Table 2. Open in new tab We show that...

	QSO	Stars	Non-id
J − W1 > 1.5	98 per cent (3583)	22 per cent(126)	92 per cent(1311)
J − W1 < 1.5	2 per cent (2)	78 per cent(460)	8 per cent(111)
J − W1 > 2	83 per cent	13 per cent	80 per cent
J − W1 < 2	17 per cent	87 per cent	20 per cent

	QSO	Stars	Non-id
J − W1 > 1.5	98 per cent (3583)	22 per cent(126)	92 per cent(1311)
J − W1 < 1.5	2 per cent (2)	78 per cent(460)	8 per cent(111)
J − W1 > 2	83 per cent	13 per cent	80 per cent
J − W1 < 2	17 per cent	87 per cent	20 per cent

Table 2.

We show that the distribution in the J − W1 colour for spectroscopic quasars, stars and non-ids. At two different cuts, the distribution of the non-ids more closely follows that for quasars. As such, we infer that the greater part of the non-identified sources are quasars that are not positively identified by our spectroscopic observations.

	QSO	Stars	Non-id
	(0.8 < z < 2.5)
J − W1 > 1.5	98 per cent (3583)	22 per cent(126)	92 per cent(1311)
J − W1 < 1.5	2 per cent (2)	78 per cent(460)	8 per cent(111)
J − W1 > 2	83 per cent	13 per cent	80 per cent
J − W1 < 2	17 per cent	87 per cent	20 per cent

	QSO	Stars	Non-id
	(0.8 < z < 2.5)
J − W1 > 1.5	98 per cent (3583)	22 per cent(126)	92 per cent(1311)
J − W1 < 1.5	2 per cent (2)	78 per cent(460)	8 per cent(111)
J − W1 > 2	83 per cent	13 per cent	80 per cent
J − W1 < 2	17 per cent	87 per cent	20 per cent

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