Embedded AGN and star formation in the central 80 pc of IC 3639

J. A. Fernández-Ontiveros; K. R. W. Tristram; S. Hönig; P. Gandhi; G. Weigelt

doi:10.1051/0004-6361/201731906

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Volume 611 (March 2018)

A&A, 611 (2018) A46

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Table 2

Mid-IR spectral lines and diagnostics measured for IC 3639.

Line/diagnostic	Value	Ref.
[Ne V]_14.3/[Ne II]_12.8	0.25 ± 0.01	Tommasin et al. (2008)
	0.33 ± 0.02^a	This work
[O Iv]_25.9/[Ne II]_12.8	0.47 ± 0.01	Tommasin et al. (2008)
	0.63 ± 0.03^a	This work
[O Iv]_25.9/([Ne II]_12.8 + [Ne III]_15.6)	0.29 ± 0.01	Fernández-Ontiveros et al. (2016)
[O Iv]_25.9/[O III]₈₈	0.51 ± 0.02	Fernández-Ontiveros et al. (2016)
EW(PAH_{6.2 μm})	0.185 ± 0.003 μm	Wu et al. (2009)
EW(PAH_{7.7 μm})	1.39 μm	LaMassa et al. (2012)
EW(PAH_{11.3 μm})	0.39 μm	LaMassa et al. 2012
EW(PAH_{17 μm})	0.13 μm	LaMassa et al. (2012)
	0.14	Wu et al. (2009), LaMassa et al. (2012)

	0.29	LaMassa et al. (2012)

S_sil	−0.312	Wu et al. (2009)

	~0.007	This work

	~1.05	This work

Notes. Thetable includes: line ratios, equivalent width (EW) of diverse PAH features, flux ratios of different PAH complexes, strength of the silicate absorption band at 9.7 μm (S_sil ), and ratios of PAH to integrated continuum. ^(a) Using the [Ne ii]_{12.8 μm} flux measured in the VISIR spectrum.

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