and found the data
is consistent with a colliding-wind
scenario. They suggest H 1-36 is a promising
X-ray target with possible jets and predict
bremsstrahlung emission from a high-velocity
component (Vs 500 km/s) with TX 3.6 x 106 K.
PN H 1-36
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PN H 1-36
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PN H 1-36

• Noisy Spectral Data Warrants Caution
• Relatively low off-axis angle suggests the
  extension is real.
• A Chandra high-resolution, on-axis observation
  should resolve the issue.

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PN H 1-36

• Noisy Spectral Data Warrants Caution
• Relatively low off-axis angle suggests the
  extension is real.
• A Chandra high-resolution, on-axis observation
  should resolve the issue.

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Hb 5 is Type I (He- and N-rich) bipolar PN with a
high-excitation emission-line spectrum. Corradi
Schwarz (1993) find a polar expansion velocity
of 250 km/s, while Pishmish et al. 2000 report
a faster, possibly collimated, wind of 400
km/s. The observed X-ray emission corresponds to
some of the brightest regions seen in the HST
WFPC2 F658N (H? NII) narrowband image.
PN HB 5
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PN HB 5
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• The spectrum is indicative of a thermal plasma
  between 2.4 and 3.4 MK with strong Neon emission.
• We find
• a Neon overabundance of 1.8-6.9 (90 confidence
  interval) relative to the solar values of Anders
  Grevesse (1989)
• FX 1.2 x 10-13 ergs/s/cm2 (unabs)
• LX 1.5 x 1032 (D/3.2 kpc)2 ergs/s

PN HB 5
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We calculate upper limit fluxes from the 3? count
rate (as determined from the count rate of a
suitable background region scaled to the proper
expected source region), a few temperatures
plugged into collisional plasma models, and
absorption values taken from the literature.
We expect most of the PNe (20-25) in our survey
will result in LX upper limits in the range 1029
- 1034 ergs/s. These upper limits will hopefully
enhance our understanding of the X-ray emission
and, in turn, the shaping of PNe.
PN VD 1-8
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References