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

N. H. P. Rhodin; L. Christensen; P. Møller; T. Zafar; J. P. U. Fynbo

doi:10.1051/0004-6361/201832992

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Volume 618 (October 2018)

A&A, 618 (2018) A129

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Table 3.

Line-flux measurements.

Quasar field	Host galaxy identifiers			Emission-line measurements
	θ^a (")	b^b (kpc)		Transition	λ₀ (Å)	FWHM (Å)	Line-flux (×10⁻¹⁷ erg s⁻¹ cm⁻²)
HE 1122–1649	3.6^c	25.6	0.68249 ± 0.00003	[O II]	3727,3729	6.3 ± 0.7	17.7 ± 2.4
				Hβ	4861.39	6.0 ± 0.5	4.8 ± 0.6
Q 0153+0009	4.9^d	36.6	0.77085 ± 0.00003	H5	4340.47	9.5 ± 1.0	3.0 ± 0.4
				Hβ	4861.33	9.5 ± 0.6	6.3 ± 0.6
				[O III]	5007	9.8 ± 0.5	7.5 ± 0.5
Q 1209+107	7.2^d	38.3	0.39238 ± 0.00001	[O II]	3727,3729	6.7 ± 0.4	41.9 ± 1.5
				H5	4340.47	5.0 ± 0.5	7.0 ± 0.7
				Hβ	4861.33	5.5 ± 0.1	14.8 ± 0.4
				[O III]	4958.91	5.6 ± 0.1	23.3 ± 0.8
				[O III]	5007	5.8 ± 0.2	72.1 ± 3.0
Q 1323–0021	1.4^d	10.2	0.71717 ± 0.00008	[O II]	3727,3729	9.6 ± 1.7	3.1 ± 0.4
Q 1436–0051	6.2^e	45.5	0.73749 ± 0.00003	[O II]	3727,3729	10.2 ± 0.7^g	11.1 ± 0.8^g
				Hβ	4861.33	7.9 ± 1.4	1.5 ± 0.3
				[O III]	5007	17.8 ± 2.7	1.3 ± 0.3
Q 1436–0051	4.4^d	34.9	0.92886 ± 0.00002	[O III]	5007	5.6 ± 0.4	7.0 ± 0.7
Q 2328+0022	1.7^d	11.9	0.65194 ± 0.00006	[O II]	3727,3729	5.5 ± 0.7	7.0 ± 0.7
Q 2335+1501	3.8^f	27.0	0.67989 ± 0.00002	[O II]	3727,3729	6.7 ± 0.4	36.3 ± 1.4
				Hβ	4861.33	6.5 ± 0.2	15.6 ± 6.2

Notes. Values for refer to the heliocentric rest-frame corrected measurement, with the quoted error reflecting the uncertainty in the profile-fit. θ is the angular separation between quasar and host, measured in arcsec. θ is translated into an impact parameter (b) measured in kpc using the the spectroscopically determined emission-line redshift and the assumed cosmology. The fluxes were integrated across the profile, and corrected for Galactic extinction assuming the Galactic E_B−V values reported in Table 1. Full-width-half-maximum (FWHM) measurements have not been corrected for the instrumental resolution.

^(a)

Un-binned angular distance relative to the quasar.

^(b)

Projected distance relative to the quasar, measured at the spectroscopic redshift.

^(c)

Chen & Lanzetta (2003);

^(d)

Rao et al. (2011).

^(e)

This work, based on Rao et al. (2011) K-band image (see Sect. 2.4).

^(f)

This work, FORS2 spectrum.

^(g)

This work, based on the Straka et al. (2016) spectrum (see Sects. 3.3, 3.6, and 3.8).

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