The deeply obscured AGN of NGC 4945 - I. Spitzer-IRS maps of [Ne V], [Ne II], H2 0−0 S(1), S(2), and other tracers

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Volume 533 (September 2011)

A&A, 533 (2011) A56

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Table 1

Line fluxes^a from the 10 × 10 pixel (~426 × 426 pc²) aperture IRS/SH map.

Line	λ ₀ ^b	Flux^c	Flux(A_V)^d	FWHM ^e
	[μm]	[10^-21 W cm^-2]	[10^-21 W cm^-2]	[km s^-1]

[S IV]	10.5105	1.61	22.03	382.68
[S IV]		0.08	1.12	30.54

H₂ 0−0 S(2)	12.2786	154.07	889.94	525.66
H₂ 0−0 S(2)		1.99	11.57	6.23

[Ne II]	12.8135	1201.08	6026.69	615.54
[Ne II]		118.85	563.35	32.37

[Ne V]	14.3217	5.34	27.93	584.70
[Ne V]		0.53	0.64	15.44

[Cl II]	14.3678	12.82	66.75	502.97
[Cl II]		0.10	0.53	4.04

[Ne III]	15.5551	127.01	741.49	640.81
[Ne III]		2.79	18.03	12.74

H₂ 0−0 S(1)	17.0348	252.60	1781.25	549.60
H₂ 0−0 S(1)		7.64	63.90	18.12

[S III]	18.7129	74.87	618.00	562.71
[S III]		1.37	10.90	9.59

Notes.

^(a)

Obtained from the co-added spectra of the whole 10 × 10 aperture of the SH map described in Sect. 3.

^(b)

Rest wavelength of the lines.

^(c)

The flux densities of each line are given in the first row. The row below shows the corresponding uncertainties.

^(d)

Flux density corrected for extinction using an average extinction value A_V ~ 36 mag estimated from the silicate-based A_V(9.85 μm) (Sect. 3.4). For [Ne V] this extinction correction may be insufficient. See Sect. 4.4.

^(e)

Line width in km s^-1 obtained from the Gaussian fit. The line profile is not corrected for the instrumental profile, which has an FWHM of 500 km s^-1.

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