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J/ApJ/636/1098      Debris disks around solar-type stars         (Bryden+, 2006)

Frequency of debris disks around solar-type stars: first results from a Spitzer MIPS survey. Bryden G., Beichman C.A., Trilling D.E., Rieke G.H., Holmes E.K., Lawler S.M., Stapelfeldt K.R., Werner M.W., Gautier T.N., Blaylock M., Gordon K.D., Stansberry J.A., Su K.Y.L. <Astrophys. J., 636, 1098-1113 (2006)> =2006ApJ...636.1098B
ADC_Keywords: Stars, F-type ; Stars, G-type ; Stars, K-type ; Infrared sources ; Stars, dwarfs Keywords: circumstellar matter - infrared: stars - Kuiper Belt - planetary systems: formation Abstract: We have searched for infrared excesses around a well-defined sample of 69 FGK main-sequence field stars. These stars were selected without regard to their age, metallicity, or any previous detection of IR excess; they have a median age of 4Gyr. Description: The FGK Survey is a Spitzer GTO program designed to search for excesses around 150 nearby, F5-K5 main-sequence field stars, sampling wavelengths from 8 to 40µm with IRS (Infrared Spectrograph) and 24 and 70µm with MIPS (Multiband Imaging Photometer). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 92 127 FGK survey stars refs.dat 113 31 References table2.dat 72 69 Measured and predicted fluxes at 24 and 70µm
See also: J/MNRAS/325/1365 : Solar neighbourhood metallicity distribution (Haywood+, 2001) J/A+AS/129/237 : G and K dwarfs abundances (Feltzing+ 1998) J/A+A/377/911 : Age-metallicity relation in solar neighbourhood (Feltzing+, 2001) J/ApJ/555/932 : IR fluxes of solar-type stars (Spangler+, 2001) J/ApJS/152/261 : Chromospheric Ca II emission in nearby stars (Wright+ 2004) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [HD] 4- 9 I6 --- HD The HD number (Cat. III/135) 11- 13 A3 --- n_HD [ab] a = Observed, b = Known planet-bearing star. 15- 22 A8 --- SpType SIMBAD MK spectral type 24- 27 F4.2 mag Vmag SIMBAD visual magnitude (2) 29- 32 F4.1 Gyr Age ? The Wright et al. (2004, Cat. J/ApJS/152/261) age (3) 34- 37 F4.2 Gyr AgeMin ? Minimum age 39- 42 F4.1 Gyr AgeMax ? Maximum age 44- 57 A14 --- r_Age Reference(s) for Age 59- 63 F5.2 [Sun] [Fe/H] ? The average [Fe/H] abundance 65- 68 F4.2 [Sun] e_[Fe/H] ? Dispersion in Abund 70 I1 --- o_[Fe/H] Number of estimates in Abund 72- 92 A21 --- Refs Additional reference(s)
Note (2): Typically from the Hipparcos satellite. Note (3): Or an average of other estimates if Wright data is unavailable.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Ref Reference code 4- 22 A19 --- Bibcode Bibcode 24- 47 A24 --- Aut Author's name 49-113 A65 --- Com Comment
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD The HD number 8 A1 --- n_HD [de] Note on IR excess (1) 10- 15 F6.1 mJy MIPS24um Measured MIPS 24µm flux density 17- 22 F6.1 mJy Star24um Predicted 24µm flux density 24- 27 F4.2 --- Rat24um The MIPS/predicted 24µm flux density ratio 29- 33 F5.1 mJy MIPS70um Measured MIPS 70µm flux density 35- 38 F4.1 mJy e_MIPS70um Uncertainty in MIPS70um 40- 44 F5.1 mJy Star70um Predicted 70µm flux density 46- 48 F3.1 --- Rat70um The MIPS/predicted 70µm flux density ratio 50- 53 F4.1 --- S/N The 70µm signal-to-noise ratio 55- 58 F4.1 --- chi70 Significance of excess (Eq. 1) 60- 64 F5.1 mJy FDust ? Dust flux density at 70mum (2) 66 A1 --- l_LDust Limit flag on LDust 67- 72 E6.2 --- LDust Dust luminosity from 70mum emission (3)
Note (1): Flag on HD, defined as follows: d = star with excess 70µm emission; e = star with excess 24µm emission. Note (2): 70µm dust fluxes have been color corrected by 15%, appropriate for ∼50K emission. Note (3): See Eq. 3. In units of the stellar luminosity
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 03-Jan-2007
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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