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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 62 1955 H and Ks photometry table5.dat 47 150 Likely bound visual pairs (P(bound)>0.99)
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
Bytes Format Units Label Explanations
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
Note (1): H and Ks magnitudes for sources #1360 and #1794 are from 2MASS (Cutri et al., 2003, Cat. II/246)
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
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
Acknowledgements: Hugues Sana, H.Sana(at)uva.nl
(End) H. Sana [ESO, Chile/UvA, Netherlands], P. Vannier [CDS] 11-Mar-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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