182
                                                                                                                                          
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We indicate the dust masses obtained using the graphite model in parenthesis for comparison.

[^1]: See http://www.apex-telescope.org/bolometer/laboca/calibration/ for details on the calibration and archive tables of sky opacities and calibration factors.

[^2]: BoA was developed at MPIfR (Max-Planck-Institut fŸr Radio Astronomy, Bonn, Germany), AIfA (Argelander-Institut f[ü]{}r Astronomie, Bonn, Germany), AIRUB (Astronomisches Institut der Ruhr-Universit[ä]{}t, Bochum, Germany), and IAS (Institut d’Astrophysique Spatiale, Orsay, France)

[^3]: http://www.astro.princeton.edu/$\sim$ganiano/Kernels.html for kernels and details on their construction.

[^4]: We note that estimating this total dust mass on a resolved scale (resolved masses added together) allows us to probe the various dust components in ISM elements with low-dust mass surface densities as well as in dense regions. Contrary to dust mass estimates derived from a global SED modelling of the region, we can avoid potential biases (namely a dust mass underestimation) caused by a poorer resolution [c.f. discussion about biases caused by non-linearities in SED models in @Galliano2011].

[^5]: c.f. further discussions about opacities in @Galliano2011, Appendix A


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abstract: 'Let $s,n \ge 2$ be integers. We give a qualitative structural description of every matroid $M$ that is spanned by a frame matroid of a complete graph and has no $U_{s,2s}$-minor and no rank-$n$ projective geometry minor, showing that every such matroid is ‘close’ to a frame matroid. We also give a similar description of every matroid $M$ with a spanning projective geometry over a field $\GF(q)$ as a restriction and with no $U_{s,2s}$-minor and no $\PG(n,q'')$-minor for any $q'' > q$, show