from hazes to bubbles: putting it all together... Greg Dobler - - PowerPoint PPT Presentation

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from hazes to bubbles: putting it all together... Greg Dobler - - PowerPoint PPT Presentation

Mar 03, 2023 168 likes •892 views

Greg Dobler (KITP/UCSB) from hazes to bubbles: putting it all together... Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz Greg Dobler (KITP/UCSB) microwaves... CMB WMAP 23 GHz Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz Greg Dobler

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Greg Dobler (KITP/UCSB)

from hazes to bubbles:

putting it all together...

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Greg Dobler (KITP/UCSB)

microwaves... WMAP 23 GHz

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Greg Dobler (KITP/UCSB)

WMAP 23 GHz CMB microwaves...

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Greg Dobler (KITP/UCSB)

WMAP 23 GHz microwaves...

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Greg Dobler (KITP/UCSB)

dust (spinning and thermal)

WMAP 23 GHz microwaves...

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WMAP 23 GHz

Greg Dobler (KITP/UCSB)

free-free

microwaves...

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WMAP 23 GHz

Greg Dobler (KITP/UCSB)

synchrotron

microwaves...

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Greg Dobler (KITP/UCSB)

microwaves...

Haslam et al. (1982) Hα (Finkbeiner, 2003) Schlegel et al. (1998) WMAP 23 GHz

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WMAP 23 GHz

Greg Dobler (KITP/UCSB)

dust (spinning and thermal Tν∝ν1.7)

microwaves...

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Greg Dobler (KITP/UCSB)

Finkbeiner, Davis, & Schlegel (1999)

dust (spinning and thermal Tν∝ν1.7)

microwaves...

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WMAP 23 GHz

Greg Dobler (KITP/UCSB)

free-free Tν∝ν-2.15

microwaves...

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Greg Dobler (KITP/UCSB)

Finkbeiner (2003)

Tν∝ν-2.15 free-free

microwaves...

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WMAP 23 GHz

Greg Dobler (KITP/UCSB)

synchrotron Tν∝ν-3.0

microwaves...

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Greg Dobler (KITP/UCSB)

synchrotron Tν∝ν-3.0

Haslam et al. (1982)

microwaves...

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WMAP 23 GHz

Greg Dobler (KITP/UCSB)

synchrotron Tν∝ν-3.0 free-free Tν∝ν-2.15 dust (spinning and thermal Tν∝ν1.7)

microwaves...

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

synchrotron Tν∝ν-3.0 free-free Tν∝ν-2.15 dust (spinning and thermal Tν∝ν1.7)

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

synchrotron Tν∝ν-3.0 free-free Tν∝ν-2.15 dust (spinning and thermal Tν∝ν1.7)

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

free-free Tν∝ν-2.15

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

free-free Tν∝ν-2.15

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

dust (spinning and thermal) Tν∝ν1.7

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

dust (spinning and thermal) Tν∝ν1.7

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

synchrotron Tν∝ν-3.0

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

synchrotron Tν∝ν-3.0

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

microwave “haze”

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

“full sky fit” microwave haze

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Greg Dobler (KITP/UCSB)

= + +

WMAP 23 GHz

“regional fit” microwave haze

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Greg Dobler (KITP/UCSB)

WMAP 23 GHz

microwave haze

what is it? (we’ll get to that) but first, what makes it unique? . diffuse and extended (~ 5 kpc x 12 kpc) . spectrum

Dobler (2012a)

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Greg Dobler (KITP/UCSB)

WMAP 23 GHz

microwave haze

what is it? (we’ll get to that) but first, what makes it unique? . diffuse and extended (~ 5 kpc x 12 kpc) . spectrum

Dobler (2012a)

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Greg Dobler (KITP/UCSB)

what is it? (we’ll get to that) but first, what makes it unique? . diffuse and extended (~ 5 kpc x 12 kpc) . spectrum consistent with synchrotron from a very hard electron population:

dN/dE ∝ E-2.0

Dobler (2012a) Dobler & Finkbeiner (2008)

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Greg Dobler (KITP/UCSB)

gamma-rays...

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

Dobler et al. (2010)

gamma-rays...

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

Dobler et al. (2010)

gamma-rays...

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visible even with no templates, no fitting, no subtraction, etc...

Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

Dobler et al. (2010)

gamma-rays...

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Greg Dobler (KITP/UCSB)

gamma-rays from the Galaxy

Fermi 2-5 GeV

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

π0 decay

gamma-rays from the Galaxy

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

π0 decay inverse Compton plus bremsstrahlung (subdominant)

gamma-rays from the Galaxy

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

π0 decay inverse Compton plus bremsstrahlung (subdominant) extragalactic plus particle contamination

gamma-rays from the Galaxy

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Greg Dobler (KITP/UCSB)

π0 decay

Fermi 2-5 GeV

gamma-rays from the Galaxy

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Greg Dobler (KITP/UCSB)

morphological tracers of emission

π0 decay Schlegel, Finkbeiner, & Davis (1998)

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Greg Dobler (KITP/UCSB)

SFD (100 μm) Fermi 2-5 GeV

Dobler et al. (2010)

morphological tracers of emission

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Greg Dobler (KITP/UCSB)

SFD (100 μm) Fermi 2-5 GeV

Dobler et al. (2010)

morphological tracers of emission

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

morphological tracers of emission

Dobler et al. (2010)

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Greg Dobler (KITP/UCSB)

Fermi 2-5 GeV

Fermi collab. (2012)

morphological tracers of emission

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Greg Dobler (KITP/UCSB)

Fermi data 2-5 GeV diffuse model 2-5 GeV Fermi “haze/bubbles”

Dobler et al. (2010)

Fermi “haze”

...and later the “Fermi bubbles”

(Su et al., 2010)

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Greg Dobler (KITP/UCSB)

Dobler et al. (2010)

the Fermi Haze a.k.a. Fermi Bubbles

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Greg Dobler (KITP/UCSB)

Dobler et al. (2010)

the Fermi Haze a.k.a. Fermi Bubbles

roughly “flat” brightness profile

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Greg Dobler (KITP/UCSB)

the Fermi Haze a.k.a. Fermi Bubbles

roughly “flat” brightness profile

Su et al. (2010)

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the Fermi haze/bubbles

Greg Dobler (KITP/UCSB)

Fermi data 2-5 GeV diffuse model 2-5 GeV Fermi “haze/bubbles”

Dobler et al. (2010)

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Greg Dobler (KITP/UCSB)

electron spectra

. the same spectrum (normalization and slope) reproduces the microwave and gamma-ray emission . the characteristic energy of the emitting electrons for microwaves is Ee~10 GeV but for gammas is Ee~1 TeV . this implies very little cooling of the cosmic-ray population

–2.0

dN/dE ∝ E

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Greg Dobler (KITP/UCSB)

= + + 23 GHz haze

Dobler (2012)

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Greg Dobler (KITP/UCSB)

= + + 23 GHz haze

Dobler (2012) WMAP “drops” here (b~-35o) Fermi “cuts off” here (b~-50o)

are they the same structure? are the Fermi edges “real”?

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Greg Dobler (KITP/UCSB)

Dobler (2012b)

are they the same structure? are the Fermi edges “real”?

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Greg Dobler (KITP/UCSB)

coincident “edge”?

Dobler (2012b)

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Greg Dobler (KITP/UCSB)

coincident “edge”? YES!

independent confirmation that the Fermi Haze/Bubbles edges are real demonstrates conclusively that the microwave and gamma-ray haze/bubbles are the same structure observed at multiple wavelengths strongly suggests an inverse Compton origin for the gamma- ray emission and that the microwave emission represents a separate component of diffuse synchrotron Dobler (2012b)

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Greg Dobler (KITP/UCSB)

Planck

The Galactic haze/bubbles is shown here in PLANCK data from 30-44 GHz A multi-wavelength composite image showing both microwaves and gamma-rays: PLANCK 30 GHz (red), 44 GHz (green), and Fermi 2-5 GeV (blue). The same structure at 2-5 GeV as seen by the Fermi Gamma-Ray Space Telescope

Planck Collaboration, 2012

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483

. divide sky into 10 regions

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483

. divide sky into 10 regions . five template fit to the data on each region independently . “stitch” together to form a full sky model and residual map

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483

. divide sky into 10 regions . five template fit to the data on each region independently . “stitch” together to form a full sky model and residual map . apply multi-template, multi-region fit to each Planck and WMAP band

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483

. divide sky into 10 regions . five template fit to the data on each region independently . “stitch” together to form a full sky model and residual map . apply multi-template, multi-region fit to each Planck and WMAP band

2.5

ν scaling yields roughly constant brightness with frequency

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483 Bayesian/Gibbs haze residual

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483

Planck wavelength coverage allows us to measure the spectrum of the haze/bubbles residual to high precision from ~20-61 GHz and with little systematic bias:

–2.55

TH ∝ ν

  • r

dN –2.1 ––– ∝ E dE

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Greg Dobler (KITP/UCSB)

Planck

Planck Collaboration, 2012, arXiv:1208.5483

excellent spatial agreement between the low latitude “edges” in microwaves and gamma-rays high latitude “edge” (spatially coincident with the gamma-ray edge) detected in Planck 30 GHz as well

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Greg Dobler (KITP/UCSB)

Dobler (2012b)

measuring B-fields in radio bubbles

since synchrotron emissivity depends

  • n the magnetic field strength B and

the electron spectrum ne, while the inverse Compton intensity is a function of the interstellar radiation field R and the electron spectrum ne, we can derive an estimate of B ~ 5 µG. emissivity = jν(B, ne) intensity = Iγ(R, ne)

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Greg Dobler (KITP/UCSB)

Dobler (2012a)

polarization

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what is it???

Greg Dobler (KITP/UCSB)

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this structure is very odd! 1.) sharp edges plus flat profile 2.) “flat” spectrum 1.) seems to imply a very contrived electron distribution since constant volume emissivity gives limb-darkened profiles and shell emissivity gives limb brightened profiles. 2.) seems to imply injection of electrons at ~TeV with a very hard spectrum the contenders:

  • wind (e.g., Crocker & Aharonian 2011): time scales too long, no Hα, violates 1.)
  • starburst: no Hα, likely violates 1.) and 2.)
  • AGN (e.g., Guo & Matthews 2011): violates 1.)
  • 2nd order Fermi acc. (e.g., Mertsch & Sarkar 2011): violates 1.), synchrotron?
  • DM annihilation (e.g., Dobler, Cholis, & Weiner 2011): violates 1.)

Greg Dobler (KITP/UCSB)

what is it???

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this structure is very odd! 1.) sharp edges plus flat profile 2.) “flat” spectrum 1.) seems to imply a very contrived electron distribution since constant volume emissivity gives limb-darkened profiles and shell emissivity gives limb brightened profiles. 2.) seems to imply injection of electrons at ~TeV with a very hard spectrum

Greg Dobler (KITP/UCSB)

what is it???

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this structure is very odd! 1.) sharp edges plus flat profile 2.) “flat” spectrum 1.) seems to imply a very contrived electron distribution since constant volume emissivity gives limb-darkened profiles and shell emissivity gives limb brightened profiles. 2.) seems to imply injection of electrons at ~TeV with a very hard spectrum the contenders:

  • wind (e.g., Crocker & Aharonian 2011): time scales too long, no Hα, violates 1.)
  • starburst: no Hα, likely violates 1.) and 2.)
  • AGN (e.g., Guo & Matthews 2011): violates 1.)
  • 2nd order Fermi acc. (e.g., Mertsch & Sarkar 2011): violates 1.), synchrotron?
  • DM annihilation (e.g., Dobler, Cholis, & Weiner 2011): violates 1.)

Greg Dobler (KITP/UCSB)

what is it???

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many puzzles... but may opportunities!

Greg Dobler (KITP/UCSB)

  • where (and how) are cosmic-rays accelerated in jets?

. jet itself? if so, then what about cooling times? . shock front? where are the microwaves? . what about limb brightening? 10 years of Fermi and/or CTA may provide answers

  • why is the brightness profile so flat?

. neither constant volume nor shell emissivity fit the data . why is the “stem” as bright or brighter than the rest of the bubble?

  • what is nature of the magnetic field in jet-blown bubbles?

. no polarized signal with WMAP (but one isn’t likely given the noise) . future polarization data may constrain magnetic turbulence in jets

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