Observational evidence of a slow downfall of star formation efficiency in massive galaxies during the past 10 Gyr

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Volume 589 (May 2016)

A&A, 589 (2016) A35

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Table 1

Summary of the various samples.

Sample	Number^a	M _∗	UVJ ^b	IR^c	Robust B/T^d
		M _⊙

Morphological decomposition ( z = 1 )
H-sample	2439	> 2 × 10¹⁰	no	no	2081 (85%)
UVJ-SF	1499	> 2 × 10¹⁰	yes	no	1280 (85%)
IR-sample	946	> 2 × 10¹⁰	yes	yes	783(83%)
IR-sample + good B/T	783	> 2 × 10¹⁰	yes	yes	100%
Gas mass measurement
CANDELS (z = 1)	4 730	> 3 × 10⁹	yes	no	...
HRS (z = 0)	131	> 10⁹	yes	no	...

Notes. We distinguish two sets of samples. First, we list the z = 1 samples we used to study the bulge-to-disk decompositions (Sect. 3). Each step of the selection process corresponds to a different row; the corresponding stellar mass distributions are shown in Fig. 2. Second, we show the two z = 1 and z = 0 samples involved in the gas content measurements (Sect. 4).

^(a)

Number of galaxies in the sample.

^(b)

Indicates if the sample is UVJ-selected.

^(c)

Indicates if the sample is IR-selected, i.e., contains only galaxies individually detected by Spitzer MIPS and/or Herschel.

^(d)

Fraction of the galaxies in the sample with a reliable bulge-to-disk decomposition.

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