Relativistic supernova 2009bb exploded close to an atomic gas cloud

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Table 2.

M AGPHYS results from the SED fitting.

logL_IR	SFR	sSFR	log M_*	log M_d	τ_V	T_cold	ξ_cold	T_warm	ξ_warm	ξ_hot	ξ_PAH	f_μ	log age_M
L_⊙)	(M_⊙ yr⁻¹)	(Gyr⁻¹)	(M_⊙)	(M_⊙)		(K)		(K)					(yr)
(¹)	(²)	(³)	(⁴)	(⁵)	(⁶)	(⁷)	(⁸)	(⁹)	(¹⁰)	(¹¹)	(¹²)	(¹³)	(¹⁴)

Notes.

⁽¹⁾

8−1000 μm infrared luminosity.

⁽²⁾

Star formation rate from SED modelling.

⁽³⁾

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

⁽⁴⁾

Stellar mass.

⁽⁵⁾

Dust mass.

⁽⁶⁾

Average V-band optical depth (A_V = 1.086τ_V).

⁽⁷⁾

Temperature of the cold dust component.

⁽⁸⁾

Contribution of the cold component to the infrared luminosity.

⁽⁹⁾

Temperature of the warm dust component.

⁽¹⁰⁾

Contribution of the warm component to the infrared luminosity.

⁽¹¹⁾

Contribution of the hot (130–250 K, mid-IR continuum) component to the infrared luminosity.

⁽¹²⁾

Contribution of the PAH component to the infrared luminosity.

⁽¹³⁾

Contribution of the ISM dust (as opposed to birth clouds) to the infrared luminosity.

⁽¹⁴⁾

Mass-weighted age.

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