Stellar Variability in a Survey of Field Stars

Everett, Mark E.; Howell, Steve B.; Belle, Gerald van; Ciardi, David R.

doi:10.1086/341682

Cited by 17 publications

(34 citation statements)

References 28 publications

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“…In comparison to Everett et al (2002), who found an overall variability fraction of 1% in their weeklong sample, the fraction here is 3-4 times in field groups 01 and 19. However, the two fractions are roughly equivalent if the amplitude level for variability is limited to the photometric uncertainties in the Everett et al (2002) study. Figures 15 and 16 show the variability fraction of sources for the field groups as a function of B À V color for the most complete magnitude sample V ¼ 17:5À22:0.…”

Section: Variability Fractions By Magnitude and Colorcontrasting

confidence: 89%

“…Recently, wide-field temporal surveys have begun to catch up, going to deeper limits and becoming increasingly more common, such as the Bright Sky Variability Survey ( BSVS; Everett et al 2002), QUEST ( Vivas et al 2004), SuperMACHO ( Becker et al 2005), and the Faint Sky Variability Survey ( FSVS; Groot et al 2003), with a variety of different science goals and target populations, probing new areas in astrophysics. A survey like the FSVS with variability sampling over hours to years samples a large range of dynamical phenomena, including mass transfer events, pulsations, and stellar activity with amplitudes $0.01 and larger.…”

Section: Introductionmentioning

confidence: 99%

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Color and Variability Characteristics of Point Sources in the Faint Sky Variability Survey

2006

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We present an analysis of the color and variability characteristics for point sources in the Faint Sky Variability Survey (FSVS). The FSVS cataloged $23 deg 2 in BVI filters from $16 to 24 mag to investigate variability in faint sources at moderate-to-high Galactic latitudes. Point-source completeness is found to be >83% for a selected representative sample (V ¼ 17:5À22:0 mag, B À V ¼ 0:0À1:5) containing both photometric B, V detections and 80% of the time-sampled V data available compared to a basic internal source completeness of 99%. Multiepoch (10-30) observations in V spanning minutes to years modeled by light-curve simulations reveal amplitude sensitivities to $0.015-0.075 mag over a representative V ¼ 18À22 mag range. Periodicity determinations appear viable to timescales of order 1 day or less using the most sampled fields ($30 epochs). The fraction of point sources is found to be generally variable at 5%-8% over V ¼ 17:5À22:0 mag. For V brighter than 19 mag, the variable population is dominated by low-amplitude (<0.05 mag) and blue (B À V < 0:35) sources, possibly representing a population of Doradus stars. Overall, the dominant population of variable sources are bluer than B À V ¼ 0:65 and have mainsequence colors, likely reflecting larger populations of RR Lyrae, SX Phe, Doradus, and W UMa variables.

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Section: Variability Fractions By Magnitude and Colorcontrasting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Color and Variability Characteristics of Point Sources in the Faint Sky Variability Survey

2006

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“…Wide field observations of field stars have also produced a number of new variable stars (e.g. Bakos et al 2002; Everett et al 2002; Hartman et al 2004).…”

Section: Introductionmentioning

confidence: 99%

Results from the Wide Angle Search for Planets Prototype (WASP0) - II. Stellar variability in the Pegasus field

Kane

Lister

Cameron

et al. 2005

Monthly Notices of the Royal Astronomical Society

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Recent wide field photometric surveys, which target a specific field for long durations, are ideal for studying both long‐ and short‐period stellar variability. Here, we report on 75 variable stars detected during the observations of a field in Pegasus using the Wide Angle Search for Planets Prototype (WASP0) instrument, 73 of which are new discoveries. The variables detected include 16 δ Scuti stars, 34 eclipsing binaries, 3 BY Draconis stars and 4 RR Lyraes. We estimate that the fraction of stars in the field brighter than V∼ 13.5 exhibiting variable behaviour with an amplitude greater than 0.6 per cent rms is ∼0.4 per cent. These results are compared with other wide field stellar variability surveys, and implications for detecting transits due to extra‐solar planets are discussed.

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“…Figure 6 displays the color-magnitude diagram, (B−R) versus R, to show difference of color distributions between pulsating and eclipsing stars. The left panel was made from the observation results of Everett et al (2002) with 222 variable stars. The right panel shows the diagram for 91 ROTSE-I δ Scuti stars whose B and R magnitudes were obtained from the USNO catalogue.…”

Section: Resultsmentioning

confidence: 99%

Multiband photometric re-classification of ROTSE-IδScuti type stars

Jin

Kim

Kwon

et al. 2003

A&A

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Abstract. We present multi-passband CCD photometry of 20 ROTSE-I δ Scuti type pulsating stars and 1 RR Lyrae star to reclassify their variable types using the comparison of amplitudes between V and I passbands. For the re-classification, we used a criterion that pulsating stars have larger amplitude differences between passbands than eclipsing binaries because brightness changes of pulsating stars are mainly due to the temperature variations. As a result, only six stars were re-confirmed as δ Scuti variables and thirteen stars turned out to be W UMa type eclipsing binaries. The other two stars were identified as one cataclysmic variable and one non-variable, respectively. Our results suggest that a number of ROTSE-I δ Scuti type stars, which do not show typical pulsating light curves of high amplitude δ Scuti stars, are W UMa type eclipsing binaries.

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Stellar Variability in a Survey of Field Stars

Cited by 17 publications

References 28 publications

Color and Variability Characteristics of Point Sources in the Faint Sky Variability Survey

Color and Variability Characteristics of Point Sources in the Faint Sky Variability Survey

Results from the Wide Angle Search for Planets Prototype (WASP0) - II. Stellar variability in the Pegasus field

Multiband photometric re-classification of ROTSE-IδScuti type stars

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