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J/A+A/614/A147      NGC 2070 point sources radial velocities     (Castro+, 2018)

Mapping the core of the Tarantula Nebula with VLT-MUSE. I. Spectral and nebular content around R136. Castro N., Crowther P.A., Evans C.J., Mackey J., Castro-Rodriguez N., Vink J.S., Melnick J., Selman F. <Astron. Astrophys. 614, A147 (2018)> =2018A&A...614A.147C (SIMBAD/NED BibCode)
ADC_Keywords: Surveys; Magellanic Clouds; Clusters, open ; Stars, early-type ; Photometry, VRI ; Radial velocities Keywords: stars: early-types - stars: massive - ISM: kinematics and dynamics - ISM: structure - galaxies: clusters: individual: R136 - Magellanic Clouds Abstract: We introduce VLT-MUSE observations of the central 2'x2' (30x30pc) of the Tarantula Nebula in the Large Magellanic Cloud. The observations provide an unprecedented spectroscopic census of the massive stars and ionised gas in the vicinity of R136, the young, dense star cluster located in NGC 2070, at the heart of the richest star-forming region in the Local Group. Spectrophotometry and radial-velocity estimates of the nebular gas (superimposed on the stellar spectra) are provided for 2255 point sources extracted from the MUSE datacubes, and we present estimates of stellar radial velocities for 270 early-type stars (finding an average systemic velocity of 271±41km/s). We present an extinction map constructed from the nebular Balmer lines, with electron densities and temperatures estimated from intensity ratios of the [SII], [NII], and [SIII] lines. The interstellar medium, as traced by Hα and [NII] λ6583, provides new insights in regions where stars are probably forming. The gas kinematics are complex, but with a clear bi-modal, blue- and red-shifted distribution compared to the systemic velocity of the gas centred on R136. Interesting point-like sources are also seen in the eastern cavity, western shell, and around R136; these might be related to phenomena such as runaway stars, jets, formation of new stars, or the interaction of the gas with the population of Wolf-Rayet stars. Closer inspection of the core reveals red-shifted material surrounding the strongest X-ray sources, although we are unable to investigate the kinematics in detail as the stars are spatially unresolved in the MUSE data. Further papers in this series will discuss the detailed stellar content of NGC 2070 and its integrated stellar and nebular properties. Description: NGC 2070 was observed as part of the MUSE SV program at the VLT in August 2014. Four overlapping fields, each with an individual field of 1'x1' and a pixel scale of 0.2''/pixel, were observed. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 78 2255 Observational catalogue for extracted MUSE sources in NGC 2070
See also: J/A+A/341/98 : The ionizing cluster of 30 Doradus. I. (Selman+ 1999) J/A+A/530/A108 : VLT-FLAMES Tarantula Survey (Evans+, 2011) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 I4 --- MUSE [13/3204] Identification in this work 6- 9 I4 --- Selman ?=- Identification from Selman et al. (1999A&A...341...98S, Cat. J/A+A/341/98), Cl* NGC 2070 SMB NNNN in Simbad 11- 14 I4 --- VFTS ?=- Identification from Evans et al. (2011A&A...530A.108E, Cat. J/A+A/530/A108), VFTS NNNN in Simbad 16 I1 h RAh Right ascension (J2000) 18- 19 I2 min RAm Right ascension (J2000) 21- 26 F6.3 s RAs Right ascension (J2000) 28 A1 --- DE- Declination sign (J2000) 29- 30 I2 deg DEd Declination (J2000) 32- 33 I2 arcmin DEm Declination (J2000) 35- 39 F5.2 arcsec DEs Declination (J2000) 41- 45 F5.2 mag Vmag V-band magnitude estimated from the MUSE data, see Sect. 3.1 for calibration of zero-point 47- 51 F5.2 mag V-I (V-I) colour estimated from the MUSE data, see Sect. 3.1 for calibration of zero-point. 53- 55 I3 km/s RVHa Estimated radial velocities from (single-component) fits to the Hα line 57- 61 F5.1 km/s e_RVHa rms uncertainty on RVHa 63- 65 I3 km/s RV[NII] Estimated radial velocities from (single-component) fits to [NII]λ6583.45 line 67- 71 F5.1 km/s e_RV[NII] rms uncertainty on RV[NII] 73- 75 I3 km/s RVHeII ?=- Estimated radial velocities from (single-component) fits to HeIIλ5411.5 absorption line (see Sect. 5,3) 77- 78 I2 km/s e_RVHeII ? rms uncertainty on RVHeII
Acknowledgements: Norberto Castro, ncastror(at)umich.edu
(End) Norberto Castro [Michigan Univ., USA], Patricia Vannier [CDS] 05-Mar-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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