WR 35a: A new double-lined spectroscopic binary | Astronomy & Astrophysics (A&A)

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Table 1

Details of the observations.

Obs. run	n	Sp. coverage	Observat.	Telesc.	Spectr.^a	Grating	Dispersion	Resolution^b
UT		[Å]		[m]		[l mm^-1]	[Å pix^-1]


Feb., 1998	1	3940–5600	CASLEO	2.15	REOSC	600	1.63	1000
Apr., 2000	3	3940–5600	CASLEO	2.15	REOSC	600	1.63	1000
Apr., 2001	1	3940–5600	CASLEO	2.15	REOSC	600	1.63	1000
Mar.–Apr., 2007	5	3650–6700	CTIO	4	R-C	632	1.01	1300
Apr., 2008	1	3650–6700	CTIO	4	R-C	632	1.01	1300
Mar., 2009	1	4030–5590	CASLEO	2.15	REOSC	600	1.63	1000
Mar.–Jun., 2009	3	4120–6930	Gemini	8.1	GMOS	B600	0.92	1500
May, 2009	1	4470–5920	Gemini	8.1	GMOS	B1200	0.48	3000
Apr., 2010	3	4040–5700	CASLEO	2.15	REOSC	600	1.63	1000
Apr., 2011	2	3930–5600	CASLEO	2.15	REOSC	600	1.63	1000
Jan.–Feb., 2013	7	3920–6730	Gemini	8.1	GMOS	B600	0.92	1400
May, 2013	1	4030–5590	CASLEO	2.15	REOSC	600	1.63	1000

Notes.(n): Number of spectra obtained per run.

^(a)

Details of the spectrographs can be found in the User’s Manuals of the respective Observatories.

^(b)

The spectral resolutions (R = λ/Δλ) were measured using Δλ as the FWHM of the calibration lamp emission lines.

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