Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/700/L73    Photospheric fluxes at 24 and 70µm    (Kospal+, 2009)

On the relationship between debris disks and planets. Kospal A., Ardila D.R., Moor A., Abraham P. <Astrophys. J. 700, L73 (2009)> =2009ApJ...700L..73K
ADC_Keywords: Stars, nearby ; Stars, ages ; Photometry, infrared Keywords: circumstellar matter - infrared: stars - Kuiper Belt - planetary systems Abstract: Dust in debris disks is generated by collisions among planetesimals. The existence of these planetesimals is a consequence of the planet-formation process, but the relationship between debris disks and planets has not been clearly established. Here we analyze Spitzer/MIPS 24 and 70um data for 150 planet-bearing stars, and compare the incidence of debris disks around these stars with a sample of 118 stars around which planets have been searched for, but not found. Together they comprise the largest sample ever assembled to deal with this question. The use of survival analysis techniques allows us to account for the large number of non-detections at 70um. We discovered 10 new debris disks around stars with planets and one around a star without known planets. We found that the incidence of debris disks is marginally higher among stars with planets, than among those without, and that the brightness of the average debris disk is not significantly different in the two samples. We conclude that the presence of a planet that has been detected via current radial velocity techniques is not a good predictor for the presence of a debris disk detected at infrared wavelengths. Description: In this table we present ages, metallicities, photospheric flux predictions at 24 and 70um, as well as observed 24 and 70um photometry (obtained with the MIPS instrument of the Spitzer Space Telescope) for our sample of 150 planet-bearing stars and 118 stars without planets. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 123 268 Photospheric predictions and MIPS photometry refs.dat 147 19 References
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Name Stallar identification 12- 15 A4 --- Pl Star with planet(SWP)/Star without planet(SWOP) 17- 22 F6.3 Gyr Age ? Age 24- 25 I2 --- r_Age ? Reference for Age, in refs.dat file 27- 33 F7.4 [-] [Fe/H] ? Metallicity (1) 35- 42 F8.2 mJy F24P Predicted photospheric flux at 24um 44- 51 F8.2 mJy F24 ? Observed flux at 24um 53- 58 F6.2 mJy e_F24 ? 1-σ uncertainty in F24 (2) 60- 66 F7.3 --- R24 ? Observed-to-predicted flux ratio at 24um (3) 68- 74 F7.3 --- chi24 ? Significance of excess emission at 24um (4) 76- 78 A3 --- IRE24 ? Excess emission at 24um (5) 80- 87 F8.2 mJy F70P Predicted photospheric flux at 70um 89- 96 F8.2 mJy F70 ? Observed flux at 70um 98-103 F6.2 mJy e_F70 ? Observed 1-sigma flux uncertainty at 70um (2) 105-111 F7.3 --- R70 ? Observed-to-predicted flux ratio at 70um (3) 113-119 F7.3 --- chi70 ? Significance of excess emission at 70um (4) 121-123 A3 --- IRE70 ? Excess emission at 70um (5)
Note (1): Metallicities are averages of values presented in the NASA/IPAC/NExScI Star and Exoplanet Database (http://nsted.ipac.caltech.edu) Note (2): 1-σ uncertainties of the observed flux include the uncertainty of the absolute calibration (4% for 24um and 7% for 70um, see the MIPS Data Handbook) Note (3): R=FObs/FPred Note (4): χ=(FObs-FPred)/σ; excess emission is significant if χ≥3 Note (5): Excess emission code: NO = no excess YES = significant excess UPL = upper limit
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number 4- 22 A19 --- BibCode BibCode 24- 44 A21 --- Aut Author's name 46-147 A102 --- Com Comments
Acknowledgements: Agnes Kospal, kospal(at)strw.leidenuniv.nl
(End) A. Kospal [Leiden Obs., Leiden Univ.], P. Vannier [CDS] 14-Jul-2009
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