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Article overview
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Synchrotron spectral index and interstellar medium densities of star-forming galaxies | Aritra Basu
; Rainer Beck
; Philip Schmidt
; Subhashis Roy
; | Date: |
9 Mar 2015 | Abstract: | The spectral index of synchrotron emission is an important parameter in
understanding the properties of cosmic ray electrons (CREs) and the
interstellar medium (ISM). We determine the synchrotron spectral index
($alpha_{
m nt}$) of four nearby star-forming galaxies, namely NGC 4736, NGC
5055, NGC 5236 and NGC 6946 at sub-kpc linear scales. The $alpha_{
m nt}$ was
determined between 0.33 and 1.4 GHz for all the galaxies. We find the spectral
index to be flatter ($gtrsim -0.7$) in regions with total neutral (atomic +
molecular) gas surface density, $Sigma_{
m gas} gtrsim
m 50~M_odot
pc^{-2}$, typically in the arms and inner parts of the galaxies. In regions
with $Sigma_{
m gas} lesssim
m 50~M_odot pc^{-2}$, especially in the
interarm and outer regions of the galaxies, the spectral index steepens sharply
to $<-1.0$. The flattening of $alpha_{
m nt}$ is unlikely to be caused due to
thermal free--free absorption at 0.33 GHz. Our result is consistent with the
scenario where the CREs emitting at frequencies below $sim0.3$ GHz are
dominated by bremsstrahlung and/or ionization losses. For denser medium
($Sigma_{
m gas} gtrsim
m 200~M_odot pc^{-2}$), having strong magnetic
fields ($sim 30~mu$G), $alpha_{
m nt}$ is seen to be flatter than $-0.5$,
perhaps caused due to ionization losses. We find that, due to the clumpy nature
of the ISM, such dense regions cover only a small fraction of the galaxy
($lesssim5$ percent). Thus, the galaxy-integrated spectrum may not show
indication of such loss mechanisms and remain a power-law over a wide range of
radio frequencies (between $sim 0.1$ to 10 GHz). | Source: | arXiv, 1503.2420 | Services: | Forum | Review | PDF | Favorites |
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