Galactic Indigestion - physics.usyd.edu.auvmoss/resources_files/VMossFermiBubbles… · Fermi...
Transcript of Galactic Indigestion - physics.usyd.edu.auvmoss/resources_files/VMossFermiBubbles… · Fermi...
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Galactic Indigestion“Giant Gamma-ray Bubbles "om Fermi-LAT: Active Galactic Nucleus
Activity or Bipolar Galactic Wind?”
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Structure
Fermi bubbles in a nutshell
Three interesting questions dealt with in this paper:
1) “How do you really know when you are seeing a signal?”
2) “How can such large bubbles be explained physically?”
3) “What questions might the Fermi bubble help to answer?”
Summary of thoughts about the paper itself
Conclusion
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Fermi bubbles in a nutshell
New data: higher resolution, sensitivity using Fermi-LAT
Data reduction: model subtraction to prove the bubble structure
Spectral fitting: flat spectrum, flat intensity, sharp edges
Origin of the bubbles/CRs: where did they come from?
Implications: what does the existence of the bubbles suggest?
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Brought to you by...
Meng SuGraduate student
- diffuse gamma-ray emission- cosmic microwave background
Tracy SlatyerGraduate student
- dark matter theory- dark matter detection
Douglas FinkbeinerAssociate Professor
- CMB dust map- WMAP haze
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Brought to you by...
Meng SuGraduate student
- diffuse gamma-ray emission- cosmic microwave background
Tracy SlatyerGraduate student
- dark matter theory- dark matter detection
Douglas FinkbeinerAssociate Professor
- CMB dust map- WMAP haze
Gregory DoblerPostdoc
- dark matter theory- gravitational lensing
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Timeline
2004 - “WMAP haze”Haze of microwave
emission found around the centre of the Galaxy (Finkbeiner et al, 2004)
2009 - “Fermi haze”Matching haze of Fermi
emission somewhat asserted to be dark matter annihilation
(Dobler et al, 2010)
2010 - “Fermi bubbles”Haze of microwave
emission found around the centre of the Galaxy
(Su et al, 2010)
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“How do you really know when you are seeing a
signal?”
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Note: 1.6 year Fermi-LAT maps, vs. first release of 1 year data
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Model subtraction
1: Fermi diffuse Galactic model (Fig. 2)
2: Dust-map/disk template model (Fig. 3)
3: Low-energy Fermi subtraction (Fig. 6)
Models show very faint signals from the raw data - with bubbles in all results
These different methods were to prove that the bubbles are real, not artifacts of a chosen data reduction technique
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Spectral properties of the bubbles
Similar to model subtraction
Splitting into components to compare their spectra (Fig. 15)
Same: if related, different: if not
Challenging to create same intensity - not a shell? (Fig. 10)
Explaining uniform intensity - magnetic reconnection?
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“How can such large bubbles be explained
physically?”
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The Galactic centre
We know the GC is a highlyactive region, with much starformation and interactions
Sagittarius A*
Massive black hole (MBH)
High velocity stars (HVSs)
Other suspects
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Origin of the bubbles
Age: 107/(v/103 km s-1) yr, where v < 103 km s-1 = > 10 Myr
Past GC activity: X-ray nebulae,diffuse X-rays, OB stellar disk
MBH accretion - not jet-shaped?
Nuclear starburst - more SNRs?
“Some large episode of energyejection in the GC...”
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Origin of the CRs
Key difficulty: generating CRsof the same energy/intensity upto 10 kpc off the plane (Fig. 28)
Are they generated:
1) In the GC?
2) Inside the bubbles?
3) In the rim of the bubbles?
Dark matter annihilation?
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“What questions might the Fermi bubbles help to
answer?”
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Gamma-ray background
Origin of gamma ray background?(blue background in the image)
The extragalactic gamma-ray BG is thought to originate from outflow
Local evidence for such outflows?
This could lead to energetic CRs thatescape galaxies to be detected as the cosmic gamma-ray background
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Hypervelocity stars
Ejection of high velocity stars - withspeeds of 60-100 km/s faster thanallowed by Galactic rotation
These are thought to originate from the MBH in the GC, in relation to accretion events and interaction
May be ejected periodically
Are the Fermi bubbles linked to their ejection?
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Future of the bubbles
Will there be fragmentation ofthe Fermi bubbles as they age?
Timescale of fragmentation andre-ejection of matter
If so, this ejection could reachthe Galactic halo
Blowout (ala supershell)?
Feedback mechanism
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Missing baryons/HVCs
Suggestion of hot gas feedback into the Galactic halo
Missing baryons
Contributing to the origin of HVCs?
It is possible that we might find tracers of past bubbles in HVCs
May provide a timescale for bubbleformation, if HVCs are linked
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Metallicity
Ejection of gas into IGM - if it ischanneled in the Galactic wind
Metal-rich vs. metal-poor outflow
Metals in the IGM thought to be an indicator of metal-rich outflow
May also help explain the value of metallicity detected in the IGM
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Comments on the paper
Thorough - it is clear that a lot of thought about possible origins of the bubbles went into it, with various scenarios presented
Indecisive - it is not very clear which of the various scenarios the authors believe is the most likely (but they don’t know yet)
Figures - it is good that there are a lot, but it seems that more thought could have gone into condensing the results, or in culling uninteresting plots for the sake of clarity (Fig. 5, 22)
Context - they put their work in context of different fields, which adds a lot to the overall impact of the paper
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Conclusions
Bubble structures present up to 50º off the plane
Coincident with WMAP haze and soft ROSAT X-rays
Origin as a large episode of energy injection associated with GC
Dark matter annihilation: possibly an efficient means of CR injection at high latitudes, but not all evidence supports this
Future data from eROSITA/Planck will better resolve structures
Need clear physical understanding of bubbles
Fermi bubbles vs. pogo ball from TotallyLooksLike.com