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Fig. 1 of "The Disappearance of the Progenitors of Supernovae 1993J and 2003gd", Maund & Smartt (2009; arXiv:0903.3772)

 A high resolution version of Fig. 1 of Maund & Smartt (2009) "The Disappearance of the Progenitors of Supernovae 1993J and 2003gd", Science in press, can be found here


Thesis: The Observed Nature of the Progenitors of Core-collapse Supernovae


A copy of my thesis "The Observed Nature of the Progenitors of Core-collapse Supernovae" is available here.


“Spectropolarimetry of the Type IIb Supernova 2001ig” - Maund et al. (2007), in press


 Figure 1 of Maund et al. (2007) "Spectropolarimetry of the Type IIb Supernova 2001ig" (astro-ph/0709.1487) you can find it here.


“Optical spectropolarimetry with incomplete datasets” - Maund (2007), A&A, accepted


 The submitted version of Maund (2007) “Optical spectropolarimetry with incomplete datasets”, accepted for publication in A&A, is available (in PDF format) here.


“The birth place of the progenitor of the type Ic Supernova 2007gr” - Crockett, Maund et al. (2007), ApJL, accepted (click here for astro-ph/0709.2354)


 Post-explosion images of the SN 2007gr site were acquired with HST WFPC2 (F450W+F814W) as part of program GO-11119.  This imaging agrees with the high resolution Gemini NIRI-ALTAIR images in our paper.
Pre- and post-explosion images are here.  Photometry of the SN at this epoch gives m(F450W)=16.029, m(F814W)=14.299.


M-ELM emission line fitting program


Below is M-ELM fit to the T+10 years spectrum of SN 1993J (original data is here). Model calculated for an edge on disk, with density that goes as r-5 and a uniform distribution of dust inside the disk (which cause the emission line profile in the red to be extinguished by 0.57m). On the main panel the dashed line is the [O III] 4959 line and the dot-dashed line is the [O III] 5007. In the side panels, the top panel is the view from the observer's perspective, the middle panel is the side-view and the bottom panel is the view from the top. The colour scheme logarithmically follows the emissivity density - blue 10-6, green 10-7.5, red 10-9.


MAUNDSPOL fits file format


 plot100 now spits out a multi-extension fits file with all the output from the reduction procedure, plus fully debiassed data, into a single file. The separate data go into separate extensions, which are listed in the table below.

Ext. Filename KEYWORD Comment
1 Fbin.fits FLUXBIN Binned flux $F_{\lambda}(bin)$
2 eFbin.fits FLUXBINERR Error on binned flux $\Delta F_{\lambda}(bin)$
3 Q.fits QSTOKES $Q$ Stokes parameter
4 eQ.fits DELTQSTOKES Error $\Delta Q$ on $Q$ Stokes parameter
5 epsQ.fits EPSQ $Q$ instrumental signature correction $\epsilon_{Q}$
6 U.fits USTOKES $U$ Stokes parameter
7 eU.fits DELTUSTOKES Error $\Delta U$ on $U$ Stokes parameter
8 epsU.fits EPSU $U$ instrumental signature correction $\epsilon_{U}$
9 epsQepsU.fits EPSQ-EPSU Difference between ISCs $\epsilon_{Q}-\epsilon_{U}$
10 theta.fits THETA Polarization angle $\theta$
11 etheta.fits DELTTHETA Error on polarization angle $\Delta\theta$
12 pzero.fits PZERO Polarization (debiassed) $P$
13 epzero.fits DELTP Error on Polarization (debiassed) $\Delta P$
14 snr.fits S/N Signal-to-noise $S/N$
15 uF.fits FLUXUNBIN Unbinned Flux $F_{\lambda}(unbin)$
16 euF.fits DELTFLUXUNBIN Error on unbinned flux $\Delta F_{\lambda}(unbin)$

Supernova SP types


From Wang & Wheeler (2008), the SP types for SN spectropolarimetry on the Stokes Q-U plane are:
NN0Null polarization
(null)N1No orientation to polarization, but polarization larger than observational errors
DD0Polarization forms elongated ellipse, which can be fit by straight line
(dominant axis)D1ellongated ellipse that cannot be fit with a straight line
LLLoop feature (applies to spectral lines only)
(loop)