2005A&A...443...41M


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.23CEST00:55:32

2005A&A...443...41M - Astronomy and Astrophysics, volume 443, 41-60 (2005/11-3)

Star-formation in NGC 4038/4039 from broad and narrow band photometry: cluster destruction?

MENGEL S., LEHNERT M.D., THATTE N. and GENZEL R.

Abstract (from CDS):

Accurately determining the star formation history in NGC 4038/4039 - ``The Antennae'' - is hampered by variable and sometimes substantial extinction. We therefore used near infrared broad- and narrow-band images obtained with ISAAC at the VLT and with SOFI at the NTT to determine the recent star formation history in this prototypical merger. In combination with archival HST data, we determined ages, extinction, and other parameters for single star clusters, and properties of the cluster population as a whole. About 70% of the Ks-band detected star clusters with masses ≥105M are younger than 10Myr (this is approximately an e-folding time for cluster ages), which we interpret as evidence of rapid dissolution but not free expansion. The total mass of K-band selected clusters is about 5 to 10x108M and represents about 3-6% of the total molecular gas. However, this takes only the detected clusters into account, and in view of the rapid dissolution, means that this is only a lower limit to the total mass of stars produced in clusters during the burst. Studies of cluster formation in other galaxies recently suggested short cluster dissolution timescales, too, which means that star formation rates may have been severely underestimated in the past. Extinction is strongly variable and very high in some regions, but around AV=1.3mag on average. Even though most clusters are detected at least in I-band, only the information about individual cluster ages and extinction allows us to avoid uncertainties of orders of magnitude in star formation rate estimates determined from optical fluxes. From the distribution of individual cluster extinction vs. age, which is significantly higher for clusters below 8-9Myr than for older clusters, we infer that this is the time by which a typical cluster blows free of its native dust cocoon.

Abstract Copyright:

Journal keyword(s): galaxies: star clusters - galaxies: individual: NGC 4038/4039 - galaxies: interactions

VizieR on-line data: <Available at CDS (J/A+A/443/41): table.dat>

Nomenclature: Table: [MLT2005b] +NN.NN+NN.NN N=1072.

Status in Simbad:  could be processed

Simbad objects: 12

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Number of rows : 12

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 NAME NGC 1569 CL* A Cl* 04 30 48.2 +64 50 59   15.45 15.22     ~ 97 1
2 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1137 3
3 [WS95] 405A Cl* 12 01 50.460 -18 52 13.89     17.0     ~ 20 0
4 NGC 4038 GiP 12 01 53.002 -18 52 03.32   10.91   9.74 11.0 ~ 1263 1
5 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1532 0
6 NGC 4039 GiP 12 01 53.8 -18 53 06   11.08   9.77   ~ 1124 1
7 [BCE2005] 157 Cl* 12 01 54.89 -18 53 04.9     23.5     ~ 21 0
8 [WS95] 342 Cl* 12 01 55.430 -18 52 19.45     19.4     ~ 17 0
9 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3683 4
10 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33   ~ 1245 4
11 GSPC S279-F * 17 48 22.7 -45 25 45           ~ 29 0
12 [WS95] 355 Cl* ~ ~     22.1     ~ 7 0

    Equat.    Gal    SGal    Ecl

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2019.10.23-00:55:32

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