Presentation is loading. Please wait.

Presentation is loading. Please wait.

Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 1 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34.

Published byBrittney Poole Modified over 8 years ago

Similar presentations

Presentation on theme: "Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 1 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34."— Presentation transcript:

1 Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 1 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

2 Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 2 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

3 Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 3 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

4 Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 4 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

5 Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 5 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

6 Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 6 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34 Information: Thank you for downloading this PowerPoint slide from The Astrophysical Journal. This slide was designed to be edited; you can: - Remove components (including this text box!) - Resize components - Apply a style or theme - Please remember to include the original article citation information.

Download ppt "Figure 4 from Power Spectrum Analysis of Polarized Emission from the Canadian Galactic Plane Survey (Image 1 of 6) R. A. Stutz et al. 2014 ApJ 787 34 doi:10.1088/0004-637X/787/1/34."

Similar presentations

Figure 4 from The Hubble Space Telescope Cluster Supernova Survey. II. The Type Ia Supernova Rate in High-redshift Galaxy Clusters (Image 1 of 3) K. Barbary.

Figure 4 from The Hubble Space Telescope Cluster Supernova Survey. II. The Type Ia Supernova Rate in High-redshift Galaxy Clusters (Image 1 of 3) K. Barbary.
Figure 7 from Effects of Circumnuclear Disk Gas Evolution on the Spin of Central Black Holes (Image 1 of 7) Umberto Maio et al. 2013 ApJ 767 37 doi:10.1088/0004-637X/767/1/37.

Figure 7 from Effects of Circumnuclear Disk Gas Evolution on the Spin of Central Black Holes (Image 1 of 7) Umberto Maio et al ApJ doi: / X/767/1/37.
Figure 6 from HST/WFC3 Near-infrared Spectroscopy of Quenched Galaxies at z ~ 1.5 from the WISP Survey: Stellar Population Properties (Image 1 of 8) A.

Figure 6 from HST/WFC3 Near-infrared Spectroscopy of Quenched Galaxies at z ~ 1.5 from the WISP Survey: Stellar Population Properties (Image 1 of 8) A.
Figure 14 from MUSCLE W49: A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. I. Data and the Mass.

Figure 14 from MUSCLE W49: A Multi-Scale Continuum and Line Exploration of the Most Luminous Star Formation Region in the Milky Way. I. Data and the Mass.
Figure 14 from The Compositional Diversity of Extrasolar Terrestrial Planets. I. In Situ Simulations (Image 1 of 4) Jade C. Bond et al. 2010 ApJ 715 1050.

Figure 14 from The Compositional Diversity of Extrasolar Terrestrial Planets. I. In Situ Simulations (Image 1 of 4) Jade C. Bond et al ApJ
Figure 4 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 9) N. M. McClure-Griffiths et al. 2012 ApJS 199 12 doi:10.1088/0067-0049/199/1/12.

Figure 4 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 9) N. M. McClure-Griffiths et al ApJS doi: / /199/1/12.
Figure 15 from Spectral Energy Distributions of QSOs at z > 5: Common Active Galactic Nucleus-heated Dust and Occasionally Strong Star-formation (Image.

Figure 15 from Spectral Energy Distributions of QSOs at z > 5: Common Active Galactic Nucleus-heated Dust and Occasionally Strong Star-formation (Image.
Figure 15 from Star Formation in the Central 400 pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects (Image 1 of 2) F. Yusef-Zadeh.

Figure 15 from Star Formation in the Central 400 pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects (Image 1 of 2) F. Yusef-Zadeh.
Figure 5 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 5) N. M. McClure-Griffiths et al ApJS doi: / /199/1/12.

Figure 5 from The Australia Telescope Compact Array H I Survey of the Galactic Center (Image 1 of 5) N. M. McClure-Griffiths et al ApJS doi: / /199/1/12.
Figure 3 from Multiple Component Outflows in an Active Region Observed with the EUV Imaging Spectrometer on Hinode (Image 1 of 11) P. Bryans et al. 2010.

Figure 3 from Multiple Component Outflows in an Active Region Observed with the EUV Imaging Spectrometer on Hinode (Image 1 of 11) P. Bryans et al
K. Decker French et al ApJ doi: / X/801/1/1 Information:

K. Decker French et al ApJ doi: / X/801/1/1 Information:
Figure 15 from Cloud–Cloud Collision as a Trigger of the High-mass Star Formation: a Molecular Line Study in RCW120 (Image 1 of 5) K. Torii et al. 2015.

Figure 15 from Cloud–Cloud Collision as a Trigger of the High-mass Star Formation: a Molecular Line Study in RCW120 (Image 1 of 5) K. Torii et al
Figure 7 from The Evolution of Dwarf Galaxy Satellites with Different Dark Matter Density Profiles in the ErisMod Simulations. I. The Early Infalls Mihai.

Figure 7 from The Evolution of Dwarf Galaxy Satellites with Different Dark Matter Density Profiles in the ErisMod Simulations. I. The Early Infalls Mihai.
Figure 9 from A Direct Measurement of the Forward Shock Speed in Supernova Remnant 0509-67.5: Constraints on the Age, Ambient Density, Shock Compression.

Figure 9 from A Direct Measurement of the Forward Shock Speed in Supernova Remnant : Constraints on the Age, Ambient Density, Shock Compression.
Figure 2 from The Role of Active Region Loop Geometry. II

Figure 2 from The Role of Active Region Loop Geometry. II
Figure 5 from The ACS LCID Project. II

Figure 5 from The ACS LCID Project. II
Qing-Wen Tang et al ApJ doi: / X/806/2/194 Information:

Qing-Wen Tang et al ApJ doi: / X/806/2/194 Information:
Figure 8 from Dust Reddened Quasars in FIRST and UKIDSS: Beyond the Tip of the Iceberg (Image 1 of 5) Eilat Glikman et al. 2013 ApJ 778 127 doi:10.1088/0004-637X/778/2/127.

Figure 8 from Dust Reddened Quasars in FIRST and UKIDSS: Beyond the Tip of the Iceberg (Image 1 of 5) Eilat Glikman et al ApJ doi: / X/778/2/127.
Figure 4 from Electron Heating by the Ion Cyclotron Instability in Collisionless Accretion Flows. II. Electron Heating Efficiency as a Function of Flow.

Figure 4 from Electron Heating by the Ion Cyclotron Instability in Collisionless Accretion Flows. II. Electron Heating Efficiency as a Function of Flow.
Figure 27 from Embedded Protostars in the Dust, Ice, and Gas In Time (DIGIT) Herschel Key Program: Continuum SEDs, and an Inventory of Characteristic Far-infrared.

Figure 27 from Embedded Protostars in the Dust, Ice, and Gas In Time (DIGIT) Herschel Key Program: Continuum SEDs, and an Inventory of Characteristic Far-infrared.

Similar presentations

Ads by Google