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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 78 2255 Observational catalogue for extracted MUSE
sources in NGC 2070
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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
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Bytes Format Units Label Explanations
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1- 4 I4 --- MUSE [13/3204] Identification in this work
6- 9 I4 --- Selman ?=- Identification from Selman et al.
(1999A&A...341...98S 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 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
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Acknowledgements:
Norberto Castro, ncastror(at)umich.edu
(End) Norberto Castro [Michigan Univ., USA], Patricia Vannier [CDS] 05-Mar-2018