J/A+A/515/A26 H and Ks photometry of Trumpler 14 (Sana+, 2010)
A MAD view of Trumpler 14.
Sana H., Momany Y., Gieles M., Carraro G., Beletsky Y., Ivanov V.D.,
De Silva G., James G.
<Astron. Astrophys. 515, A26 (2010)>
=2010A&A...515A..26S 2010A&A...515A..26S
ADC_Keywords: Clusters, open ; Stars, double and multiple ; Photometry, infrared
Keywords: instrumentation: adaptive optics - stars: early-type -
stars: pre-main sequence - binaries: visual -
open clusters and associations: individual: Tr 14
Abstract:
We present adaptive optics (AO) near-infrared observations of the core
of the Tr 14 cluster in the Carina region obtained with the ESO
multi-conjugate AO demonstrator, MAD. Our campaign yields AO-corrected
observations with an image quality of about 0.2' across the 2" field
of view, which is the widest AO mosaic ever obtained. We detected
almost 2000 sources spanning a dynamic range of 10 mag. The pre-main
sequence (PMS) locus in the colour-magnitude diagram is well
reproduced by Palla & Stahler isochrones with an age of 3 to
5x105yr, confirming the very young age of the cluster. We derive a
very high (deprojected) central density n0∼4.5(±0.5)x104pc-3
and estimate the total mass of the cluster to be about
∼4.3+3.3-1.5x103M☉, although contamination of the field of
view might have a significant impact on the derived mass. We show that
the pairing process is largely dominated by chance alignment so that
physical pairs are difficult to disentangle from spurious ones based
on our single epoch observation. Yet, we identify 150 likely bound
pairs, 30% of these with a separation smaller than 0.5" (∼1300AU). We
further show that at the 2σ level massive stars have more
companions than lower-mass stars and that those companions are
respectively brighter on average, thus more massive. Finally, we find
some hints of mass segregation for stars heavier than about
10M☉. If confirmed, the observed degree of mass segregation
could be explained by dynamical evolution, despite the young age of
the cluster.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 62 1955 H and Ks photometry
table5.dat 47 150 Likely bound visual pairs (P(bound)>0.99)
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See also:
J/ApJ/549/578 : BV photometry of Trumpler 14 and 16 (Degioia-Eastwood+, 2001)
J/ApJ/589/509 : Chandra observations of Trumpler 14 and 16 (Evans+, 2003)
J/A+A/418/525 : Collinder 232 + Trumpler 14/16 UBVRI phot. (Carraro+, 2004)
J/A+A/476/199 : Trumpler 14 JHKL' photometry (Ascenso+, 2007)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq Sequential identifier
7- 8 I2 h RAh Right ascension (J2000.0)
10- 11 I2 min RAm Right ascension (J2000.0)
13- 18 F6.3 s RAs Right ascension (J2000.0)
21 A1 --- DE- Declination sign (J2000.0)
22- 23 I2 deg DEd Declination (J2000.0)
25- 26 I2 arcmin DEm Declination (J2000.0)
28- 32 F5.2 arcsec DEs Declination (J2000.0)
35- 40 F6.3 mag Hmag H-band magnitude (1)
43- 47 F5.3 mag e_Hmag One-sigma error bar on the H-band magnitude
50- 55 F6.3 mag Ksmag Ks-band magnitude (1)
58- 62 F5.3 mag e_Ksmag One-sigma error bar on the Ks-band magnitude
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Note (1): H and Ks magnitudes for sources #1360 and #1794 are from 2MASS
(Cutri et al., 2003, Cat. II/246)
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- ID1 Primary ID for the components of the pair
5 A1 --- --- [-]
6- 9 I4 --- ID2 Secondary IDs for the components of the pair
12- 17 F6.3 mag Hmag1 H-band magnitude of the primary component
20- 25 F6.3 mag Ksmag1 Ks-band magnitude of the primary component
28- 33 F6.3 mag Hmag2 H-band magnitude of the secondary component
36- 41 F6.3 mag Ksmag2 Ks-band magnitude of the secondary component
44- 47 F4.2 arcsec Sep Separation between the components
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Acknowledgements:
Hugues Sana, H.Sana(at)uva.nl
(End) H. Sana [ESO, Chile/UvA, Netherlands], P. Vannier [CDS] 11-Mar-2010