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J/ApJ/653/675    Spitzer 24µm photometry of A dwarfs              (Su+, 2006)

Debris disk evolution around A stars. Su K.Y.L., Rieke G.H., Stansberry J.A., Bryden G., Stapelfeldt K.R., Trilling D.E., Muzerolle J., Beichman C.A., Moro-Martin A., Hines D.C., Werner M.W. <Astrophys. J., 653, 675-689 (2006)> =2006ApJ...653..675S
ADC_Keywords: Stars, dwarfs ; Stars, A-type ; Photometry, infrared Keywords: circumstellar matter - infrared: stars - planetary systems: formation Abstract: We report 24 and/or 70um measurements of ∼160 A-type main-sequence stars using the Multiband Imaging Photometer for Spitzer (MIPS). Description: The majority (128) of the stars in this study are from the Spitzer Guaranteed Time Observation (GTO) programs (ASTAR, FAB4, and DIRTY12), for which most were selected because they had known ages based on cluster membership or association with moving groups. An additional 32 stars are included from the Spitzer calibration observations. In total, our sample includes 160 stars ranging in spectral type from B6 to A7, but mostly (∼85%) from B9 to A7. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 158 160 Sample of stars and MIPS measurements table2.dat 65 19 Information on the additional IRAS stars refs.dat 42 23 References
See also: J/ApJ/620/1010 : Spitzer 24µm photometry of A dwarfs (Rieke+, 2005) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Source name 10 A1 --- n_Name [de] Note: d = Herbig Ae/Be star, x = Be star 12- 44 A33 --- AOR The Spitzer observation AOR key(s) 45- 52 A8 --- SpType MK spectral type 54- 58 F5.1 pc Dist Distance 60- 70 A11 --- Loc The Cluster/Moving Group source locate in 72- 74 I3 Myr Age Source age (2) 76 A1 --- n_Age [f] Young star (2) 78- 85 A8 --- r_Age Reference(s) on Age, in refs.dat file 87- 93 F7.2 mJy F24 ? Spitzer/MIPS 24 micron flux density 95-100 F6.2 mJy e_F24 ? Uncertainty in F24um 102-107 F6.2 --- S/N24 ? Signal-to-noise ratio of F24um 109-115 F7.3 --- R24 ? The 24 micron Excess Ratio (4) 117-119 A3 --- IRE24 Infrared excess at 24 microns? (5) 121 A1 --- n_IRE24 [s] star disregarded having 24um excess due to low excess significance (χ24<3) 123 A1 --- l_F70 The 3σ limit flag on F70um 124-131 F8.2 mJy F70 ? Spitzer/MIPS 70 micron flux density 133-139 F7.2 mJy e_F70 ? Uncertainty in F70um 141-146 F6.2 --- S/N70 ? Signal-to-noise ratio of F70um 148-154 F7.3 --- R70 ? The 70 micron Excess Ratio (4) 156-158 A3 --- IRE70 Infrared excess at 70 microns? (5)
Note (2): Age is set to 0 for the young stars that are below the ZAMS on the Herzsprung-Russel diagram Note (4): Ratio of measured flux density to expected photospheric flux density. Note (5): IR excess is classified using the 3-σ criteria excess higher than 1.06 at 24um and 1.55 at 70um: YES = having an infrared excess NO = being detected but with no excess above the 3σ confidence level UPL = having only an upper limit.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Name 10- 13 F4.2 mag Ksmag 2MASS Ks magnitude 15- 17 I3 Myr Age Age (1) 19- 24 A6 --- SpType MK spectral type 27- 31 F5.3 Jy F25 Flux at 25um 33- 37 F5.3 --- R25 Ratio between measured flux and predicted flux based on Ks-[24]color at 25um 39- 43 F5.3 Jy F60 Flux at 60um 45- 49 F5.2 --- R60 Ratio between measured flux and predicted flux based on Ks-[24]color at 60um 51- 54 F4.2 --- e_R60 rms uncertainty on R60um 56- 59 F4.2 --- chi60 Significance of excess emission at 60um, i.e. (R60um-1)/e_R60um 61- 65 F5.2 --- U60 2σ upper limit on R60um, i.e., R60+2e_R60um
Note (1): Reference for age used can be found in Rieke et al. (2005, Cat. J/ApJ/620/1010).
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- 42 A19 --- Aut Author's name
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 31-Jul-2008
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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