2015A&A...576A.110N


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.18CEST05:06:13

2015A&A...576A.110N - Astronomy and Astrophysics, volume 576A, 110-110 (2015/4-1)

Deep near-infrared adaptive-optics observations of a young embedded cluster at the edge of the RCW 41 H II region.

NEICHEL B., SAMAL M.R., PLANA H., ZAVAGNO A., BERNARD A. and FUSCO T.

Abstract (from CDS):

We investigate the star formation activity in a young star forming cluster embedded at the edge of the RCW41 Hii region. As a complementary goal, we aim to demonstrate the gain provided by wide-field adaptive optics (WFAO) instruments to study young clusters. We used deep, JHKs images from the newly commissioned Gemini-GeMS/GSAOI instrument, complemented with Spitzer IRAC observations, in order to study the photometric properties of the young stellar cluster. GeMS is a WFAO instrument that delivers almost diffraction-limited images over a field of ∼2' across. The exquisite angular resolution allows us to reach a limiting magnitude of J∼22 for 98% completeness. The combination of the IRAC photometry with our JHKs catalog is used to build color-color diagrams, and select young stellar object (YSO) candidates. The JHKs photometry is also used in conjunction with pre-main sequence evolutionary models to infer masses and ages. The K-band luminosity function is derived, and then used to build the initial mass function (IMF) of the cluster. We detect the presence of 80 YSO candidates. Those YSOs are used to infer the cluster age, which is found to be in the range 1 to 5Myr. More precisely, we find that 1/3 of the YSOs are in a range between 3 to 5Myr, while 2/3 of the YSO are ≤3Myr. When looking at the spatial distribution of these two populations, we find evidence of a potential age gradient across the field that suggests sequential star formation. We construct the IMF and show that we can sample the mass distribution well into the brown dwarf regime (down to ∼0.01M). The logarithmic mass function rises to peak at ∼0.3M, before turning over and declining into the brown dwarf regime. The total cluster mass derived is estimated to be 78±18M, while the ratio derived of brown dwarfs to star is 18±5%. When comparing it with other young clusters, we find that the IMF shape of the young cluster embedded within RCW41 is consistent with those of Trapezium, IC348, or Chamaeleon I, except for the IMF peak, which happens to be at higher mass. This characteristic is also seen in clusters like NGC6611 or even Taurus. These results suggest that the medium-to-low mass end of the IMF possibly depends on environment.

Abstract Copyright:

Journal keyword(s): instrumentation: adaptive optics - instrumentation: high angular resolution - stars: low-mass - HII regions - stars: formation - stars: pre-main sequence

CDS comments: Fig.13 objects not identified.

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 887 0
2 NGC 661 GiG 01 44 14.5986547790 +28 42 21.153100307   13.0       ~ 92 0
3 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 942 3
4 NGC 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1181 1
5 IC 348 OpC 03 44 34 +32 09.8           ~ 1203 1
6 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3308 0
7 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14324 1
8 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1432 1
9 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1057 1
10 NAME Taurus Cluster Cl* 06 10.1 +09 05           ~ 62 0
11 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1544 1
12 NAME VELA MOL RIDGE MoC 08 53 -45.0           ~ 130 0
13 IRAS 09149-4743 mul 09 16 43.2 -47 56 26           ~ 24 1
14 TYC 8170-333-1 HII 09 16 58.2090062072 -47 57 47.392462164   13.36 12.96     ~ 21 0
15 NAME Cha I MoC 11 06 48 -77 18.0           ~ 933 1
16 NGC 3603 HII 11 15 24 -61 15.0           ~ 920 2
17 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 920 2
18 NGC 7538 OpC 23 13 37 +61 30.0           ~ 814 0

    Equat.    Gal    SGal    Ecl

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2019.10.18-05:06:13

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