from hazes to bubbles
play

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

Mar 03, 2023 •168 likes •888 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

  1. Greg Dobler (KITP/UCSB) from hazes to bubbles: putting it all together...

  2. Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz

  3. Greg Dobler (KITP/UCSB) microwaves... CMB WMAP 23 GHz

  4. Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz

  5. Greg Dobler (KITP/UCSB) microwaves... dust (spinning and thermal) WMAP 23 GHz

  6. Greg Dobler (KITP/UCSB) microwaves... free-free WMAP 23 GHz

  7. Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz synchrotron

  8. Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz Haslam et al. (1982) Schlegel et al. (1998) H α (Finkbeiner, 2003)

  9. Greg Dobler (KITP/UCSB) microwaves... dust (spinning and thermal T ν ∝ ν 1.7 ) WMAP 23 GHz

  10. Greg Dobler (KITP/UCSB) microwaves... dust (spinning and thermal T ν ∝ ν 1.7 ) Finkbeiner, Davis, & Schlegel (1999)

  11. Greg Dobler (KITP/UCSB) microwaves... free-free T ν ∝ ν -2.15 WMAP 23 GHz

  12. Greg Dobler (KITP/UCSB) microwaves... free-free T ν ∝ ν -2.15 Finkbeiner (2003)

  13. Greg Dobler (KITP/UCSB) microwaves... WMAP 23 GHz synchrotron T ν ∝ ν -3.0

  14. Greg Dobler (KITP/UCSB) microwaves... synchrotron T ν ∝ ν -3.0 Haslam et al. (1982)

  15. Greg Dobler (KITP/UCSB) microwaves... dust (spinning and thermal T ν ∝ ν 1.7 ) free-free T ν ∝ ν -2.15 WMAP 23 GHz synchrotron T ν ∝ ν -3.0

  16. Greg Dobler (KITP/UCSB) = + + dust (spinning and thermal T ν ∝ ν 1.7 ) free-free T ν ∝ ν -2.15 WMAP 23 GHz synchrotron T ν ∝ ν -3.0

  17. Greg Dobler (KITP/UCSB) = + + dust (spinning and thermal T ν ∝ ν 1.7 ) free-free T ν ∝ ν -2.15 WMAP 23 GHz synchrotron T ν ∝ ν -3.0

  18. Greg Dobler (KITP/UCSB) = + + free-free T ν ∝ ν -2.15 WMAP 23 GHz

  19. Greg Dobler (KITP/UCSB) = + + free-free T ν ∝ ν -2.15 WMAP 23 GHz

  20. Greg Dobler (KITP/UCSB) = + + dust (spinning and thermal) T ν ∝ ν 1.7 WMAP 23 GHz

  21. Greg Dobler (KITP/UCSB) = + + dust (spinning and thermal) T ν ∝ ν 1.7 WMAP 23 GHz

  22. Greg Dobler (KITP/UCSB) = + + WMAP 23 GHz synchrotron T ν ∝ ν -3.0

  23. Greg Dobler (KITP/UCSB) = + + WMAP 23 GHz synchrotron T ν ∝ ν -3.0

  24. Greg Dobler (KITP/UCSB) = + + WMAP 23 GHz

  25. Greg Dobler (KITP/UCSB) = + + microwave “haze” WMAP 23 GHz

  26. Greg Dobler (KITP/UCSB) = + + microwave haze “full sky fit” WMAP 23 GHz

  27. Greg Dobler (KITP/UCSB) = + + microwave haze “regional fit” WMAP 23 GHz

  28. 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 microwave haze WMAP 23 GHz Dobler (2012a)

  29. 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 microwave haze WMAP 23 GHz Dobler (2012a)

  30. 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 Dobler (2012a) Dobler & Finkbeiner (2008) consistent with synchrotron from a very hard electron population: dN/dE ∝ E -2.0

  31. Greg Dobler (KITP/UCSB) gamma-rays...

  32. Greg Dobler (KITP/UCSB) gamma-rays... Dobler et al. (2010) Fermi 2-5 GeV

  33. Greg Dobler (KITP/UCSB) gamma-rays... Dobler et al. (2010) Fermi 2-5 GeV

  34. Greg Dobler (KITP/UCSB) gamma-rays... Dobler et al. (2010) Fermi 2-5 GeV visible even with no templates, no fitting, no subtraction, etc...

  35. Greg Dobler (KITP/UCSB) gamma-rays from the Galaxy Fermi 2 - 5 GeV

  36. Greg Dobler (KITP/UCSB) gamma-rays from the Galaxy Fermi 2 - 5 GeV π 0 decay

  37. Greg Dobler (KITP/UCSB) gamma-rays from the Galaxy Fermi 2 - 5 GeV inverse Compton plus bremsstrahlung (subdominant) π 0 decay

  38. Greg Dobler (KITP/UCSB) gamma-rays from the Galaxy Fermi 2 - 5 GeV inverse Compton plus bremsstrahlung (subdominant) extragalactic plus particle contamination π 0 decay

  39. Greg Dobler (KITP/UCSB) gamma-rays from the Galaxy Fermi 2 - 5 GeV π 0 decay

  40. Greg Dobler (KITP/UCSB) morphological tracers of emission Schlegel, Finkbeiner, & Davis (1998) π 0 decay

  41. Greg Dobler (KITP/UCSB) morphological tracers of emission Fermi 2 - 5 GeV SFD ( 100 μ m) Dobler et al. (2010)

  42. Greg Dobler (KITP/UCSB) morphological tracers of emission Fermi 2 - 5 GeV SFD ( 100 μ m) Dobler et al. (2010)

  43. Greg Dobler (KITP/UCSB) morphological tracers of emission Fermi 2 - 5 GeV Dobler et al. (2010)

  44. Greg Dobler (KITP/UCSB) morphological tracers of emission Fermi 2 - 5 GeV Fermi collab. (2012)

  45. Greg Dobler (KITP/UCSB) Fermi data 2 - 5 GeV Dobler et al. (2010) diffuse model 2 - 5 GeV Fermi “haze/bubbles” Fermi “haze” ...and later the “ Fermi bubbles” (Su et al., 2010)

  46. Greg Dobler (KITP/UCSB) the Fermi Haze a.k.a. Fermi Bubbles Dobler et al. (2010)

  47. Greg Dobler (KITP/UCSB) the Fermi Haze a.k.a. Fermi Bubbles Dobler et al. (2010) roughly “flat” brightness profile

  48. Greg Dobler (KITP/UCSB) the Fermi Haze a.k.a. Fermi Bubbles Su et al. (2010) roughly “flat” brightness profile

  49. Greg Dobler (KITP/UCSB) the Fermi haze/bubbles Fermi data 2 - 5 GeV diffuse model 2 - 5 GeV Fermi “haze/bubbles” Dobler et al. (2010)

  50. Greg Dobler (KITP/UCSB) electron spectra . the same spectrum (normalization and slope) reproduces the microwave and gamma-ray emission –2.0 dN/dE ∝ E . the characteristic energy of the emitting electrons for microwaves is E e ~10 GeV but for gammas is E e ~1 TeV . this implies very little cooling of the cosmic-ray population

  51. Greg Dobler (KITP/UCSB) = + + 23 GHz haze Dobler (2012)

  52. Greg Dobler (KITP/UCSB) = + + 23 GHz haze WMAP “drops” here ( b~-35 o ) Fermi “cuts off” here ( b~-50 o ) Dobler (2012) are they the same structure? are the Fermi edges “real”?

  53. Greg Dobler (KITP/UCSB) Dobler (2012b) are they the same structure? are the Fermi edges “real”?

  54. Greg Dobler (KITP/UCSB) Dobler (2012b) coincident “edge”?

  55. Greg Dobler (KITP/UCSB) Dobler (2012b) 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 coincident “edge”? YES!

  56. Greg Dobler (KITP/UCSB) Planck The Galactic haze/bubbles is shown here in PLANCK data from 30-44 GHz The same structure at 2-5 GeV as seen by the Fermi Gamma-Ray Space Telescope A multi-wavelength composite image showing both microwaves and gamma-rays: PLANCK 30 GHz (red), 44 GHz (green), and Fermi 2-5 GeV (blue). Planck Collaboration, 2012

  57. Greg Dobler (KITP/UCSB) Planck . divide sky into 10 regions Planck Collaboration, 2012, arXiv:1208.5483

  58. Greg Dobler (KITP/UCSB) Planck . 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 Planck Collaboration, 2012, arXiv:1208.5483

  59. Greg Dobler (KITP/UCSB) Planck . 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 Planck Collaboration, 2012, arXiv:1208.5483

  60. Greg Dobler (KITP/UCSB) Planck . 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 Planck Collaboration, 2012, arXiv:1208.5483

  61. Greg Dobler (KITP/UCSB) Planck Bayesian/Gibbs haze residual Planck Collaboration, 2012, arXiv:1208.5483

  62. Greg Dobler (KITP/UCSB) Planck 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 T H ∝ ν or dN –2.1 ––– ∝ E dE Planck Collaboration, 2012, arXiv:1208.5483

  63. Greg Dobler (KITP/UCSB) Planck 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 Planck Collaboration, 2012, arXiv:1208.5483

  64. Greg Dobler (KITP/UCSB) measuring B-fields in radio bubbles since synchrotron emissivity depends on the magnetic field strength B and the electron spectrum n e , emissivity = j ν (B, n e ) while the inverse Compton intensity is a function of the interstellar radiation field R and the electron spectrum n e , intensity = I γ (R, n e ) we can derive an estimate of B ~ 5 µ G. Dobler (2012b)

  65. Greg Dobler (KITP/UCSB) polarization Dobler (2012a)

  66. Greg Dobler (KITP/UCSB) what is it???

Download Presentation
Download Policy: The content available on the website is offered to you 'AS IS' for your personal information and use only. It cannot be commercialized, licensed, or distributed on other websites without prior consent from the author. To download a presentation, simply click this link. If you encounter any difficulties during the download process, it's possible that the publisher has removed the file from their server.

Recommend

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Bubbles, bubbles

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Bubbles, bubbles

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Bubbles, bubbles everywhere Bubbles, bubbles everywhere Why are bubbles important? Bubbles trace the location of energy input to the ISM Supernovae Stellar winds

489 views • 32 slides
Micro-Bubbles By: Givi Basishvili Xavier Marrero What are Micro-Bubbles? Small bubbles

Micro-Bubbles By: Givi Basishvili Xavier Marrero What are Micro-Bubbles? Small bubbles

Micro-Bubbles By: Givi Basishvili Xavier Marrero What are Micro-Bubbles? Small bubbles (>10m; 0.000001meters) Can hold: Oxygen - Genetic Info (DNA) - Drugs - Used for Medical Purposes 10m Purpose Deliver Chemicals

742 views • 18 slides
3M Glass Bubbles iM16K 3M Glass Bubbles iM16K 3M Glass Bubbles and Other Additives

3M Glass Bubbles iM16K 3M Glass Bubbles iM16K 3M Glass Bubbles and Other Additives

3M Glass Bubbles iM16K 3M Glass Bubbles iM16K 3M Glass Bubbles and Other Additives Classified by Aspect Ratio 3M Glass Bubbles Talc Glass Fiber 0.46 0.6 g/cc 2.8 g/cc 2.5 g/cc 20 m 20 m 20 m Low Hig h 1:1 20:1 30

663 views • 30 slides
Bubbles for Fama PRESENTER Robin Greenwood, Harvard Business School Bubbles for Fama o Fama does

Bubbles for Fama PRESENTER Robin Greenwood, Harvard Business School Bubbles for Fama o Fama does

Bubbles for Fama PRESENTER Robin Greenwood, Harvard Business School Bubbles for Fama o Fama does not believe in bubbles, which he defines as irrational strong price increase that implies a predictable strong decline . o Famas argument:

4.01k views • 40 slides
DAN Research Project 2009 February until May Introduction DCS without bubbles Bubbles

DAN Research Project 2009 February until May Introduction DCS without bubbles Bubbles

DAN Research Project 2009 February until May Introduction DCS without bubbles Bubbles without DCS Endothelial dysfunction without DCS Endothelial dysfunction with or without bubbles What is the cause of bubbles production ?

678 views • 36 slides
Bubbles for Fama PRESENTER Robin Greenwood, Harvard Business School DISCUSSANT Bubbles for Fama

Bubbles for Fama PRESENTER Robin Greenwood, Harvard Business School DISCUSSANT Bubbles for Fama

Bubbles for Fama PRESENTER Robin Greenwood, Harvard Business School DISCUSSANT Bubbles for Fama o Fama does not believe in bubbles, which he defines as irrational strong price increase that implies a predictable strong decline . o

795 views • 40 slides
Quiet Bubbles H. Hong D. Sraer June 9, 2011 Motivation: Loud versus Quiet Bubbles Classic

Quiet Bubbles H. Hong D. Sraer June 9, 2011 Motivation: Loud versus Quiet Bubbles Classic

Quiet Bubbles H. Hong D. Sraer June 9, 2011 Motivation: Loud versus Quiet Bubbles Classic speculative episodes associates high prices, high price volatility and high turnover (Hong and Stein 07). Internet stocks during 1996-2000: (1)

516 views • 26 slides
Asset Price Bubbles and Bubbly Debt Jan Werner ****** Andrzej Malawski Memorial Session Krak

Asset Price Bubbles and Bubbly Debt Jan Werner ****** Andrzej Malawski Memorial Session Krak

Asset Price Bubbles and Bubbly Debt Jan Werner ****** Andrzej Malawski Memorial Session Krak ow, October 2017 p. 1/2 Understanding Asset Price Bubbles price = fundamental value + bubble . Economic Theory: Price bubbles are rare and

686 views • 29 slides
Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures 1.Observational surveys for infrared bubbles Spitzer bubbles & the Milky Way Project 2.Theory of bubble formation & triggered star

668 views • 33 slides
Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures

Triggered star formation, HII regions and Spitzer bubbles Mark Thompson Outline of the lectures 1.Observational surveys for infrared bubbles Spitzer bubbles & the Milky Way Project 2.Theory of bubble formation & triggered star

569 views • 30 slides
Quiet Bubbles by Harrison Hong and David Sraer Discussant: Georgy Chabakauri, LSE 4th Paul

Quiet Bubbles by Harrison Hong and David Sraer Discussant: Georgy Chabakauri, LSE 4th Paul

Quiet Bubbles by Harrison Hong and David Sraer Discussant: Georgy Chabakauri, LSE 4th Paul Woolley Centre Conference Discussion Model Overview In contrast to equity bubbles credit bubble of 2003-2007 was quiet: prices were high but price

302 views • 9 slides
We are learning to: Write in sentences Just for today we will add speech bubbles to the

We are learning to: Write in sentences Just for today we will add speech bubbles to the

sharing a shell day 3 speech bubbles.notebook June 04, 2020 We are learning to: Write in sentences Just for today we will add speech bubbles to the pictures. Can I share your shell? sharing a shell day 3 speech bubbles.notebook June 04,

89 views • 8 slides
Rational Bubbles and Middlemen Yu Awaya Kohei Iwasaki Makoto Watanabe University of Rochester

Rational Bubbles and Middlemen Yu Awaya Kohei Iwasaki Makoto Watanabe University of Rochester

Rational Bubbles and Middlemen Yu Awaya Kohei Iwasaki Makoto Watanabe University of Rochester University of Wisconsin VU Amsterdam/ TI December 25, 2019 1 / 65 Motivation Bubbles: Continuous price increases, interrupted by a sudden

936 views • 65 slides
The Graphs of Planar Soap Bubbles David Eppstein Computer Science Dept., University of

The Graphs of Planar Soap Bubbles David Eppstein Computer Science Dept., University of

The Graphs of Planar Soap Bubbles David Eppstein Computer Science Dept., University of California, Irvine Symposium on Computational Geometry Rio de Janeiro, Brazil, June 2013 Soap bubbles and soap bubble foams Soap molecules form double

189 views • 17 slides
Electron bubbles and Weyl fermions in chiral superfluid 3 He-A Oleksii Shevtsov James A. Sauls

Electron bubbles and Weyl fermions in chiral superfluid 3 He-A Oleksii Shevtsov James A. Sauls

Electron bubbles and Weyl fermions in chiral superfluid 3 He-A Oleksii Shevtsov James A. Sauls Northwestern University, Evanston, IL 60208 USA October 12, 2016 (1) Introduction to superfluid 3 He and e -bubbles (2) Transport and AHE of e

951 views • 61 slides
CAN MACROPRUDENTIAL POLICIES ADDRESS ASSET PRICE BUBBLES? SOLE MARTINEZ PERIA MACRO-FINANCIAL

CAN MACROPRUDENTIAL POLICIES ADDRESS ASSET PRICE BUBBLES? SOLE MARTINEZ PERIA MACRO-FINANCIAL

CAN MACROPRUDENTIAL POLICIES ADDRESS ASSET PRICE BUBBLES? SOLE MARTINEZ PERIA MACRO-FINANCIAL DIVISION RESEARCH DEPARTMENT IMF DISCLAIMER: THESE ARE MY PERSONAL VIEWS AND NOT THOSE OF THE IMF 1 BUBBLES ARE COMMON 2 AND EVENTUALLY

256 views • 13 slides
Characterization of tails through hazard rate and convolution closure properties Anastasios G.

Characterization of tails through hazard rate and convolution closure properties Anastasios G.

Introduction. Matuszewska Indices Class ER Class D Pitman Result Class A Further Results Characterization of tails through hazard rate and convolution closure properties Anastasios G. Bardoutsos, Dimitrios G. Konstantinides Department of

631 views • 28 slides
Welcome to the SRA Webinar Series All of our Webinars are available to members as videos online

Welcome to the SRA Webinar Series All of our Webinars are available to members as videos online

Welcome to the SRA Webinar Series All of our Webinars are available to members as videos online at SRA.org (you must be logged in as a member) With Appreciation to our Cosponsors SRA National Capital Area Chapter Risk Policy and Law Specialty

325 views • 7 slides
Siting/Conventional Facilities Status Steve Dixon PIP-II Machine Advisory Committee Meeting

Siting/Conventional Facilities Status Steve Dixon PIP-II Machine Advisory Committee Meeting

Siting/Conventional Facilities Status Steve Dixon PIP-II Machine Advisory Committee Meeting 15-17 March 2016 Agenda Progress over the last year Current Activities Plans for CD-1 2 S. Dixon | 2016 P2MAC 3/15/2016 Progress Over

433 views • 16 slides
PMRA Environmental Risk Assessment Pest Management Regulatory Agency Environmental Risk

PMRA Environmental Risk Assessment Pest Management Regulatory Agency Environmental Risk

PMRA Environmental Risk Assessment Pest Management Regulatory Agency Environmental Risk Assessment Daniel G Sauv, MSc. Senior Evaluation Officer, Environmental Risk Section III Environmental Assessment Directorate Scientific Evaluation and

683 views • 18 slides
Joe Levine s Purple Haze Physical/Phenomenal Gaps n P = the complete microphysical truth

Joe Levine s Purple Haze Physical/Phenomenal Gaps n P = the complete microphysical truth

Joe Levine s Purple Haze Physical/Phenomenal Gaps n P = the complete microphysical truth n Q = a phenomenal truth n Q1: Is there an epistemic gap between P and Q? n Q2: Is there an ontological gap between P and Q? The

336 views • 31 slides
Indirect Dark Matter constraints Indirect Dark Matter constraints with radio observations with

Indirect Dark Matter constraints Indirect Dark Matter constraints with radio observations with

Indirect Dark Matter constraints Indirect Dark Matter constraints with radio observations with radio observations In collaboration with E.Borriello and G.Miele, University of Naples Federico II Alessandro Cuoco, Florence, Institute

459 views • 21 slides
A i r q u a l i t y m o n i t o r i n g : a n I C N u s e c a s e ? K a n c h a n a K a n

A i r q u a l i t y m o n i t o r i n g : a n I C N u s e c a s e ? K a n c h a n a K a n

A i r q u a l i t y m o n i t o r i n g : a n I C N u s e c a s e ? K a n c h a n a K a n c h a n a s u t i n t E R L a b , A s i a n I n s t i t u t e o f T e c h n o l o g y T h a i l a n d 1 PROBLEM In 2012, WHO

484 views • 19 slides
FOG; COMPOSITING 1 OUTLINE Fog Compositing Blending Transparency Clipping

FOG; COMPOSITING 1 OUTLINE Fog Compositing Blending Transparency Clipping

FOG; COMPOSITING 1 OUTLINE Fog Compositing Blending Transparency Clipping 3D Textures Noise 2 FOG Atmospheric haze Provides more realism in a scene Also provides more sense of scene depth Simple

967 views • 33 slides

More recommend