A new massive double-lined spectroscopic binary system: The Wolf-Rayet star WR 68a

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Volume 581 (September 2015)

A&A, 581 (2015) A49

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Table 1

Details of the observing material.

Date-obs.	n	Sp. coverage	Observat.	Telesc.	Spectr.^a	Grating	Detector	Dispersion	Resolving^b
UT		[Å]		[m]		[l mm^-1]		[Å pix^-1]	power

2007, Mar. 30	2	3650−6700	CTIO	4	R−C	632	Loral 3k	1.01	1300
2007, Apr. 1−3	4	3650−6700	CTIO	4	R−C	632	Loral 3k	1.01	1300
2008, Apr. 19−23	7	3650−6700	CTIO	4	R−C	632	Loral 3k	1.01	1300
2008, Jun. 16	1	3650−6750	LCO	6.5	IMACS f/4	600	SITe (Mosaic 1)	0.4	3300
2009, Mar. 24−27	7	4030−5590	CASLEO	2.15	REOSC SD	600	Tek1024	1.63	1000
2009, Jul. 23	1	3890−5520	LCO	2.5	B−C	1200	Marconi#1	0.79	2500
2009, Jul. 26	1	3540−6700	LCO	2.5	B−C	600	Marconi#1	1.55	1200
2009, Jul. 27	1	3890−5520	LCO	2.5	B−C	1200	Marconi#1	0.79	2500
2009, Aug. 14−17	3	4040−5700	CASLEO	2.15	REOSC SD	600	Tek1024	1.63	1000
2010, Apr. 10−11	2	3930−5600	CASLEO	2.15	REOSC SD	600	Tek1024	1.63	1000
2010, Aug. 2−8	4	3930−5600	CASLEO	2.15	REOSC SD	600	Tek1024	1.63	1000
2011, Apr. 6−11	2	3930−5600	CASLEO	2.15	REOSC SD	600	Tek1024	1.63	1000
2013, May 12	1	3930−5600	CASLEO	2.15	REOSC SD	600	Tek1024	1.63	1000

Notes. “n”: number of spectra taken per run.

^(a)

Details of the spectrographs can be found in the user manuals of the respective observatories.

^(b)

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

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