Introduction

Since their first spectroscopy study (Searle & Sargent 1972) blue compact galaxies (hereafter BCGs) were classified as evolutionary young systems due to the fact of their metal content is many times lower than that of large galaxies. I Zw 18 as the BCG with exceptionally small metallicity (Z = 1/56 Z $_{\odot}$ ) was even suggested as candidate to local truly young galaxy forming its first stellar generation. In fact, great majority of several hundred BCGs with measured abundance of heavy elements have Z in the range of 1/10 to 1/3 of Z $_{\odot}$ . Only a few percent of them have metallicities lower than 1/15 Z $_{\odot}$ (or 12+log(O/H) < 7.74). However namely such galaxies are the most interesting from the point of view the study early chemical evolution of galaxies. Moreover, as demonstrated recently by Izotov and Thuan (1999), namely BCGs with Z lower than 1/20 Z $_{\odot}$ are the best candidates to local young galaxies.

Our group during several recent years is involved in the search for and study of such extremely low-metallicity galaxies. In the frame of this project such interesting objects were discovered as SBS 0335-052 (Izotov et al 1990), 0335-052W (Pustilnik et al. 1997, Lipovetsky et al. 1999) and HS 0822+3542 (Kniazev et al. 1999) with Z in the range 1/50 to 1/36 of Z $_{\odot}$ , that is the most metal-deficient galaxies after I Zw 18. Here we report on the discovery of two new very low-metallicity BCGs, found in the frame of ongoing project The Hamburg/SAO Survey for Emission-Line galaxies (HSS) (Ugryumov et al. 1999, Pustilnik et al. 1999). These galaxies are very nearby and comparatively bright, what makes them very suitable for detailed studies.

**Table 1:** Some observational and derived parameters of new metal-poor BCGs
Value	1013+3809	1442+4250
Right ascention (1950.0)	10^h13^m27.6^s	14^h42^m17.9^s
Declination (1950.0)	+38 $^\circ$ 09 $^\prime$ 43 $^{\prime\prime}$	+42 $^\circ$ 50 $^\prime$ 13 $^{\prime\prime}$
Velocity(hel)(km sec^-1)	1198 $\pm$ 6	780 $\pm$ 42
Distance (Mpc)	20.7	13.1
B-mag	16.5 $^{\dag }$	16.0 $^{\ddag }$
M_B	-15.1	-14.6
12+log(O/H)	7.58 $\pm$ 0.04	7.68 $\pm$ 0.04
Angular size ( $^{\prime\prime}$ )	12 $\times$ 12 $^{\dag }$	60 $\times$ 12 $^{\ddag }$
Linear size (kpc)	1.3 $\times$ 1.3	4.2 $\times$ 0.9
$^{\dag }$ KUG data; $^{\ddag }$ UGC data.

**Figure 1:** DSS-2 images of galaxies HS 1013+3809 (up) and HS 1442+4250 (buttom). The North is up, the East is to left. Isophotes in white show the morphology of the brightest parts.
$\begin{figure}\centerline{% \psfig{figure=HS_1013+3809_2d.ps,height=15cm}} \vs... ...psfig{figure=HS_1442+4250_2d.ps,height=15cm}} \vspace{-4cm} \par\end{figure*}$

**Table 2:** Relative intensities of emission lines in the spectra of HS 1013+3809 and HS 1442+4250 and some derived parameters
	Galaxy
	1013+3809		1442+4250
Ion	F( $\lambda$ )/F(H $\beta$ )	I( $\lambda$ )/I(H $\beta$ )	F( $\lambda$ )/F(H $\beta$ )	I( $\lambda$ )/I(H $\beta$ )
3727 [O II] .....................	0.830 $\pm$ 0.050	0.911 $\pm$ 0.055	0.649 $\pm$ 0.033	0.663 $\pm$ 0.035
4101 H $\delta$ .........................	0.270 $\pm$ 0.013	0.296 $\pm$ 0.021	0.191 $\pm$ 0.005	0.253 $\pm$ 0.009
4340 H $\gamma$ ........................	0.449 $\pm$ 0.012	0.474 $\pm$ 0.017	0.425 $\pm$ 0.010	0.472 $\pm$ 0.013
4363 [O III] ...................	0.114 $\pm$ 0.010	0.118 $\pm$ 0.010	0.123 $\pm$ 0.009	0.121 $\pm$ 0.009
4861 H $\beta$ ........................	1.000 $\pm$ 0.012	1.000 $\pm$ 0.012	1.000 $\pm$ 0.011	1.000 $\pm$ 0.012
4959 [O III] ...................	1.416 $\pm$ 0.016	1.398 $\pm$ 0.016	1.734 $\pm$ 0.021	1.661 $\pm$ 0.021
5007 [O III] ...................	4.303 $\pm$ 0.045	4.233 $\pm$ 0.045	5.076 $\pm$ 0.045	4.852 $\pm$ 0.045
6563 H $\alpha$ ........................	...	...	3.053 $\pm$ 0.028	2.772 $\pm$ 0.029

T_e ...............................	18000 $\pm$ 868		16876 $\pm$ 665
C(H $\beta$ ) dex ....................	0.14 $\pm$ 0.02		0.09 $\pm$ 0.01
F(H $\beta$ )( $\times10^{16})$ erg s^-1cm^-2Å^-1	544		186
EW(H $\beta$ ) Å ....................	117 $\pm$ 1.0		144.6 $\pm$ 1.2
EW(abs) Å ...................	0.65 $\pm$ 0.98		5.65 $\pm$ 0.48
z (obs.)...........................	0.00407 $\pm$ 0.00003		0.00260 $\pm$ 0.00014

**Figure 2:** Spectrum of galaxy HS 1013+3809. The same spectrum in the bottom scaled 1/20 is to show the ratios of strong lines.
**Figure 3:** Spectrum of galaxy HS 1442+4250. The same spectrum in the bottom scaled 1/60 is to show the ratios of strong lines.
$\begin{figure}\par\centerline{% \psfig{figure=HS1013_spec.ps,height=10cm,angle=... ...erline{% \psfig{figure=HS1442_spec.ps,height=10cm,angle=-90}} \par\end{figure}$