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J/ApJ/697/1578         A debris disk study of Praesepe           (Gaspar+, 2009)

The low level of debris disk activity at the time of the late heavy bombardment: a Spitzer study of Praesepe. Gaspar A., Rieke G.H., Su K.Y.L., Balog Z., Trilling D., Muzzerole J., Apai D., Kelly B.C. <Astrophys. J., 697, 1578-1596 (2009)> =2009ApJ...697.1578G
ADC_Keywords: Clusters, open ; Photometry, infrared ; Stars, dwarfs Keywords: circumstellar matter - infrared: stars - open clusters and associations: individual (Praesepe, M44, NGC 2632, Beehive) - planetary systems: formation - stars: evolution Abstract: We present 24um photometry of the intermediate-age open cluster Praesepe. We assemble a catalog of 193 probable cluster members that are detected in optical databases, the Two Micron All Sky Survey (2MASS), and at 24um, within an area of ∼2.47deg2. Mid-IR excesses indicating debris disks are found for one early-type and for three solar-type stars. Corrections for sampling statistics yield a 24um excess fraction (debris disk fraction) of 6.5%±4.1% for luminous and 1.9%±1.2% for solar-type stars. The incidence of excesses is in agreement with the decay trend of debris disks as a function of age observed for other cluster and field stars. Description: We used MIPS to observe Praesepe as part of the GTO program PID 30429 (2007 May 30). The center part of the cluster (8h40m21s, 19°38'40") was imaged using three scan maps. Out of the 193 cluster members that we detected at all wavelengths in the combined catalog (SDSS, WEBDA and 2MASS), 29 were early (B5-A9) and 164 later (F0-M0) spectral types. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 111 193 Photometry of Praesepe members in the 24µm band
See also: II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009) II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) I/257 : Proper Motions in Praesepe (Wang+, 1995) J/A+A/510/A27 : Very low mass stars in Praesepe (Boudreault+, 2010) J/AJ/134/2340 : Membership of Praesepe and Coma Berenices clusters (Kraus+, 2007) J/AJ/124/1570 : JHKs photometry in Praesepe (Adams+, 2002) J/A+A/375/989 : JHK photometry of Praesepe low-mass stars (Bouvier+, 2001) J/A+AS/109/29 : Very low mass stars in Praesepe (Hambly+, 1995) : WEBDA database access Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Identification number 5 I1 h RAh Hour of right ascension (J2000) 7- 8 I2 min RAm Minute of right ascension (J2000) 10- 14 F5.2 s RAs Second of right ascension (J2000) 16 A1 --- DE- Sign of declination (J2000) 17- 18 I2 deg DEd Degree of declination (J2000) 20- 21 I2 arcmin DEm Arcminute of declination (J2000) 23- 27 F5.2 arcsec DEs Arcsecond of declination (J2000) 29- 33 F5.2 mag gmag SDSS g-band magnitude 34 A1 --- f_gmag [*] magnitude calculated from B (1) 36- 40 F5.2 mag rmag SDSS r-band magnitude 41 A1 --- f_rmag [*] magnitude calculated from V (1) 43- 47 F5.2 mag Ksmag 2MASS Ks-band magnitude 49- 53 F5.2 mag e_Ksmag Ksmag uncertainty 55- 59 F5.2 mag [24] Spitzer/MIPS 24um band magnitude (2) 61- 64 F4.2 mag e_[24] 24um-band magnitude uncertainty 66- 71 F6.2 mJy F24 Spitzer/MIPS 24um flux (2) 73- 76 F4.2 mJy e_F24 F24 uncertainty 78- 82 F5.1 mas/yr pmRA ? Proper motion in right ascension 83 A1 --- --- [0] 85- 89 F5.1 mas/yr pmDE ? Proper motion in declination 90 A1 --- --- [0] 92- 94 I3 --- WJJP ? Number from Wang et al. 1995, Cat. I/257 (<Cl* NGC 2632 WJJP NNN> in Simbad) 96-111 A16 --- 2MASS 2MASS identification (HHMMSSss+DDMMSSs)
Note (1): The r and/or g magnitudes marked with a star were calculated from B and V WEBDA magnitudes as described in Section 3, while the rest are the original SDSS values. Note (2): The [24] magnitudes are the ones that were calibrated to the 2MASS Ks magnitudes, while the mJy values in the F24 column are the original flux values.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-May-2011
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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