On the origin of [Ne II] emission in young stars: mid-infrared and optical observations with the Very Large Telescope

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Table 4

Results for the [Ne II] line obtained from the VISIR spectra.

[1]	[2]	[3]	[4]	[5]	[6]	[7]
Name	Flux	Spitzer flux^♣	FWHM	Peak^†	v _rad	v_rad Ref.
	(10^-15 erg cm^-2 s^-1)	(10^-15 erg cm^-2 s^-1)	(km s^-1)	(km s^-1)	(km s^-1)

Detected lines
MHO 1	8.0 (1.5)	120^♢	26.7 (3.3)	−121.8 (6.6)	16.0 (6.4)^♠	Bertout & Genova (2006)
V892 Tau	179 (16)	< 180	26.0 (3.4)	−2.13 (6.5)	16.0 (6.4)^♠	Bertout & Genova (2006)
CoKu Tau 1	20.4 (2.5)	120	55.2 (3.3)	3.6 (1.5)	15.0 (0.8)	White & Hillenbrand (2004)
FS Tau A	16.6 (1.7)	77	26.8 (1.7)	−2.9 (0.7)	17.1 (0.1)	This work
SST042936+243555	7.8 (1.7)	11	26.0 (3.8)	−89.1 (6.6)	16.0 (6.4)^♠	Bertout & Genova (2006)
V853 Oph	3.7 (0.8)	16	26.5 (3.9)	−35.8 (1.6)	−8.9 (0.1)	This work
EC 92	4.2 (1.2)	15	16.2 (4.3)	−31.3 (2.3)	−7.1 (1.5)	Covey et al. (2006)

Upper limits
MHO 2	< 0.5	120^♢	...	...	16.0 (6.4)^♠	Bertout & Genova (2006)
XZ Tau	<5.2	32	...	...	17 (7)	Folha & Emerson (2000)
L1551 IRS 5	<4.3	580	...	...	8.2 (1.5)	Covey et al. (2006)
UY Aur A	<2.4	49^♢	...	...	18 (3)	Barbier-Brossat & Figon (1999)
UY Aur B	<1.2	49^♢	...	...	18 (3)	Barbier-Brossat & Figon (1999)
VZ Cha	< 2.3	3.8	...	...	19.0 (1.7)	Torres et al. (2006)
RXJ1111.7-7620	<3.3	5.1	...	...	15.5 (0.3)	Torres et al. (2006)
IRS 60	<1.6	14	...	...	−2.2	Torres et al. (2006)

Notes. The peak is given in the stellocentric frame. Errors are reported between parentheses.

^(♣)

Spitzer fluxes come from Güdel et al. (2010) or Baldovin-Saavedra et al. (2011).

^(†)

The error in the center was calculated considering the contribution of the error in the Gaussian fit and in the stellar radial velocity.

^(♠)

In these cases there is no radial velocity in the literature, the average radial velocity of Taurus was assumed.

^(♢)

The binary systems UY Aur (A, B) and MHO 1/2 cannot be separated in the Spitzer spectrum, therefore the flux reported is for the system.

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