Stellar masses, metallicity gradients, and suppressed star formation revealed in a new sample of absorption selected galaxies

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Volume 618 (October 2018)

A&A, 618 (2018) A129

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Table 1.

Absorber characteristics and photometry of the candidate host galaxies explored with our FORS2 campaign.

Quasar field	E_B−V^⋆	z_abs	log₁₀ [N_H I (cm⁻²)]	[M/H]_abs		z_phot	Filter	Magnitude (AB)	A_λ^⋆ (mag)
Quasar field	E_B−V^⋆	z_abs	log₁₀ [N_H I (cm⁻²)]	Tracer	(dex)	z_phot	Filter	Magnitude (AB)	A_λ^⋆ (mag)
HE 1122-1649	0.0369	0.6819^a	20.45 ± 0.05^a,^b	Fe	−1.40 ± 0.05^b	0.69^c	U	23.19 ± 0.08^c	+0.05^‡
							V	23.01 ± 0.06^c	+0.03^‡
							I	22.33 ± 0.03^c	+0.02^‡
							J	22.10 ± 0.10^c	+0.01^‡
							H	21.72 ± 0.09^c	+0.01^‡
Q 0153+0009	0.0300	0.7714^d	^d, ^e	Cr	−0.52 ± 0.20^e	0.745 ± 0.040^f	u′	24.96 ± 0.70^g	0.15
							g′	24.30 ± 0.38^f	0.11
							r′	23.18 ± 0.24^f	0.08
							i′	22.24 ± 0.18^f	0.06
							z′	21.18 ± 0.50^f	0.04
							J	21.43 ± 0.07^f	0.03
							H	21.39 ± 0.10^f	0.02
							K	21.01 ± 0.07^f	0.01
Q 1209+107	0.0217	0.6295^d	^d	Fe	−0.9± 0.40^h,^†	0.644 ± 0.100^f	g′	r > 21.02^f	–
							i′	21.93 ± 0.11^f	–
							J	21.36 ± 0.06^f	–
							H	20.72 ± 0.05^f	–
							K	19.89 ± 0.03^f	–
		0.3930^d	^d	Zn	0.04 ± 0.20ⁱ	0.3922± 0.0003^j,^⋆⋆	u′	23.21 ± 0.18^f	0.11
							g′	21.55 ± 0.11^f	0.08
							r′	22.68 ± 0.76^f	0.06
							i′	21.48 ± 0.10^f	0.04
							J	22.04 ± 0.11^f	0.02
							H	22.64 ± 0.18^f	0.01
							K	21.83 ± 0.13^f	0.01
Q 1323–0021	0.0232	0.7160^d	^k	Zn	^k	0.182 ± 0.244^f	u′	24.89 ± 0.81^f	0.12
							g′	22.64 ± 0.22^f	0.09
							r′	21.90 ± 0.14^f	0.06
							i′	22.03 ± 0.23^f	0.05
							m_{11200 Å}	20.20 ± 0.15 k	0.02
							m_{13500 Å}	19.90 ± 0.25^k	0.02
							K	19.16 ± 0.13^l	0.01
Q 1436–0051	0.0321	0.7377^d	^d	Zn	−0.05 ± 0.12^m	–	g′	22.49 ± 0.10ⁿ	–
							r′	21.62 ± 0.06ⁿ	–
							i′	20.82 ± 0.05ⁿ	–
							z′	20.69 ± 0.08ⁿ	–
							J	20.19 ± 0.03^f	0.03
							H	19.82 ± 0.03^f	0.02
							K	17.54 ± 0.05^f	0.01
		0.9281^d	18.4± 0.98^o	Zn	−0.05± 0.55^o,^p	–	u′	26.22 ± 1.20^f	0.16
							g′	23.72 ± 0.17ⁿ	–
							r′	22.95 ± 0.12ⁿ	–
							i′	22.14 ± 0.10ⁿ	–
							z′	21.97 ± 0.15ⁿ	–
							J	21.07 ± 0.06^f	0.03
							H	20.80 ± 0.06^f	0.02
							K	18.76 ± 0.15^f	0.01
Q 2328+0022	0.0345	0.6519^d	^d	Zn	−0.49± 0.22^q	0.815 ± 0.242^f	u′	22.60 ± 0.78^f	0.17
							g′	23.23 ± 0.14^f	0.13
							r′	22.61 ± 0.17^f	0.09
							i′	21.37 ± 0.11^f	0.07
							z′	21.01 ± 0.45^f	0.05
							J	>20.04 ± 0.13^f	0.03
							H	>19.23 ± 0.02^f	0.02
							K	>19.89 ± 0.04^f	0.01
Q 2335+1501	0.0598	0.6798^d,^e	19.70 ± 0.30^p	Zn	0.07 ± 0.34^p	–	u′	23.90 ± 0.78^g	0.29
							g′	22.76 ± 0.14^g	0.23
							r′	21.84 ± 0.09^g	0.16
							i′	21.33 ± 0.09^g	0.12
							z′	21.56 ± 0.48^g	0.09
Q 2353–0028	0.0257	0.6044^d	^d,^r	Zn	−0.92 ± 0.32^r	0.844 ± 0.300^f	u′	23.44 ± 0.59^g	0.13
							g′	23.35 ± 0.23^g	0.10
							r′	22.71 ± 0.18^g	0.07
							i′	21.85 ± 0.13^g	0.05
							z′	21.69 ± 0.37^g	0.04
							J	20.48 ± 0.05^f	0.02
							H	20.05 ± 0.04^f	0.01
							K	19.27 ± 0.02^f	0.01

Notes.

^(⋆)

Galactic E_B−V reddening and A_λ towards the absorbing galaxy assuming the Schlafly & Finkbeiner (2011) re-calibrated extinction maps.

^(⋆⋆)

Cristiani (1987) identified emission-lines 2σ from z_abs, 7.1 arcsec from the quasar sightline. Le Brun et al. (1997) resolved the candidate into two interacting objects, the emission lines originating in one of them.

^(†)

Boissé et al. (1998), their Table 6, report a metallicity and introduced a typical uncertainty of 0.1–0.2 dex. Due to a poorly constrained N_HI, we assign a conservative error of 0.40 dex.

^(‡)

The magnitudes in Chen & Lanzetta (2003) were corrected for Schlegel & Finkbeiner Davis (1998) extinctions. Here we report the conversion to the Schlafly & Finkbeiner (2011) maps.

References.

^(a)

de la Varga et al. (2000);

^(b)

Ledoux et al. (2002);

^(c)

Chen & Lanzetta (2003);

^(d)

Rao et al. (2006);

^(e)

Péroux et al. (2008);

^(f)

Rao et al. (2011);

^(g)

Ahn et al. (2014, SDSS DR10);

^(h)

Boissé et al. (1998);

⁽ⁱ⁾

Péroux et al. (2011);

^(j)

Cristiani (1987);

^(k)

Møller et al. (2018);

^(l)

Hewett & Wild (2007);

^(m)

Meiring et al. (2008);

⁽ⁿ⁾

Meiring et al. (2011);

^(o)

Straka et al. (2016);

^(p)

Meiring et al. (2009);

^(q)

Péroux et al. (2006);

^(r)

Nestor et al. (2008)

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