Effect of galaxy mergers on star-formation rates

W. J. Pearson; L. Wang; M. Alpaslan; I. Baldry; M. Bilicki; M. J. I. Brown; M. W. Grootes; B. W. Holwerda; T. D. Kitching; S. Kruk; F. F. S. van der Tak

doi:10.1051/0004-6361/201936337

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Volume 631 (November 2019)

A&A, 631 (2019) A51

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Table 1.

Summary of data used.

Data	Resolution	Magnitude limit	Redshift range	Mass limit	Training sample	Complete sample
	(arcsec)			log(M_⋆/M_⊙)	per class	(Mass limited)
SDSS	1.4	17.77	0.005 < z ≤ 0.1	10.1	3003	206 037

KiDS	0.77	19.8 ^(a)	0.00 < z ≤ 0.15	9.6	1917	1270

CANDELS-z000	0.15	24.5	0.00 < z ≤ 0.60	8.3	694 ^(b)	2072
CANDELS-z060	0.15	24.5	0.60 < z ≤ 0.85	8.7	694 ^(b)	2004
CANDELS-z085	0.15	24.5	0.85 < z ≤ 1.21	9.1	694 ^(b)	2031
CANDELS-z121	0.15	24.5	1.21 < z ≤ 1.66	9.4	694 ^(b)	2010
CANDELS-z166	0.15	24.5	1.66 < z ≤ 4.00	9.9	694 ^(b)	1910

Notes. The SDSS and KiDS limiting magnitudes are in r-band while the CANDELS limiting magnitude in H-band.

^(a)

As the training set is derived from GAMA classifications, the limiting magnitude is that of the GAMA survey not that of the KiDS survey.

^(b)

The CANDELS network was trained with 694 galaxies per class for galaxies with 0.00 < z ≤ 4.00. The galaxies were split into the redshift bins shown after classification.

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