Local Bubble contribution to the 353-GHz dust polarized emission

Skalidis, R.; Pelgrims, Vincent

doi:10.1051/0004-6361/201936547

Cited by 27 publications

(16 citation statements)

References 55 publications

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“…Similar regions of alignment are found in the |θ − χ dust | map. This is not a surprise, since at high latitudes, the absorbing and emitting dust column is likely the same (as shown by Skalidis & Pelgrims 2019;Planck Collaboration et al 2020b). At high latitudes, the large areas of alignment are particularly above the Galactic centre near Loop I.…”

Section: Large-scale Overview and Choice Of Loopssupporting

confidence: 58%

Revisiting the distance to radio Loops I and IV using Gaia and radio/optical polarization data

Panopoulou,

Dickinson,

Readhead

et al. 2021

Preprint

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Galactic synchrotron emission exhibits large-angular-scale features known as radio spurs and loops. Determining the physical size of these structures is important for understanding the local interstellar structure and for modeling the Galactic magnetic field. However, the distance to these structures is either debated or entirely unknown. We revisit a classical method of finding the location of radio spurs by comparing optical polarization angles with those of synchrotron emission as a function of distance. We consider three tracers of the magnetic field: stellar polarization, polarized synchrotron radio emission, and polarized thermal dust emission. We employ archival measurements of optical starlight polarization and Gaia distances, and construct a new map of polarized synchrotron emission from WMAP and Planck data. We confirm that synchrotron, dust emission, and stellar polarization angles all show a statistically significant alignment at high Galactic latitude. We obtain distance limits to three regions towards Loop I of 112±17 pc, 122±32 pc, and < 105 pc. Our results strongly suggest that the polarized synchrotron emission towards the North Polar Spur at b > 30 • is local. This is consistent with the conclusions of earlier work based on stellar polarization and extinction, but in stark contrast with the Galactic center origin recently revisited on the basis of X-ray data. We also obtain a distance measurement towards part of Loop IV (177±17 pc) and find strong evidence that its synchrotron emission arises from chance overlap of structures located at different distances. Future optical polarization surveys will allow the expansion of this analysis to other radio spurs.

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Section: Large-scale Overview and Choice Of Loopssupporting

confidence: 58%

Revisiting the distance to radio Loops I and IV using Gaia and radio/optical polarization data

Panopoulou,

Dickinson,

Readhead

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Similar regions of alignment are found in the |θ − χ dust | map. This is not a surprise, since at high latitudes the absorbing and emitting dust column is likely the same (as shown by Skalidis & Pelgrims 2019;Collaboration et al 2020b). At high latitudes, the large areas of alignment are particularly above the Galactic center near Loop I.…”

Section: Large-scale Overview and Choice Of Loopsmentioning

confidence: 68%

Revisiting the Distance to Radio Loops I and IV Using Gaia and Radio/Optical Polarization Data

Panopoulou

Dickinson

Readhead

et al. 2021

ApJ

View full text Add to dashboard Cite

Galactic synchrotron emission exhibits large angular scale features known as radio spurs and loops. Determining the physical size of these structures is important for understanding the local interstellar structure and for modeling the Galactic magnetic field. However, the distance to these structures is either under debate or entirely unknown. We revisit a classical method of finding the location of radio spurs by comparing optical polarization angles with those of synchrotron emission as a function of distance. We consider three tracers of the magnetic field: stellar polarization, polarized synchrotron radio emission, and polarized thermal dust emission. We employ archival measurements of optical starlight polarization and Gaia distances and construct a new map of polarized synchrotron emission from WMAP and Planck data. We confirm that synchrotron, dust emission, and stellar polarization angles all show a statistically significant alignment at high Galactic latitude. We obtain distance limits to three regions toward Loop I of 112 ± 17 pc, 135 ± 20 pc, and <105 pc. Our results strongly suggest that the polarized synchrotron emission toward the North Polar Spur at b > 30° is local. This is consistent with the conclusions of earlier work based on stellar polarization and extinction, but in stark contrast with the Galactic center origin recently revisited on the basis of X-ray data. We also obtain a distance measurement toward part of Loop IV (180 ± 15 pc) and find evidence that its synchrotron emission arises from chance overlap of structures located at different distances. Future optical polarization surveys will allow the expansion of this analysis to other radio spurs.

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“…The map might also prove relevant for foreground corrections to the CMB, especially for CMB polarization studies. It was shown that most of the Galactic infrared polarization at high latitudes (|b| > 60) comes from close-by regions around 200-300 pc (Skalidis & Pelgrims 2019). Correction maps have so far been based on infrared observations, and could be biased through different starlight illumination or differing dust temperatures.…”

Section: Introductionmentioning

confidence: 99%

Resolving nearby dust clouds

Leike

Glatzle

Enßlin

2020

A&A

143

176

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Aims. Mapping the interstellar medium in 3D provides a wealth of insights into its inner working. The Milky Way is the only galaxy for which detailed 3D mapping can be achieved in principle. In this paper, we reconstruct the dust density in and around the local super-bubble. Methods. The combined data from surveys such as Gaia, 2MASS, PANSTARRS, and ALLWISE provide the necessary information to make detailed maps of the interstellar medium in our surrounding. To this end, we used variational inference and Gaussian processes to model the dust extinction density, exploiting its intrinsic correlations. Results. We reconstructed a highly resolved dust map, showing the nearest dust clouds at a distance of up to 400 pc with a resolution of 1 pc. Conclusions. Our reconstruction provides insights into the structure of the interstellar medium. We compute summary statistics of the spectral index and the 1-point function of the logarithmic dust extinction density, which may constrain simulations of the interstellar medium that achieve a similar resolution.

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Local Bubble contribution to the 353-GHz dust polarized emission

Cited by 27 publications

References 55 publications

Revisiting the distance to radio Loops I and IV using Gaia and radio/optical polarization data

Revisiting the distance to radio Loops I and IV using Gaia and radio/optical polarization data

Revisiting the Distance to Radio Loops I and IV Using Gaia and Radio/Optical Polarization Data

Resolving nearby dust clouds

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