Potential scientific synergies in weak lensing studies between the CSST and Euclid space probes

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Table 1.

Designed performance of CSST, Euclid, LSST, and DES.

Telescope/	Band	λ_eff	Δλ (FWHM)	Detection limit	Pixel scale	PSF size
project		(Å)	(Å)	(mag)	(arcsec)	(arcsec)
CSST ^(a)	NUV	2880	694	25.4		0.135
	u	3726	866	25.4		0.135
	g	4734	1455	26.3		0.135
	r	6107	1417	26.0	0.074	0.135
	i	7548	1465	25.9		0.145
	z	8975	1082	25.2		0.165
	y	9606	542	24.4		0.165

Euclid^(b)	VIS	6726	3699	24.5	0.1	0.18
	Y	10 678	2665	24.0	0.3	0.62
	J	13 333	4052	24.0	0.3	0.63
	H	17 328	5023	24.0	0.3	0.70

LSST ^(c)	u	3734	623	26.1		0.81
	g	4731	1427	27.4		0.77
	r	6139	1359	27.5		0.73
	i	7487	1247	26.8	0.2	0.69
	z	8671	1022	26.1		0.68
	y	9677	855	24.9		0.71

DES ^(d)	g	4734	1295	24.7		1.11
	r	6342	1485	24.4		0.95
	i	7748	1480	23.8	0.263	0.88
	z	9139	1475	23.1		0.83
	y	9880	660	21.7		0.90

Notes.

^(a)

The detection limits are the 5σ limiting magnitudes of point sources and the PSF sizes are the radii at 80% encircled energy (Zhan 2021);

^(b)

For Euclid VIS band, the detection limit is the 10σ limiting magnitude of extended sources and the PSF size is defined as the FWHM, while for Euclid NIR bands, the limits are the 5σ limiting magnitudes of point sources and the PSF sizes are the radii at 80% encircled energy (Laureijs et al. 2011);

^(c)

The detection limits for LSST bands are the 5σ depth of point sources after ten year observations and the PSF sizes are the FWHM (Ivezić et al. 2019);

^(d)

The detection limits for DES bands are the 10σ depth of point sources and the PSF sizes are the FWHM (Abbott et al. 2021).

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