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J/AJ/132/1202   RR Lyrae in Northern Sky Variability Survey   (Kinemuchi+, 2006)

Analysis of RR Lyrae stars in the Northern Sky Variability Survey. Kinemuchi K., Smith H.A., Wozniak P.R., McKay T.A. <Astron. J., 132, 1202-1220 (2006)> =2006AJ....132.1202K
ADC_Keywords: Surveys ; Stars, variable ; Photometry ; Abundances, [Fe/H] Keywords: Galaxy: disk - stars: variables: other Abstract: We use data from the Northern Sky Variability Survey (NSVS), obtained from the first-generation Robotic Optical Transient Search Experiment (ROTSE-I), to identify and study RR Lyrae variable stars in the solar neighborhood. We initially identified 1197 RRab (RR0) candidate stars brighter than the ROTSE median magnitude V=14. Periods, amplitudes, and mean V magnitudes are determined for a subset of 1188 RRab stars with well-defined light curves. Metallicities are determined for 589 stars by the Fourier parameter method and by the relationship between period, amplitude, and [Fe/H]. We comment on the difficulties of clearly classifying RRc (RR1) variables in the NSVS data set. Distances to the RRab stars are calculated using an adopted luminosity-metallicity relation with corrections for interstellar extinction. The 589 RRab stars in our final sample are used to study the properties of the RRab population within 5kpc of the Sun. The Bailey diagram of period versus amplitude shows that the largest component of this sample belongs to Oosterhoff type I. Metal-rich ([Fe/H]>-1) RRab stars appear to be associated with the Galactic disk. Our metal-rich RRab sample may include a thin-disk, as well as a thick-disk population, although the uncertainties are too large to establish this. There is some evidence among the metal-rich RRab stars for a decline in scale height with increasing [Fe/H], as was found by Layden. The distribution of RRab stars with -1<[Fe/H]←1.25 indicates that within this metallicity range the RRab stars are a mixture of stars belonging to halo and disk populations. Description: The NSVS database (See http://skydot.lanl.gov/) is constructed from observations taken from ROTSE-I. The NSVS is based on a year's worth of observations, beginning in 1999 April and ending in 2000 March. The data used for this work were obtained from a version of the NSVS database at the University of Michigan. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 41 589 Photometric Metallicity of NSVS RRab Stars table4.dat 49 1188 NSVS RRab Properties
See also: J/AJ/119/1901 : ROTSE all-sky surveys for variable stars (Akerlof+, 2000) J/AJ/128/2965 : Red variables in the NSVS (Williams+, 2004) J/A+A/312/111 : [Fe/H] from RR Lyrae light curves (Jurcsik+, 1996) http://skydot.lanl.gov : NSVS database Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 I8 --- NSVS Northern Sky Variability Survey ID number 10- 14 F5.2 [-] [Fe/H]AP The Sandage (2004AJ....128..858S) [Fe/H] value 16- 19 F4.2 [-] e_[Fe/H]AP The 1σ uncertainty in [Fe/H]AP 21- 25 F5.2 [-] [Fe/H]JK ? The Jurcsik & Kovacs (1996, Cat. J/A+A/312/111) [Fe/H] value 27- 30 F4.2 [-] e_[Fe/H]JK ? The 1σ uncertainty in [Fe/H]JK 32- 36 F5.2 [-] [Fe/H] The best estimate of [Fe/H] 38- 41 F4.2 [-] e_[Fe/H] The 1σ uncertainty in [Fe/H]
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 8 I8 --- NSVS Northern Sky Variability Survey ID number 10- 19 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000) 21- 30 F10.6 deg DEdeg Declination in decimal degrees (J2000) 32- 38 F7.5 d Per Period 40- 43 F4.2 mag Vamp ROTSE amplitude, scaled to Johnson V band 45- 49 F5.2 mag Vmag Mean intensity-weighted V band magnitude
History: From electronic version of the journal References: Wozniak et al., 2004AJ....127.2436W, NSVS, ftp://skydot.lanl.gov/pub/projects/skydot/nsvs/red_variables/
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 25-Apr-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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