Astronomy & Astrophysics manuscript no. 24414a c ESO 2015 January 20, 2015

The VLT-FLAMES Tarantula Survey XVIII. Classifications and radial velocities of the B-type

C. J. Evans1, M. B. Kennedy2, P. L. Dufton2, I. D. Howarth3; N. R. Walborn4, N. Markova5, J. S. Clark6, S. E. de Mink7,8,9?, A. de Koter7,10, P. R. Dunstall2, V. Henault-Brunet´ 11, J. Ma´ız Apellaniz´ 12??, C. M. McEvoy2, H. Sana13, S. Simon-D´ ´ıaz14,15, W. D. Taylor1, J. S, Vink16

1 UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK 2 Department of Physics & Astronomy, Queen’s University Belfast, Belfast BT7 1NN, Northern Ireland, UK 3 Dept. of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 Institute of Astronomy with NAO, Bulgarian Academy of Sciences, PO Box 136, 4700 Smoljan, Bulgaria 6 Department of Physics & Astronomy, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK 7 Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH, Amsterdam, The Netherlands 8 Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA 9 Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 10 Institute voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium 11 Department of Physics, Faculty of Engineering & Physical Sciences University of Surrey Guildford, GU2 7XH, UK 12 Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18008 Granada, Spain 13 ESA/STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA 14 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 15 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 16 Armagh Observatory, College Hill, Armagh, BT61 9DG, UK

ABSTRACT

We present spectral classifications for 438 B-type stars observed as part of the VLT-FLAMES Tarantula Survey (VFTS) in the 30 Doradus region of the . Radial velocities are provided for 307 apparently single stars, and for 99 targets with radial-velocity variations which are consistent with them being spectroscopic binaries. We investigate the spatial distribution of the radial velocities across the 30 Dor region, and use the results to identify candidate runaway stars. Excluding potential runaways and members of two older clusters in the survey region (SL 639 and ), we determine a systemic velocity for 30 Dor of 271.6 ± 12.2 km s−1 from 273 presumed single stars. Employing a 3-σ criterion we identify nine candidate runaway stars (2.9 % of the single stars with radial-velocity estimates). The projected rotational velocities of the candidate runaways appear to be significantly dif- ferent to those of the full B-type sample, with a strong preference for either large (≥ 345 km s−1) or small (≤ 65 km s−1) rotational ve- locities. Of the candidate runaways, VFTS 358 (classified B0.5: V) has the largest differential radial velocity (−106.9 ± 16.2 km s−1), and a preliminary atmospheric analysis finds a significantly enriched nitrogen abundance of 12 + log (N/H) & 8.5. Combined with a −1 large rotational velocity (ve sin i = 345 ± 22 km s ), this is suggestive of past binary interaction for this . Key words. open clusters and associations: individual: NGC 2060, NGC 2070, Hodge 301, SL 639 – stars: early-type – stars: funda- mental parameters

1. Introduction cal information on the high-mass population of 30 Dor, which will underpin quantitative analyses of the spectra in future pa- The VLT-FLAMES Tarantula Survey (VFTS) is a European pers. Detailed classifications for the 352 O-type spectra (with Southern Observatory (ESO) Large Programme that has ob- discussion of notable morphological groups) were presented by tained multi-epoch optical spectroscopy of over 800 massive Walborn et al. (2014), while classifications for the smaller sam- stars in the 30 Doradus region of the Large Magellanic Cloud

arXiv:1501.04108v1 [astro-ph.SR] 16 Jan 2015 ples of Wolf–Rayet and late-type stars were given in Paper I. (LMC). An overview of the survey, including details of the stel- Here we present spectral classifications for 438 B-type objects lar photometry, spectroscopic observations and data reduction, from the survey. Of these, only 74 (17%) have previously pub- was given by Evans et al. (2011; hereafter Paper I). lished classifications based on digital data, many of which were The VFTS observations are the first optical spectroscopy for obtained at a lower spectral resolving power. many of the targets, and provide a wealth of new morphologi- To complement the spectral classifications, we also present Send offprint requests to: C. J. Evans at [email protected] estimates of radial velocities for the B-type sample. These es- ? Einstein Fellow timates provide insights into the different populations within ?? Current address: Departamento de Astrof´ısica, Centro de 30 Dor, and enable identification of candidate runaway stars that Astrobiolog´ıa (INTA-CSIC), Campus ESA, Apartado Postal 78, have been ejected from their birth sites. In the context of run- 28 691 Villanueva de la Canada,˜ Madrid, Spain away stars, the size of the VFTS sample is unprecedented for a

1 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars single, young star-forming region. The survey has revealed ∼20 For stars that appear to be single (Dunstall et al., in prep.) O-type runaway candidates (Evans et al. 2010, Sana et al., in the LR02 and LR03 spectra were normalised then merged, with prep.), with an apparent connection with rapid rotation (Walborn the σ-clip levels for cosmic rejection and relative weightings et al. 2014, Sana et al., in prep.). There are also a number of stars based on the signal-to-noise (S/N) ratios of the individual spec- with moderate (projected) rotational velocities in the peripheral tra. Finally, for classification, the merged LR02 and LR03 spec- regions of 30 Dor, which could perhaps be very rapid rotators tra were combined, then smoothed and rebinned to R = 4 000. (but with low inclinations; see Walborn et al. 2014, for a dis- For stars identified as having significant but relatively modest ve- −1 cussion of their spectra). For completeness, we note that two locity variations (∆ vr ≤ 40 km s ), the individual spectra were additional O2-type stars near 30 Dor, Sk−68◦ 137 and BI 253 similarly co-added and degraded (as the variations were within ( = VFTS 072), were suggested as runaways by Walborn et al. the effective velocity resolution of the rebinned data). For single- −1 (2002a) on the basis of their remote locations for their apparent lined binaries with ∆ vr > 40 km s , the single-epoch LR02 youth. and LR03 spectra with the best S/N ratio were combined and In his pioneering study, Blaauw (1961) noted that the frac- then smoothed/rebinned. We were careful in these cases to en- tional incidence of Galactic runaways is larger among O stars sure that any velocity offsets between features in the small over- than among B stars, a result substantiated by subsequent authors, lap region between the LR02 and LR03 data were not misinter- and which also emerged in the simulations from Portegies Zwart preted. The small number of double-lined binaries were classi- (2000). In this paper we therefore complement the studies of the fied from inspection of the individual spectra. O-type runaways in the VFTS with analysis of the B-type stars. In particular, the number and mass spectrum of the ejected run- aways from 30 Dor will provide important constraints on models 3. Spectral classification of cluster formation and evolution (e.g. Fujii & Portegies Zwart 2011). The estimated radial velocities presented here, combined The spectra were classified by visual comparison to the B-type with those from the O-type stars (Sana et al. 2013), will also pro- Galactic standards from Sota et al. (2011) and Sana et al. (in vide an important input for comparisons with theoretical predic- prep.), while also taking into account the effects of the reduced tions, e.g. in the context of simulations to investigate the initial metallicity of the LMC compared to the (which can af- conditions leading to the distinct clump identified to the north- fect the appearance of both the metal and helium absorption east of (Sabbi et al. 2012). lines; e.g. Markova et al. 2009). This was achieved for the lu- In Section 2 we summarise the relevant features of the VFTS minous, low-gravity objects by interpolating between the avail- data and their post-processing. Section 3 sets out the framework able Galactic standards and those for supergiants in the Small within which the spectra were classified and discusses notable Magellanic Cloud (Lennon 1997), and with reference to the objects. Section 4 details the methods we used to estimate radial framework developed for the LMC by Fitzpatrick (1988, 1991). velocities for each target, followed by a discussion of members Classifications of the dwarfs and giants were also informed by of the two oldest clusters in the survey region (Hodge 301 and comparisons with the standards from Walborn & Fitzpatrick SL 639) in Section 5. Finally, in Section 6, we use our velocity (1990) and the LMC stars classified by Evans et al. (2006). estimates to identify candidate single-star and binary runaways The primary diagnostic lines are the ionisation ratios of sil- and discuss their nature and potential origins. In parallel to this icon, while also taking into account the appearance of the he- study, Dunstall et al. (in prep.) have exploited the multi-epoch lium and magnesium (λ4481) lines. For reference, the primary VFTS observations to investigate the multiplicity properties of temperature-sequence criteria used to classify the VFTS sample the B-type sample. are summarised in Tables 1 and 2 (for supergiants and dwarfs, respectively). Example temperature sequences for supergiants, giants and dwarfs are shown in Figures A.1, A.2 and A.3, re- 2. Observations and data processing spectively. At a given spectral type, luminosity classes were as- All of the VFTS data discussed here were obtained using signed from the width of the Balmer lines and (at the earliest the Medusa–Giraffe mode of the Fibre Large Array Multi- types) from the intensity of the silicon absorption lines, while Element Spectrograph (FLAMES) instrument on the Very Large also taking into account the possible effects of rotational broad- Telescope (VLT). The Medusa fibres (which subtend 100. 2 on the ening on the spectra. Example luminosity sequences for B0.2, sky) were used to relay light from up to 130 targets simultane- B1, and B2.5 types are shown in Figures A.4, A.5, and A.6, re- ously to the Giraffe spectrograph (see Pasquini et al. 2002). spectively. Full details of the observational strategy and reduction of the The supergiants and bright giants (i.e. class I and II objects) data are given in Paper I. In brief, the ESO Common Pipeline have rich absorption-line spectra. Given the importance of spec- Library FLAMES recipes were used to undertake bias sub- tral peculiarities in the context of CNO abundances, and the in- traction, fibre location, summed extractions of each object, di- fluence of metallicity effects, these luminous objects were classi- vision by a normalised flat-field, and wavelength calibration. fied independently by three of the authors (CJE, NM, and NRW) Subsequent processing included correction of the spectra to the with a typical consistency of 0.5 subtypes/luminosity class from heliocentric frame, sky subtraction, and rejection of significant the first pass; final types were adopted following discussion of cosmic rays. individual objects as required. The larger sample of dwarfs and The Medusa observations used three of the standard Giraffe giants, which exhibited a considerable range in data quality, was settings (LR02, LR03, and HR15N), providing spectral cover- classified by CJE. In many instances these classifications are less age of λ3960-5071 A˚ (at resolving powers, R, of 7 000 to 8 500), precise than those possible for the luminous objects, but they and λ6442-6817 A˚ (at R = 16 000). These resolutions are greater should provide sufficient morphological information to enable than for most published standards so, for the purposes of classifi- robust subdivisions of the sample in future analyses. cation, the data were degraded to an effective resolving power of Each merged spectrum was classified in the framework de- R = 4 000, ensuring consistency with the approach to the classi- scribed above. After initial classification of all the spectra, care- fication of the O-type stars by Walborn et al. (2014). ful checks were undertaken to ensure self-consistency within

2 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Table 1. Primary temperature-sequence criteria for B-type supergiants. 3.1. Emission-line objects + Type Criteria Where appropriate, spectra were initially classified as ‘Be ’ on the basis of Fe II emission lines in the LR02 and LR03 spectra B0 Si IV λλ4089, 4116 >> Si III λ4553 > He II λ4542 B0.2 Si IV λ4089 > Si III λ4553 >> He II λ4542 (see discussion by Evans et al. 2006); the Fe II lines were pre- B0.5 Si IV λ4089 > Si III λ4553; He II λ4542 absent/marginal ferred over the blue-violet Balmer lines owing to the significant B0.7 Si IV λ4089 ∼ Si III λ4553; He II λ4686 absent/marginal (and variable) contamination of the latter by nebular emission. B1 Marginal Si IV λ4116; Si III λ4553 > Si IV λ4089 Independently of the blue-region classifications, we in- B1.5 Weak/marginal Si IV λ4089, weak Mg II λ4481 spected the Hα profiles of every target to investigate their mor- B2 Si III λ4553 > Mg II λ4481; Si IV λ4089 absent phologies. The greater resolution of the Hα observations and the B2.5 Si III λ4553 ∼ Mg II λ4481; weak Si II λλ4128-32 extended wings from disc emission made it easier to distinguish B3 Si III λ4553 < Mg II λ4481; Si II λλ4128-32 present contributions from Be-type Balmer emission and nebular con- B5 He I λ4471 > Mg II λ4481; Si II λλ4128-32 ∼ He I λ4121 tamination than in the blue, but these classifications should still B8 He I λ4471 ∼ Mg II λ4481; Si II λλ4128-32 ∼ He I λ4144 B9 He I λ4471 < Mg II λ4481; Si II λλ4128-32 > He I λ4144 be treated with some caution. The Hα morphologies are encoded in the fourth column of Table 7 (with the notation explained in Notes. Example spectra are shown in Figure A.1. the corresponding footnote). Objects classified as ‘Be+’ from the LR02/LR03 spectra were seen to display Hα emission in all cases. Approximately 30 additional stars display Be-like Hα emission without Fe II Table 2. Primary temperature-sequence criteria for B-type dwarfs. emission. The Hα emission in luminous supergiants most likely arises from their stellar winds, but for less luminous objects such Type Criteria emission is the primary Be diagnostic. To preserve the distinc- B0 Si IV λ4089 > Si III λ4553> He II λ4542 tion of the lines seen in emission, the standard ‘e’ suffix is used B0.2 Si IV λ4089 > Si III λ4553; He II λ4542 marginal B0.5 He II λ4542 absent; Si III λ4116 marginal/absent in the classifications for the (non-supergiant) stars where only B0.7 He II λ4686 marginal/absent; Si III λ4116 marginal/absent Hα is seen in emission. B1 Si III λ4553 > Si IV λ4089; Si IV λ4116, He II λ4686 absent The complex star-formation history of 30 Dor means that B1.5 Si IV λ4089 absent; Si III λ4553 ∼ Mg II λ4481 our sample will span a range of stellar ages, so we are unable to B2 Si III λ4553 < Mg II λ4481 comment on the incidence of the Be-phenomenon for a single, B2.5 Si III λ4553 absent; Si II λλ4128-32 marginal co-eval population. Nonetheless, we note that the incidence of the Be-type classifications for the dwarf and giant stars is 18% Notes. Example spectra are shown in Figure A.3. (70/388 objects). This is in good agreement with the Galactic fraction (≥ 17%, Zorec & Briot 1997), and that reported for the field population near NGC 2004 in the LMC (of 16 and 17.5%, from Evans et al. 2006 and Martayan et al. 2006, respectively). the sample. An overlapping sample of ten B0-type stars was classified independently (by NRW) for the study by Walborn 3.1.1. B[e]-type spectra et al. (2014), with excellent agreement (to within one luminosity Two targets in the Medusa–Giraffe sample show forbidden-line class) in all instances. emission characteristic of the B[e] category. VFTS 698 is a The catalogue of classifications and radial-velocity estimates double-lined binary system with a B[e]-like spectrum, compris- for the B-type objects from the VFTS is presented in Table 7 ing what appears to be an early B-type secondary in orbit around (available online). For convenience, supplementary information a veiled, more massive companion (see Dunstall et al. 2012). is also provided for each star on its binary status (from Dunstall The second B[e] object is VFTS 822, shown in Figure 2 together et al., in prep.), Hα morphology (see Section 3.1), optical pho- with VFTS 1003 (the B[e]-like object from Paper I). Given the tometry (from Paper I), alternative identifications used in the lit- intensity of its Si II λλ4128-32 and Mg II λ4481 absorption, the erature, and previous spectral classifications. spectrum of VFTS 822 was classified as mid-late B[e] (∼B5-8); The S/N ratios of the supergiant spectra were particularly further discussion of its possible pre-main-sequence nature was good (typically > 100 for both the LR02 and LR03 regions; given by Kalari et al. (2014). see Figure A.1). This allowed us to provide consistent indi- Although the nature of VFTS 1003 remains uncertain at cations of the nitrogen enhancement/deficiency compared to present, the number of evolved B[e] stars (at most two) in the morphologically-normal stars (via Nstr and Nwk qualifiers), as VFTS is clearly small compared to the number of normal super- diagnosed from the CNO absorption features in the λλ4640- giants. This is in keeping with the small number of sgB[e] stars 4650 region (Walborn 1976). The significant differences in in Galactic clusters (see the appendix of Clark et al. 2013), argu- CNO morphology are illustrated by the two B1.5 Ia spectra in ing that the B[e] phenomenon in evolved supergiants must be a Figure 1. Atmospheric analysis of the supergiants, including es- relatively brief phase or originate from a rare process. timates of nitrogen abundances and a thorough study of the line- broadening in their spectra, will be presented by McEvoy et al. (2015) and Simon-D´ ´ıaz et al. (in prep.), respectively. 3.1.2. VFTS 766: A peculiar emission-line star Given the wide range in quality of the dwarf and giant spec- VFTS 766 displays strong Hα emission and inspection of its tra, we do not comment on CNO morphologies in their classifi- blue-region spectrum (see Figure 2) revealed it as a peculiar ob- cations. Equally, while we employ the ‘n’ and ‘(n)’ indications ject. At first glance its spectrum appears to be that of a mid-late of broadening (see e.g. Table 3 from Sota et al. 2011) at all lumi- B-type supergiant (B5-B8, as traced by e.g. Si II, Mg II), but nosity classes, there are likely to be some lacunae (cf. the quan- with superimposed metallic absorption lines, which are consis- titative ve sin i estimates from Dufton et al. 2013). tent with a cooler component. This seemingly composite appear-

3 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. 1. Differing CNO morphologies in early B-type supergiants illustrated by VFTS 431 (‘Nstr’) and VFTS 578 (‘Nwk’). In addition to the Balmer lines, the absorption features identified are: C II λ4267; He I λλ4009, 4026, 4121, 4144, 4388, 4471, 4713; Mg II λ4481; N II λλ3995, 4601-07-14-21-31, 4640-43 (blended with O II); O II λλ4070, 4254, 4317-19, 4350, 4367, 4414-17, 4591-96, 4650, 4661, 4674-76; Si III λλ4553- 68-74. ance can indicate a circumstellar shell or disc observed edge-on, supergiant phase and are about to enter a luminous blue variable and this hypothesis is supported by the twin-peaked Hβ shell- (LBV) phase (Clark et al. 2012; Groh et al. 2014). This suggests like emission profile. Its near- and mid-IR colours1 place it in that VFTS 003, 430, and 533 might be on the verge of LBV- the region in the J, J − [3.6] colour-magnitude diagram which like behaviour, although we note that VFTS 430 appears some- is occupied by early-type stars associated with free-free/bound- what subluminous compared to the blue supergiants in 30 Dor, free emission, and we find no evidence of hot dust (cf. Bonanos and is significantly fainter than VFTS 533 (even accounting for et al. 2009). its apparently greater line-of-sight extinction, see photometry Similar emission profiles are observed in some low- in Table 7). Later-type BHGs have been observed to undergo luminosity supergiant B[e] stars (e.g. S59, Gummersbach et al. LBV-like photometric and spectroscopic behaviour (e.g. Smith 1995), with examples that also appear to lack dusty discs (Graus et al. 2004; Clark et al. 2012, with potential implications for et al. 2012, although none have yet been discovered in the edge- VFTS 424 and 458 here), suggesting that these two evolution- on orientation required to yield shell profiles). However, we ary phases are essentially synonymous for such stars. speculate that VFTS 766 is a classical Be star, in which the twin- peaked emission in the wings of the Balmer profiles gives rise to the supergiant-like appearance. An example of this effect is the On further inspection of their spectra, broad emission wings development of a circumstellar disc in the classical edge-on Be were identified in the Hβ profiles of each of the BHGs, except for star o And, which conspires to yield a narrower absorption fea- VFTS 430. This Hβ morphology is seen in some LBVs and other ture than the underlying photospheric profile (Clark et al. 2003). luminous supergiants (e.g. Walborn & Fitzpatrick 2000), and is Another example is provided by the Be star 48 Lib (see Rivinius also present in VFTS 739 in our sample (classified as A0 Ip but, et al. 2013, and references therein), which has previously been given its omission from Paper I, included here in the B-type classified as a supergiant (Houk & Smith-Moore 1988). sample). The spectra and evolutionary status of these potential This possible explanation for the nature of VFTS 766 is sup- LBV precursors/candidates will be discussed in more depth by ported by its magnitude relative to other stars in our sample. Walborn et al. (in prep.). Spectroscopic monitoring to identify an episode of disc loss, dur- ing which the (uncontaminated) photospheric Balmer line pro- files might be observed, would clarify its luminosity type and true evolutionary status. 3.1.4. Comparisons with X-Ray observations

3.1.3. Blue hypergiants We compared our sample with the point-source detections from We identifed five blue hypergiants (BHGs) in our sample, observations in 30 Dor with the Chandra X-ray Observatory namely: VFTS 003 (B1 Ia+), 424 (B9 Ia+p), 430 (B0.5 (Townsley et al. 2006, 2014); none of the VFTS B-type stars Ia+((n)) Nwk), 458 (B5 Ia+p) and 533 (B1.5 Ia+p Nwk). Recent is detected in the extant X-ray data. A new X-ray Visionary theoretical and observational studies suggest that early-type Project is now underway, ‘The Tarantula Revealed by X-rays (T- BHGs might be massive stars which have passed through a blue ReX)’, which will observe 30 Dor with Chandra for 2 Ms. This will push far deeper than the existing data, and we will revisit 1 VFTS 766: J = 15.14, H = 15.01, Ks = 14.76 (from Paper I); the VFTS sample once the T-ReX observations and analysis are [3.6] = 14.28, [4.5] = 14.06, [5.8] = 13.64 (from Meixner et al. 2006). complete.

4 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. 2. Spectra of three peculiar Be-type stars from the VFTS, in which each spectrum has been smoothed and rebinned to R = 4 000 for clarity. In addition to the Balmer lines, the emission lines identified in VFTS 1003 are [S II] λ4069; Fe II λλ4173, 4179, 4233, 4303, 4352, 4385, 4481, 4491, 4508, 4515, 4520-23, 4549, 4556; [Fe II] λλ4244, 4277, 4287, 4358-59, 4414-16. Emission lines identified in VFTS 822 are Fe II λλ4584, 4620.5, 4629. Absorption lines identified in VFTS 766 are He I λλ4009, 4026, 4121, 4144, 4388, 4471, 4713; Si II λλ4128-32; Mg II λ4481.

4. Stellar radial velocities Following the approach taken by Dufton et al. (2013), we used different sets of diagnostic lines (as summarised in Table 3) de- 4.1. Single stars pending on the ve sin i of the star. −1 Radial-velocity estimates for the stars identified as apparently For narrow-lined spectra (defined as ve sin i . 150 km s ), single by Dunstall et al. (in prep.) were obtained from Gaussian we used three non-diffuse He I lines and four isolated metal lines fits to selected absorption lines in the merged LR02 and LR03 listed as ‘Set 1’ in Table 3. Where possible, radial velocities were spectra of each object (at the native resolution of the data, with- estimated from Si III λ4553 in both the merged LR02 and LR03 out the degrading applied for classification purposes). This ap- spectra, giving up to eight individual estimates for the narrow- proach is consistent with that used by Sana et al. (2013) for lined objects. analysis of the O-type stars, albeit (necessarily) using a different We note that He I λ4121 is potentially affected by blending subset of absorption lines. We note that the choice of Gaussian with O II λλ4120.28/54. In many instances these features could profiles may not be appropriate for fitting the wings of the lines be resolved and a double Gaussian profile was fitted to estimate in the presence of different broadening mechanisms, but they the He I and O II line centres; in cases where the O II lines were should suffice for robust estimates of the centres of our chosen weaker or unresolved, they do not appear to have unduly influ- lines. enced the results (see Table 3, in which the residual for He I We also considered a cross-correlation method to estimate λ4121 is consistent with the other lines). the radial velocities. However, given the range in temperature Radial-velocity estimates for stars with broader lines were and luminosity of the sample, as well as the varying data quality more difficult, particularly for spectra with significant nebular and problems of nebular contamination, the selection of suitable contamination. In these cases, velocities were estimated by fit- template spectra for cross-correlation was not trivial and would ting the five He I lines listed as ‘Set 2’ in Table 3, for which the have introduced additional uncertainties (relating to e.g. the pro- profiles are expected to be effectively symmetric2. jected rotational velocities, ve sin i). Thus, we did not pursue this approach further. Representative examples are shown in Figure 3. The lower panel shows fits to the Si III triplet for two narrow-lined stars, VFTS 053 and 159, which have ve sin i ≤ 40 (i.e. less than the 4.1.1. Line selection velocity resolution of the data) and 96 ± 9 km s−1, respectively (from Dufton et al. 2013). As an example of a spectrum of a v sin i The large range in e and effective temperature for the sam- rapidly-rotating star which also suffers nebular contamination, ple meant that it was not possible to use a single set of diagnostic lines for all stars. Moreover, the large intrinsic width and nebu- 2 3 3 lar contamination of the Balmer lines precluded their use; sim- He I P → D transitions were excluded because of the presence of ilarly, nebular emission affects some of the stronger He I lines. significant 3P → 3F components.

5 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Table 3. Rest wavelengths used to estimate radial velocities (vr) for the narrow- and broad-lined stars (Sets 1 and 2, respectively). Values in the final column are average differences (∆) between the velocity estimates for each line and the final velocity for each star.

Ion λ[A]˚ ∆ [km s−1] Set 1 He I 4120.82 −0.8 ± 6.7 C II 4267.13 1.1 ± 5.1 He I 4437.55 −0.4 ± 5.4 Si III 4552.62 0.3 ± 6.1 (LR02) −1.6 ± 5.8 (LR03) Si III 4567.84 −0.8 ± 6.4 Si III 4574.76 −1.7 ± 7.0 He I 4713.15 2.1 ± 4.5 Set 2 He I 4009.26 −0.8 ± 11.3 He I 4143.76 0.1 ± 9.0 He I 4387.93 2.7 ± 9.1 He I 4713.15 2.8 ± 7.1 He I 4921.93 −3.5 ± 8.7

Notes. Wavelengths are taken from the NIST atomic spectra database (Kramida et al. 2012); the adopted value for C II is the average of the two stronger transitions.

the upper panel of Figure 3 shows the Gaussian fit to He I λ4388 −1 for VFTS 636 (ve sin i = 371 ± 35 km s ; Dufton et al. 2013). For three stars with later/peculiar types – VFTS 272 (possi- ble shell star), 739 (A0 Ip), and 766 (B5-8e, see Section 3.1.2) – we employed weak Fe II and Ti II absorption lines to estimate ve- locities, although we note that in VFTS 272 and 766 they might Fig. 3. Examples of Gaussian fits used to estimate radial velocities (vr) not be representative of the true (stellar) radial velocity, as these for the B-type sample. Upper panel: Fit to He I λ4388 in a rapidly- lines could trace cooler features associated with a disc of mate- rotating object (VFTS 636) with nebular contamination. Lower panel: rial (see e.g. the discussion of VFTS 698 by Dunstall et al. 2012). Fits to the Si III triplets (λλ4553-68-74) of VFTS 053 and 159.

4.1.2. Mean velocities Radial-velocity estimates for the single stars were obtained by calculating an average of the n individual measurements (vi), VFTS, finding excellent agreement between our velocity es- weighted by the estimated central depth (di) from the Gaussian timates and those from Sana et al. (2013, see discussion in fit of each line, i.e. Section A.2.1). We also investigated the internal consistency of our results from the selected lines by calculating the average dif- Pn i = 1 vi di ference (∆) of the individual measurements for each line com- vr = Pn . (1) i = 1 di pared to the adopted mean velocity for each target. The means and standard deviations of these differences are given in col- The sample standard deviation (σ) for each star was similarly umn 3 of Table 3, with no significant shifts seen for any of the calculated as a weighted average: diagnostic lines compared to the adopted radial velocities. Pn 2 2 i = 1(vi − vr) di σ = Pn . (2) i = 1 di 4.2. Radial velocities of the binaries In cases where the central depths of the absorption lines were To complement the analysis of the single stars, we also inves- less than twice the inverse of the continuum S/N ratio, the in- tigated the radial velocities of the single-lined binaries in the dividual estimates were excluded from the above calculations sample. We obtained single-epoch velocity estimates (vsingle) for (to avoid their larger uncertainties degrading the results from each system using measurements from the best LR02 spectra (in stronger lines). For stars with estimates from three (or more) terms of S/N ratio of the co-added exposures from a given night, absorption lines, we present their estimated mean velocities and which span three hours at most). standard deviations in columns 7 and 8 of Table 7. For complete- Given the reduced spectral coverage of the LR02 data com- ness, the line-by-line estimates from Sets 1 and 2 for the single pared to the full LR02 + LR03 range, we used all of the available stars are detailed in Tables A.1 and A.2, respectively; the mean lines from Table 3 to estimate vsingle (except for He I λ4121, uncertainty of the estimates for the 307 (presumed) single stars given the nearby O II feature and the lower S/N ratio of the is 7.8 km s−1 (and with a median uncertainty of 6.2 km s−1). single-epoch spectra compared to the quality of the co-added As a check on our results, we used the methods described spectra of the single stars). Line-by-line estimates and the date above to analyse a sample of the late O-type stars from the for which they were measured are listed in Table A.3. Mean ve-

6 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars locities and standard deviations for the selected epoch were then From analysis of (HST) imaging, estimated using the same methods as for the single stars. Grebel & Chu (2000) estimated Hodge 301 to be 20-25 Myr The mean single-epoch velocities serve as an absolute ref- old. From narrow-band imaging they also identified 19 Be-type erence point for the inter-epoch differential velocities calculated stars, eight of which (VFTS 272, 276, 279, 282, 283, 287, 293, by Dunstall et al. (in prep.) yielding absolute estimates for each and 301) have spectroscopy from the VFTS. The Hα spectra of epoch. We then calculated the mean and standard deviation of each of these contain significant nebular emission (with mul- the multi-epoch estimates to obtain a velocity estimate for each tiple components in all sightlines except towards VFTS 293). single-lined binary. These values are presented in Table 7, and Nonetheless, broad Be-like Hα emission is present in each ob- are flagged as ‘B’ (binary) in the ninth column. We note that the ject, except for VFTS 276 (GC00-Be2). typical uncertainty on the cross-correlation results from Dunstall Grebel & Chu (2000) noted two potential blue stragglers in et al. was less than 5 km s−1, while the typical error on the ab- the cluster, which they argued were too luminous for the main- solute estimates determined here from the single-epoch data was sequence population (but less luminous than expected for su- 9 km s−1; i.e. the uncertainties in our estimates will generally be pergiants). The first, VFTS 270 (WB97-2), is a seemingly unre- dominated by the analysis presented here. markable B3 Ib star. The second is VFTS 293 (WB97-9, GC00- Full orbital solutions are presently unavailable for the B-type Be1), classified here as B2 III-II(n)e. From two previous ob- binaries, so we strongly caution the reader that the velocity esti- servations, Walborn & Blades (1997) noted small shifts of its mates in Table 7 are not their centre-of-mass, systemic velocities absorption features (relative to superimposed nebular emission) (although, as discussed in the Appendix, in many instances they and possible weak He II λ4686 emission at one epoch. If the may provide reasonable estimates). He II emission were real, Walborn & Blades speculated that it might be an X-ray binary. There is no evidence of λ4686 emis- sion in the LR03 FLAMES spectra (albeit all taken on the same 4.3. Spatial distribution night, see Paper I), but small line-profile variations are seen in the absorption features in the multi-epoch LR02 spectra. In addition to NGC 2070 (the main 30 Dor cluster, which in- More intriguing is VFTS 310 on the periphery of the clus- cludes R136 at its core) and NGC 2060 (the association to the ter and classified as O9.7 V: (Walborn et al. 2014). With such a south-west), there are two smaller clusters in the VFTS sur- classification, VFTS 310 would be expected to be significantly vey: Hodge 301 (Hodge 1988) and SL 693 (Shapley & Lindsay younger than the other cluster members, as shown by its loca- 1963); their relative locations are shown in Figure 4. Both clus- tion in the Hertzsprung–Russell (H–R) diagram of the cluster ters appear older than NGC 2060 and 2070 as they contain (Figure 5, see Section 5.3 for details). The star appears oth- evolved supergiants, from B- through to M-types. erwise unremarkable, with a low projected rotational velocity We calculated weighted mean velocities (v , and their stan- r v sin i ≤ −1 dard deviations) for the full sample of single stars, for the ( e 40 km s , Dufton et al. 2013) and a radial veloc- v = ± −1 subsamples associated with the four distinct stellar assocations ity ( r 272.3 2.8 km s , Sana et al. 2013) which is con- in the survey region (NGC 2060, NGC 2070, Hodge 301, and sistent with those in NGC 2070 and the local field population. SL 639, as defined in Table 4), and for the field population of Moreover, it does not appear to be a runaway from Hodge 301 stars outside the four clusters. These results, which exclude can- (see Section 6). Whether this is a true blue straggler or simply a didate runaway stars (see Section 6), are summarised in Table 4. line-of-sight coincidence remains uncertain at this time. The results for the two younger star-forming regions (i.e. NGC 2060 and 2070) are in excellent agreement with the field 5.2. SL 639 population of B-type stars in the region, but the two older clus- 00 ters (Hodge 301 and SL 639) appear at slightly lower recession Adopting a 20 radius (∼4.9 pc), sixteen of the VFTS targets velocities, suggesting that they are kinematically distinct from are within SL 693. Fourteen are in the B-type sample, with their 4 the rest of the sample. The weighted mean velocity for the membership of SL 639 indicated in the final column of Table 7 . 273 single stars excluding these two clusters (and potential run- Ten of these stars are early-B dwarfs/giants, with six of them dis- aways) is v = 271.6 ± 12.2 km s−1. playing Be-like Hα emission. The remaining four are comprised r of two supergiants (VFTS 827, B1.5 Ib; VFTS 831, B5 Ia) and two bright giants (VFTS 826, B1 IIn; VFTS 829, B1.5-2 II). 5. Spectral content of the older clusters There are previous age estimates for SL 693. From consider- ation of its main-sequence turn-off, Hodge (1983) estimated its The VFTS data comprise the first comprehensive spectroscopy age to be 18 Myr (although he noted a large uncertainty com- in Hodge 301 and SL 639, so we briefly discuss these clusters in pared to the theoretical models of the time). A larger estimate turn. of 30 Myr was given by Santos et al. (1995) from its reddening- corrected, integrated (U − B)0 colour and adopting an empirical calibration of colour vs. age from Bica et al. (1990). 5.1. Hodge 301 00 There are 20 VFTS targets within a 20 radius (chosen to conser- 5.3. H–R diagram vatively identify likely members, and corresponding to ∼4.9 pc, assuming a distance modulus of 18.5 mag). Fifteen of these were Motivated by the apparent similarities of the two clusters in classified as B-type and their likely membership of the cluster is terms of their spectral content, we constructed an H–R dia- indicated in the final column of Table 73. 4 The two others are VFTS 820 and 828 (A0 Ia and Early M, respec- 3 The five others are: VFTS 310 (O9.7 V:, Walborn et al. 2014) and tively, from Paper I). The only other VFTS target within a 3500 (8.5 pc) VFTS 271, 281, 289, and 294 (A7 II, Mid-late K, Late G/Early K, and radius is VFTS 839 at ∼2500 (6 pc), classified as G-type in Paper I. All A0 Ib, respectively, from Paper I). Three additional stars (VFTS 263, three of these cooler objects have radial velocities consistent with mem- 291, and 317) are also nearby, at radii from the adopted centre of ∼2500. bership of the LMC.

7 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. 4. Spatial distribution of the B-type single stars (cyan circles) and spectroscopic binaries (open blue squares) with radial-velocity estimates; the nine candidate runaways, labelled by their VFTS identifiers, are marked in red. The spatial extents of NGC 2070, NGC 2060, SL 639, and Hodge 301 (as defined in Table 4), are indicated by the overlaid dashed circles. The underlying image is from a V -band mosaic taken with ESO’s Wide Field Imager on the 2.2 m telescope at La Silla.

gram in order to compare the properties of their likely members. The H–R diagram is shown in Figure 5, with SL 639 and Ahead of detailed quantitative analysis of the VFTS spectra and Hodge 301 members indicated by the filled black and open red pending extinction analysis of the whole sample, we adopted ef- circles, respectively. Evolutionary tracks and isochrones (for fective temperatures (Teff ) on the basis of the spectral types in non-rotating models) from Brott et al. (2011) are also plotted for Table 3 using the calibrations of Trundle et al. (2007), and in- comparison. As noted earlier, the late O-type star in Hodge 301, terpolating between the Galactic and SMC temperatures for A- VFTS 310, stands out as a blue straggler with Teff > 30 kK. type supergiants from Evans & Howarth (2003); cooler objects Tailored atmospheric and extinction analyses of these ob- were omitted given the larger uncertainties in their spectral clas- jects should help to provide further insight in due course. sifications. Stellar luminosities were estimated using the opti- Nonetheless, the stars in SL 639 appear marginally younger cal photometry from Paper I, intrinsic colours from Fitzgerald than those in Hodge 301. From qualitative comparison with the (1970), bolometric corrections from Balona (1994), and assum- isochrones, we estimate an age in the range of 10-15 Myr for ing RV = 3.5 (see Appendix C of Doran et al. 2013). SL 639, significantly younger than the estimate of 30 Myr from Santos et al. (1995). There is a larger spread in the inferred ages

8 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Table 4. Mean radial velocities ( vr ) and standard deviations (σ) of the stellar associations identified within 30 Doradus.

Region No. of stars Radius α δ vr ± σ [0] [J2000.0] All 298 ...... 270.4 ± 12.4 NGC 2070 78 2.40 05 38 42.0 −69 06 02.0 271.2 ± 12.4 NGC 2060 22 2.40 05 37 45.0 −69 10 15.0 273.7 ± 13.4 Hodge 301 14 0.33 05 38 17.0 −69 04 01.0 261.8 ± 5.5 SL 639 11 0.33 05 39 39.4 −69 11 52.1 253.5 ± 3.9 Field 173 ...... 271.3 ± 11.8 All (excl. H 301/SL 639) 273 ...... 271.6 ± 12.2

Notes. These statistics exclude the nine candidate runaways identified in Table 5. For consistency, the central positions adopted for NGC 2060 and NGC 2070 are those used by Sana et al. (2013). Approximate centres for Hodge 301 and SL 639 were adopted using the coordinates of WB97-5 (Walborn & Blades 1997) and VFTS 828, respectively.

NGC 2060, NGC 2070, and the surrounding field population (i.e. excluding Hodge 301 and SL 639). Employing a threshold of |δvr| > 3σ we identified eight candidate runaways and then re- calculated the mean velocities (and dispersions) excluding these objects. Reapplying a 3-σ threshold provided one additional can- didate, while a second iteration did not reduce the velocity dis- persion further. The mean velocities and dispersions for the dif- ferent spatial samples (excluding potential runaways) are pre- sented in Table 4. The cumulative distribution of the velocity estimates for the 307 single stars is shown in Figure 6, with the ±3σ threshold (i.e. ±36.6 km s−1) for identification of runaway stars indicated by the vertical dotted lines. Our adopted velocity threshold is comparable in magnitude to the limit used by Blaauw (1961), which was that candidate runaways have a space velocity which differs by more than 40 km s−1 from the systemic velocity of the region in which they formed. (In this context, our radial-velocity estimates should serve as lower limits to the 3-D space velocities.) In contrast, Portegies Zwart (2000) adopted a lower threshold of 25 km s−1 in his theoretical study of the origins and characteristics of run- aways. Given the limitations of the B-type data and the relatively small number of lines available for some objects, we did not con- sider a comparably low threshold. Details of the nine candidate runaways are summarised in Fig. 5. Hertzsprung–Russell diagram for the VFTS objects observed in Table 5, and their locations are shown in Figure 4. Four of SL 639 (black circles) and Hodge 301 (red, open circles). Also plotted the candidates have differential velocities in the range of 3.2- are evolutionary tracks for initial masses of 8, 10, 12, 15, 20, 25 M 3.6 σ, thus their status as candidates will depend strongly on the (solid lines), the zero-age main sequence (dashed line), and isochrones adopted velocity criteria. Moreover, our adopted velocity thresh- (3, 5, 10, 15, 20, and 25 Myr, dotted lines) for the non-rotating mod- els from Brott et al. (2011). The apparent blue straggler in Hodge 301 old (the dispersion of the weighted mean velocities in the sam- (VFTS 310) is a late O-type star. ple) was employed without consideration of the uncertainty on the radial-velocity estimate for a given star. Thus, VFTS 467, al- though formally with a radial velocity of 4.2σ from the systemic value, has a large uncertainty on its estimated velocity. Indeed, for the stars in Hodge 301 of 15 ± 5 Myr, overlapping with the only three He I lines were available for this star and the λ4144 lower estimate of 20 Myr from the photometric study of Grebel estimate (277.5 km s−1) is comparable to the systemic value. & Chu (2000). Adopting isochrones calculated for the rotating models from Brott et al. had little impact on these results; e.g. The choice to use weighted means to investigate the assuming an intial rotational velocity of 301 km s−1, the inferred spatially-different samples in Section 4.3 was motivated by the ages were only marginally younger (by ∼1 Myr). fact that approximately 10 % of our velocity estimates have un- certainties of ≥ 15 km s−1 (each of which is a broad-lined star, i.e. used the Set 2 lines from Table 3). To investigate the de- 6. Candidate runaways pendence of the number and identity of the candidate runaways on these adopted means, we repeated the above steps for both 6.1. Single stars the (unweighted) mean and median velocities of the sample. To identify candidate runaways in the B-type sample we com- The mean velocity for the 281 stars (not including those in pared the radial-velocity estimates for each star with the initial Hodge 301 and SL 639) was 269.8 = 16.4 km s−1, with a median weighted mean and standard deviation calculated for the stars in value of 270.7 km s−1. Adopting either of these systemic values

9 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Table 5. Candidate runaway stars identified from the radial-velocity analysis of the VFTS B-type spectra.

VFTS Classification vr (vr − vr) |vr − vr|/σ ve sin i rd [km s−1] [km s−1] [km s−1][0] [pc] 242 B0 V-IV 216.0 ± 3.6 −55.6 ± 12.7 4.6 ≤40 5.96 86.6 298 B1-2 V-IIIe+ 332.1 ± 4.0 60.5 ± 12.8 5.0 431 ± 15 3.92 57.1 358 B0.5: V 164.7 ± 10.7 −106.9 ± 16.2 8.8 345 ± 22 3.02 44.0 368 B1-3 V 229.6 ± 12.4 −42.0 ± 17.4 3.4 380: 1.20 17.5 467 B1-2 Ve+ 322.3 ± 30.2 50.7 ± 32.6 4.2 355 ± 29 9.54 138.7 616 B0.5: V 227.4 ± 10.7 −44.2 ± 16.2 3.6 ≤40 1.26 18.3 625 B1.5 V 310.7 ± 9.2 39.1 ± 15.3 3.2 64 ± 12 2.57 37.4 831 B5 Ia 210.4 ± 6.2 −61.2 ± 13.7 5.0 41 7.91 115.0 851 B2 III 229.4 ± 0.3 −42.2 ± 12.2 3.5 ≤40 7.18 104.4

Notes. Estimates of ve sin i are from Dufton et al. (2013) except for VFTS 831, which is taken from McEvoy et al. (2015). Projected distances from the core of R136 are from Paper I.

and a 3-σ threshold (taking the dispersion as 16.4 km s−1) led to identification of the five most significant runaways from Table 5 (i.e. VFTS 242, 298, 358, 467, and 831), with a second iteration providing one additional candidate (VFTS 616). The final mean velocity from these calculations is 270.1 ± 13.9, in good agree- ment with the equivalent subsample in the final row of Table 4. From these checks we conclude that the four most significant candidates (VFTS 242, 298, 358, and 831) are secure as poten- tial runaways, with five more tenative candidates as discussed above. For the members of Hodge 301, VFTS 309 is a poten- tial outlier (at 3.6σ) compared to the mean velocity for the cluster in Table 4. Indeed, excluding its vr estimate from the calculated mean and dispersion for Hodge 301 gives −1 vr = 261.5 ± 5.0 km s , such that VFTS 309 is then a 4.1σ out- lier. However, its velocity is also in reasonable agreement with those for stars in NGC 2060 and NGC 2070, so we are unable to confirm it as a potential runaway from Hodge 301. Finally, we Fig. 6. Cumulative distribution of estimated radial velocities for the 307 single B-type stars. The dashed vertical line indicates the weighted note that the velocity estimate for VFTS 310 is not significant as −1 mean velocity of the sample, vr = 271.6 km s (calculated excluding a potential runaway from Hodge 301. stars in the two older clusters and the candidate runaways). The vertical With our adopted velocity criteria, the nine candidate run- dotted lines are the 3σ thresholds adopted for identification of potential −1 aways correspond to 2.9 % of the sample of 307 single stars runways (±36.6 km s ). with radial-velocity estimates. This lower fractional share of run- aways compared to the O-type stars (Sana et al., in prep.) is in qualitative agreement with recent N-body predictions for the mass-spectrum of runaways (Banerjee et al. 2012; Banerjee & −1 Kroupa 2012), although quantitative comparison with the pre- and the fifth with ve sin i = 64 ± 12 km s . Meanwhile, the re- −1 dictions is complicated by the different criteria employed (e.g. maining four stars each have estimates of ve sin i ≥ 345 km s . Banerjee et al. used a radial distance threshold for a star to be To investigate the significance of these results, we ran Monte considered a runaway). We note that the distribution in Figure 6 Carlo simulations using the ve sin i distributions from Dufton is slightly asymmetric, with two thirds of the candidates hav- et al. (2013). We note that the results from Dufton et al. were for ing negative differential velocities. This could point to veiling of the unevolved B-type sample (i.e. dwarf and giant objects), so more distant runaways by the , although this is not seen we exclude VFTS 831 from the following discussion. in the results for the O-type stars (in which a greater fraction We generated random rotational velocities for eight stars are seen to have positive differential velocities, Sana et al., in drawn from the distribution of Dufton et al., and repeated prep.), suggesting that small-number statistics likely explain the this 106 times to estimate the probability of recovering rota- asymmetry. tional velocities consistent with our eight (non-supergiant) run- away candidates (i.e. four stars with ve sin i ≤ 65, and four with −1 4 6.2. Rotational velocities of candidate runaways ve sin i ≥ 345 km s ). We then repeated these runs 10 times to estimate the dispersion on the probabilities. In a second test Estimated projected rotational velocities (from Dufton et al. we limited the low velocity subsample to the three stars with −1 2013; McEvoy et al. 2015) for our candidate B-type runaways ve sin i ≤ 40 km s (i.e. excluding VFTS 625, which has the are included in Table 5. There appears to be a dichotomy in their least significant runaway velocity), together with the four rapid rotation rates, as highlighted by Fig. 7. Five stars have small ro- rotators. We found low probabilities for recovering the observed tational velocities, with the estimates for four stars effectively ve sin i values from both tests (as summarised in Table 6), with limited by the velocity resolution of the data (i.e. ∼40 km s−1) significance levels of 3.0 and 3.2σ, respectively.

10 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Table 6. Probability tests to investigate the rotational velocities of the 6.3.1. VFTS 358 candidate runaway stars compared to those for the full (unevolved) B- type sample from Dufton et al. (2013). This star has the largest differential velocity from the −1 estimated systemic value (δvr = −106.9 ± 16.2 km s ) and also has a relatively large projected rotational velocity 4 6 −1 Test (from 10 repeats of 10 runs) n P (ve sin i = 345 ± 22 km s ; Dufton et al. 2013). This prompted −1 4 × ve sin i ≤ 65 & 4 × ve sin i ≥ 345 km s 10 ± 3 0.0010 us to investigate its physical properties, in part to see if there was −1 3 × ve sin i ≤ 40 & 4 × ve sin i ≥ 345 km s 6 ± 2 0.0006 any evidence of past binary interaction (see e.g. de Mink et al.

−1 2014). 4 × ve ≤ 100 & 4 × ve ≥ 340 km s 395 ± 20 0.0395 −1 Detailed analysis was complicated by the rapid rotation, 3 × ve ≤ 60 & 4 × ve ≥ 340 km s 181 ± 13 0.0181 which made estimation of the atmospheric parameters and el- ement abundances difficult. However, using similar methods as Notes. ‘n’: number of Monte Carlo runs (from 106 sets) for which the simulated rotational velocities are consistent with those of the candidate those used by Hunter et al. (2007), we undertook a preliminary runaways (and translated into a fractional probability, P , in the final analysis using a grid of model atmospheres calculated using the column); the quoted uncertainties are the standard deviations from 104 TLUSTY and SYNSPEC codes (Hubeny 1988; Hubeny & Lanz repeat runs. 1995; Hubeny et al. 1998; Lanz & Hubeny 2007); further details of the grids are given by Ryans et al. (2003) and Dufton et al. (2005)5. We estimated the effective temperature (Teff ) and gravity (log g) of VFTS 358 by fitting rotationally-broadened profiles to the Hδ,Hγ and He II λ4686 lines, assuming solar helium abun- dances. This gave estimates of Teff ' 29 kK and log g ' 3.5 dex, although we were unable to estimate the microturbulence be- cause of the paucity of observable metal lines (which also pre- cluded use of the silicon ionisation balance to estimate the tem- perature). Absorption from N II λ3995 appears to be present in the spectrum (with an equivalent width of ∼120 mA),˚ although its identification is marginal, as shown in Figure 8. Rotationally- broadened model spectra for our adopted physical parameters (and an assumed microturbulence of 5 km s−1) are shown for three nitrogen abundances: 12 + log (N/H) = 6.9 (the approxi- mate baseline N-abundance for the LMC, see discussion by Hunter et al. 2007), 7.7, and 8.5 dex plotted in red, green, and blue, respectively. This comparison suggests significant nitro- Fig. 7. Comparison of the projected rotational velocities (ve sin i) with gen enrichment, with an abundance of & 8.5 dex (the maximum the differential radial velocities (δvr) compared to the mean systemic abundance considered in our grid). Tests for theoretical pro- velocity of the B-type sample. Uncertainties on ve sin i of ±10 % are files with a microturbulence of 20 km s−1 (which is larger than adopted for VFTS 368 and 831 (with the latter plotted as an open sym- bol given its supergiant classification). normally found for stars with this gravity, e.g. Hunter et al. 2007) implied a similarly large nitrogen abundance. Fitting a rotationally-broadened profile to the N II λ3995 line leads to −1 −1 ve sin i = 342 km s (cf. 345 km s from the helium lines) and a central wavelength of 3995.06 A˚ (cf. the laboratory wavelength We also investigated the probabilities compared to the cumu- of 3995.00 A).˚ This agreement provides some support that the lative distribution function of unprojected rotational velocities feature is indeed from N II absorption. v ( e) from Dufton et al. (their Table 6). In this case we are limited The neutral helium lines in the observed spectrum appear by the unknown inclination angles of our targets but, assuming somewhat stronger than those in the best-fitting model (e.g. the some relatively conservative lower-limits, we repeated tests sim- He I λλ4009, 4026 lines in Figure 8) suggesting that the he- ilar to those above (in which we adopt the nearest available value lium abundance might also be enhanced. In turn, this would from Dufton et al. for our upper limit, i.e. 340 km s−1). These tend to decrease the Teff estimated from the He II line (and the tests are formally less significant (Table 6), but provide further surface gravity). Tests using cooler models indicated that the support that the rotational velocities of our candidate runaways change in nitrogen abundance would be modest. For example, do not appear to be randomly drawn from the distribution for a change in effective temperature of −2 kK leads to a change in the larger B-type sample. We note that this agrees with similar 12 + log (N/H) of approximately −0.2 dex. Hence, the nitrogen conclusions regarding the rotational velocities of the O-type run- abundance would still be significantly greater than the baseline aways (Walborn et al. 2014, Sana et al., in prep.). value for the LMC. At present we are limited by the quality of the VFTS spec- 6.3. Atmospheric analysis of two candidate runaways trum but from this preliminary analysis there is evidence of sig- nificant nitrogen enrichment (and maybe also helium) in the pho- Atmospheric analysis of the B-type spectra is now underway tosphere of VFTS 358. Indeed, the estimated nitrogen abundance within the VFTS project. In the context of the current study, we is the largest obtained so far from the VFTS survey (including were particularly motivated to investigate the properties of the results from the B-type supergiants from McEvoy et al. (2015). two most noteworthy runaway candidates, VFTS 358 and 831; we now comment briefly on our findings for these two objects. 5 See also http://star.pst.qub.ac.uk

11 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

estimate of 0.15 × δvr max. For stars with vr above (or below) the systemic velocity, we then subtract (or add) this estimated error, to give a corrected velocity estimate, vcorr. Using the same 3σ criteria discussed above we then looked for potential runaways. Only one single-lined system, VFTS 730, was found to be −1 a potential runaway, with vcorr = 324.0 km s (a 4.3 σ outlier cf. the adopted systemic velocity). Its range of observed veloc- −1 ities is relatively small (δvr max = 16.6 km s , thus only just above the detection threshold employed by Dunstall et al.) but it could be, for example, a long-period system with an eccentric orbit. Indeed, inspection of its velocity estimates as a function of epoch show them to be monotonically decreasing from 332 to 316 km s−1, suggesting it as a long-period system. Further in- vestigation of this (and other) binary systems will require com- prehensive spectroscopic monitoring to determine their centre- of-mass velocities and other orbital parameters.

Fig. 8. Section of the VFTS 358 spectrum showing, from left-to-right, 6.5. Origins of candidate runaways the H,N II λ3995, and He I λλ4009, 4026 lines; we note that H is complicated by absorption from the interstellar Ca H line (as well as The production of runaways is thought to be from one of nebular emission). Model spectra for our adopted physical parameters two channels, with evidence in support of both mechanisms and 12 + log (N/H) = 6.9, 7.7, and 8.5, are overplotted in red, green, (Hoogerwerf et al. 2000). In the dynamical-ejection scenario the and blue, respectively. runaway is ejected via gravitational interaction between single- binary or binary-binary systems in a dense star cluster (Poveda et al. 1967). In the binary-ejection scenario, the primary star ex- plodes as a , leaving behind a neutron star or black The large velocity offset, high rotation rate, enhanced nitrogen hole. In most cases the compact object leaves the system de- (and possibly helium) all fit, at least qualitatively, with a scenario pending on the magnitude and direction of the birth kick, and in which VFTS 358 is the former secondary of an interacting bi- the companion is ejected with a velocity approximately equal to nary that became unbound at the explosion of the primary star. its orbital velocity (Blaauw 1961; Eldridge et al. 2011). The complex star-formation history of 30 Dor makes it hard to cleanly attribute our candidate runaways to either of the two 6.3.2. VFTS 831 scenarios. R136 is sufficiently young (1–2 Myr; de Koter et al. VFTS 831 is remarkable in two regards. First as a luminous B- 1998; Massey & Hunter 1998) that none of its members is type supergiant, likely to be the evolved descendent of a formerly thought to have undergone a supernova explosion. Thus, any more massive O-type star, and secondly because, from the defi- runaways from R136 would have to be ejected via dynamical in- nition used in Table 4, it is located within SL 639 (≈1200. 5 from teractions. However, as noted above, the VFTS region contains −1 the visual centre). With vr = 210.4 ± 6.2 km s it also appears several older subclusters and associations, including NGC 2060, to be runaway compared to the other targets in SL639. A model- which contains a (e.g. Chu et al. 1992), and atmosphere analysis of the spectrum of VFTS 831 has been pre- Hodge 301 which was argued by Grebel & Chu (2000) as a likely sented by McEvoy et al. (2015), who classified it as an appar- site of tens of past supernovae from consideration of its mass ently single star. It is one of the cooler objects in the supergiant function. sample, with Teff = 14,000 K and log g = 2.1. One of the important diagnostics might prove to be the con- Following the discussion in Section 6.2, VFTS 831 does nection with the observed rotational velocities (Fig. 7), in which not appear particularly remarkable in terms of stellar rota- the apparently rapid rotators could have a binary origin. For ex- tion. Indeed, it has a relatively low projected rotational veloc- ample, the theoretical discussions by de Mink et al. (2013), and ity and a substantial contribution from macroturbulent broad- the suggestion that the high-ve sin i tail of the distribution of −1 ening (ve sin i, ΘRT) ∼(40, 65) km s , as found in most B- the rotational velocities for the VFTS O-type stars could be ac- type supergiants (see e.g. Markova et al. 2014; Simon-D´ ´ıaz & counted for by past binary interactions (Ram´ırez-Agudelo et al. Herrero 2014). From the intrinsically strong N II λ3995 sin- 2013). Detailed dynamical analysis of the O-type stars in the sur- glet transition, McEvoy et al. estimated a nitrogen abundance of vey has been underway in parallel to the current work, and the 12 + log (N/H) = 7.94. Although large, this is consistent with the broader question of the origins of runaway stars from 30 Dor is other single supergiants in the sample, which have abundances discussed in more depth by Sana et al. (in prep.). spanning approximately 6.8 to 8.1 dex. 7. Summary 6.4. Single-lined binaries We have presented comprehensive spectral classifications and For completeness we also investigated the velocities of single- radial-velocity estimates for the B-type stars observed in the lined binaries for potential runaway systems. In the final col- VFTS. We now briefly summarise our main findings: umn of Table A.3 we include the observed range of velocities, δvr max, from Dunstall et al. (in prep.). Following the arguments – The members of the two older clusters, Hodge 301 and laid out in Section A.3 of the Appendix, we adopt an estimated SL 639, appear kinematically distinct from those in the error on the true systemic velocity compared to the single-epoch younger clusters and general field population.

12 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

– The preliminary H-R diagram for stars in Hodge 301 and References ∼ SL 639 (Figure 5) suggests an age of 10-15 Myr for Andrews, A. D. & Lindsay, E. M. 1964, Irish AJ, 6, 241 the population of SL 639, slightly younger than that of Balona, L. A. 1994, MNRAS, 267, 1060 Hodge 301 (15 ± 5 Myr). Banerjee, S. & Kroupa, P. 2012, A&A, 547, A23 – The systemic velocity for 273 single stars, excluding Banerjee, S., Kroupa, P., & Oh, S. 2012, ApJ, 746, 15 those in the two older clusters and candidate runaways, is Bica, E., Santos, Jr., J. F. C., & Alloin, D. 1990, A&A, 235, 103 −1 Blaauw, A. 1961, Bull. Astron. Inst. Netherlands, 15, 265 vr = 271.6 ± 12.2 (s.d.) km s . Bohannan, B. & Epps, H. W. 1974, A&AS, 18, 47 – Employing a 3-σ velocity threshold, we identify nine sin- Bonanos, A. Z., Massa, D. L., Sewiło, M., et al. 2009, AJ, 138, 1003 gle stars as candidate runaways (2.9 % of the single stars Bosch, G. L., Terlevich, R., Melnick, J., & Selman, F. 1999, A&AS, 137, 21 with radial-velocity estimates). These are mostly unevolved, Brott, I., de Mink, S. E., Cantiello, M., et al. 2011, A&A, 530, A115 Brunet, J. P., Imbert, M., Martin, N., et al. 1975, A&AS, 21, 109 early B-type objects, but include a B5-type supergiant Chu, Y.-H., Kennicutt, R. C., Schommer, R. A., & Laff, J. 1992, AJ, 103, 1545 (VFTS 831). Clark, J. S., Najarro, F., Negueruela, I., et al. 2012, A&A, 541, A145 – There appears to a bimodal distribution of rotation rates in Clark, J. S., Ritchie, B., & Negueruela, I. 2013, A&A, 560, A11 −1 Clark, J. S., Tarasov, A. E., & Panko, E. A. 2003, A&A, 403, 239 the candidate runaways. Five stars have ve sin i ≤ 65 km s , −1 de Koter, A., Heap, S. R., & Hubeny, I. 1998, ApJ, 509, 879 while the others have ve sin i ≥ 345 km s . de Mink, S., Langer, N., Izzard, R. G., Sana, H., & de Koter, A. 2013, ApJ, 764, – Excluding VFTS 831 (because of its evolved nature), there is 166 a remarkably small probability (∼0.001%) that the projected de Mink, S., Sana, H., Langer, N., Izzard, R. G., & Schneider, F. R. N. 2014, rotational velocities for our other eight candidate runaways ApJ, 782, 7 Doran, E. I., Crowther, P. A., de Koter, A., et al. 2013, A&A, 558, A134 could be randomly drawn from those for the full (unevolved) Dufton, P. L., Langer, N., Dunstall, P. R., et al. 2013, A&A, 550, A109 B-type sample. Dufton, P. L., Ryans, R. S. I., Trundle, C., et al. 2005, A&A, 434, 1125 – VFTS 358 has the largest velocity offset from the sys- Dunstall, P. R., Fraser, M., Clark, J. S., et al. 2012, A&A, 542, A50 −1 Eldridge, J. J., Langer, N., & Tout, C. A. 2011, MNRAS, 414, 3501 temic velocity of 30 Dor (δvr = −106.9 ± 16.2 km s ) −1 Evans, C. J. & Howarth, I. D. 2003, MNRAS, 345, 1223 and appears to be rotating rapidly (ve sin i = 345 km s ). Evans, C. J., Lennon, D. J., Smartt, S. J., & Trundle, C. 2006, A&A, 456, 623 Preliminary spectral analysis suggests evidence of signifi- Evans, C. J., Taylor, W. D., Henault-Brunet,´ V., et al. 2011, A&A, 530, A108; cant nitrogen enrichment, perhaps indicative of past binary (Paper I) interaction. Evans, C. J., Walborn, N. R., Crowther, P. A., et al. 2010, ApJ, 715, L74 Feast, M. W., Thackeray, A. D., & Wesselink, A. J. 1960, MNRAS, 121, 337 Fitzgerald, M. P. 1970, A&A, 4, 234 The classifications presented here will underpin the quan- Fitzpatrick, E. L. 1988, ApJ, 335, 703 titative analyses in progress on this substantial part of the Fitzpatrick, E. L. 1991, PASP, 103, 1123 VFTS data. For example, they will enable investigation of the Fujii, M. S. & Portegies Zwart, S. 2011, Sci, 334, 1380 v sin i Graus, A. S., Lamb, J. B., & Oey, M. S. 2012, ApJ, 759, 10 mass/temperature dependence (if any) of the estimated e Grebel, E. K. & Chu, Y.-H. 2000, AJ, 119, 787 results from Dufton et al. (2013), particularly when also com- Groh, J., Meynet, G., Ekstrom, S., & Georgy, C. 2014, A&A, 564, A30 bined with the results for the O-type stars from Ram´ırez- Gummersbach, C. A., Zickgraf, F.-J., & Wolf, B. 1995, A&A, 302, 409 Agudelo et al. (2013). In the longer-term, the ongoing proper- Hodge, P. 1983, ApJ, 264, 470 motion studies using HST imaging (programme GO12499, P.I. Hodge, P. 1988, PASP, 100, 1051 Hoogerwerf, R., de Bruijne, J. H. J., & de Zeeuw, P. T. 2000, ApJ, 544, L133 Lennon) will add another dimension to our studies of the com- Houk, N. & Smith-Moore, M. 1988, Michigan Catalogue of Two-dimensional plex dynamics in this region, by providing tangential velocities Spectral Types for the HD Stars. Vol. 4, Declinations −26◦ to −12◦ (see Sabbi et al. 2013). (Department of Astronomy, University of Michigan) Our radial-velocity estimates should also lend themselves to Howarth, I. D. 2012, A&A, 548, A16 Howarth, I. D. 2013, A&A, 555, A141 detailed investigation of the structural properties of the VFTS Hubeny, I. 1988, Computer Physics Communications, 52, 103 sample (e.g. using the techniques discussed by Parker et al. 2014; Hubeny, I., Heap, S. R., & Lanz, T. 1998, in Astronomical Society of the Wright et al. 2014), particularly when combined with the results Pacific Conference Series, Vol. 131, Properties of Hot Luminous Stars, ed. for the O-type stars from Sana et al. (2013); this should provide I. Howarth, 108 Hubeny, I. & Lanz, T. 1995, ApJ, 439, 875 further insights into the formation and evolutionary history of Hunter, I., Dufton, P. L., Smartt, S. J., et al. 2007, A&A, 466, 277 the massive-star population in the region. Kalari, V. M., Vink, J. S., Dufton, P. L., et al. 2014, A&A, 564, L7 Finally, there is an ongoing monitoring programme of Kramida, A., Ralchenko, Y., & Reader, J. and NIST ASD Team. 2012, in NIST FLAMES spectroscopy to characterise a subset of the O-type bi- Atomic Spectra Database (v5.0); http:/physics.nist.gov/asd (National Institute ∼ of Standards and Technology, Gaithersburg, MD.) naries (PI: Sana); a similar monitoring programme for the 100 Lanz, T. & Hubeny, I. 2007, ApJS, 169, 83 binaries discussed here and by Dunstall et al. (in prep.) would Lennon, D. J. 1997, A&A, 317, 871 be valuable to determine the full orbital parameters of the lower- Markova, N., Bianchi, L., Efremova, B., & Puls, J. 2009, BlgAJ, 12, 21 mass population of binaries, while also providing robust esti- Markova, N., Puls, J., Simon-D´ ´ıaz, S., et al. 2014, A&A, 562, A37 mates of centre-of-mass velocities to better explore their dynam- Martayan, C., Hubert, A.-M., Floquet, M., et al. 2006, A&A, 445, 931 Massey, P. & Hunter, D. A. 1998, ApJ, 493, 180 ics in the context of ejected runaways. McEvoy, C. M., Dufton, P. L., Evans, C. J., et al. 2015, A&A, arXiv:1412.2705 Meixner, M., Gordon, K. D., Indebetouw, R., et al. 2006, AJ, 132, 2268 Acknowledgements. Based on observations at the European Southern Melnick, J. 1985, A&A, 153, 235 Observatory Very Large Telescope in programme 182.D-0222. We thank Mark Parker, J. W. 1993, AJ, 106, 560 Gieles for helpful discussions regarding the candidate runaways, and the referee Parker, R. J., Wright, N. J., Goodwin, S. P., & Meyer, M. R. 2014, MNRAS, 438, for their constructive comments. STScI is operated by AURA Inc., under NASA 620 contract NAS 5-26555. SdM acknowledges support for this work by NASA Pasquini, L., Avila, G., Blecha, A., et al. 2002, Msngr, 110, 1 through an Einstein Fellowship grant, PF3-140105. JMA acknowledges support Portegies Zwart, S. F. 2000, ApJ, 544, 437 by grants AYA2010-17631 and AYA2010-15081 of the Spanish Ministry of Poveda, A., Ruiz, J., & Allen, C. 1967, Bolet´ın de los Observatories to Economy and Competitiveness. SS-D acknowledges funding from the Spanish Tonantzintla y Tacubaya, 4, 86 Government Ministerio de Econom´ıa y Competitividad (MINECO) through Ram´ırez-Agudelo, O. H., Simon-D´ ´ıaz, S., Sana, H., et al. 2013, A&A, 560, A29 grants AYA2010-21697-C05-04, AYA2012-39364-C02-01 and Severo Ochoa Rivinius, T., Carciofi, A. C., & Martayan, C. 2013, A&ARv, 21, 69 SEV-2011-0187, and the Canary Islands Government under grant PID2010119. Ryans, R. S. I., Dufton, P. L., Mooney, C. J., et al. 2003, A&A, 401, 1119

13 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

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14 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page wk broad but weak emission extends redwards IV α α 224 . . . ◦ 69 − Set Alt. ID Comments ] σ 1 − r [km s 265.2 2.1 1 Sk 280.9 31.0 B . . . Walborn et al. (2014) Spectral classifications and radial velocities for B-type stars in the VFTS. V v − 0.06 283.30.08 2.4 285.3 1 3.6 . . . 2 ...... 0.060.07 263.6 288.1 4.40.07 7.2 2 279.8 1 . . . 2.0 . . . 1 ...... 0.02 285.6 3.0 1 ...... − − − − − − Table 7. − − − − α V B a 16.18a 0.11a 16.20 293.2 21.6 0.04 B 278.0 . 30.5 . . B ...... a 16.62 0.17 279.2 11.9 B . . .a 16.20a 0.07 15.79 270.2 22.8 0.06a B 299.4 16.94 . 18.4 . . . . . 0.14 B 287.0 . . . 19.0 B ...... aa 16.18 14.71 0.06 0.09 290.3 273.1 11.3 42.5 B B ...... X X X X X X X X X . . . q? + 083084085 B1.5 V B1.5 V B1.5 V ...... a a 15.91 a 16.84 16.48 0.10 0.18 287.3 276.2 3.7 3.8 2 2 ...... 060062068 B1.5 II-Ib((n))069 B3 III071 B1-1.5e075 B0.7 Ib-Iab . .078 . B1: V082 B1 V B1 V a B0.5 Ib-Iab ...... 16.12 0.62 a q? e . . . 284.2 . 13.59 . . . . 16.27 . 15.65 14.3 . . . a 0.17 0.15 1 0.77 a a 16.65 280.7 287.5 254.8 a . . . 13.61 16.93 1.7 24.0 0.03 2.7 16.63 1 2 0.03 268.4 1 0.21 297.2 ST92 . . 1-17 . 4.3 . . . 283.1 10.5 2 3.7 1 . . . 2 ...... B1 III [ST92] Composite spectrum? ...... 044048050 B2 V052 B1 V053 B0 V054 B0.2 III-II B1 III B0 V ...... a . a . a . 16.62 a . . . 16.72 14.55 16.77 f 0.14 f 15.28 0.18 274.1 16.60 283.1 0.09 3.3 2.0 0.21 276.4 2 265.7 1 2.0 . . . 19.9 . . . 1 2 ...... Si VFTS Spectral Type001003 B1.5:004 V Mult.?005 B1 Ia H 007 B2 V008 B2 V(n)009 B1-2 V010 B0.5: V(n)013 B1-1.5 . . V .015 B2 V017 B1.5 V a . B0.5 . . . V . . B0 . . V . . . 16.93 . a a 0.05 a a 16.25 16.87 282.1 . . . . . 16.92 . 16.74 0.02 0.16 4.2 0.07 a 0.03 282.6 283.1 a 2 271.3 10.8 281.1 16.79 2.6 . 16.36 . . 6.9 2 1.6 2 0.04 0.13 2 . . 2 . . . . 287.1 290.9 ...... 3.9 4.3 1 2 ...... 018020022 B1.5 V B2.5: V(n) B0-0.5 V-IIIe030 ...... 031033 B3-5e (shell) e a034 B1.5 V036 B1-1.5 V 16.67 16.70037 B1.5 Ve038 B1: Vn . . . 0.55 0.06039 B2 III: 040 258.8 B1.5 V . . .041 e B0:e 16.3 . . .043 B1-2 Vn 16.34 . 2 . . . B2: . V . B2 ? V(n) ...... 0.10 . e 16.41 ...... a 16.14 . 0.00 . . . . . 16.61 . . a . 280.0 0.13 . . . a e 16.54 . 308.3 0.10 8.4 . . 13.8 270.8 16.85 1 . 14.52 . a . 0.06 18.4 1 . . 278.0 . 0.10 . 16.49 . 0.52 . 2 . . . 291.4 4.1 H ...... 12.6 2 2 ...... ST92 1-02 . . . ST92 1-01 ...... B1 V [ST92] ...... 024025027 B0.2 III-II028 B1-1.5 V 029 B1 III-II B0.7 Ia Nwk B1 V ...... f 16.02 q? . . . 13.48 0.37 285.7 0.24 a 4.4 273.5 16.73 1 4.4 . . 1 ...... H

15 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page emission wings α emission α emission wings α Set Alt. ID Comments ] σ 1 − r [km s continued V v − 0.060.02 284.0 294.30.03 7.4 3.8 2 . . . 1 ...... 0.08 . . . 272.0 . . . 4.2 1 . . .0.07 Weak 254.1 but broad H 0.02 . . . 2.6 293.5 15.2 1 . . B ...... 0.08 284.00.03 24.4 267.5 B 6.1 ...... 1 ...... 0.01 ...... 0.02 . . 272.8 . 6.8 B 2 ...... − − − − − − − − − − Table 7. α V B f 16.81 0.00 281.8 14.5 B T88-10 . . . ff 16.43 16.68 0.05 0.06 281.8 294.5 13.3 23.7 B B ...... a 16.24 0.25 259.6 12.6 B ...... a 16.21 0.16 296.7 11.5a Ba 16.19 ST92 1-31 16.21 0.08 0.20 . . . 302.2 15.9 .a . . B B0.5 16.03 V . [ST92]; .e . Walborn . et . al. . (2014) . . 16.01 . 0.01a 270.9 52.5 16.95 B 0.08 ...... Broad, weak H . . . a 16.13 0.31 254.9 12.7 B ...... a 16.69 a 16.49 0.07a 283.7 14.8 16.93 B 0.09a . . . 294.5 16.31a 6.4 16.86 0.10a B 274.0 16.91 . 0.06 . . 69.9 268.1 B 12.9 ST92 1-82 B ...... B2 V [ST92] . . . X X X X X X X X X X X X X X X X X ...... e 16.26 e 15.33 0.44 283.8 0.20 18.3 285.7 2 19.3 T88-11, ST92 1-64 2 . . . B1: [ST92] ...... e e 16.54 16.93 0.35 0.16 300.4 274.4. 10.0 . . 5.6 1. . . e 2 ST92 1-67. . . 16.08 . e . . 15.58 0.12 e 277.9 14.83 0.05 13.0 271.9 B1: 0.09 [ST92] 2 7.1 253.6 . . . 2 8.0 ...... 1 ST92 1-89 . . . B1 V [ST92] . . . + + + + + + + 146152 B2: V B2 IIIe . . . e 15.32 0.25 274.3 2.9 1 . . . B2 V [Paper I]; weak H 155156 B0.7: V B1-1.5 V-IIIe 157159 B2 V B2.5 III . . . a 15.61 158161 B1-1.5 Ve 162164 B1 V B0.7 V B2: V-IIIe . . . a 16.69 0.24 262.6 7.9 1 ...... 137144 B0.7 V B0.7: V . . . a 16.85 0.11 284.0 3.1 2 ST92 1-55 B1 V [ST92] 097099100 B0 IV 101 B2-2.5 V106 B1.5 V107 B0.7: Vne111 B0.2 V 112 B1: V 118 B2 III . . .119 Early B + Early B 121 B1 IV ...... 122 B0.7 V a124 B1 IV126 B1.5 e 16.78 a V127 B2.5 III 16.39 . 16.68 .133 B1 . V134 B2: V(n) 0.32 0.22135 B0.5 V . . a . B1 277.3 V(n) 257.6 . . B1: . V-IIIne 14.40 . . . 4.8 1.4 . a . . 2 2 a . 16.36 . . . a . . a ST92 . 1-33 . 15.96 . 16.53 0.07 . . . a 16.61 a 275.8 0.06 0.24 16.93 16.78 283.4 0.24 a 3.9 260.7 289.4 0.07 2.8 16.85 17.6 1 243.3 2.2 1 . 2 B1 . . V 0.02 [ST92] 1 5.5 ...... 262.8 ST92 2 1-46 . . . 9.4 . . . 2 . . . B1 . V . . [ST92] ...... 200 B1-1.5 IIIe . . . 204 . . B2 . III VFTS Spectral Type088095 B0: V-III(n) Mult.? B0.2 V H . . . e(?) . . . 15.24 a 16.06 166167170 B2: V-IIIe 179 B1 V181 B1 IV183 B1 V 186 B0.5 V189 B0 IV-III194 B1 IV195 B0.7: V 196 B2 . . V-IIIe . . .199 B0.5 . V B2 IIIe . . . . . a .202 Early B + a Early B 203 16.07 . . B2 . a 16.03 V a B1-1.5 V 0.01 16.24 16.51 0.15 a 286.9 278.7 0.15 0.38 15.79 5.0 278.9 2.7 256.1 2 0.11 11.9 . . 1 . . 1.7 . . 264.3 . . . 2 . . 1 . 10.6 f . . a . . . 1 . 16.77 16.16 . . . 0.13 276.6 2.3 . . . 1 . . . . ST92 . 1-90 . B0 IV (Walborn et al. 2014) . . . B2 V [ST92]

16 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page profile, probable emission; member of H 301 α in some LR02 epochs I em. (poss. cross-contamination from VFTS 507) α emission?; member of H 301 α ; member of H 301 asymmetric, possible weak P-Cygni? α Set Alt. ID Comments ] σ 1 − r [km s continued V v − 0.060.12 273.1 272.0 2.6 13.2 10.03 B . . 287.5 . . . . 63.00.08 B 261.4 . . .0.010.09 8.2 289.20.04 277.4 15.8 2 281.2 9.1 B . . . 6.5 . . . B ...... 2 ...... 0.01 . . . 268.5 13.5 2 ...... Broad but weak H ...... 0.01 264.20.010.13 4.4 252.90.07 256.8 14.1 3 270.80.06 5.9 GC00-Be5 2 12.80.01 260.5 1 . . .0.02 B 252.1 19.70.08 GC00-Be2 272.7 . . . 6.0 2 278.4 3.9 2 GC00-Be7 4.4 1 Member WB97-6, of GC00-Be4 H 2 301 ...... Only nebular H B2 III [WB97]; known triple, . inc. . GC00-Be10; . member of Str. H Si 301 II Member of H 301 ...... 0.07 264.9 2.3 1 WB97-2 Member of H 301 0.03 267.6 8.7 1 . . .0.04 269.2 11.9 B . . . B0 IV (Walborn et al. 2014) . . . − − − − − − − − − − − − − − − − − − − Table 7. α V B f 16.56 f 16.58 f 16.51 f 16.82 e? 15.07 e 15.50 0.04 276.4 12.8 B ST92 1-96 . . . a 14.99 0.15 257.3 36.8a B 15.63 . . . 0.38 249.2 7.9 B ST92 1-99 . . . a . . . 15.85 0.01 224.2 52.6 B . . . Weak secondary He a 16.83a 16.49 0.45aa 275.8 16.68 0.00 28.8 16.70 297.6 0.02 B 35.8 268.5 . . . B 65.4 . . . B ...... X X X X X X X X X X X X X . . . e 16.73 0.05 262.6 14.1 2 GC00-Be8 Member of H 301 . . . e 16.02 0.11 263.9 25.8 2 ...... e e 16.80 16.65 0.05 0.11 270.1 272.1 16.8 14.5 2 1 ...... + (shell?) . . . e 16.00 + + + + 218219220 B1.5 V 221 B3-5 V-III224 B0.7 V B1 V B1-2 V-IIIe 228229 . . .230 B0.7 V232 B1.5 Vn . . . f233 B1.5 III234 B3 . . Ia . 16.93237 B1-2 f V-IIIe238 B1.5 V 0.04 f 16.66239 B1-1.5 V-IVe . . . .240 B2.5 . 282.5 . V 16.27 0.03 B1 . V . 12.6 . . . . B1-2 f V 282.6 (SB2) f 2 ...... a 16.46 3.3 . . e 16.48 . . . . 16.59 1 e a 16.40 . . 0.00 . a . . . 15.93 14.52 0.44 272.8 . . 0.23 . 16.22 279.7 11.0 f 0.06 0.50 248.2 2 7.5 a 11.9 287.9 288.6 0.11 16.84 10.5 . 2 247.0 2 . 16.41 . 2.5 10.3 1 . . . . . 1 . . 0.02 . . 2 . . . ST92 1-104 274.7 ...... 6.5 2 . . . . B2: . . [ST92] ...... 225 B0.7-1 III-II 241 B0 V-IV . . .263 a B2: V-IIIe 16.65 242246247 B0 V-IV248 B1 III 254 B2 V255 B2: V 257 B1-2 Ve258 B2: V . .261 B0.7-1.5 . V B1.5 V B5 Ia f ...... 16.82 a 0.04 e . 16.88 . . 216.0 16.90 . . . 3.6 0.02 a 0.03 293.6 1 a? 250.7 16.34 . 4.1 . . 12.33 5.6 0.10 2 2 0.03 287.3 . . . 285.0 . . . 5.9 2.2 1 1 ...... B0 IV (Walborn et al. 2014) ...... H 211212213 B1 V 214 B1 III215 B2 III:e B0 IV-III B1.5 V ...... a a 15.18 15.84 0.02 0.27 286.2 275.4 2.5 1.7 2 1 ST92 1-95 . . . B1 V [ST92] . . . 273274276 B2.5 V B1 V(n)279 B1.5 V282 B2: Ve 284 B3-5 III(n)e286 . . . . B1 . V . B0.7 V . . . a . . a . 16.74 a 16.94 e 15.84 0.03 . 16.11 . 253.8 . . . . 4.9 a f 1 16.84 15.83 ...... VFTS Spectral Type206209 B3 III: Mult.? B1 V H . . . a227 16.33 B2 V 278 B2.5 V 283 B1.5 V-III(n)e . . . e 15.31 272 B3: IIIe 270 B3 Ib . . . a 14.35 268269 B1.5 Ve B8 Ia . . . q? 12.90 0.05 266.9 2.1 1 R132, WB97-1 B0.5 Ia [Mk]; complex H

17 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page em. in broad photospheric abs. α em. (but strong nebular) α 0 NW; member of H 301 emission shoulders . 00 1 α ∼ 5) Poss. broad, weak H . 00 0 ∼ 136 . . . ◦ 68 − Set Alt. ID Comments ] σ 1 − r [km s 268.4 9.0 2 GC00-Be3 GC00-Be6 is continued V v − 0.03 269.4 7.7 2 P93-01250.07 264.1 2.9 1 Mk 60, . P93-0195 . . B0 I [Mk]; O9.7 II [WB97] 0.060.06 279.4 266.2 7.3 17.3 1 B0.04 . . . P93-0050 292.2 43.4 B P93-0097 ...... 0.02 . 0.02 270.00.04 10.9 . . . 269.4 2 6.0 ...... 2 . . . P93-0207 P93-0202 B1 V . [B99] . . . . . 0.03 258.60.13 5.6 274.60.06 25.1 2 250.1 B P93-0003 8.8 . . . 2 P93-0014 . . . . . Poss. . double-peaked core H 0.01 263.5 1.9 1 . . .0.03 287.4 46.0 B P93-0009 Member of H 301 . . . 0.06 272.7 2.0 1 Sk 0.10 321.7 50.4 B ...... 0.08 264.7 11.40.140.04 2 263.60.07 260.4 GC00-Be90.01 4.9 307.7 1.9 250.0 12.0 2 10.05 7.8 . 2 . .0.03 WB97-9, GC00-Be1 288.9 1 . . . 276.7 45.8 . . . Member 12.1 of H B 301 B2p?, B2 2 V var. [WB97]; . . member . of H 301 . . . Member of H 301 ...... − − − − − − − − − − − − − − − − − − − − − − Table 7. − − α V B f 16.30 0.03 295.0 10.5 B ...... f 16.82 0.03 266.6 29.9 B P93-0193 . . . f 15.92 0.00 266.7 14.7 B P93-0075 B1:: V: [P93] f 16.84 a 15.98 0.08 246.8 24.9 B P93-0136 . . . a 16.26 e 16.72a 16.94 0.14 278.6 11.1 B P93-0076 O9:: V: [P93] a 15.53 a 16.59 e 14.85 0.12 234.7 46.1a B 16.36 WB97-8 B5:p [WB97] X X X X X X X X X X X X . . . e 16.76 0.17 276.9 11.1 2 P93-0006 ...... e 16.11 0.23 291.3 22.1 2 . . . Be [Paper I] . . . e. . . 16.68 e 0.24 332.1 4.0 2 ...... + + + + + 362363 B1-3 V-III B0.2 III-II ...... e? a 16.98 14.88 0.44 ...... P93-0176 (at 364365 B2.5: V B2 V . . . f 16.24 366367 B1-1.5 V B1-2 Vn ...... f a 16.83 15.92 351353354 B0.5 V 358 B2 V-III359 B0.5: Vn B0.5: V B0.5 V ...... a a 16.60 f 15.91 0.13 16.87 0.00 292.7 250.7 0.00 3.3 12.3 164.7 1 10.7 2 P93-0138 P93-0141 2 P93-0158 ...... B0.2: III [B99] 334335336 B0.7 V 337 B2.5 III340 B1 V 342 B2: V-IIIe 343 B0.7 V347 B1 V 348 B1-1.5 V349 B0 . V . . B0.7 V B1 V a . . . 16.29 . . . f 0.18 . . . . f . . 16.89 248.7 . 16.45 . . 2.2 a 0.24 a 2 0.04 251.7 16.68 16.27 f 16.2 240.5 P93-0053 0.01 16.50 0.04 2 9.3 267.5 267.8 P93-0088 2 2.5 4.0 P93-0099 1 2 P93-0116 P93-0118 ...... Walborn et . al. . . (2014) 331 B1.5 V . . . a 16.71 322324 B1.5-2 Ve B0.2 V 330 B2 III(n)e . . . e 16.14 0.18 267.7 4.4 2 . . . Broad, weak H 309313315 B2 V-III320 B0 V-IV321 B1 Ib B1-2 V-IIIe B1: V .326 . . . . . B1-2 e(?) Vn . . . 16.19 a . . . 16.32 0.00 a 281.8 0.07 14.81 a . . . 7.6 270.7 16.89 0.03 2 3.3 a 261.6 . . . 1 16.53 1.5 . . . 1 . . . Member of H 301 B0 IV (Walborn et al. 2014) . . . 308 B2 V325 . . . B1 V a 15.88 307 B1 II-Ib . . . a 13.56 302305 B1.5 Ib B2: V . . . a 15.53 0.32 264.8 1.6 1 ...... 288291292 B2.5 III:n293 B5 II-Ib 295 B2.5 V(n)296 B2 III-II(n)e297 B0-0.5 V298 B2 III . . .299 B1.5 V300 B1-2 V-IIIe ...... 301 B0.5 f V B1-2 Vn . . . 16.58 B2: f e Ve . 16.47 14.95 . 0.13 . . f . . 258.0 16.33 a . . 7.2 . f 15.45 2 16.64 a . . . 0.04 16.41 251.7 2.2 1 ...... Member of H 301 VFTS Spectral Type287 B2.5 Vne Mult.? H . . . e 16.58

18 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars em. α emission α emission α em. continued on next page α nebular emission; poss. (not prob.) stellar em. nebular emission; poss. (not prob.) stellar em. nebular emission; poss. (not prob.) stellar em. α α α Set Alt. ID Comments ] σ 1 − r [km s continued V v − 0.520.03 . . . 279.8 4.7 . . . 2 ...... P93-9013 B2: V [P93] . . . 0.58 275.2 10.9 2 ...... 0.040.03 265.4 264.4 4.0 1.3 1 2 . . . P93-0668 B0 III [WB97]; B0.2 V [B99] . . . 0.09 ...... 0.04 . . . 265.8 . . . 4.8 2 . . .0.15 Strong, structured H 264.6 5.8 . . . 2 ...... 0.020.03 . .0.18 . 239.4 . . 8.9 . . . . 2 ...... Cross-cont. of fibre (on-sky) by VFTS 402; prob. broad shallow H − − − − − − − − − − − Table 7. α V B f 16.13 0.16 ...... P93-0572 . . . f 16.83 0.11 . . .f . . . 16.32 ...... a 16.39 0.01 260.5 10.9 B P93-0684 B0: I [B99] a 16.32 0.11 270.9 17.7 B . . .e 15.11 . . . 0.64a 218.3 48.7 16.66 B 0.08 P93-0538 ...... P93-0616 B0-1 III [WB97]; B0.2 III-I [B99] . . . aa 16.36 16.20 0.19 0.02 291.5a 296.4 21.7 22.1 16.10 B Ba . . . 0.20 . . . 16.42 224.5 64.2 0.06 B 276.4 . . . 9.5 B P93-0305 ...... B0-0.5 V [B99] X X X X X X X X X X X . . . e. . . 15.48 e 0.17 16.32 269.7 23.3 0.02 2 ...... P93-9011 ...... e 15.58 0.10 286.3 24.2 2 ...... + + + ((n)) Nwk + p . . . e? 12.67 0.60 276.3 2.1 1 Mk B, P93-0662 A0 Ia [Mk]; BN6 Iap [WB97]; poss. intrinsic H p . . . e? 11.74 0.33 263.2 2.6 1 R138 A0: I: [F60], A0 I [W84]; A0 Ia [Mk]; prob. intrinsic H + + 394395 B0.7 V B1:e ...... f e 16.93 16.95 463 B0.7-1.5 V . . . f 16.92 462 B0.5-0.7 V . . . a 16.27 459461 B2 V B1.5 V . . . a 16.83 453458 B0.5 V B5 Ia . . . a 15.31 423424 B1 Ia: Nwk B9 I . . . e? 13.51448449 0.43452 B1-3 V 278.3 B1-2 V B1-2 4.3 V 1 Mk 52, P93-0493 ...... f B1 f Ia [Mk & W86]; 16.85 BC1 a Ia [WB97]; prob. 16.91 P-Cyg-like intrinsic emission 16.44 0.33 0.03 267.0 265.8 9.2 12.3 2 2 P93-0632 ...... 396397401 B0.5 V 403 B1-2 V407 B1-2 IIIe 408 B1-2 V411 B0.5: V413 B2: V-IIIe 414 B1-3 V-III417 B2 V . . .420 B1-3 V-III421 B2 Ib . . . B0.5 a . Ia . . Nwk B2: . . V . 16.68425 f f426 . . . 0.01 17.12 f428 . B0.5: . V . . 16.97 . . B1.5430 276.7 V 16.93 f 0.19 . B0.5 .431 . V 13.2 0.08 a433 B0.5 251.2 Ia f 16.89 . . 2 .434 B1.5 Ia 16.48 . Nstr . f . 3.4438 13.02 B1-3 V-III P93-0338 0.03442 B1.5: . . V . 15.51 2 0.02 f . . 264.2447 B1-3 . 0.25 V . . . 283.5 P93-0364 B1-2 11.6 16.42 V . 273.1 . 0.34 . . . . f . . B2 . V 4.4 2 260.7 . 3.4 f . . . . . 16.50 12.5 1 f . . e? . 1 17.04 . 1 B0.5-1.5 0.06 . 12.05 . 16.19 V f [B99] Mk . 54, . . P93-0488 0.06 276.2 . . . 16.87 0.11 0.01 . 13.6 270.7 . . . f . 270.2 286.5 . 0.05 2 7.6 16.99 2.4 8.5 B0.5 Ia . . 1 [Mk . . & . a . W86]; B0.5-0.7 Ia 1 2 [WB97] 0.07 P93-0511 Strong, 15.79 structured H . R137, . P93-0525 . P93-0548 ...... P93-0560 . . . B0.5 . Ia: [F60], B0.7-1.5 [W84]; B1 . . Ia . P93-0591 [Mk]; poss. intrinsic B0-1: H . I . . [B99] Strong, structured H . . . VFTS Spectral Type368374375 B1-3 V Mult.?376 B0 V(n) H 377 B0.5: V 378 B1: V381 B0-0.5 V 383 B1.5: V384 B1.5 V . . .387 B0.5: V 388 B0 V-III391 B1-2 f IIIe . . B0.5 . V 16.68 B0.5: . V . . . . f . 0.01 . f . . 229.6 16.33 a 12.4 16.98 0.04 a 16.11 2 0.26 271.6 16.72 . . . 0.07 7.2 . . . 242.1 0.49 1 264.8 . 8.0 . . P93-0260 5.5 1 . . . 1 P93-0280 P93-0271 P93-0287 . . . B0.5: V [B99] ‘Star 4’ in . . P93-293/304 . field from Walborn et B2 al. V (2002b) [B99]

19 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page abs. with embedded double-peaked em.? α em. (likely cross-contamination from VFTS 507) emission α α Set Alt. ID Comments ] σ 1 − r [km s continued V v − 0.13 278.6 26.3 2 ...... 0.07 268.9 15.1 2 P93-9018 . . . 0.02 279.9 8.5 B ...... 0.04 279.8 18.4 2 ...... 0.100.02 267.0 257.1 11.2 19.3 10.05 2 . . . 275.4 . . . 4.8 2 ...... − − − − − − − Table 7. α V B f 13.76 0.16 289.6 9.5 B Mk 38, P93-0930 O9 I [Mk]; O9.7 Iab [W86]; OC9.7 Ib [WB97]; Walborn et al. (2014) e? 15.67 0.78 262.0 34.9 B . . . Prob. intrinsic H a 16.60 0.06 265.6 10.3 B ...... a 16.66a 15.74 0.22a 279.9 0.08 14.2 16.69 287.2 B 68.8 0.08a . . . B 278.2 15.66 P93-0849 73.5 B 0.21a 278.2 . . . 23.1 16.13 B . . O9-B0 . V [B99] Walborn et al. (2014) ...... a 15.83 0.15 314.5 94.0 B P93-1247 B2-3 III [WB97]; B0.5 IV [B99] q? 12.55 0.23 277.7 8.8 B Mk 12, P93-1257 B0.5 Ia [Mk]; B0-0.5 Ia [W86]; B0 Ia [WB97] ae? 15.11 0.02 263.4 24.9 B P93-1191 B0.2-1 III-IV [B99]; broad H X X X X X X X X X X X . . . e 16.91 0.38 322.3 30.2 2 ...... e 15.48 0.28 280.0 15.6 2 ...... p Nwk . . . q 11.82 0.29 254.7 4.4 1 R142, P93-0987 B [F60]; B0.5-0.7 I [W84]; B0 Ia [Mk] + + + 606 B0-0.5 V(n) VFTS Spectral Type467469 B1-2 Ve Mult.? B0 V H . . . f? 16.09 0.00 275.6 2.6 1 P93-0714 Broad, shallow H 496499501 B0 Vn 504 B0.7 V516 B0.5 V 520 B0.7 V523 B1.5 V525 B1: V (SB2?) B1-3533 V-III B0534 Ia . . .535 B1.5 Ia 540 B0 IV . . .541 B1-2 f V-III . . .547 B0 . . V . 16.77548 B0.5 f Ia Nwk551 B3-5 a V-III f 16.27 0.06553 B0-0.5 V 16.61556 B1 . . V 293.1 . 17.05 0.61558 B1 V 10.1 . . 0.03 .567 B1.5-2 V 251.4 0.01 f568 B3 . 2 . . 256.8 . III . . 14.2572 B1 271.0 V(n) q 10.9 P93-0848 16.53573 B0.5: 1 V 6.9 f f575 1 13.12 B1 V P93-0861 0.34 B0-0.5 . . V 2 . . 16.55 . 16.79 . . . . B0.7 . 0.13 271.1 . III . P93-0909 269.6 0.23 0.03 7.5 . f . . . . . f a 247.0 3.1 255.9 . . 1 . 16.82 O9-B0: V 16.88 10.3 [B99] 17.00 a . 1 2.7 . f P93-0995 . . . . 0.13 2 . f . . P93-9024 16.69 0.04 1 16.29 0.06 284.7 P93-9026 f 260.5 16.79 a . . 276.3 . . . 0.01 . 0.24 7.1 10.2602 16.94 16.38 4.6 . . 0.15 . 605 272.1 . 2 . 2 . B0.7 280.3 1 13.3 V 0.03 0.15 . . . B1-2 . . . . V . . . . . 2 . 6.9 . 249.4 . . . . B0.5 Ia [P93] P93-1155 2 . . 4.1 ...... P93-1172 P93-9028 1 ...... P93-1160 Walborn et al. . . (2014) . . . . f f B0.2 III . 16.71 . [B99] . . . . . 16.85 . . . . B1:: . V [P93] 0.09 B1: III: 301.0 [B99] 1.6 2 . . . P93-1326 . . . 489 B1 Vn . . . f 16.54 576578580 B1 Ia Nwk 584 B1.5 Ia Nwk589 B0-0.5 Vn590 B1.5 V591 B0.5 V (SB2?) 593 B0.7 Iab . . .598 B0.2 Ia 600 B2.5 . V . . B0.2 V f B0.5 V(n) . . . a 14.52 . . . 16.62 f 0.40 . . 274.5 q? . 0.05 16.95 ...... 12.49 283.3 4.9 0.05 f 2.6 1 0.22 a f 253.3 16.84 2 254.1 P93-1184 16.40 16.94 5.7 P93-1217 6.2 0.09 2 0.34 291.5 1 . . 259.4 . 3.7 R141, P93-1253 3.0 1 1 B1 Ia [WB97]; . . B1: . II-I [B99] O9.5-B0.5 . . V . [B99] B0.5: [F60]; B0.5 I [W86]; BN0.5 Ia [WB97] ...... 473474478 B2: V480 B0.5: V(n)485 B0.7 V-III486 B0.5: V B1.5 V B1-2ne ...... a . . . f a . . 16.67 . 16.85 16.72 f 0.07 f 16.94 0.32 264.1 16.90 272.2 14.0 0.43 2 3.3 278.3 . 1 . . 4.6 P93-0738 1 . . . B2 Ia [B99] ...... 471 B1 V . . . a 16.36

20 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page em. shoulders α abs. with prob. embedded double-peaked em. α em. shoulders α B0.2 III [B99]; see discussion in Paper I 140; BE74-422 . . . ◦ 68 − Set Alt. ID Comments ] σ 1 − r [km s continued V v − 0.05 264.4 12.0 2 P93-1805 . . . 0.11 255.3 13.3 2 . . .0.10 271.1 15.7 2 . . .0.02 . . . 265.8 2.3 1 Sk Broad, shallow H 0.10 286.2 3.0 10.08 . . 255.5 . 2.1 1 P93-9036 ...... − − − − − − Table 7. 13.09 0.16 ...... Mk 11; P93-1500 B0.5 Ia [Mk]; B0-0.5 Ia [W86]; B0 Ib [WB97]; α V B f 14.48 0.28 276.7 23.8 B P93-1674 B0.5-0.7 I [WB97]; B1 Ib [B99] f 16.64 0.09 250.8 62.7 B ...... f 16.12 0.08 251.3 39.1 B ...... a 16.43 0.07 268.3 80.8 B P93-1834 . . . ee 16.55 13.68 0.18 0.44 263.7 . . 8.3 . B . . . P93-1799 . . . Mk 02, P93-1797; AL-377 Discussed in detail by Dunstall et al. (2012) . . . a 16.61 0.04 299.3 32.3 B ...... aa 14.99 14.29 0.17 0.28 276.8 295.8 38.9 23.0 B B . . . P93-1737 B1 Iab [P93]; B1 Iab [WB97]; B1.5 III [B99] B0.5 III [WB97]; B1 II-III [B99] − ae? 16.43 0.11 274.2 16.1 B P93-1604 B1 V [B99]; broad H X X X X X X X X X X . . . e 16.78 0.07 265.1 19.9 2 ...... e 16.64 0.21 243.4 22.5 2 ...... + + 701705 B0.7 V B0.7 V . . . f 16.60 0.26 266.6 10.1 2 P93-1820 . . . 697698699 B1-2 Ve Mid B + Early B B0.2-0.5 Vn . . . f 16.19 672673675 B0.7 II Nwk?676 B1 V678 B1 Iab Nwk 681 B0.7 V683 B1: V . . . B0.7 V B2 Ve e . . . 14.59 . . . . 0.23 f . . . . . a 279.5 16.98 . . . a 16.52 3.2 f 0.03 16.95 1 e 0.07 16.55 277.1 P93-1661 16.33 272.1 0.41 1.5 0.06 18.7 270.2 1 264.0 11.2 2 14.5 P93-1664 2 P93-1686 1 P93-1689 P93-1714 B0.7 Ia [WB97]; B1 III [B99] ...... VFTS Spectral Type610612616 B0 Vn Mult.?618 B0.5-0.7 V H 623 B0.5: V624 B1-3 V625 B0.2 V628 B0.2-0.5 Vn .629 B1.5 . . V . . .632 B0.5: V 633 B1-2 . Ve . . a636 B2 Vn . a . . . . .637 B1 V . 16.53 . . a640 B0 16.73 Vn641 B1-2 f V f . + 0.20 . Early 16.48 . B B2 a 0.17 V 16.70643 B0.5: 16.98 I . . 245.8 . 0.09 16.10644 f . . . 0.38646 B1.5 227.4 0.11 8.4 V . . 0.14 . 16.91 B1-2 . . 10.7 Ve . 265.3 . 2 . . . . B0.5 . III(n) 268.5 a . . 1 . 0.11 4.9 P93-1354 a 1.9 . 15.97 ...... P93-1389 a . 310.7 . . . 2 . 1 16.50 . 9.2 16.53 . 0.12 ...... f . P93-1419 . . . . . 284.7 0.19 1 P93-1395 0.06 16.82 11.1 274.0 a P93-1418 241.5 e e? 2 B0-0.2 7.2 0.16 III 16.41 [B99] 14.94 5.2 16.62 B1: P93-1460 V:: [B99] 256.0 2 2 0.13 0.14 0.15 P93-1464 5.0 . 250.9 . B1 . . . III . 263.9 [WB97]; 248.6 . B0-0.2 . . III-I 2 [B99] 8.2 20.2 4.8 ...... P93-1489684 2 2 2685686 B1-1.5 P93-1508 B0-2 . V . V P93-1527 . [B99] 687 B1-3 V-IIIe 689 . B0.7 . III . 690 B1.5 Ib((n)) Nwk 692 B3:e (shell)696 B0.2 . . V ...... B0.2 V B0.7 Ib-Iab . . Nwk . B1 III [WB97]; B1 f IV [B99]; . . prob. . broad H . 16.91 ...... e . . 0.13 . . . q? 16.51 278.6 12.73 a 13.1 f 0.08 16.46 2 16.17 . . . 0.09 P93-1722 0.05 272.7 . . . 271.2 14.7 . . . 1 2.5 P93-1763 P93-1772 1 P93-1786 ...... 653659662 B0-0.5 V665 B0-0.5 V(n) B3-5 III: 668 B0.5 V 670671 B0.7 V ...... B0.7 V B0.7 V a a 15.96 16.63 . . . 0.04 0.22 . . . . 264.9 . . . a . . a 4.6 16.60 a . . . 2 16.02 16.43 0.10 . P93-1584 . . 0.15 269.2 P93-1554 286.1 2.3 13.8 1 2 P93-1611 P93-1621 B0: V: [P93]; B0-1 V [B99] O9: III:p [P93] . . . B0.5-1 III [WB97]; B0.2-0.5 III [B99] 650 B1.5 V666 B0.5 V . . . f 16.98 . . . a 16.42

21 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page em. shoulders α em. α shoulders α 250 Weak double-peaked H ◦ 69 − Set Alt. ID Comments ] σ 1 − r [km s continued V v − 0.07 265.5 6.50.10 20.06 270.0 P93-9041 306.8 22.1 16.2 B B P93-9043 ...... 0.06 298.4 4.8 2 ...... 0.10 326.5 6.8 B P93-9045 B1.5 [P93] 0.02 ...... 0.12 258.8 40.3 B0.07 . . .0.01 253.2 253.70.11 4.0 6.1 243.4 3 11.4 1 . . . . 2 ...... 0.06 278.3 8.0 B . . . Poss. broad, weak H − − − − − − − − − − − Table 7. α V B ff 16.64 15.99 f 17.00 0.08 265.0 18.9 B P93-1898 . . . f 16.83 0.19 312.4 27.6 B P93-2151 . . . f 16.86 0.10 270.7 7.3 B P93-2210 . . . a 16.68 0.25 250.6 38.7 B P93-1868 . . . a 16.19 0.16a 239.2 26.3 15.41 B P93-1955 . . . a 16.93 a 16.48 a 15.46 0.19a 258.9 27.2 16.15a B 15.96 0.09 . . . 280.7 27.8 B ...... X X X X X X X X X X X X X ...... e e 16.30 14.55 0.43 0.02 268.9 284.4 4.9 14.1 1 2 ...... e 14.59 0.06. . . 281.6 13.5 e 1 15.66 AL-382; BE74-424 0.32 272.7 11.5 . . . 2 ...... e 16.53 0.27 274.0 12.0 2 ...... e 15.80 e 16.89 0.04 278.9 0.00 12.1 284.9 2 6.9 . . . 2 ...... e 15.89 0.24 268.9 17.2 2 ...... + + + + + + + + 719720 B1 V B2 V . . . f 16.74 723725726 B0.5 V 727 B0.7 III729 B1-2 V730 B3 III B0.2 III B1 IV(n) ...... a . . . . . a 15.84 a 16.40 a 0.11 16.74 14.97 0.03 285.3 249.7 0.18 0.25 1.8 12.1 272.9 268.6 1 2 10.9 3.0 P93-1961 . . . 1 1 P93-1969 ...... O9-B0 III [WB97]; B0.7 IV . [B99] . . . . . 740741742 B0.7 III B2 V B2 V ...... a 16.50 a 16.97 0.35 267.3 0.29 1.9 263.2 10.9 1 2 ...... 732734735 B1.5 Iap Nwk B0.7 V B1-2 IIIe . . . q? . . . 13.03 a 0.19 267.3 16.31 1.4 0.15 1 263.7 Mk 01, P93-1987; 8.9 BI 256 2 B1 Ia [Mk]; B2 I [B99] P93-1991 . . . 738739 B0.5 IIIe A0 Ip . . . e 12.26 0.31 250.5 1.9 3 Sk 745747 B2.5 II-Ib B0.5 V ...... f 16.59 e? 15.28 0.28 275.7 0.12 270.2 3.7 2.5 1 2 . . . P93-2022 B0.5: V [P93]; prob. broad, shallow H . . . 748749752 B0.7 V B0.7 V B2 V ...... a a 16.78 16.76 0.16 0.13 260.4 264.8 3.6 7.2 1 2 P93-2023 P93-2025 ...... 757762766 B3 III(n) B1.5 V B5-8e784 . . . B1: V . . . . f . . a 16.78 e 16.46 0.26 15.34 273.4 0.22 259.0 6.3 12.6 2 1 ...... 754756 B1.5 V B0.5 IIIe 772779780 B3-5 V-III781 B1 II-Ib . . . B1.5 V786 B0.7: V-IIIe a789 B1-2 . . IIIe . 16.55792 B0.5-2 V a 0.26 B2 V . . . 240.2 16.89 4.0 f 2 . . . 16.73 P93-2036 a 16.88 0.21 263.6 . . . 15.5 2 ...... 788 B1 III 794 B1-2 V-IIIe 795796798 B1 III799 B1-2 Ve B1 V B0.5-0.7 V ...... a 16.35 a 0.41 16.71 270.1 0.44 9.0 247.1 1 19.5 . . 2 ...... 800 B1-2 IIIe 712713714 B1 V715 B2: V 718 B1 Ia: Nwk B1 V B2.5 III ...... a f 16.13 15.57 0.21 0.33 255.1 283.4 10.9 1.9 1 1 P93-1859 P93-1875 . . . B0:: V: [P93] VFTS Spectral Type707709 B0.5 V Mult.? B2.5: V H ...... a a 15.59 16.58 0.07 275.0 2.0 1 P93-1840 B1 V [P93]

22 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars continued on next page abs.? II abs. plus nebular em. α em. shoulders α Set Alt. ID Comments ] σ 1 − r [km s 251.9 3.4 1 . . . Member of SL 639 continued V v − 0.07 278.00.080.06 9.7 277.4 274.5 10.7 1 7.1 . 1 . .0.14 2 ...... 0.09 282.5 27.0 . . B ...... 0.06 298.7 9.6 B P93-2313 B0.5: V [P93]; broad H 0.09 229.4 0.3 1 ...... 0.05 278.2 4.6 1 ...... 0.12 261.8 5.70.07 1 285.50.02 . . . 6.9 252.7 1 8.3 . . . 2 ...... − − − − − − − − − − − Table 7. − − α V B f 16.03 f 15.34 0.31 254.3 14.4 B . . . Member of SL 639 a 16.07 a 15.19 0.33 240.3 22.1 B . . . Member of SL 639 e 15.48 a 16.15 0.18 256.9 11.6 B ...... e 15.37e 0.02 16.36 274.9 0.18 8.3 236.7 B 11.2 . . . B ...... X X X X X X X X . . . e 16.29 0.33 244.8 34.7 2 . . . Be [Paper I]; member of SL 639 . . . e 15.54 0.25 247.7 4.6 2 ...... e 16.78 0.33 258.9 15.1 2 ...... e 16.28 0.10 ...... + + + + + + 836837 B1.5 IIIe B1 V . . . e 15.71 0.18 253.3 1.4 2 . . . Member of SL 639 829831832 B1.5-2 II833 B5 Ia834 B1 V835 B1-3 V B1.5 III B1 Ve ...... a ...... 15.13 q? . . a . 13.04 a 0.41 16.50 261.4 16.96 0.29 e 4.9 210.4 0.37 0.22 1 263.6 6.2 277.0 . . . 8.5 1 5.9 2 . . 2 ...... Member of SL 639 Member of SL 639; poss. H Member of . . SL . 639 838840 B1: II(n) B1.5: Ve ...... a e 15.81 16.74 0.28 0.24 263.4 236.7 4.5 8.9 2 2 ...... Member of SL 639; spurious Si 845846847 B1 II B2.5 V B0.7-1 IIIne ...... a f 15.30 16.78 0.15 0.11 259.9 258.4 1.4 4.4 1 2 P93-2305 . . . B1 III [P93] . . . 841842 B2.5 Ia B1-2 IIIe 848 B1.5 IIIe . . . a 15.83 0.89 258.0 3.0 1 ...... 850 B1 III 851 B2 III . . . f 15.83 853 B1-2 Ve 854 B1-3 V-IIIe 855857860 B3 Ib864 B1.5 V B1.5 V B1.5 V ...... a a f 15.34 16.26 f 16.67 0.27 0.17 16.64 248.8 0.13 255.4 252.6 3.0 3.8 3.0 1 2 1 ...... 866 B1.5 V . . . a 16.24 867868869 B1 Ib Nwk872 B2 V874 B1-1.5 V875 B0 V-IV876 B1.5 IIIe 877 B2 . V . .879 B3-5 III(n)e B1-3 V-IIIe . . . a B3 . . V-III . . . . 14.63 a . . a . a 0.13 . 16.76 . . 16.65 275.7 16.09 e . . . 0.05 0.27 2.7 f 16.30 288.8 261.5 1 16.46 f 0.00 6.4 2.3 BI 261 16.73 251.0 2 1 9.5 . . 0.11 . . . . 2 275.7 . . 4.9 . 1 ...... 804811813 B2: V814 B2 V815 B2.5 Ve817 B2.5 V821 B1.5 V822 B1 III-II823 B0 V-IV . .824 Mid-late . B[e]825 . B2-3 . . . III:e . .826 B1.5-2 Ve . . f .827 B1.5-2 V-IIIe . . . e a . B1 . . . . IIn . 17.03 B1.5 a Ib 16.54 16.56 a . 0.05 . a . p 16.81 ...... 256.5 16.68 15.53 15.60 0.05 e 9.0 e 0.19 e 271.6 0.17 0.37 . . 16.06 . 2 255.7 16.20 16.36 251.9 9.1 ...... 5.4 0.17 11.8 e 1 0.33 0.36 262.0 2 1 . . 252.9 . . 14.85 245.9 . . 8.2 . P93-2252 15.6 . . 12.4 . . . 0.17 2 2 2 . . . 242.8 ...... 9.0 2 . . . . B1.5 . . Ia [P93] . . . Member of SL 639 Discussed in detail by Member Kalari Member of et Member of SL al. of 639 SL (2014) 639 SL 639 Member of SL 639 VFTS Spectral Type801 B1.5 V Mult.? H . . . f 15.94

23 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars (stellar) = ); (9) method/lines used to σ (photospheric) absorption, ‘e’ = P-Cygni profile (used classically to distinguish = ) and standard deviation ( r v morphology: ‘a’ α Set Alt. ID Comments ] σ 1 − photometry from Paper I; (7) & (8) estimated radial velocity ( V r [km s − B continued V v and − 0.060.10 283.0 283.3 1.50.04 9.4 10.07 258.4 2 . . 238.3 . 5.5 . . . 50.8 1 B ...... V − − − − Table 7. α V B a 16.49a 0.13 16.18 a . . .a 16.13 16.48 . . . 0.02 0.07 B . . . 273.6 . . . 8.3 . . . B B ...... X X X X flat, with no indication of the nature of the line profiles outside the region of nebular emission (i.e. no strong, broad emission); ‘q’ = : ‘1’ and ‘2’ refer to the lines listed in Table 3, ‘3’ indicates the three stars for which other metal lines were used, ‘B’ indicates that the estimate is the mean value from the multi-epoch r v Column entries are: (1) VFTS identifier; (2) Spectral classification; (3) Binary status (from Dunstall et al., in prep.) (4) H 882883885 B0 V(n)886 B0.5 V 888 B1.5 V889 B1 V890 B0.5 V 891 B1-2 Ve . B2 . V . B2 V . . . a . . . 15.96 . . a . 15.90 f e 16.82 0.01 16.56 264.0 0.37 5.4 263.1 1 12.1 . . . 2 ...... VFTS Spectral Type880881 B1-2 Ve Mult.? (shell) B0.5 III H . . . e . . . 16.66 a 0.06 270.4 15.66 18.7 2 ...... Notes. emission; ‘f’ from a ‘p’ suffix, which simply indicates peculiar); (5) & (6) estimate data available (see Section 4.2,classifications with and other the relevant limitations comments. ofBI Aliases/past these (Brunet classifications as are et estimates from: al. of R/F601997); 1975); (Feast the B99 W84 et (Bosch centre-of-mass (Walborn al. et velocities 1984); 1960); al. discussed AL Mk 1999). in (Andrews The (Melnick Section & crosschecks 1985); A.3); Lindsay with W86 (10) 1964); the Sk Alternative (Walborn catalogues 1986); identifiers (Sanduleak from 1970); used T88 Andrews BE74 & in (Testor (Bohannan Lindsay et the & (1964) literature; al. Epps and (11) 1988); 1974); Bohannan Previous ST92 & (Schild Epps (1974) & employed Testor the 1992); updated P93 astrometry (Parker from 1993); Howarth (2012, WB97 2013). (Walborn & Blades

24 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Appendix A: Ancillary material A.1. Spectral montages To illustrate the spectral sequences as a function of lumi- nosity class, examples of VFTS B-type spectra are shown in Figures A.1, A.2, and A.3. The principal lines used in classifica- tion, as summarised in Tables 1 and 2 are indicated in each fig- ure. Luminosity sequences at spectral types B0.2, B1 and B2.5 are shown in Figures A.4, A.5 and A.6, respectively. For clarity, the spectra in all six figures have been smoothed and rebinned to an effective resolving power of R = 4 000.

A.2. Detailed velocity estimates For completeness, we list the individual velocity estimates from each line, calculated using the rest wavelengths given in Table 3. Tables A.1 and A.2 present the results for stars using the Set 1 and Set 2 diagnostic lines, respectively; results for the binary stars (following the discussion outlined in Section 4.2) are given in Table A.3.

A.2.1. Comparison with published velocity estimates The methods and line sets adopted to estimate radial veloci- ties (vr) for the B-type stars differ to those employed by Sana et al. (2013) for the O-type objects from the survey. As a con- sistency check between the two studies, we analysed 45 of the apparently-single, late O-type stars (with O9.5 and O9.7 types) Fig. A.7. Comparison of radial velocities (vr) estimated using the and compared our velocity estimates with those from Sana et al. methods in this paper with results from Sana et al. (2013), in which We find a mean and standard deviation between the two methods ∆v = vr − vSana, and the plotted uncertainties are the standard devi- −1 of ∆v = 0.5 ± 6.2 km s (where ∆v = vr − vSana). ations of both estimates added in quadrature. The upper panel shows The differential results (∆v) for the 45 stars are shown in the ∆v results in the sequence of VFTS identifiers (i.e. increasing right Figure A.7 (with the standard deviations added in quadrature). ascension), while the lower panel shows ∆v as a function of ve sin i. For the purposes of global analysis of the sample and identifica- tion of potential runaways, these results are in excellent agree- ment. As a further check of any systematic trends arising from the different methods, the lower panel of Figure A.7 shows the same differential velocities, but now as a function of estimated ve sin i (from Dufton et al. 2013); no obvious systematic differ- ence is present.

A.3. Centre-of-mass velocities We have investigated the expected differences between our mean values and centre-of-mass velocities using a Monte Carlo tech- nique. We assumed a sinusoidal velocity curve (i.e. circular or- bit) and, adopting the observational sampling of Field A of the survey (Table A.1 of Paper I), we calculated ranges of observed velocities (i.e. δv ) and their resulting mean velocity. We as- r max Fig. A.8. Typical errors in the average radial velocities (calculated for sumed a random initial phase, and considered periods ranging the observational sampling of Field A of the VFTS) for simulated bina- from one day up to several years. ries compared to their true centre-of-mass velocities (as a percentage of These simulated mean velocities provide us with an estimate the expected range in radial velocities, δvrmax, see text for details). of the expected error compared to the genuine centre-of-mass ve- locity. For a given period, we can then average these differences over the range of assumed phases to find a typical error. The ratio of this typical error to δvr max is shown in Figure A.8. For bina- they illustrate that the mean multi-epoch vr values should pro- ries with periods of . 250 d, the expected error is approximately vide reasonable estimates of the centre-of-mass velocities for 12-15 % of δvr max, with this increasing for longer periods, and short-period systems (. 250 d), which display relatively small then tending to a value of ∼25 % for periods & 350 d (greater peak-to-peak variations. than the maximum time-sampling of the real data). These simplistic simulations (e.g. not taking into account po- tential eccentric orbits) have probably underestimated the un- certainties but, given the observational cadence of the survey,

25 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. A.1. Example B-type supergiants (Class Ia). The primary diagnostic lines for spectral classification are identified. In the spectrum of VFTS 525 these are: He II λλ4542, 4686; Si III λλ4553-68-74; Si IV λλ4089, 4116; those identified in VFTS 269 are: He I λλ4009, 4026, 4121, 4144, 4388, 4471, 4713; Mg II λ4481; Si II λλ4128-32. The broad λ4428 diffuse interstellar band is also evident in some sightlines. 26 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. A.2. Example B-type giants (Class III). The identified lines are the same as those in Figure A.1; nebular lines have been truncated in VFTS 335 as indicated.

27 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. A.3. Example B-type dwarfs (Class V). The identified lines are the same as those in Figure A.1; nebular lines have been truncated in three spectra as indicated.

28 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. A.4. Example luminosity sequence at B0.2. The identified lines are the same as those in Figure A.1; we note the greater intensity of the metallic lines with increasing luminosity (including the C III + O II features at ∼λ4650).

Fig. A.5. Example luminosity sequence at B1. The identified He and Si lines are the same as those in Figure A.1.

29 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars

Fig. A.6. Example luminosity sequence at B2.5. The identified He and Si lines are the same as those in Figure A.1 and the nebular lines have been truncated in VFTS 335 as indicated.

30 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars n σ r v continued on next page 4713 λ He I 4575 λ Si III 4568 λ Si III 4553 λ Si III 4553 λ (LR02) (LR03) Si III 4438 λ He I Line-by-line radial-velocity estimates for single stars using the Set 1 absorption lines. 4267 λ C II Table A.1. 4121 λ VFTS He I 003010024028 268.3029 289.9031 . . .034 263.3 271.3044 288.0 .046 . . 275.0050 280.0 269.2 . 282.8 . .052 292.9 284.5053 242.3 292.6060 282.3 . . 268.0 . 284.2062 265.8 276.4 285.3 289.5 296.6069 275.1 248.5 292.9075 254.9 283.8082 277.7 289.8 279.7 278.7 263.9 287.6095 282.7 . 280.2 . . . 277.0 . 230.1 .111 271.4 303.9 286.1 282.7113 280.1 286.1 273.9 280.7 291.2119 284.6 264.0 293.1 285.7 284.6 279.2121 238.7 268.1 292.7 281.2 299.4 308.7124 279.4 . . 277.7 . 288.9 288.2126 274.2 296.5 281.5 . 271.9 280.1 . . 264.8 . . .152 274.3 280.6 282.5 276.7 236.0 284.1159 287.5 291.5 289.0 329.1 276.1 281.4 282.7161 282.5 252.8 296.1 271.2 .164 285.9 . 262.8 276.7 . 282.3 . 278.6 273.4 . . 277.8 283.0 . . . 280.5170 261.0 265.4 290.1 . 298.6 277.0 . . 297.7178 283.8 . 284.5 . . 252.0 265.2 281.6 . . .183 275.4 278.2 289.7 . 285.8 . . . . . 281.9186 269.0 288.6 274.4 281.6 274.9 279.0 2.1 289.9 . 280.1 .200 . 295.2 287.9 . . . . . 273.5 283.6 255.3 . . 282.2 . . . 285.7 .202 8 . 289.1 257.9 . 283.7 . 285.6 274.5 . 268.5209 281.3 256.8 275.6 4.4 265.4 265.3 296.7 274.8 . 4.4 294.7 .214 285.3 279.0 . 248.6 293.5 279.7 3.0 287.9 287.1220 251.0 8 275.5 285.7 281.2 276.5 7 239.8 285.5 295.5 . 277.5226 . 271.5 8 . 275.7 . 280.0 . . 279.8 280.5 . . 278.5 3.9 .232 264.0 278.9 273.3 276.6 . 247.7 282.4 284.5 280.0 . 283.1 287.1 285.0 . 242.2234 278.5 284.4 288.1 272.8 4 274.3 251.2 . 281.5 . .235 289.5 273.6 281.9 8.4 2.0 276.4 271.7 274.5 . . 308.3 7.6 279.8 . 253.9237 277.3 282.2 7.2 290.3 272.2 284.2 265.0 269.1 270.0 . .241 5 286.8 8 297.7 . . 287.4 244.5 . . 13.8 7 282.6 2.0 287.5 274.9 316.2 6 270.3 2.0242 14.3 286.2 254.0 266.0 275.2 276.1 4 253 265.4 8 268.0 306.5 255.4 7 291.0 . 2.7 276.6 275.8 8 . 197.1 283.5 . 280.7258 277.4 253.6 257.0 252.6 296.7 283.3 281.9 287.4 .261 . 273.1 8 307.0 . 215.8 292.7 272.0 269.5 256.8 . 1.7 .268 . 272.4 . 279.3 . . 2.4 272.0 254.2 283.8 . . 268.7 . 294.3 257.0 182.9269 274.9 288.4 275.1 285.5 7 275.3 297.2 283.3 285.4270 8 292.6 281.0 284.1 . . . 4.2 275.8 269.0 278.0 . 3.8 259.4273 . 10.5 . 258.1 . . . 283.4 278.6 . . . .276 . 287.5 8 . 275.1 267.7 280.2 267.4 196.6 7 288.2 257.8 5 289.4 274.2 268.4 286.5 . 275.8 . 268.1 .284 267.7 275.8 266.3 286.4 2.8 254.1 279.4293 262.5 277.5 3.7 256.3 246.6 2.2 274.3 218.4296 291.1 8 . 3.9 252.7 . . 269.2 2.6 267.5 287.2 299.0 6 271.1 185.2 269.1297 283.7 8 251.9 . 281.8 273.8 . 278.4 282.9 . . . 265.1 . 271.3 2.9 280.6 6 302 8 284.6 259.0 255.9 6.1 . 264.3 . 275.7 .303 8 220.6 . 256.2 . 278.7 279.9 263.8 . . . .307 294.7 8 268.5 287.1 252.6 265.3 276.0 255.6 186.0 284.5 268.2 263.8 273.7 281.2 .308 . 269.3 . 265.1 260.6 . 2.7 253.4 ...... 280.3 263.0 269.7 3.2 264.3 252.1 256.1 214.5 263.4 8 287.8 274.2 252.8 . . 277.3 278.0 . 246.6 282.2 285.1 270.7 260.9 8 178.6 10.6 262.6 277.6 260.8 264.1 264.1 274.4 276.6 261.7 . 1.7 . 254.5 . 300.4 8 262.0 . 282.6 282.0 . 273.2 7.9 . 7 278.2 217.0 2.3 275.4 262.5 255.7 10.0 281.4 273.1 243.2 273.2 290.1 281.9 295.5 266.0 196.4 261.8 266.0 3 265.6 259.0 . 257.2 8 . 3 . 1.7 250.9 2.6 267.4 284.2 280.9 288.6 . 258.3 273.6 . . 191.2 272.2 249.9 8 206.0 253.6 282.6 265.5 241.8 7 268.5 264.2 255.3 264.0 273.3 262.3 . . . 2.5 265.6 261.7 6.5 8.0 250.7 287.9 282.6 . . 273.9 8 286.3 . 249.5 250.7 260.9 284.8 7 217.2 2.4 267.6 250.9 3 268.6 245.2 261.8 10.5 267.4 264.4 17.3 262.9 3.3 8 289.2 8.7 8 . 238.1 . 216.0 . 7 4 287.3 269.8 253.1 266.6 8 271.8 . 268.1 248.0 . . 258.7 269.5 3.6 287.3 . . 267.6 262.6 . 285.0 258.5 7 270.7 266.9 5.9 262.8 261.6 270.9 266.8 264.9 246.9 2.2 272.0 261.8 7 2.1 2.1 253.8 265.2 . . . 7 2.3 256.8 . . 5 8 . 261.3 4.9 272.7 270.9 8 252.2 . 5.9 . . 8 272.1 267.9 . . . 3.9 260.4 8 251.7 14.5 8 260.5 273.9 264.8 1.9 3 2.2 269.7 7 263.7 250.0 1.6 272.7 8 8 270.5 7.8 2.0 263.5 5 8 4.2 1.9 6 7

31 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars n σ r v continued on next page 4713 λ He I 4575 λ Si III 4568 λ Si III 4553 λ Si III 4553 λ (LR02) (LR03) Si III 4438 λ He I continued 4267 λ C II Table A.1. 4121 λ VFTS He I 310313315316 272.8331 265.5346 259.5347 269.1 264.2353 286.5 269.8360 296.8 263.7363 267.6 265.3 268.7369 296.8 274.1 270.5370 260.0 268.9 261.8376 258.5 263.3 275.6381 269.9 263.0 290.1 278.6384 269.4 237.2 260.4 .413 . 262.1 . 262.8 268.4 . . .417 267.1 246.9 260.0 265.4 289.8420 270.0 275.3 241.5 271.5423 263.4 277.2 260.2 260.3424 265.2 271.1 . 249.6 . 267.0 263.5 .426 289.0 268.1 . . 264.8 . 277.9 227.5 . . .431 268.7 286.1 265.1 . . .452 264.7 261.1 265.1 258.0 270.7 241.8458 267.1 263.0 290.4 256.2 . 269.2 . .469 231.8 . 274.7 265.2 . . 283.7 . 280.1 275.2 . .471 268.3 268.2 264.8 264.3 254.5 275.9 260.6478 246.2 267.4 276.3 258.8 270.0480 264.4 275.4 290.8 277.8 271.3 239.5 267.5 274.5498 274.4 . 254.2 . 263.8 . . 269.1 259.3 . 245.7 . 271.8 283.0504 252.3 264.1 265.9 273.4 277.3 270.2 224.0 273.2516 271.9 259.7 279.1 270.7 264.4 266.1 . . .533 289.5 229.6 278.7 . . 275.7 271.3 . 3.7 261.6 268.9535 256.9 266.2 281.0 240.6 274.1 268.8 266.6 3.3 269.1 251.1 274.0 . 263.8 . .540 8 265.8 248.1 262.6 . . 1.5 279.4 277.3 . 259.0541 269.3 8 257.4 257.2 3.4 274.7 261.9 284.7 223.6 . 271.5553 . 263.8 8 . 296.7 7.3 267.5 260.0 267.6 . 258.1 . . 282.0 .560 . 273.1 8 15.4 267.4 . 267.8 255.0 246.3 241.1 261.8569 273.7 8 265.5 . . 260.7 . 2.5 272.2 8 . 259.2 . 292.7 .572 263.0 235.6 278.8 . . . 271.6 . . 264.1 271.3 .578 270.8 8 265.4 263.5 . 252.0 281.0 . 262.7 . 274.8 264.6 . . 249.1 . 3.3590 . . 229.8 ...... 279.2 2.9 234.6 274.5 256.0 .593 269.1 271.7 255.7 7 274.9 235.4 2.9 268.1 274.7594 8 265.8 264.5 264.3 4.6 269.1 240.6 . 279.3 . 264.1 .598 273.7 8 279.8 . 285.5 275.6 . . . . . 264.8 . . . 242.1 .607 . 259.8 8 274.3 . . 271.4 292.6 . . 246.8 277.6 273.9 . 271.3 4.4 . . 271.6 .616 . . 266.0 272.5 274.6 5.5 260.7 266.6 . . 8.0 .622 246.9 270.6 279.3 4 285.5 . 274.6 . .623 8 . 12.5 . 256.4 . 7 291.3 287.7 264.0 . 252.1 249.3 . 263.4 266.5 270.6 . 273.1 228.3625 272.1 271.6 271.0 231.3 273.3 264.0 265.9 8 . 294.4 . 278.3 .627 263.7 298.6 . . 245.6 . 275.5 281.8 283.5 3.4 263.2630 7.2 279.4 . 266.7 . 251.8 . 270.2 292.9 4.3 262.0639 251.0 277.0 253.4 . 306.7 . 7 237.6 . . 279.2 3 . 259.3 . 4.4 . 2.6 265.6 . .650 273.2 . . 271.5 274.4 270.0 . 7 277.7 2.4 276.3 269.5666 246.8 278.2 251.0 292.9 4 7 268.3 275.6 267.7 . 281.4 .668 281.3 8 . 265.4 277.4 263.3 316.9 2.1 267.0 246.6 237.4 . 252.8 270.7 . .672 284.5 288.0 265.3 266.8 2.6 272.2 277.7 282.2 279.7 . . .673 8 11.2 267.9 4.0 255.5 254.6 288.1 276.3 7.6 . .681 259.1 8 . . 271.6 . . . . 270.2 266.0 . 3.3 289.6 8 6 248.8690 243.4 . 246.0 245.1 . 4 . 287.7 . 270.5 . . 269.7 . . . 269.9692 267.6 8 268.5 276.4 278.8 256.8 . 289.3 . 259.1 . 263.8 243.8 . . 266.2 . 254.7 . 254.9 269.6 . . 265.1 247.7 286.5 252.5 267.8 246.3 249.0 213.1 285.7 241.8 278.3 270.8 269.1 302.8 275.7 271.0 . 269.7 4.4 264.6 258.0 . 278.0 277.1 . 273.9 273.4 280.1 256.8 256.9 267.2 4.6 251.4 . 247.0 . 267.1 8 . 261.0 283.0 264.8 276.3 6.3 269.6 . 266.4 . 10.9 283.3 249.0 . 250.3 215.2 . 4 . 14.2 267.5 . 275.2 2.7 299.5 279.0 255.4 264.0 280.6 258.6 4 5 4.6 273.5 275.4 4 3.1 265.3 267.3 269.0 258.3 7 249.4 264.0 270.3 252.6 8 271.1 7 253.7 267.8 274.5 . 282.8 274.6 . 220.5 . 1.9 277.1 274.1 294.9 4.1 252.4 255.9 . 280.1 . 7.5 . 278.0 . . 7 . 269.5 4.9 266.9 254.1 269.4 8 . 262.1 274.4 . . 3 247.1 291.5 272.3 8 270.1 225.6 282.7 274.6 6.2 280.2 273.9 253.4 13.1 258.8 266.7 279.8 3.7 258.8 271.8 7 227.4 283.9 253.7 . 4 . . . . . 7 271.5 4.5 275.8 271.1 283.0 . . 10.7 . 277.5 280.5 252.5 8 14.5 301.8 270.8 8 . 266.3 . 268.5 . 268.0 268.4 300.8 8 324.5 259.4 290.2 271.4 285.6 277.9 1.9 268.8 279.2 2.7 257.8 269.5 10.7 3.0 271.3 7 310.7 286.2 3 268.2 2.9 . 5.8 255.5 3 8 . 277.3 . 278.7 7 284.4 9.2 3.0 269.2 8 2.1 5 8 280.3 2.3 277.1 279.5 8 269.6 268.2 8 1.5 272.7 3.2 271.2 8 14.7 264.0 7 2.5 8 14.5 8 6

32 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars , from eqn. 2); σ n σ r v , from eqn. 1); (12) standard deviation ( r v 4713 λ He I 4575 λ Si III 4568 λ Si III 4553 λ Si III 4553 λ (LR02) (LR03) Si III 4438 λ He I continued 4267 λ C II Table A.1. . σ 4121 and λ r v VFTS He I 696707711712 261.0714 277.3725 235.8727 249.2 265.9728 279.4 276.9729 286.1 253.7732 274.7 240.2 263.7735 256.4 285.1 276.1740 254.4 285.9 258.0745 264.1 275.7748 265.8 . 267.0 . . 267.7 283.0753 276.0 265.6 261.1 286.3756 254.5 279.4 268.0 266.5762 258.3 275.7 265.3 252.6772 284.9 267.9 274.0 271.3 271.5 245.9795 285.9 261.6 274.4 250.0 267.5801 274.4 276.1 259.6 271.2807 266.3 266.5 244.5 278.1 283.3 270.0 276.9811 268.2 275.5 266.5 273.1 283.3 271.6814 269.0 234.0 283.8 253.0 261.0817 261.9 . . 292.4 . 254.1 260.0 264.5 267.2823 266.2 284.2 278.2 246.8 281.4 294.0 272.1 .829 . 283.2 . 282.3 262.2 284.9 267.1 260.3 235.2831 264.4 234.7 .835 . 269.2 . . . 269.1 284.5 . 235.0 . . . 276.2 265.8 281.6 .841 289.8 259.3 . 274.8 272.4 . 278.6 271.5 292.6 . 284.5 . . 270.7845 259.1 245.8 267.9 223.6 269.9 265.8 258.2851 257.0 276.0 275.0 265.8 276.3 260.6 287.3855 285.6 266.3 260.2 252.5 2.3 244.4 288.8 274.5 279.8 . . .860 272.1 . . 287.8 271.6 259.5 . 257.2 211.0 2.0 245.0 267.4 267.7 . .864 8 . . 265.5 . 229.5 . 252.5 8.7 283.4 255.1866 273.0 8 . 275.6 271.3 246.5 . . 288.9 258.6 285.3 266.7867 289.2 8 277.3 299.6 255.6 10.9 258.9 1.9 203.4 270.1 284.4 261.4868 261.1 . 266.7 . 278.2 . 228.7 1.8 265.8 254.3 . 267.5 . . 7 . .872 8 . 271.4 258.6 251.4 268.6 255.8 253.7 261.5 290.2 .879 8 . 269.6 271.4 . 252.0 9.6 267.3 259.6 258.4 . .881 206.8 . . 10.9 277.5 . 264.6 . 259.9 275.3 262.2 272.9 249.6 229.4885 250.2 8 256.4 276.3 268.5 1.4 267.3 249.6 8 .886 255.9 . 273.7 301.8 281.2 . 275.6 290.9 3.0 275.7 . . 249.4 . . . . 259.6 8 286.2 283.3 258.2 1.9 260.4 202.6 271.0 . 256.5 . 5 . 255.1 270.1 280.1 . . 3.7 269.6 249.7 260.9 ...... 246.4 8 . 253.9 . 277.2 3.6 281.6 253.9 274.4 268.9 256.6 8 . . 282.9 . . 4.2 257.9 261.6 . . . . 271.8 8 13.5 . 206.7 266.3 . 266.5 . 289.9 . 264.6 4.9 255.5 8 242.8 255.2 264.5 243.1 277.9 8 276.9 275.3 257.7 4 . . . 256.6 282.6 . . . . . 260.1 . 259.9 280.3 259.0 279.0 250.3 215.6 292.2 287.6 249.8 265.6 270.1 255.5 255.5 . 259.5 251.7 . . 12.6 246.3 . 275.1 . 263.8 . 277.4 281.7 250.9 9.0 291.0 278.0 5 259.8 260.9 229.8 265.3 267.2 253.7 210.5 281.0 10.7 . 263.1 . 281.9 6 . 251.9 260.0 246.8 267.3 1.7 9.7 248.8 7 6.1 260.3 275.0 11.8 271.6 210.4 281.8 6 243.8 261.4 264.8 5 262.6 264.3 251.9 3 . 7 . . . 291.4 . . . . . 9.1 6.2 258.0 263.9 248.5 277.5 4.9 252.4 3.4 259.9 278.8 5 8 250.7 282.5 7 3.0 257.7 . 8 . 248.0 . 1.4 248.8 8 229.5 261.6 248.3 . . . 285.0 262.9 252.6 13.1 8 280.5 3.0 281.7 262.5 4 229.4 3.0 261.8 278.2 8 275.7 253.0 . . 8 260.5 . 293.7 0.3 5.7 261.5 4.6 285.9 2.7 5 8 7 2.3 285.5 8 263.5 263.5 283.0 8 273.6 6.9 1.5 258.4 264.0 7 275.7 8 5.5 5.4 4.9 8 7 5 ) used in calculation of n Column entries are: (1) VFTS identifier; (2-10) estimated radial velocities from each line; (11) weighted mean velocity for each star ( Notes. (13) number of lines (

33 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars n σ r v continued on next page 4922 λ He I 4713 λ He I 4388 λ He I 4144 λ He I 4009 Line-by-line radial-velocity estimates for single stars using the Set 2 absorption lines. λ Table A.2. VFTS001 He I 004005007 287.9008 299.2012 281.7013 282.1 279.4020 282.6 293.7036 284.0 . . .038 290.5 282.6 283.3040 254.5 266.1 280.1043 244.0 285.6048 274.3 295.5 279.2 306.2054 303.5 271.9 . . . 276.2066 281.2 271.4 273.4068 282.0 274.3 278.4 284.5070 310.8 246.8 273.7 . . . 272.9071 289.9 269.0 260.1 . . 276.5 . 289.4078 297.9 278.4 278.9 272.5080 297.1 302.7 295.5 283.3 283.1 297.8083 282.1 265.6 274.1 . . 282.6 . 259.7084 . 278.7 . 10.8 . 273.7 . . 264.5 . 273.8085 279.6 4.2 291.7 291.3 286.2 307.2 289.0 2.6 5 088 290.2 274.1 . . 4 . 282.7100 271.3 284.0 281.1 5 285.7 . . 235.3 290.9 . 243.2101 306.1 284.5 283.0 289.7 . . . 280.6104 266.5 . 6.9 284.2 . . 1.6 290.5 270.9 4.3109 258.8 242.3 4.9 255.2 276.3 4 278.0 279.0 3 122 . 279.5 . . 5 289.9 . 16.3 . 264.9 4 . 279.2127 291.9 267.5 242.6 270.8 283.1 269.6 282.8 4.1128 283.9 4 254.1 258.1 . . . 273.5 18.4134 263.6 289.0 291.4 5 280.1 . 265.7 281.0 . .137 274.1 285.4 235.5 312.1 277.1 3 232.5 272.9 293.4 12.6141 4.4 294.5 19.9 293.3 . . . 258.5148 277.4 3.3 253.7 13.6 285.2 3 263.5 4 294.7 269.5 5 149 254.8 287.3 288.9 279.7 249.4 4 268.1 259.8 5 156 271.3 12.5 279.5 . 24.0 . 283.1 . 283.5158 268.4 258.0 273.2 256.2 . . 284.1 . 5 166 . 259.7 . 4 . 279.7 . . . 242.7 . 3.7 .167 280.3 . 281.2 4.3 272.0 284.4 276.2 272.9 5.1181 264.7 5 268.9 . . 272.7 4 . 274.1187 275.3 287.3 5 287.0 284.3 3.8188 285.3 . 275.4 . 268.5 . 269.0 . . 281.2 . 285.2 . .194 284.0 . 267.4 5 3.7 276.4 . . . 257.1196 3.6 284.1 267.0 . . 278.2 271.2 . 282.1 3 201 277.3 7.4 312.8 257.6 290.6 . . 4 . 308.9203 287.3 270.3 271.9 4 310.1 4.7 238.2205 284.1 289.0 . 4.8 264.5 . . 1.4 294.1 268.7 280.4207 265.1 290.2 5 284.3 4 285.1 3 210 . 5.6 278.5 . 278.2 260.7 . 275.7 . . 284.2 . 273.8212 277.4 286.0 263.8 243.3 267.1 . . 4 . 270.7 17.6219 285.8 270.3 293.4 . . 281.4 . 280.9221 284.0 290.2 8.7 286.3 262.8 5.5 272.8 3 264.5 294.8224 284.6 278.1 . . 4 274.6 . 278.4 5.2 3 228 . 3.1 278.4 . . 9.4 287.4 . . . 276.8 8.8229 269.1 . 249.6 . 289.8 . 5 296.1 4 275.7 9.6 3 230 288.8 . 235.1 . . 5 288.0 279.6233 283.0 273.9 283.8 5 298.5 297.4 286.9 283.2234 256.5 268.6 285.7 266.9 . . 279.1 . 289.4 18.3238 251.7 282.1 259.2 274.4 258.4 284.1 5.0 19.3239 278.9 280.4 257.3 285.7 3 281.7 270.2 . . 280.8 265.9 . 244.4 5 5.6 283.6 3 11.9 277.9 263.3 282.6 254.8 14.8 272.7 286.4 299.2 3 292.4 . 8.5 267.2 . 4 13.0 273.9 . 251.1 279.2 5 271.9 265.0 256.9 . . 4 272.8 . 276.4 5 276.7 292.6 292.5 278.7 271.3 7.1 285.5 284.9 279.2 . . 277.9 . 256.3 6.8 297.2 4 290.5 247.5 3.7 254.6 5 7.8 . . 286.2 . 269.4 9.7 267.4 . . . 5 282.1 4.3 3 277.9 5 . . 261.4 . 2.5 262.3 . . . 5 261.7 285.7 282.5 5 281.2 8.2 ...... 12.6 229.9 263.9 5 227.9 279.7 6.5 258.9 3 25.8 272.8 5 247.0 7.5 248.2 3 268.4 268.5 11.0 10.3 5 11.9 13.5 3 5 274.7 4 5 6.5 4

34 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars n σ r v continued on next page 4922 λ He I 4713 λ He I 4388 λ He I 4144 λ He I 4009 continued λ Table A.2. VFTS247 He I 254263274 293.9279 251.6282 250.0283 278.8 289.5286 242.1 256.3287 241.5 267.8288 260.0 256.3 291.6292 277.0 266.4 252.2295 282.5 253.5 291.8298 264.2 248.2 251.3300 304.5 256.9 279.6 278.5301 254.0 . . . . 242.3 . .309 334.0 246.4 . . . 257.3320 280.6 296.5 261.9 . . . 272.9321 256.7 267.7 262.4322 265.8 288.2 327.3 240.8 293.6 261.0 295.8326 241.7 290.0 259.7 264.5328 . 263.4 . . 258.9 . . 235.6 . . 4.1 .330 250.7 . 284.0 289.3 281.0 . . . 336.2335 269.5 300.2 236.0 248.6 5 265.7 285.5340 252.9 275.3 5.6 297.8 270.1 251.2 260.5 280.9343 262.6 261.1 262.5 14.1 284.5 4 252.1 282.4 16.8348 250.2 19.7 257.6 244.0 . 14.1 . . 318.1 . .349 294.4 . . 254.2 . 4 264.7 . 320.2 3 262.3 6.0 5 354 278.4 262.6 238.1 4 269.3 258.0 277.9358 294.1 261.8 5 247.2 263.6 256.1365 4.4 258.2 268.0 264.7 265.0 . . . 307.5 7.2 322.7367 . 250.1 . . 254.0 . . 4 . 272.9 . 4.9 . 11.4368 297.7 . 148.3 269.2 5 267.5 276.7 251.8373 273.1 307.7 5 280.0 . 3 . . 258.9387 328.2 275.8 12.1 332.1 265.1 281.8 241.0 12.0394 268.4 272.3 . 249.2 . . 165.1 272.0 . . 5 397 245.2 . . 262.5 . . 4.0 266.0 3 272.3 7.6401 9.0 246.6 316.5 271.7 . . 258.9 . 259.5 3 403 247.1 264.7 291.3 5 215.7 . . 4 . 175.4414 276.9 279.4 247.1 258.6 274.2 . . 313.7 . 262.9 22.1421 250.1 259.2 262.1 294.3 11.1 267.7 272.7425 250.9 5.6 245.9 . 3 . 221.4 248.7 . 227.1 8.8428 8.8 285.2 4 259.1 . . 227.7 . 275.1 4.4 3 447 301.9 273.0 268.4 5 246.4 4 308.0 2.2448 251.7 268.6 . 296.2 . . 5 247.6 228.1449 240.5 277.0 5 261.9 . 16.2 . 234.8 269.4 . 290.2452 264.6 265.4 264.5 . . . 301.2453 . 9.3 229.0 . 4 259.1 267.8 . 260.5 . . . 255.7 7.7461 250.7 276.0 284.6 . . 4 270.0 . 254.3463 262.9 5 4.0 272.5 . 12.3 . 269.4 . 261.1467 . 263.2 . 10.9 164.7 . 281.0 . . . 279.4 3 473 . 252.8 . 4 . 269.6 . . . 297.9 6.0 5 10.7474 . 276.8 . . 261.5 . . . 266.6485 . 331.7 . 229.6 . 5 266.0 . 3 . . 269.0486 . 225.4 . 271.4 . 283.9 . . . 275.1 12.4489 . 244.9 . 286.3 . 286.0 . . . 258.0495 260.3 . 282.5 . 239.4 . 5.4 277.5 3 263.6 24.2499 . 276.4 . 276.7 . 264.1 . . . 279.7 3 523 . 282.6 . 269.7 . 8.9 248.8 . 3 . . 275.9 13.2530 258.9 . 277.7 . 256.5 251.2 . 269.7 355.6 23.3 3 539 . 308.2 . 264.2 . 264.0 . 3 . . 276.4543 281.8 265.8 3.4 247.2 . 3 . 256.9 264.6 . 274.3 11.6 313.5 252.7 276.2 273.4 . . 246.7 . 275.7 3 294.8 286.5 4.8 288.8 . 3 . . 300.7 5.8 13.6 267.0 249.6 269.5 . . 258.6 . 277.2 3 265.8 . . . 5 8.5 276.0 . 3 . 276.7 o9.2 . 280.7 258.7 . 12.3 . . 284.5 3.6 3 . . 4 . 257.5 . . . 264.7 275.2 . . 4 264.4 . 5 . . 254.5 . 289.2 254.9 10.9 276.2 269.2 279.8 1.3 . . . 251.2 257.1 . . 4 322.3 . . . . 3 264.1 . . 265.6 . 4.7 . 19.3 . . 30.2 . . . . 14.0 . . 3 4 275.4 . 3 . 272.6 . . . 4 280.0 . . . 268.9 . 4.8 7.8 15.6 . . . 15.1 3 . . 293.1 . 5 3 . . 271.0 . 3 10.1 290.3 271.5 6.9 3 14.2 253.1 11.4 3 3 3.3 3 3

35 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars n σ r v continued on next page 4922 λ He I 4713 λ He I 4388 λ He I 4144 λ He I 4009 continued λ Table A.2. VFTS547 He I 551554556 265.9563 294.9567 266.9568 251.9 259.6570 282.5 . . .574 283.5 274.9580 268.7 . 240.9 . .584 253.9 277.6592 268.2 277.7 272.5 247.3600 279.1 268.4602 250.8 261.7 . . . 280.9605 234.4 267.9 . . . 279.4610 278.6 246.4 285.7 . . .615 300.0 248.3 . . . 322.8620 287.8 316.7 268.0 269.5624 . 245.3 . . 277.0 . . . 284.0 . .629 . . 246.9 . . 299.4 261.3632 . 286.9 . . 293.6 . . 245.0 . 261.2 . .633 240.6 . 260.9 255.9 249.6 290.7636 280.4 284.7 275.6 . . 250.2 . 302.9 10.3 271.2640 260.5 285.4 272.1 276.1 . . . 287.9643 274.8 265.3 7.1 266.9 . 3 10.2 . . 254.4 270.3644 272.1 . . 267.5 . 2.9 237.7 . . . . 254.6 . . 3 646 264.9 4 281.4 . 13.3 . 264.7 . 292.2 12.4 3 659 . 247.3 . 280.3 . 277.2 . . . 259.9660 . 216.8 . 4 279.4 . . 3 . . 278.9 8.4670 . 255.4 . . 6.9 252.4 . . 297.9 . 282.9 237.8 30.4671 279.0 265.5 283.3 5 252.5 279.4 3 676 . . 253.3 . 266.9 . 3 . 243.2 . . . .678 279.8 285.5 257.4 2.6 261.5 . . 232.8 . 253.3679 312.9 248.7 251.3 261.0 5.7 264.3 18.4 266.9 242.6 13.2 3 683 278.6 281.3 295.0 301.0 250.1 3 684 245.8 265.7 4 269.7 3 26.3 271.9 278.0 270.1 278.3685 262.7 262.1 262.9 274.7 1.6 274.6 265.7 . .699 . . 8.4 261.5 . 4 11.8 261.0 . 249.7 . 10.0 . . 3 701 265.3 266.0 . . . 4 284.7 . 278.7 . 5 .709 260.2 229.7 4 253.4 268.2 . . 274.0 . 254.4720 252.2 4.9 280.4 11.1 265.1 261.9 277.5 237.7726 281.6 266.3 4 256.0 287.6 7.2 5 19.9734 304.1 258.1 225.1 263.8 270.2 . .738 . . 294.0 . 269.0 241.5 . 5 249.5 . 3 . 264.6 . 263.6 5.0741 250.9 267.5 263.6 . . .747 247.7 305.2 5 5.2 271.6 . . 264.9 . 278.5749 263.9 265.8 269.4 8.2 272.6 248.6 301.0 267.5 242.0 3 754 269.1 240.7 . . 237.3 4 286.1 . 256.2 4.6 20.2757 4.8 274.6 269.1 259.3780 253.4 . 257.2 . 13.8 265.9 257.1 . 5 273.8 3 258.9 4 292.4 . .781 255.3 . 234.5 270.5 . . . 261.4 5 14.7786 264.9 269.9 . 13.3 . 299.4 265.5 . 265.7789 270.2 265.4 272.1 274.6 . 3 . . 302.4 . .794 306.1 . 268.0 4 244.0 11.2 255.5 1.8 18.7 298.0796 271.1 283.0 275.3 . . . 271.7798 . 245.2 . 4 . 5 245.0 . 3 15.7 . . 258.0800 243.4 . 267.8 . 302.0 278.6 . 260.9 . . 272.2 . 242.9804 284.1 274.7 4 290.2 22.5 271.4 13.1813 266.7 279.1 264.4 283.6 239.2 298.4 242.3815 265.5 276.7 277.7 4 266.6 271.6 3 270.9 287.2 12.0823 244.5 248.6 288.0 . 264.2 4.8 . . 10.1 249.7 285.8 . 6.5 271.1 . 267.9 . 254.3 3 261.0 263.7 238.7 252.1 264.0 5 247.2 3 12.1 4 263.2 294.8 259.8 237.2 . . 270.2 . 290.7 8.9 4 10.9 279.5 284.4 271.8 . . 264.8 . 250.4 266.1 230.7 259.9 . . 4 240.2 . 286.3 2.5 5 14.1 253.1 . . 273.4 . 7.2 5 . 3 . 243.4 . 268.5 4.0 245.5 260.4 . . . 5 262.0 248.9 6.3 11.4 5 ...... 5 . 5 274.0 . . 219.1 272.7 ...... 266.3 . . . . 12.0 11.5 263.6 247.1 . . 4 278.9 255.9 . 3 15.5 19.5 257.4 284.9 286.3 12.1 245.3 3 5 268.9 6.9 3 272.1 255.7 274.5 256.5 17.2 3 5.4 262.0 7.1 9.0 3 5 4 3 8.2 4

36 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars , from eqn. 2); (9) σ , from eqn. 1); (8) standard deviation ( n r v σ r v 4922 λ He I 4713 λ He I 4388 λ He I 4144 λ He I 4009 continued λ Table A.2. VFTS824 He I 825826832 223.0833 . . .836 241.6838 259.6 258.8840 286.6842 252.7 243.1 244.1843 270.3 262.4 248.9846 246.9 277.0848 192.8 251.8 256.5853 241.8 295.3 260.2 258.5857 249.2 225.1 . 276.4 . .869 242.5 260.6 255.1875 239.5 237.0 281.0 258.2 . .876 289.5 . 253.6 250.1 244.7880 298.0 246.4 . . . 277.9 260.4882 245.8 230.8 264.5 . . 245.9 . 275.2889 254.1 262.9 256.7 . . . 277.1 12.4 283.1 . . . 242.8 . 249.9 . . 210.8 262.7 280.1 242.8 268.5 263.6 272.8 5 284.5 252.9 261.1 . . . 260.5 9.0 . . . 265.0 283.1 8.5 15.6 277.0 257.2 5 296.1 234.1 259.1 . 285.1 . . . . . 5 255.1 . 3 . . 235.9 263.4 257.3 5.9 253.3 269.0 236.7 . . 4 . 287.0 . . 244.8 . 280.6 4.5 1.4 . . . 265.9 252.7 277.9 8.9 250.3 . 34.7 . 4 . 3 . . . 4 247.7 8.8 4 258.4 . . 294.0 255.4 ...... 261.7 4 . 4.6 258.9 4.4 254.4 3.8 288.8 4 15.1 3 252.7 5 271.2 242.4 251.0 6.4 3 251.8 8.3 4 283.3 9.5 270.4 4 263.1 4 18.7 9.4 12.1 3 4 4 . σ and r v ) used in calculation of n Column entries are: (1) VFTS identifier; (2-6) estimated radial velocity from each line; (7) weighted mean velocity for each star ( Notes. number of lines (

37 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars r max δv 6.4 16.9 7.99.1 20.0 23.1 9.5 25.4 9.5 25.4 21.630.531.0 52.6 11.9 65.7 11.3 72.1 42.5 21.4 22.8 28.4 18.4 111.4 19.0 51.2 11.5 56.3 13.3 40.1 23.7 23.8 15.9 32.4 15.2 56.5 52.5 39.7 14.5 38.7 12.6 136.6 24.4 34.2 14.8 34.0 59.7 69.9 32.5 12.9 185.9 12.7 28.7 36.813.2 31.0 12.8 84.5 63.0 33.6 30.0 15.8 121.7 52.6 32.0 28.835.8 152.1 65.4 63.2 11.9 89.5 12.8 163.8 46.1 27.8 45.8 33.0 50.4 103.5 25.1 107.8 46.0 123.3 17.3 64.3 14.7 118.0 11.1 40.8 43.4 36.7 24.9 31.8 10.5 103.6 29.9 57.8 21.7 25.6 22.1 67.5 64.2 65.5 58.5 17.7 168.0 48.710.9 38.9 14.2 120.8 68.8 29.1 73.5 35.5 141.4 23.1 180.0 58.7 r ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± v continued on next page n σ single v 4553 λ Si III 4438 λ He I 4388 λ He I 4267 λ C II 4169 λ Line-by-line radial-velocity estimates for single-lined binaries using absorption lines in the LR02 observations. He I 4144 λ Table A.3. He I 4009 λ VFTS009 MJD 54817 He I 302.0 293.5 . . . 293.8 288.7189 54824 . . . 194.6 291.5 180.5225 293.6240 54815 . . . 4.8 54809 272.8 5 293.2 112.2 . . . 265.9 130.1 272.6 172.4 . . . 264.3 . . . 259.8 ...... 263.8 125.3 181.5396 264.6 9.0 . . . 54809 265.4 3 224.2 274.0 4.5 . .534 . 7 281.6 289.2 54828 123.2 275.1 . . . 7.0 3 292.4 224.2 . . . 270.1 257.4 ...... 281.3 . . . 275.4 258.0 . . . 21.5 3 277.9 270.9 6.3 5 278.2 015017018 54817025 54828027 54860 289.3033 54828 250.3037 54748 292.8041 54748 300.0 310.7097 54828 327.1 261.8106 54748 255.2 295.5107 54748 297.7 308.3118 54822 295.9 . . . 335.3133 54822 . . . 252.5135 . . 54824 . 290.8 . . . 288.2144 54824 289.0 . . . 297.2146 340.5 54817 272.8157 . 54815 . . 294.8 . . . 289.2162 . 291.6 54748 . . 257.9 . 288.8 . . 282.0179 303.5 54828 347.0 277.8 281.7 . 54815 . . 238.1 302.8195 309.9 54824 256.4 . . . 263.1 295.6199 . . . . 247.8 . 294.2 . 329.8 302.1 . . . 274.6204 . 294.7 54824 . . 324.7 270.0206 299.0 54828 . . . 243.8211 . . 287.7 . 54815 285.9 277.1 . . . 285.0213 . . . . 263.7 54815 . . 281.6 . . . . . 261.5 . . . . 302.2215 . 303.3 54817 . . 252.5 . . .218 . . . 54804 288.5 259.2 . 292.5 . 299.9 . 281.5 54822 273.4 301.0 . . . . . 280.7227 . . . . 304.1 . 282.9 54815 . . 303.6 374.6 270.7 . 270.6 . 254.7 . . . . 281.2 292.9 342.7 283.1 299.2246 . 54804 . 318.0 . 265.4 . . . . 286.2 . 280.3248 . . . 296.8 . 305.3 343.3 . 297.5 . 3.2 . 273.4 273.2255 . . 258.2 . 280.6 54809 . . 253.3 . 284.9 . . 358.3257 . . . 297.7 . 54824 6 18.0 . . . . . 9.0 . . 264.9 .278 . 256.5 54804 286.0 302.2 299.1 269.6 . 275.5 . 6.3 279.2 . 292.9291 6 264.4 290.5 54817 3 241.0 9.3 249.6 . . 274.8 .299 . . . . 54828 . 3 . 257.5 273.1 318.1 276.3 . . . 4.1 . 278.0 .305 . 7 233.0 279.2 54748 297.0 285.8 . . 280.9 294.3 254.3 279.6324 290.8 . . . . 290.9 . 54822 . 3 279.9 . 287.0 247.3 291.6 4.9 313.5325 . . . . 54817 . . 308.7 6.4 205.3 . . 6.1 290.3 . 255.7334 282.9 54815 3 . 255.6 287.0 . 346.1 . . 364.9 298.2 . 252.7336 . 7 283.7 54748 3 291.7 10.6 283.2 273.2 300.8 304.1 . . 270.2 249.7 . 269.0337 266.4 54817 302.2 296.0 . . . 3.5 . 299.4 3 . 206.1342 . 4.0 279.2 54824 253.6 261.6 . . . 3.0 . . 357.3 353.5351 . . . 274.3 . 272.2 303.1 . 54809 . 3 296.7 . 269.0 293.7 270.7 244.2 5 297.7359 284.4 54794 3 241.8 . . 291.7 . 280.4 281.8 297.7364 10.1 . 201.1 293.5 54794 . . 255.4 2.2 287.4 9.9 294.5 6.1 253.1 278.9374 . . . 374.6 338.3 . 54824 . . 266.5 279.0 7 299.8 . 273.3375 . 4 . . 309.2 249.7 280.4 54822 . 3 12.8 6 270.6 . 231.6 . . 261.5383 . 294.5 317.0 54809 20.7 . 200.5 . 281.8 268.5 295.8 . 270.9 3.7 3 283.7 297.1388 239.3 54809 247.3 362.5 5.0 250.8 . . 3 . 313.4 . . 308.1 54809 . 6 259.6 276.2 270.8 269.0 293.2 . . . . . 238.3 254.9430 . 7 238.6 54824 284.0 301.5 275.9 272.4 200.7 280.4 . . 268.1 . 295.4459 272.1 257.6 254.9 357.5 315.9 . . . 224.4496 . . 318.7 . 54824 292.1 270.7 9.4 352.6 3.3 248.9501 267.9 . 11.5 . . 237.8 . 54828 . . . 284.7 . 8.5 . 295.7 . 233.2 . 187.5 . 320.3520 . . 301.1 . 54794 3 6 4 193.2 367.1 325.0525 7 . 7.6 247.7 54815 . 302.5 . 265.7 9.1 277.4 305.8 276.4 260.9 257.3 . 279.2 54822 . 227.6 . 249.2 264.4 . 5 . 307.1 . 281.6 279.6 54748 3 ...... 207.7 256.4 ...... 5.2 . 287.5 . 355.6 . . 232.6 304.7 280.6 . . . . 272.0 . 249.9 . 255.1 267.7 225.4 299.7 . 5 . . . . 274.8 . 260.4 305.6 . . 263.4 . . 14.5 . . 277.4 357.8 . . . 296.7 201.9 227.9 . . 275.5 309.8 . 274.4 286.6 . 303.9 . . 257.7 4 . . . 13.3 . . 231.4 . 293.9 . . . 299.7 . . 25.7 . 297.2 7.9 . . 5.3 . . 275.8 . . 9.5 . 5 . 14.8 . 3 202.2 309.6 7 276.5 236.6 277.5 300.9 6 327.9 5.9 . 5 269.2 . 9.0 3 . . 304.2 324.0 . 226.3 297.6 . 288.9 234.7 7 . 270.8 319.9 252.4 . 6 268.5 . 268.7 275.0 . 306.7 255.9 . . 274.6 275.3 . . . . 321.7 . . . . . 230.8 . . 296.9 . 254.2 21.5 . . 267.4 . 211.7 7.3 5.9 . . . 247.8 5 274.5 288.6 5.3 4 7 293.9 282.2 8.3 232.1 289.0 266.2 251.5 7 328.5 287.4 292.2 . . 8.6 . . 4 . . 15.6 13.5 246.8 . . 254.4 . . . . 6 266.7 . . 3 291.0 6 . . . 246.6 . 313.5 295.0 278.6 254.8 266.6 261.0 216.0 311.6 288.9 22.2 320.5 263.8 . . 297.8 . 6.8 18.2 . . 3 . 208.1 5 3.7 3 293.0 291.5 262.7 317.0 276.4 3 296.4 252.9 8.0 12.3 278.6 4.8 12.7 224.5 4 7.3 6 7 5 12.2 218.3 3 278.2 289.6 287.2 3 260.5 279.9

38 C. J. Evans et al.: VFTS: Classifications & radial velocities for the B-type stars ) in r max ) used in n δv r max δv 8.5 20.7 8.8 21.3 8.3 20.8 6.8 16.6 8.07.3 18.0 19.9 9.68.3 26.2 20.0 8.3 20.5 24.934.994.0 55.5 74.6 10.3 178.7 62.732.3 28.8 39.1 152.7 16.1 103.1 23.8 100.8 38.9 37.2 23.0 59.5 90.0 80.8 56.8 38.722.1 174.9 16.2 100.9 18.9 53.1 26.3 39.4 52.4 40.3 62.1 27.227.6 87.4 27.8 61.0 70.7 70.1 14.422.127.0 34.7 43.6 11.6 66.0 11.2 27.1 50.8 26.6 121.0 r ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± v , from eqn. 2); (12) number of lines ( σ n σ single v 4553 λ Si III 4438 , from eqn. 1); (11) standard deviation ( λ He I single v 4388 λ He I 4267 λ C II 4169 λ continued He I 4144 λ Table A.3. He I (and standard deviation) calculated from the multi-epoch measurements from Dunstall et al. (in prep.); (14) maximum difference ( r v 4009 λ VFTS548 MJD575 54822 He I 54828 262.4606 229.8 54828 292.5 228.6 255.1 . . . 232.3 264.2705 225.9 . 54809 . . . . . 224.9 168.6 299.4 264.0752 219.1 183.5 54817 270.4 . . . 261.7 . . . . .799 .827 266.7 295.7 54809 260.5 54828 226.9 . . . 286.5 281.3850 288.4 244.8 3.4 . . .877 14.4 54828 6 266.7 276.6 172.1 4 263.4 245.6 54815 255.4 8.0 279.9 . 281.6 . 6 . 234.4 . . 260.4 . 265.6 249.0 270.2 240.2 267.6 243.1 163.7 . . . 263.3 247.8 238.2 . . . 173.8 242.5 271.2 7.0 236.9 241.8 4 . . . 234.6 265.3 268.3 260.7 241.2 7.7 232.3 271.6 207.4 243.1 5 7.0 258.8 5.5 232.2 . 7 . . 7 270.7 241.8 254.3 . . 9.4 . 6 256.9 228.2 14.2 3 236.7 576589591 54815 54794628 54804 285.4637662 . . 54824 . 285.6665 54809 287.6675 54804 236.6686 54804 274.1 288.1687 54748 235.9 . .697 . 288.5 54804 264.5 265.7 54748 260.0 235.3713 285.8 54794 297.8 287.1715 282.1 316.7 223.8 275.7718 54794 264.8 . . . 267.4719 54809 294.3 . . . 292.8723 54828 284.9 239.4 . . . 312.1730 204.8 267.4 54804 262.6 280.6 273.9 54794 286.9 323.0779 . 311.1 54822 . . 230.7 274.9 233.7784 . 285.6 201.3 . . 279.6 . 283.0788 . . . 274.2 54809 . 261.2 . 326.8 278.7 320.8792 54748 298.1 253.5 263.7 54824 289.8 319.0 208.8 248.0 . . . 283.7 237.1 54815 265.5 262.6 339.3 . . . 333.0 265.4834 253.2 293.9 295.6 . . . . .837 . 285.7 315.2 265.0 . . . 248.7847 206.7 . . 294.0 . 54809 267.8 265.0 259.2 . . . 264.1 . 54828 . . 3.8 . 292.5 . 302.7 . 314.4874 . . . 54822 286.8 211.0 205.8 293.2 281.9 7 . 244.2 . 279.3 . 306.0 239.9883 54828 270.7 . . 262.0 . 264.5 317.6 . . . . 2.8 . 268.0888 . 6.3 234.9 303.8 . . 377.0 . . . 207.1890 . 285.5 54828 321.6 6 246.7 280.5 277.5 5 . . 301.8 226.9891 . 266.0 327.8 54815 267.7 277.7 299.9 299.3 298.2 314.5 54828 257.9 254.6 326.4 . . . . 314.0 . . 54815 . . 265.3 . 246.0 4.5 245.2 317.6 . . 4.5 271.6 . 277.4 . 232.5 . 11.9 . 256.3 5.4 . . . . 7 . . . . 16.5 . 6 8.8 271.7 289.1 . . 3 . 301.7 7 20.3 276.7 267.0 . . 271.1 3 249.4 274.2 . 326.7 7 247.9 274.6 279.8 250.8 276.8 240.1 . 219.4 . 3 . 292.9 299.3 275.5 295.8 278.7 . 6.7 304.9 . 251.3 . . . . . 276.5 . . . 334.2 281.3 . 250.8 265.2 11.6 . 237.0 5 219.3 . . . . 235.6 . . 6 . . 263.7 278.3 . 10.4 4.8 . . 247.7 . 315.2 316.7 323.9 270.0 280.4 . 2.3 . 6 . 7 . 300.7 . . . . . 332.1 3 283.3 265.0 2.1 239.2 . 2.9 . . 308.1 314.2 250.6 . 12.6 7 . . 3 . . . 271.9 ...... 295.5 4 258.9 271.3 306.8 214.9 302.0 286.2 7.7 326.5 . . . 31.9 6 9.4 302.2 283.4 . 213.8 . 279.9 . . . . 288.6 278.3 3 4 5.0 312.4 274.8 280.7 330.5 302.0 . 275.6 . 308.4 . 5 . . 9.5 . 240.3 9.6 321.4 5.8 279.0 6 4 3 316.2 7.1 274.9 289.9 298.7 6.1 282.5 6 7 17.3 305.8 238.3 273.6 3 5.3 3 ...... ; (13) estimated mean σ and single v Column entries are: (1) VFTS identifier; (2) Modified Julian Date (MJD) of the co-added observations used for these measurements (see Appendix of Paper I for details of exposures); (3-9) Notes. estimated radial velocity from each line; (10) weighted mean (single-epoch) velocity for each star ( calculation of the radial velocity estimates between the available epochs.

39