Designing future dark energy space missions - I. Building realistic galaxy spectro-photometric catalogs and their first applications

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Volume 504 / No 2 (September III 2009)

A&A, 504 2 (2009) 359-371

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Table 4:

Characteristics of the three surveys discussed in the text, assuming an efficient 1.5 m space telescope with an obscuration of 0.6 m and a total telescope throughput (CCD, mirror, grism) of 70% using a survey efficiency of 75%.
	DEEP-vis-NIR	DEEP-NIR	WIDE-NIR
probe	WL	WL	BAO
$T_{\rm obs}$	240 ks	240 ks	1200 s
$\lambda$ in $\mu$ m	0.6-1.7	1-1.7	1-1.7
3 $\sigma$ at 1.2 $\mu$ m	$5\times 10^{-18}$	$5\times 10^{-18}$	$1\times 10^{-16}$
		ergs cm^-2 s^-1
area needed	10 deg²	10 deg²	20 000 deg²
mission time	0.2 yrs	0.2 yrs	2 yrs
		FOV of 0.5 deg²
nbr density (5 $\sigma$ )	60	35	5
		gal/arcmin²
z[1line $3\sigma$ ]	0<z<3.5	0.5<z<3.5	0.5<z<1.5
$m_{\rm lim}$ [1line $3\sigma$ ]	$I\sim 27$	$I\sim 26.5$	$H\sim 22$
%[1line $3\sigma$ ] Ell	40	27	0
%[1line $3\sigma$ ] Sac	60	51	1
%[1line $3\sigma$ ] Sdm	77	63	10
%[1line $3\sigma$ ] SB	95	74	45

The %[1line $3\sigma$ ] Ell represent the percentage of Elliptical galaxies spectroscopically found using a success criterion of 1 line detected at $3\sigma$ compared to the total population of Elliptical galaxies. With the same criterion, we define the percentage of Sac for early spiral galaxies, Sdm for late spiral galaxies, and SB for starburst galaxies.

Source LaTeX | All tables | In the text

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