Type Ia SNe Spectropolarimetry

Details Type Ia SNe Spectropolarimetry Type Ia SNe Spectropolarimetry

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21920304z&link_type=abstract

American Astronomical Society, AAS Meeting #219, #203.04

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Scientific paper

We present optical spectropolarimetry of 7 Type Ia SNe taken with FORS2 at the Very Large Telescope of ESO Paranal Observatory. Our observations extend from pre-maximum to late phases,sampling the different types of asymmetries revealed as the photosphere recedes through deeper layers.
With this limited sample of SNe, already, we find that polarimetric characteristics of type Ia's are quite varied. We confirm that typical continuum polarization is low ( 0.3 %), indicating low degree of global asymmetry. We also find that line polarization, related to local chemical, density, or excitation, asymmetries is fairly common, and shows a diverse behavior.
We present results on the SiII 6355 and CaII IR triplet features.
Line polarization in Si II, when present, shows a smooth evolution, increasing from early pre-maximum phases, peaking close to maximum light, and decreasing for couple of weeks after maximum, when it disappears. This behavior was known from the study of previous, smaller, samples. Our larger sample adds variety to the known evolution, suggesting to re-evaluate what we understand as typical.
Ca II IR triplet evolution is puzzling. Strong calcium line polarization is found at different phases of the light curve in many SNe, while some others show none. The line polarization does evolve with time, but, rather than decreasing after maximum, in many cases shoots up. When present, the feature is persistent. One SN shows it approximately two months after maximum.
We interpret the observations connecting the spectropolarimetric signals with the different stages of the explosion revealed at various SN phases. We emphasize the importance of enlarging the sample of SN observed in spectropolarimetry, extending the time of coverage, as well as increasing the time sampling near maximum.
P.Z. acknowledges support by Iniciativa Cientifica Milenio through the
Millennium Center for Supernova Science (NC10-064-F) and Conicyt (Beca de Doctorado)

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