Loops and spurs: the angular power spectrum of the Galactic synchrotron background

Research output: Contribution to journal › Journal article › Research › peer-review

Standard

Loops and spurs : the angular power spectrum of the Galactic synchrotron background. / Mertsch, Philipp; Sarkar, Subir.

In: Journal of Cosmology and Astroparticle Physics, Vol. 2013, No. 6, 041, 01.06.2013.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Mertsch, P & Sarkar, S 2013, 'Loops and spurs: the angular power spectrum of the Galactic synchrotron background', Journal of Cosmology and Astroparticle Physics, vol. 2013, no. 6, 041. https://doi.org/10.1088/1475-7516/2013/06/041

APA

Mertsch, P., & Sarkar, S. (2013). Loops and spurs: the angular power spectrum of the Galactic synchrotron background. Journal of Cosmology and Astroparticle Physics, 2013(6), [041]. https://doi.org/10.1088/1475-7516/2013/06/041

Vancouver

Mertsch P, Sarkar S. Loops and spurs: the angular power spectrum of the Galactic synchrotron background. Journal of Cosmology and Astroparticle Physics. 2013 Jun 1;2013(6). 041. https://doi.org/10.1088/1475-7516/2013/06/041

Author

Mertsch, Philipp ; Sarkar, Subir. / Loops and spurs : the angular power spectrum of the Galactic synchrotron background. In: Journal of Cosmology and Astroparticle Physics. 2013 ; Vol. 2013, No. 6.

Bibtex

@article{6cfc43f2494a420bbdd9a13d790b31bc,
title = "Loops and spurs: the angular power spectrum of the Galactic synchrotron background",
abstract = "We present a new model of the diffuse Galactic synchrotron radiation, concentratingon its angular anisotropies. While previous studies have focussed on either the variation of the emissivity on large (~kpc) scales, or on fluctuations due to MHD turbulence in the interstellar medium, we unify these approaches to match the angular power spectrum. We note that the usual turbulence cascade calculation ignores spatial correlations at the injection scale (~100 pc) due to compression of the interstellar medium by of O(1000) old supernova remnants — the {\textquoteleft}radio loops{\textquoteright} only four of which are visible in radio maps. This new component naturally provides the otherwise missing power on intermediate and small scales in the all-sky map at 408 MHz. Our model can enable more reliable subtraction of the synchrotron foreground for studies of CMB anisotropies or searches for dark matter annihilation. We conclude with some remarks on the relevance to modelling of the polarised foreground.",
author = "Philipp Mertsch and Subir Sarkar",
year = "2013",
month = jun,
day = "1",
doi = "10.1088/1475-7516/2013/06/041",
language = "English",
volume = "2013",
journal = "Journal of Cosmology and Astroparticle Physics",
issn = "1475-7516",
publisher = "IOP Publishing",
number = "6",

}

RIS

TY - JOUR

T1 - Loops and spurs

T2 - the angular power spectrum of the Galactic synchrotron background

AU - Mertsch, Philipp

AU - Sarkar, Subir

PY - 2013/6/1

Y1 - 2013/6/1

N2 - We present a new model of the diffuse Galactic synchrotron radiation, concentratingon its angular anisotropies. While previous studies have focussed on either the variation of the emissivity on large (~kpc) scales, or on fluctuations due to MHD turbulence in the interstellar medium, we unify these approaches to match the angular power spectrum. We note that the usual turbulence cascade calculation ignores spatial correlations at the injection scale (~100 pc) due to compression of the interstellar medium by of O(1000) old supernova remnants — the ‘radio loops’ only four of which are visible in radio maps. This new component naturally provides the otherwise missing power on intermediate and small scales in the all-sky map at 408 MHz. Our model can enable more reliable subtraction of the synchrotron foreground for studies of CMB anisotropies or searches for dark matter annihilation. We conclude with some remarks on the relevance to modelling of the polarised foreground.

AB - We present a new model of the diffuse Galactic synchrotron radiation, concentratingon its angular anisotropies. While previous studies have focussed on either the variation of the emissivity on large (~kpc) scales, or on fluctuations due to MHD turbulence in the interstellar medium, we unify these approaches to match the angular power spectrum. We note that the usual turbulence cascade calculation ignores spatial correlations at the injection scale (~100 pc) due to compression of the interstellar medium by of O(1000) old supernova remnants — the ‘radio loops’ only four of which are visible in radio maps. This new component naturally provides the otherwise missing power on intermediate and small scales in the all-sky map at 408 MHz. Our model can enable more reliable subtraction of the synchrotron foreground for studies of CMB anisotropies or searches for dark matter annihilation. We conclude with some remarks on the relevance to modelling of the polarised foreground.

U2 - 10.1088/1475-7516/2013/06/041

DO - 10.1088/1475-7516/2013/06/041

M3 - Journal article

VL - 2013

JO - Journal of Cosmology and Astroparticle Physics

JF - Journal of Cosmology and Astroparticle Physics

SN - 1475-7516

IS - 6

M1 - 041

ER -

ID: 97171852