Access to Astronomical Catalogues

← Click to display the menu
J/A+A/450/253       JHKL photometry of RCW57/NGC3576           (Maercker+, 2006)

L-band (3.5 micron) IR-excess in massive star formation. II. RCW 57/NGC 3576. Maercker M., Burton M.G., Wright C.M. <Astron. Astrophys. 450, 253 (2006)> =2006A&A...450..253M
ADC_Keywords: H II regions ; Photometry, infrared Keywords: stars: circumstellar matter - stars: formation - stars: evolution - stars: Hertzsprung-Russel (HR) and C-M diagrams - stars: planetary systems: protoplanetary disks - stars: pre-main sequence Abstract: L-band data of RCW 57 at 3.5 micron taken with SPIREX (South Pole Infrared Explorer) is presented. The photometry was combined with 2MASS JHK data at 1.25 -2.2 micron. Colour-colour and colour-magnitude diagrams are constructed and used to determine the sources with infrared excess. These are interpreted as circumstellar disks, and enable the fraction of sources with disks (the cluster disk fraction or CDF) to be determined. We find that more than 50% of the sources detected at L-band in RCW 57 have an IR-excess. Description: Magnitudes for all sources (including foreground sources and sources below the 90% completeness limit) in RCW 57. Stars with measurements in all four bands are listed first. Then stars with measurements in K_s and L only, and finally stars just detected in L-band. The coordinates for sources found in all four bands are from the 2MASS point source catalogue (PSC), positions for the remaining stars are determined by reference to 2MASS images. The L-band errors are combined from the errors in daophot and the errors due to the zero point correction. Sources only detected in the K_s- and L-bands have magnitudes determined from this work. For sources not detected at J, H or K_s the upper limits on these magnitudes are 15.8, 15.1 and 14.3 respectively. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 11 11 49.8 -61 18 14 NGC 3576 = RCW 57A ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table5.dat 120 251 Magnitudes for all sources (including foreground sources and sources below the 90% completeness limit) in RCW 57
See also: J/A+A/438/663 : JHKL photometry of 30 Dor (Maercker+, 2005) Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 I3 -- Seq Sequential number in paper 6- 7 I2 h RAh Right ascension J2000 (hours) 9- 10 I2 min RAm Right ascension J2000 (minutes) 12- 15 F4.1 s RAs Right ascension J2000 (seconds) 18 A1 -- DE- Declination J2000 (sign) 19- 20 I2 deg DEd Declination J2000 (degrees) 22- 23 I2 arcmin DEm Declination J2000 (arcmin) 25- 28 F4.1 arcsec DEs Declination J2000 (arcsec) 31- 34 F4.1 mag Jmag ? 2MASS PSC J-band magnitude 37- 40 F4.2 mag e_Jmag ? Error in J-band magnitude (1) 43- 46 F4.1 mag Hmag ? 2MASS PSC H-band magnitude 49- 52 F4.2 mag e_Hmag ? Error in H-band magnitude (1) 55- 58 F4.1 mag Kmag ? 2MASS PSC K-band magnitude 61- 64 F4.2 mag e_Kmag ? Error in K-band magnitude (1) 67- 70 F4.1 mag Lmag ? SPIREX PSC L-band magnitude 73- 76 F4.2 mag e_Lmag ? Error in L-band magnitude (1) 79- 82 A4 --- Note [e, fg] Notes (2) 84-120 A37 --- Com Comments (3)
Note (1): A '---' as error indicates a 95% confidence upper limit for the 2MASS magnitude in the PSC. Note (2): Notes as follows: e = stars with IR-excess fg = Likely foreground stars Note (3): Identifications: No NN = Stars matched with Barbosa et al. (2003AJ....126.2411B) FBDC NNNa and [FP74] RCW 57 IRS 1 in Simbad Persi NNN = Stars matched with Persi et al. (1994A&A...282..474P) [PRT94] NNN in Simbad
Acknowledgements: Matthias Maercker, maercker(at)astro.su.se
(End) Matthias Maercker [Stockholm Obs.], Patricia Vannier [CDS] 16-Dec-2005
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

catalogue service

© UDS/CNRS

Contact