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J/AJ/135/907    Variables in Praesepe identified with KELT     (Pepper+, 2008)

A photometric survey for variables and transits in the field of Praesepe with the kilodegree extremely little telescope. Pepper J., Stanek K.Z., Pogge R.W., Latham D.W., Depoy D.L., Siverd R., Poindexter S., Sivakoff G.R. <Astron. J., 135, 907-921 (2008)> =2008AJ....135..907P
ADC_Keywords: Planets ; Stars, variable ; Photometry, infrared Cross identifications ; Photometry, RI Keywords: planetary systems - stars: activity Abstract: The Kilodegree Extremely Little Telescope (KELT) project is a small aperture, wide-angle search for planetary transits of solar-type stars. In this paper, we present the results of a commissioning campaign with the KELT telescope to observe the open cluster Praesepe for 34 nights in early 2005. Light curves were obtained for 69337 stars, out of which we identify 58 long-period variables and 152 periodic variables. Sixteen of these are previously known as variable, yielding 194 newly discovered variable stars for which we provide properties and light curves. We also searched for planetary-like transits, finding four transit candidates. Follow-up observations indicate that two of the candidates are astrophysical false positives, with two candidates remaining as potential planetary transits. Description: The commissioning campaign targeted a field centered on Praesepe (also called M44 and NGC 2632), an open cluster at a distance of 180parsecs. Our observation were centered on a 10.8°x10.8° field located at J2000 08:40:06 +19:41:06. The observing campaign was conducted every clear night from UTC 2005 February 13 until 2005 April 27, obtaining 5220 images. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 109 210 Variable stars identified in KELT observations of Praesepe
See also: B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2010) J/A+A/375/989 : JHK photometry of Praesepe low-mass stars (Bouvier+, 2001) J/AJ/124/1570 : JHKs photometry in Praesepe (Adams+, 2002) J/ApJS/175/191 : Variables from 2MASS calibration fields (Plavchan+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [KP] 3- 8 I6 --- KP [100169/414644] KELT identification number 10 A1 --- n_KP [a] 'a' indicates a Praesepe member 12- 17 F6.3 mag Rmag KELT RK band magnitude (1) 19- 27 F9.5 deg RAdeg Right Ascension in decimal degrees (J2000) 29- 36 F8.5 deg DEdeg Declination in decimal degrees (J2000) 38- 43 F6.3 mag Jmag ? 2MASS J band magnitude 45- 50 F6.3 mag Hmag ? 2MASS H band magnitude 52- 57 F6.3 mag Ksmag ? 2MASS KS band magnitude 59- 75 A17 --- 2MASS 2MASS identification (JHHMMSSss+DDMMSSs) 77 A1 --- f_2MASS [b] Multiple 2MASS matches (2) 79- 85 F7.4 d Per ? Period 87- 90 A4 --- Kclass KELT classification (EB, LPV, or Puls) 92-100 A9 --- XID GCVS/NSV identification 102-109 A8 --- Vclass GCVS/NSV classification (3)
Note (1): The RK filter is a very braod R filter; the combined Filter+CCD response has effective wavelength = 691nm, effective width = 318nm. Note (2): 'b' indicates stars which matched to more than one 2MASS source within the 9.5" matching radius. The 2MASS ID and JHK colors in the table are for the closest match within the radius. Note (3): Classification as follows: V = Variable (no classification) SR = Semiregular variable RR Lyr = RR Lyrae-type variable BY Dra = BY Draconis-type variable Algol = Algol-type eclipsing system W UMa = W UMa-type eclipsing system EA/SD = Algol-type eclipsing system / semidetached EA/DS/RS = Algol-type eclipsing system / detached system with a subgiant / RS Canum Venaticorum-type system (strong CaII H and K emission lines of variable intensity)
Nomenclature Note: Variable stars designated by <Cl* NGC 2632 KP NNNNNN> in Simbad. History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 24-Jun-2010
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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