Table 4: The FWHM of the Br $\gamma$ line compared with that of the hydrogen Pf25 line. The Pf23 line is stronger than the Pf25, but this line is heavily contaminated by residuals of atmospheric lines. For the fitting of 18006nr766 the Pf23 line is used, because Pf25 is not detected. In the last column the flux-ratio of Br $\gamma$ and Pf25 is listed.
Object
FWHM Br $\gamma$ FWHM Pf25 Pf25/Br $\gamma$

(km s^-1) (km s^-1)

08576nr292 220 $\pm$ 2 - -

11097nr1218 191 $\pm$ 3 - -

07299nr618 138 $\pm$ 2 - -

16164nr3636 132 $\pm$ 1 273 $\pm$ 8 0.3

18006nr766 99 $\pm$ 1 282 $\pm$ 13 0.1

06412nr121 147 $\pm$ 1 269 $\pm$ 7 0.2

15411nr1955 106 $\pm$ 1 140 $\pm$ 37 0.08

16571nr1281 204 $\pm$ 1 328 $\pm$ 8 0.2

**Table 4:** The *FWHM* of the Br $\gamma$ line compared with that of the hydrogen Pf25 line. The Pf23 line is stronger than the Pf25, but this line is heavily contaminated by residuals of atmospheric lines. For the fitting of 18006nr766 the Pf23 line is used, because Pf25 is not detected. In the last column the flux-ratio of Br $\gamma$ and Pf25 is listed.
Object	FWHM Br $\gamma$	FWHM Pf25	Pf25/Br $\gamma$
	(km s^-1)	(km s^-1)
08576nr292	220 $\pm$ 2	-	-
11097nr1218	191 $\pm$ 3	-	-
07299nr618	138 $\pm$ 2	-	-
16164nr3636	132 $\pm$ 1	273 $\pm$ 8	0.3
18006nr766	99 $\pm$ 1	282 $\pm$ 13	0.1
06412nr121	147 $\pm$ 1	269 $\pm$ 7	0.2
15411nr1955	106 $\pm$ 1	140 $\pm$ 37	0.08
16571nr1281	204 $\pm$ 1	328 $\pm$ 8	0.2

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