Topological defects can source scalar, vector and tensor modes in the early universe. The vector modes have power on small scales and can generate E and B polarization; the B signal can be quite distinctive, and used to constrain defect models with future data.
This paper appears to take some previous results for the Bmode power spectrum and multiply them by l^4, so e.g. in Fig 1 the power is very blue. Of course to be consistent you also have to multiply the noise and the any other spectrum of interest by l^4 as well, so you seem to gain nothing by doing this. Is there some point I have missed?
The paper also defines a 'local' scalar [tex]\tilde{B}[/tex] by taking two derivatives of the polarization tensor. However you gain nothing by doing this; with noisy or nonbandlimited data you cannot calculate derivatives on a scale L without having data available over a scale L  the nonlocality just hits you in a different form (see astroph/0305545 and refs).
[1003.0299] The local Bpolarization of the CMB: a very sensitive probe of cosmic defects
Authors:  Juan GarciaBellido, Ruth Durrer, Elisa Fenu, Daniel G. Figueroa, Martin Kunz 
Abstract:  We present a new and especially powerful signature of cosmic strings and other topological or nontopological defects in the polarization of the cosmic microwave background (CMB). We show that even if defects contribute 1% or less in the CMB temperature anisotropy spectrum, their signature in the local $\tilde{B}$polarization correlation function at angular scales of tens of arc minutes is much larger than that due to gravitational waves from inflation, even if the latter contribute with a ratio as big as $r\simeq 0.1$ to the temperature anisotropies. Proposed Bpolarization experiments, with a good sensitivity on arcminute scales, may either detect a contribution from topological defects produced after inflation or place stringent limits on them. Even Planck should be able to improve present constraints on defect models by at least an order of magnitude, to the level of $\ep <10^{7}$. A future fullsky experiment like CMBpol, with polarization sensitivities of the order of $1\mu$Karcmin, will be able to constrain the defect parameter $\ep=Gv^2$ to a few $\times10^{9}$, depending on the defect model. 
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[1003.0299] The local Bpolarization of the CMB: a very sen
The main point is that vector components of defects' contribution to CMB polarization anisotropies peak at scales smaller than those from inflation.
On the other hand, the ordinary E and Bmodes depend nonlocally on the Stokes parameters, so they cannot be used to put constraints on causal sources like defects using the angular correlation function of E and Bmodes on small scales. That is the reason why Baumann and Zaldarriaga [0901.0958] suggested using instead the local modes. Those are the true causal modes, written in terms of derivatives of the Stokes parameters.
These local Bmodes then have power spectra that are much bluer than the nonlocal ones, and hence enhance the small scale (highl) end of the spectrum. It is by looking at the angular correlation functions at small separations (tens of arcmin) that one has a chance to measure the defect's contribution to the local Bmodes, and distinguish it from the one of inflation.
Of course, the usual white noise power spectrum for polarization will also be modified by this [tex]\ell^4[/tex] factor, but by a suitable gaussian smoothing of the data (following Baumann&Zaldarriaga), we can indeed obtain large signal to noise ratios for binned data at small angular scales.
Baumann&Zaldarriaga looked at the modelindependent signature of inflation at angles [tex]\theta>2[/tex] degrees. What we have realiazed is that, although modeldependent, the signal at angles [tex]\theta < 1[/tex] degrees can be much more significant. In fact, the feature at small angles is rather universal. The differences between defect models (and we considered four different ones) is just in the height and width of the first and second oscillations in the angular correlation functions (related to the heigth and position of the angular power spectrum). Therefore, with sufficient angular resolution one could not only detect defects (if they are there) but also differentiate between different models.
On the other hand, the ordinary E and Bmodes depend nonlocally on the Stokes parameters, so they cannot be used to put constraints on causal sources like defects using the angular correlation function of E and Bmodes on small scales. That is the reason why Baumann and Zaldarriaga [0901.0958] suggested using instead the local modes. Those are the true causal modes, written in terms of derivatives of the Stokes parameters.
These local Bmodes then have power spectra that are much bluer than the nonlocal ones, and hence enhance the small scale (highl) end of the spectrum. It is by looking at the angular correlation functions at small separations (tens of arcmin) that one has a chance to measure the defect's contribution to the local Bmodes, and distinguish it from the one of inflation.
Of course, the usual white noise power spectrum for polarization will also be modified by this [tex]\ell^4[/tex] factor, but by a suitable gaussian smoothing of the data (following Baumann&Zaldarriaga), we can indeed obtain large signal to noise ratios for binned data at small angular scales.
Baumann&Zaldarriaga looked at the modelindependent signature of inflation at angles [tex]\theta>2[/tex] degrees. What we have realiazed is that, although modeldependent, the signal at angles [tex]\theta < 1[/tex] degrees can be much more significant. In fact, the feature at small angles is rather universal. The differences between defect models (and we considered four different ones) is just in the height and width of the first and second oscillations in the angular correlation functions (related to the heigth and position of the angular power spectrum). Therefore, with sufficient angular resolution one could not only detect defects (if they are there) but also differentiate between different models.

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Re: [1003.0299] The local Bpolarization of the CMB: a very
I think it is clear from the normal power spectra that the sourced vector mode Bpolarization peaks at much smaller scales than the gravitational wave spectrum: mostly scales subhorizon at recombination as opposed to tensor modes which decay on subhorizon scales. I agree that with low enough noise this is an interesting signal (and has been calculated many times before), though it needs to be distinguished from other possible vector mode sources like magnetic fields.
I thought the point of the Baumann paper was to make a nice picture showing visually the structure of the correlations. The E and B modes contain exactly the same information as the tilde versions; in the same way the WMAP7 papers make some nice plots of the polarizationtemperature correlation to visually show a physical effect, but these constrain the same information as the usual power spectra. In the Gaussian limit the usual E/B spectra contain all the information on the defect power spectrum.
Only Q and U can actually be measured locally on the sky (in one pixel you cannot calculate any spatial derivatives). The twopoint Q/U correlations can be calculated from the usual E and B spectra.
I thought the point of the Baumann paper was to make a nice picture showing visually the structure of the correlations. The E and B modes contain exactly the same information as the tilde versions; in the same way the WMAP7 papers make some nice plots of the polarizationtemperature correlation to visually show a physical effect, but these constrain the same information as the usual power spectra. In the Gaussian limit the usual E/B spectra contain all the information on the defect power spectrum.
Only Q and U can actually be measured locally on the sky (in one pixel you cannot calculate any spatial derivatives). The twopoint Q/U correlations can be calculated from the usual E and B spectra.