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Table 1.

Instruments used in this study.

Telescope Instrument Filters Platescale Field of view Epoch Min./Max. Ref.
[pixel−1]
CTIO (Blanco) Flaugher+10 g, r, i, z, y 027 1.1° radius 2014–2018 (1)
KPNO (Mayall) NEWFIRM J, H, Ks 04 28′ × 28′ 2015 (2)
CFHT MegaCam r, i 018 1° × 1° 2005–2015 (3)
CFHT WIRCam y, J, H, Ks 03 20′ × 20′ 2007–2008 (4)
CFHT CFH12K I, z 021 42′ × 28′ 1999–2002 (5)
INT WFC u, v, b, β, y (Strömgren), U, B, V, Z, g, r, i(a) 033 34′ × 34′ 2000–2015 (6)
UKIRT WFCAM J, Ks 04 40′ × 40′(b) 2006–2012 (7)
LCO Swope Direct CCD i 043 15′ × 14′ 2013 (8)
VST OmegaCam r 021 1° × 1° 2014 (9)
ESO (2.2 m) WFI R, I(a) 024 34′ × 33′ 2002 (10)
Subaru HSC y 017 1.8° radius 2015 (11)
Palomar 48″ PTF g, r 10 33 × 22 (c) 2010–2012 (12)
OMM (1.6 m) CPAPIR I, J, H 089 30′ × 30′ 2012–2015 (13)

Notes.

(a)

As well as various narrow and medium bands.

(b)

The chip layout has large gaps between detectors, and the coverage of the focal plane is only partial

(c)

One of the 12 detectors is dead.

References. (1) Flaugher et al. (2010); (2) Autry et al. (2003); (3) Boulade et al. (2003); (4) Thibault et al. (2003); (5) Cuillandre et al. (2000); (6) Ives (1998); (7) Casali et al. (2007); (8) Rheault et al. (2014); (10) Baade et al. (1999); (11) Miyazaki et al. (2018); (12) Rahmer et al. (2008); (13) Thibault et al. (2002).

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