Table 1: Observed emission line fluxes (unit: 10^-14 W m^-2 $\mu$ m^-1) for the most prominent lines which are well separated (no blends). The fluxes were absolute calibrated with respect to the ASAS-3 photometry ( $m_V = 11\hbox{$.\!\!^{\rm m}$ }34$ ) by folding standard filter curves. The main uncertainty originates from the "definition'' of the continuum around the lines.
Line July, 19 ${\rm th}$ 20 ${\rm th}$ 21 ${\rm th}$ 22 ${\rm nd}$

H $_{\alpha }$ 2.1 2.1 2.0 1.8

H $_\beta$ 6.3 5.9 5.5 5.5

H $_\gamma$ overexp. 58.5 66.0 63.4

Fe II 418 nm 1.8 1.7 1.5 1.6

Fe II 423 nm 1.5 1.5 1.2 1.1

Fe II 517 nm 7.7 7.0 7.6 7.2

Fe II 527 nm 2.6 2.2 2.5 2.5

Fe II 532 nm 3.7 3.2 3.7 3.4

N II 464nm 1.6 1.6 1.6 1.5

Na I 589nm 4.6 4.0 3.7 3.7

O I 777nm 7.5 7.7 7.7 7.4

Ca II 849+854nm overexp. 56.3 54.6 48.9

Ca II 866 nm overexp. 27.3 27.3 24.6

**Table 1:** Observed emission line fluxes (unit: 10^-14 W m^-2 $\mu$ m^-1) for the most prominent lines which are well separated (no blends). The fluxes were absolute calibrated with respect to the ASAS-3 photometry ( $m_V = 11\hbox{$.\!\!^{\rm m}$ }34$ ) by folding standard filter curves. The main uncertainty originates from the "definition'' of the continuum around the lines.
Line	July, 19 ${\rm th}$	20 ${\rm th}$	21 ${\rm th}$	22 ${\rm nd}$
H $_{\alpha }$	2.1	2.1	2.0	1.8
H $_\beta$	6.3	5.9	5.5	5.5
H $_\gamma$	overexp.	58.5	66.0	63.4
Fe II 418 nm	1.8	1.7	1.5	1.6
Fe II 423 nm	1.5	1.5	1.2	1.1
Fe II 517 nm	7.7	7.0	7.6	7.2
Fe II 527 nm	2.6	2.2	2.5	2.5
Fe II 532 nm	3.7	3.2	3.7	3.4
N II 464nm	1.6	1.6	1.6	1.5
Na I 589nm	4.6	4.0	3.7	3.7
O I 777nm	7.5	7.7	7.7	7.4
Ca II 849+854nm	overexp.	56.3	54.6	48.9
Ca II 866 nm	overexp.	27.3	27.3	24.6

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