Searching for transits in the Wide Field Camera Transit Survey with difference-imaging light curves

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Table 13

List of extremely-short period M-dwarf eclipsing binary systems found in this work.

Object	α	δ	Period (days)	t ₀	dp/dp	J	u	g	r	i	z	(r − i)	(i − z)	rms(AP)	rms(DI)

19c3-12753	294.3839	36.9062	0.1859752355	2 454 317.8449795	1.56	17.87	24.93	22.80	21.09	20.08	19.17	1.01	0.91	0.041	0.028
19b2-04235	293.3342	36.4255	0.1974392134	2 454 317.9485581	1.52	17.32	22.68	22.07	20.16	19.43	18.77	0.74	0.66	0.027	0.023
19c2-10801	294.2404	36.3471	0.1977343597	2 454 317.9436689	0.88	17.78	25.86	21.37	20.24	19.66	19.36	0.59	0.29	...	0.049
19e3-11606	293.2310	36.6396	0.2106563732	2 454 317.7894282	1.45	17.97	25.01	21.71	20.31	19.67	19.40	0.65	0.26	0.062	0.050
19c1-00478	293.8732	36.4661	0.2261831592	2 454 317.8755733	1.57	17.18	23.53	20.44	19.40	18.70	18.35	0.69	0.36	0.028	0.022

Notes. Extremely-short period M-dwarf eclipsing binary systems with periods below 0.23 days. We list the period, epoch, eclipse depth ratio, the WFCAM J-band, and SDSS ugriz photometry for each candidate. The last two columns provide information on the 4σ clipped rms of the light curves after removing the periodic signal. In general, the precision of the DI light curves is significantly better than the precision of the AP light curves. This is due to the fact that all objects are fainter than 17 mag in the J-band, which is in the regime where DI light curves present an improvement over AP light curves (see Sect. 3).

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