The environmental dependence of the stellar mass function at z ~ 1 - Comparing cluster and field between the GCLASS and UltraVISTA surveys

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Volume 557 (September 2013)

A&A, 557 (2013) A15

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Table 1

Ten GCLASS clusters selected from SpARCS for follow-up spectroscopic and photometric observations.

Name^a	z _spec	RA	Dec	K_s-band IQ	K_lim^b	M _⋆ ,lim^c	Limit from bc03^d
		J2000	J2000	PSF FWHM [′′]	[mag_AB]	[M_⊙]

SpARCS-0034	0.867	00:34:42.086	–43:07:53.360	1.01	21.53	10.42	10.43
SpARCS-0035	1.335	00:35:49.700	–43:12:24.160	0.40	23.60	9.92	9.95
SpARCS-0036^e	0.869	00:36:45.039	–44:10:49.911	1.23(J)	22.11(J)	10.53	10.50
SpARCS-0215	1.004	02:15:23.200	–03:43:34.482	1.00	21.73	10.45	10.46
SpARCS-1047^f	0.956	10:47:32.952	57:41:24.340	0.61	22.68	10.17	10.04
SpARCS-1051^f	1.035	10:51:05.560	58:18:15.520	0.86	22.96	9.99	9.99
SpARCS-1613	0.871	16:13:14.641	56:49:29.504	0.81	22.55	9.97	10.02
SpARCS-1616	1.156	16:16:41.232	55:45:25.708	0.84	22.65	10.33	10.20
SpARCS-1634	1.177	16:34:35.402	40:21:51.588	0.77	22.88	10.14	10.13
SpARCS-1638	1.196	16:38:51.625	40:38:42.893	0.66	23.00	10.13	10.09

Notes. These clusters form the basis of this study.

^(a)

For full names we refer to Muzzin et al. (2012).

^(b)

80% completeness limit for simulated sources.

^(c)

Corresponding mass completeness limit based on the galaxy in UltraVISTA with the highest M/L fitted at this redshift at K_lim.

^(d)

Mass limit from a synthetic spectrum with τ = 10 Myr starting at age of universe at that redshift with no dust (Bruzual & Charlot 2003).

^(e)

For SpARCS-0036 we used to J-band as the selection band since it is significantly deeper than the K_s-band. The image quality and magnitude limits refer to the J-band for this cluster.

^(f)

Since the BCG is offset from the centre, this is a better approximation for the cluster centre (different from Muzzin et al. 2012).

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