Classical Cepheids in the Galactic thin disk - I. Abundance gradients via non-local thermodynamic equilibrium spectral analysis

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Table A.1

Spectroscopic sample.

Spectrograph	N. of spectra	N. of stars	Resolution (R)	Coverage [Å]
HARPS^a	231	29	∼115000	[3790-6900]
SES^b	400	64	∼ 55000	[3860-8800]
FEROS^c	339	161	∼48000	[3500-9200]
UVES^d	373	224	∼40000	[3800-9400]
HARPS-N^e	40	29	∼115000	[3780-6910]
ESPaDOnS^f	16	13	∼81000	[3700-10500]

Notes. ^(a) High Accuracy Radial velocity Planet Searcher (HARPS, Mayor et al. 2003). ^(b) STELLA échelle Spectrograph (SES, Strassmeier et al. 2004, 2010). ^(c) The Fiber-fed Extended Range Optical Spectrograph (FEROS, Kaufer et al. 1999). ^(d) Ultraviolet and Visual Echelle Spectrograph (UVES, Dekker et al. 2000). ^(e) High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (HARPS-N, Cosentino et al. 2012). ^(f) Echelle SpectroPolarimetric Device for the Observation of Stars (ESPaDOnS, Donati et al. 2006).

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