Host galaxies of SNe Ic-BL with and without long gamma-ray bursts

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Table A.1.

Geometric properties of the host galaxies: the axial ratio b/a, the position angle PA (measured with respect to the north in the counter clockwise direction) and the inclination i.

SN/GRB	b/a	PA (deg)	i (deg)	offset_depr (kpc)
SN2005ks	0.31 ± 0.05	−10 ± 4	76	2.12
SN2005nb	0.41 ± 0.02	38 ± 3	69	6.14
SDSS-IISN14475	0.11 ± 0.18	−5 ± 10	–	^*
SN2006nx	0.74 ± 0.04	75 ± 10	43	5.69
SN2007bg	–	–	–	–
SN2007ce^a	<1	58 ± 13	0	0.65^†
	0.72 ± 0.04	10 ± 3	45	4.00
SN2007I	0.61 ± 0.01	−36 ± 2	54	1.68
PTF10aavz	0.56 ± 0.05	76 ± 2	56	5.57
SN2010ah	0.14 ± 0.01	7 ± 1	–	^*
SN2010ay	0.61 ± 0.06	60 ± 5	54	0.24
PTF10qts	0.79 ± 0.15	49 ± 30	40	2.07
PTF10vgv	0.45 ± 0.02	45 ± 2	66	2.02
PTF10xem	0.48 ± 0.03	−40 ± 5	64	6.51
PTF11cmh	0.73 ± 0.05	−52 ± 10	44	5.82
PTF11lbm	0.20 ± 0.02	−71 ± 1	–	^*
PTF12as	0.79 ± 0.03	−78 ± 30	39	3.65
PTF13alq	<0.15	45 ± 25	0	0.90^†
PTF13ebw	0.45 ± 0.02	−27 ± 2	66	10.92
PTF13u	0.83 ± 0.01	37 ± 7	35	13.86
LSQ14bef	0.24 ± 0.01	−78 ± 2	82	8.08
PTF14dby	<1	50 ± 140	0	0.75^†
PTF14gaq	0.62 ± 0.05	−85 ± 7	53	5.75
iPTF15dld^a	<1	−85 ± 151	0	0.20^†
	0.17 ± 0.02	−42 ± 2	–	^*
SN2016coi	0.76 ± 0.02	−42 ± 4	42	2.95
SN2016dst	–	–	0	1.08^†
SN2017dcc	0.58 ± 0.01	−78 ± 3	56	4.06
SN2017fgk	0.30 ± 0.01	61 ± 1	77	0.82

GRB 980425	0.84 ± 0.02	−14 ± 2	34	2.33
GRB 030329	0.77 ± 0.05	−82 ± 3	39	0.93
GRB 031203A	0.83 ± 0.03	87 ± 5	35	0.62
GRB 060218	<1	46 ± 30	0	0.08^†
GRB 100316D	–	–	0	2.48^†
GRB 130702A	0.54 ± 0.02	20 ± 3	59	0.92
GRB 161219B	0.11 ± 0.05	26 ± 3	–	^*
GRB 171205A	0.81 ± 0.01	−62 ± 5	43	7.82

Notes. The calculated deprojected offset (with respect to the centre of the galaxy) is given in the final column. We do not provide errors for i and offset_depr due to large uncertainties introduced in the measurement of the former.

^(*)

Galaxy is not included in the deprojection study because b/a < 0.2.

^(†)

Galaxy assumed to be a spheroid observed at i = 0, i.e. no deprojection is applied to the offset.

^(a)

The first line corresponds to the measurement assuming the host galaxy is only the bright (blue) region near the SN explosion. The second line is obtained in cases where the host galaxy is the whole complex.

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