2017A&A...602A..56K


Query : 2017A&A...602A..56K

2017A&A...602A..56K - Astronomy and Astrophysics, volume 602A, 56-56 (2017/6-1)

Uncrowding R 136 from VLT/SPHERE extreme adaptive optics.

KHORRAMI Z., VAKILI F., LANZ T., LANGLOIS M., LAGADEC E., MEYER M.R., ROBBE-DUBOIS S., ABE L., AVENHAUS H., BEUZIT J.L., GRATTON R., MOUILLET D., ORIGNE A., PETIT C. and RAMOS J.

Abstract (from CDS):

This paper presents the sharpest near-IR images of the massive cluster R 136 to date, based on the extreme adaptive optics of the SPHERE focal instrument implemented on the ESO Very Large Telescope and operated in its IRDIS imaging mode.The crowded stellar population in the core of the R 136 starburst compact cluster remains still to be characterized in terms of individual luminosities, age, mass and multiplicity. SPHERE/VLT and its high contrast imaging possibilities open new windows to make progress on these questions.Stacking-up a few hundreds of short exposures in J and Ks spectral bands over a field of view (FoV) of 10.9''x12.3'' centered on the R 136a1 stellar component, enabled us to carry a refined photometric analysis of the core of R 136. We detected 1110 and 1059 sources in J and Ks images respectively with 818 common sources. Thanks to better angular resolution and dynamic range, we found that more than 62.6% (16.5%) of the stars, detected both in J and Ks data, have neighbours closer than 0.2'' (0.1''). The closest stars are resolved down to the full width at half maximum (FWHM) of the point spread function (PSF) measured by Starfinder. Among resolved and/or detected sources R 136a1 and R 136c have optical companions and R 136a3 is resolved as two stars (PSF fitting) separated by 59±2 mas. This new companion of R 136a3 presents a correlation coefficient of 86% in J and 75% in Ks. The new set of detected sources were used to re-assess the age and extinction of R 136 based on 54 spectroscopically stars that have been recently studied with HST slit-spectroscopy (Crowther et al., 2016MNRAS.458..624C) of the core of this cluster. Over 90% of these 54 sources identified visual companions (closer than 0.2''). We found the most probable age and extinction for these sources are 1.8+1.2–0.8Myr, AJ=(0.45±0.5)mag and AK=(0.2±0.5)mag within the photometric and spectroscopic error-bars. Additionally, using PARSEC evolutionary isochrones and tracks, we estimated the stellar mass range for each detected source (common in J and K data) and plotted the generalized histogram of mass (MF with error-bars). Using SPHERE data, we have gone one step further and partially resolved and studied the initial mass function covering mass range of (3-300)M at the age of 1 and 1.5Myr. The density in the core of R 136 (0.1-1.4pc) is estimated and extrapolated in 3D and larger radii (up to 6pc). We show that the stars in the core are still unresolved due to crowding, and the results we obtained are upper limits. Higher angular resolution is mandatory to overcome these difficulties.

Abstract Copyright: © ESO, 2017

Journal keyword(s): open clusters and associations: individual: RMC 136 - stars: luminosity function, mass function - stars: massive - instrumentation: adaptive optics - instrumentation: adaptive optics

VizieR on-line data: <Available at CDS (J/A+A/602/A56): catalog.dat>

Status at CDS : All or part of tables of objects will not be ingested in SIMBAD.

CDS comments: Table A.1 Some [HSH95] objects not in SIMBAD.

Simbad objects: 45

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Number of rows : 45
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6418 1
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16265 1
3 NAME 30 Dor Region reg 05 38.0 -69 06           ~ 210 0
4 H88 301 Cl* 05 38 16 -69 04.0   11.18 10.89     ~ 70 0
5 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1121 2
6 [HSH95] 42 ** 05 38 42.1802 -69 06 02.384           O3V+O3V 14 0
7 BAT99 106 WR* 05 38 42.291 -69 06 03.45   12.83 12.93     WN5h 59 0
8 Cl* NGC 2070 MH 454 * 05 38 42.30 -69 06 02.6   14.06       ~ 17 0
9 Cl* NGC 2070 MH 474 * 05 38 42.35 -69 06 01.8   13.56       ~ 15 0
10 Cl* NGC 2070 MH 480 * 05 38 42.37 -69 06 01.8   14.28       ~ 10 0
11 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1884 1
12 Cl* NGC 2070 MH 509 * 05 38 42.42 -69 06 01.8   13.78 13.73     O3III 20 0
13 BAT99 108 WR* 05 38 42.43 -69 06 02.2   12.78 12.77     WN5h 74 0
14 BAT99 109 WR* 05 38 42.45 -69 06 02.2   13.09 13.38     WN5h 45 0
15 BAT99 110 WR* 05 38 42.47 -69 06 02.0   13.73 13.73     O2If* 38 0
16 CXOU J053842.4-690601 * 05 38 42.482 -69 06 01.07   14.33 14.49     O2-3.5V 17 0
17 Cl* NGC 2070 MH 551 * 05 38 42.52 -69 06 03.8   14.64 14.81     O3V 14 0
18 Cl* NGC 2070 MH 608 * 05 38 42.68 -69 06 02.1   14.49 14.39     ~ 16 0
19 CXOU J053842.7-690601 * 05 38 42.720 -69 06 01.99   14.67 14.63     O3III 15 0
20 BAT99 111 WR* 05 38 42.765 -69 06 03.36   13.51 13.66     WN9ha 44 0
21 BAT99 112 WR* 05 38 42.9162 -69 06 04.938   12.95 12.86     WN5h 55 0
22 RMC 136a Cl* 05 38 43.3 -69 06 08           ~ 144 2
23 NGC 3603 OpC 11 15 11 -61 15.5           ~ 1022 1
24 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13192 0
25 [HSH95] 48 * ~ ~     14.72     O3III 9 0
26 [HSH95] 92 * ~ ~           O3V 5 0
27 [HSH95] 52 * ~ ~     14.76     O3V 7 0
28 [HSH95] 58 * ~ ~     14.82     O3III 8 0
29 [HSH95] 62 * ~ ~     14.96     ~ 6 0
30 [HSH95] 65 * ~ ~     15.12     ~ 6 0
31 [HSH95] 69 * ~ ~     15.16     ~ 6 0
32 [HSH95] 73 * ~ ~           O9V 5 0
33 [HSH95] 90 * ~ ~           ~ 5 0
34 [HSH95] 94 * ~ ~           O3V 5 0
35 [HSH95] 45 * ~ ~     14.62     O3V 7 0
36 [HSH95] 35 * ~ ~     14.42     O3V 7 0
37 [HSH95] 30 * ~ ~     14.26     O3V 7 0
38 [HSH95] 49 * ~ ~     14.74     O3V 7 0
39 [HSH95] 71 * ~ ~     15.17     ~ 6 0
40 [HSH95] 112 * ~ ~           O8.5III 5 0
41 [HSH95] 66 * ~ ~     15.13     O3V 7 0
42 [HSH95] 64 * ~ ~     15.06     O7V 7 0
43 [HSH95] 31 * ~ ~     14.35     ~ 7 0
44 [HSH95] 50 * ~ ~     14.75     ~ 6 0
45 [HSH95] 46 * ~ ~     14.67     ~ 7 0

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2022.10.02-01:58:03

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