RV from multiwaveband galaxy polarimetry in the vicinity of supernovae

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Table 3

Comparison between published R_V from data of SNe and our estimates in the vicinity of SNe within the host.

Supernova	R_V	Reference/method	This work	∆R_V (σ)
2001da	$1.82 \pm_{0.53}^{0.76}$ $1.82 \pm _{0.53}^{0.76}$	Phillips et al. (2013)/(a)	3.94 ± 0.99*	1.70
2006cm	$1.95 \pm_{0.33}^{0.46}$ $1.95 \pm _{0.33}^{0.46}$	Phillips et al. (2013)/(a)	3.43 ± 0.87*	1.50
2007fb	$2.17 \pm_{0.60}^{0.53}$ $2.17 \pm _{0.60}^{0.53}$	Phillips et al. (2013)/(a)	3.68 ± 1.34*	1.05
2007le	$1.3 \pm_{0.2}^{0.3}$ $1.3 \pm _{0.2}^{0.3}$	Burns et al. (2014)/(b)	2.51 ± 0.39	2.46

	$1.7 \pm_{0.2}^{0.2}$ $1.7 \pm _{0.2}^{0.2}$	Burns et al. (2014)/(c)		1.85

2010ev	1.54 ± 0.65	Gutiérrez et al. (2016)/(b)	3.42 ± 0.89*	1.71

	$1.54 \pm_{0.59}^{0.57}$ $1.54 \pm _{0.59}^{0.57}$	(Phillips et al. 2013)/(a)		1.78

2012cg	2.7 ± 0.5	Mandel et al. (2011)/(a)	3.17 ± 0.73*	0.53

	$2.6 \pm_{0.7}^{0.8}$ $2.6 \pm _{0.7}^{0.8}$	Amanullah et al. (2015)/(b)		0.53

	$2.7 \pm_{0.7}^{0.9}$ $2.7 \pm _{0.7}^{0.9}$	Amanullah et al. (2015)/(c)		0.40

	$1.7 \pm_{0.6}^{0.8}$ $1.7 \pm _{0.6}^{0.8}$	Amanullah et al. (2015)/(c′)		1.36

	$3.6 \pm_{1.0}^{1.5}$ $3.6 \pm _{1.0}^{1.5}$	Amanullah et al. (2015)/(c″)		0.35

Notes. Methods listed are: (a) fit of SN colors at peak with Markov chain Monte Carlo; (b) fit of SN colors at peak following (O’Donnell 1994); (c) fit of SN colors at peak following (Fitzpatrick 1999); (c′) same as (c), but at [−5; +5] days from maximum subsample; and (c″) same as (c), but at [+10;+20] days after the maximum subsample. In the fourth column, the estimate for R_V is shown, fit with the Serkowski relation to HG photopolarimetryin the vicinity of SNe. An asterisk (*) indicates the use of INLA for spatial inference using the values obtained through the method presented in Section 4.

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