A Universal Luminosity Function for Radio Supernova Remnants Laura Chomiuk University of Wisconsin--Madison.

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Presentation transcript:

A Universal Luminosity Function for Radio Supernova Remnants Laura Chomiuk University of Wisconsin--Madison

Are SNRs fundamentally the same across galaxies? The brightest SNR in M33 is ~10 times less luminous than the brightest SNR in NGC Lacey & Duric (2001)

Radio SNRs in Other Galaxies NGC cm NGC 4449 H  SNR H II region Background source 8 SNRs found in NGC 4449 by Chomiuk & Wilcots (2009).

SNRs in 19 Nearby Galaxies LMCSMC IC 10 M 33NGC 1569 NGC 300 NGC 4214NGC 2366 M 82 NGC 7793 NGC 253 NGC 4449 M 81 M 83 NGC 4736 NGC 6946 NGC 4258 M 51 Arp 220

Cumulative Luminosity Functions

Composite SNR Luminosity Function  =  0.07

LF scaling factor (assuming  = -2.13) Approximately linear relation: Arp 220: outlier?

We can rewrite dN/dL as: dN/dt is the production rate of SNRs,  SFR. dL/dt describes the luminosity evolution of SNRs. Therefore, the SNR LF can be described as:

From Berezhko & Volk (2004) 3 cm cm cm -3 Some Approximations Radio SNRs are in the adiabatic phase. In the adiabatic phase, the CR energy does not depend on time or ISM density. E CR /E SN  constant.

Therefore, it is the magnetic field that determines dL/dt. Standard prescription for magnetic field amplification: Making these simplifications, we find an expression for the time evolution of synchrotron luminosity: And for the luminosity function:  = -2.1 A very good fit to the data!

The L max --SFR relation Best fit to data Prediction for statistical sampling from Monte Carlo simulations Just a statistical sampling effect?

Cas A on the L max --SFR relation Only a 3% probability that a galaxy with L max  L Cas A has a SFR > 2 M  /year

Conclusions The SNR LF is remarkably similar across galaxies. It is consistent with a power law of constant index and scaling  SFR. The SNR LF is well fit with models of diffusive shock acceleration + magnetic field amplification, given a few simplifying assumptions. Galaxies with higher SFRs host more luminous SNRs; this can be completely explained by statistical sampling effects. The luminosity of Cas A implies that current estimates of the Milky Way SFR may be too high.

Model the SNR LFs as power laws The four “best” galaxies (N SNR >20) all have similar best-fit  : weighted mean  =  0.10 M  0.17 M  0.25 NGC  0.29 M  0.26

Is there a dependence on ISM density? Line marks theoretical prediction: A/SFR   0 0.5

There are claims that B 2   0 v s 3 instead of   0 v s 2. From Vink (2004). This would predict dL/dN  L Decidedly not in agreement with the SNR LF data.