CCD ensemble photometry on an inhomogeneous set of exposures

Honeycutt, R. K.

doi:10.1086/133015

Cited by 176 publications

(143 citation statements)

References 2 publications

(2 reference statements)

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“…These were supplied to AstroVar, a custom interactive program optimized for the detection and study of variables in large data sets. AstroVar is based on the method of incomplete ensemble photometry (Honeycutt 1992), expanding the initial implementation by adding interactive graphical interfaces, as well as time series analysis. Light curves were examined for stars whose variability exceeded 3 of the scatter of constant stars at the corresponding mean magnitude level.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

WIYN Open Cluster Study. XV. Photometric Monitoring of Open Clusters: New Variables in NGC 188

Kafka

Honeycutt

2003

Astron J

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Photometric monitoring of the central 17 0 Â 17 0 of the old open cluster NGC 188 with the WIYN 3.5 m telescope has resulted in the discovery of a number of new variable stars, down to 21.5 mag in V, 35 of which have well-determined periods. The variability types of the fainter stars of the sample (18-21.5 mag) remain uncertain. However, most of the brighter stars (15-18 mag) probably make up the low-luminosity extension of the already known W UMa population of NGC 188. We also report the discovery of two longer period variables on the subgiant branch of the cluster CMD, most likely FK Comae stars, which suggests that the cluster may provide significant insight on the formation and evolution of contact binary systems. Alternatively, these objects may represent a new kind of pulsation variables.

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Section: Observations and Data Reductionmentioning

confidence: 99%

WIYN Open Cluster Study. XV. Photometric Monitoring of Open Clusters: New Variables in NGC 188

Kafka

Honeycutt

2003

Astron J

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“…Typically, RoboScope obtains one or two 4 minute exposures per clear night for each of D140 program stars. The data are reduced using the method of incomplete ensemble photometry (Honeycutt 1992). For DI Lac, 85 ensemble stars were used in 987 exposures over nine observing seasons from 1990 November to 1998 November.…”

Section: Optical Photometrymentioning

confidence: 99%

Long‐Term Optical and X‐Ray Observations of the Old Novae DI Lacertae and V841 Ophiuchi1

Hoard¹,

Szkody²,

Honeycutt³

et al. 2000

PUBL ASTRON SOC PAC

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ABSTRACT. We present an analysis of ground-based optical photometry and spectroscopy and Rossi X-Ray T iming Explorer X-ray observations of the old novae DI Lacertae and V841 Ophiuchi. Our optical photometry data (obtained with the automated photometry telescope RoboScope) comprise an almost decade-long light curve for each star, while the contemporaneous spectroscopy and X-ray observations repeatedly sampled each nova during separate intervals of B45È55 days in length. The long-term optical light curves of both novae reveal quasi-periodic variability on typical timescales of D30È50 days with amplitudes of *V D 0.4È0.8 mag. V841 Oph also displays a long-term, sinusoidal modulation of its optical light on a timescale of 3.5È5 yr. The optical spectra of these novae display quite di †erent characteristics from each other, with DI Lac showing narrow Balmer emission cores situated in broad absorption troughs while V841 Oph exhibits strong single-peaked Balmer, He I, and He II emission lines. We Ðnd little change between spectra obtained during di †erent optical brightness states. The X-ray count rates for both novae were very low counts s~1), and there was no reliable correlation between X-ray and optical brightness. The ([1.5 combined X-ray spectrum of DI Lac is best Ðt by a bremsstrahlung emission model (with kT D 4 keV and cm~3) ; the X-ray spectrum of V841 Oph is too weak to allow model Ðtting. We discuss the N H \ 1.8 ] 1022 possible origin of variability in these old novae in terms of magnetic activity on the secondary star, dwarf nova type disk instabilities, and the "" hibernation ÏÏ scenario for cataclysmic variable stars.

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“…The standard procedure was used for reduction of the photometric data (de-biasing, dark frame subtraction and flat-fielding) by software AIP4WIN2.0 (Berry & Burnell 2006). We used aperture photometry with radius of 1 The use of numerous comparison stars scattered over the CCD field increases considerably the statistical accuracy of the comparison magnitude (Gilliland & Brown 1988, Honeycutt 1992. Table 5.…”

Section: Observationsmentioning

confidence: 99%

Observations and light curve solutions of the W UMa binaries V796 Cep, V797 Cep, CSS J015341.9+381641 and NSVS 3853195

Kjurkchieva

Popov

Ibryamov

et al. 2017

Res. Astron. Astrophys.

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Photometric observations in Sloan g' and i' bands of four W UMa binaries, V796Cep, V797 Cep, CSS J015341.9+381641 and NSVS 3853195, are presented. Our observations showed that CSS J015404.1+382805 and NSVS 3853195 are the same star. We determined the initial epochs T 0 of all targets and improved the period of NSVS 3853195. The light curve solutions of our data revealed that the components of each target are almost the same in mass, temperature, radius and luminosity. The stellar components are of G and K spectral types and undergo partial eclipses. All systems have barely-overcontact configurations and belong to H subtype W UMa binaries. We established that the relation between the luminosity ratio l 2 /l 1 and mass ratio q of our targets is approximately l 2 /l 1 = q 1.5 .

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CCD ensemble photometry on an inhomogeneous set of exposures

Cited by 176 publications

References 2 publications

WIYN Open Cluster Study. XV. Photometric Monitoring of Open Clusters: New Variables in NGC 188

WIYN Open Cluster Study. XV. Photometric Monitoring of Open Clusters: New Variables in NGC 188

Long‐Term Optical and X‐Ray Observations of the Old Novae DI Lacertae and V841 Ophiuchi1

Observations and light curve solutions of the W UMa binaries V796 Cep, V797 Cep, CSS J015341.9+381641 and NSVS 3853195

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