J/A+A/628/A60 Star cluster formation in a tidal debris (Fensch+, 2019)
Massive star cluster formation and evolution in tidal dwarf galaxies.
Fensch J., Duc P.-A., Boquien M., Elmegreen D.M., Elmegreen B.G.,
Bournaud F., Brinks E., de Grijs R., Lelli F., Renaud F., Weilbacher P.M.
<Astron. Astrophys. 628, A60 (2019)>
=2019A&A...628A..60F 2019A&A...628A..60F (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Clusters, globular ; Photometry, CCD ;
Photometry, HST
Keywords: galaxies: dwarf - galaxies: irregular -
galaxies: star clusters: general - galaxies: stellar content -
galaxies: star formation - galaxies: interactions
Abstract:
The formation of globular clusters remains an open debate. Dwarf
starburst galaxies are efficient at forming young massive clusters
with similar masses as globular clusters and may hold the key to
understanding their formation.
We study star cluster formation in a tidal debris - including the
vicinity of three tidal dwarf galaxies - in a massive gas dominated
collisional ring around NGC 5291. These dwarfs have physical
parameters which differ significantly from local starbursting dwarfs.
They are gas-rich, highly turbulent, have a gas metallicity already
enriched up to half-solar, and are expected to be free of dark matter.
The aim is to study massive star cluster formation in this as yet
unexplored type of environment.
We use imaging from the Hubble Space Telescope using broadband filters
covering the wavelength range from the near- ultraviolet to the
near-infrared. We determine the masses and ages of the cluster
candidates by using the spectral energy distribution- fitting code
CIGALE, carefully considering age-extinction degeneracy effects on the
estimation of the physical parameters. Results. We find that the tidal
dwarf galaxies in the ring of NGC 5291 are forming star clusters with
an average efficiency of about 40%, comparable to blue compact dwarf
galaxies. We also find massive star clusters for which the photometry
suggests that they were formed at the very birth of the tidal dwarf
galaxies and have survived for several hundred million years.
Therefore our study shows that extended tidal dwarf galaxies and
compact clusters may be formed simultaneously. In the specific case
observed here, the young star clusters are not massive enough to
survive for a Hubble time. However one may speculate that similar
objects at higher redshift, with higher star formation rate, might
form some of the long lived globular clusters.
Description:
Position and fluxes of the detected star clusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 151 1290 Cluster positions and flux
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Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Cluster [0/1289] Cluster number
6- 15 F10.6 deg RAdeg Right ascension (J2000.0)
17- 26 F10.6 deg DEdeg Declination (J2000.0)
28 A1 --- l_F336W Upper limit flag on F336W
29- 39 E11.5 mJy F336W Flux in F336W band (1)
41- 51 E11.5 mJy e_F336W ? 1-sigma uncertainty on F336W flux
53 A1 --- l_F475W Upper limit flag on F475W
54- 64 E11.5 mJy F475W Flux in F475W band (1)
66- 76 E11.5 mJy e_F475W ? 1-sigma uncertainty on F475W flux
78 A1 --- l_F606W Upper limit flag on F606W
79- 89 E11.5 mJy F606W Flux in F606W band (1)
91-101 E11.5 mJy e_F606W ? 1-sigma uncertainty on F606W flux
103 A1 --- l_F814W Upper limit flag on F814W
104-114 E11.5 mJy F814W Flux in F814W band (1)
116-126 E11.5 mJy e_F814W ? 1-sigma uncertainty on F814W flux
128 A1 --- l_F160W Upper limit flag on F160W
129-139 E11.5 mJy F160W Flux in F160W band (1)
141-151 E11.5 mJy e_F160W ? 1-sigma uncertainty on F160W flux
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Note (1): Only clusters with no or only one upper limit on flux measurements
were considered in the paper.
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Acknowledgements:
Jeremy Fensch, jfensch(at)eso.org
(End) Jeremy Fensch [ESO, Germany], Patricia Vannier [CDS] 10-Jul-2019