Relativistic supernova 2009bb exploded close to an atomic gas cloud

M. J. Michałowski; G. Gentile; T. Krühler; H. Kuncarayakti; P. Kamphuis; J. Hjorth; S. Berta; V. D’Elia; J. Elliott; L. Galbany; J. Greiner; L. K. Hunt; M. P. Koprowski; E. Le Floc’h; A. Nicuesa Guelbenzu; E. Palazzi; J. Rasmussen; A. Rossi; S. Savaglio; A. de Ugarte Postigo; P. van der Werf; S. D. Vergani

doi:10.1051/0004-6361/201732356

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Volume 618 (October 2018)

A&A, 618 (2018) A104

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Table 3.

G RASIL results from the SED fitting.

log L_IR	SFR_IR	SFR_SED	SFR_UV	sSFR_SED	log M_*	log M_dust	log T_dust	A_V	log age_M
(L_⊙)	(M_⊙ yr⁻¹)	(M_⊙ yr⁻¹)	(M_⊙ yr⁻¹)	(Gyr⁻¹)	(M_⊙)	(M_⊙)	(K)	(mag)	(yr)
(¹)	(²)	(³)	(⁴)	(⁵)	(⁶)	(⁷)	(⁸)	(⁹)	(¹⁰)
10.74	5.21	3.69	0.54	0.14	10.43	8.93	21	0.96	9.93

Notes.

⁽¹⁾

8–1000 μm infrared luminosity.

⁽²⁾

Star formation rate from L_IR (Kennicutt 1998).

⁽³⁾

Star formation rate from SED modelling.

⁽⁴⁾

Star formation rate from UV emission (Kennicutt 1998).

⁽⁵⁾

Specific star formation rate (≡SFR_SED/M_*).

⁽⁶⁾

Stellar mass.

⁽⁷⁾

Dust mass.

⁽⁸⁾

Dust temperature.

⁽⁹⁾

Mean dust attenuation at V-band.

⁽¹⁰⁾

Mass-weighted age.

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