The 64 Mpixel wide field imager for the Wendelstein 2m telescope: design and calibration

Kosyra, R.; Gössl, Claus; Hopp, U.; Lang-Bardl, Florian; Riffeser, A.; Bender, Ralf; Seitz, S.

doi:10.1007/s10686-014-9414-1

Cited by 23 publications

(27 citation statements)

References 26 publications

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“…We observed K2-95 with the 2.0 m Fraunhofer telescope Wendelstein , using the Wide Field Imager (WFI) (Kosyra et al 2014) on Mt.Wendelstein in the Bavarian Alps. An independent transit detection from a ground-based facility serves not only for period confirmation and estimation of its uncertainty, but as evidence for the planetary nature of the transit from a common eclipse depth at different wavelengths.…”

Section: Photometric Follow-upmentioning

confidence: 99%

K2 Discovers a Busy Bee: An Unusual Transiting Neptune Found in the Beehive Cluster

et al. 2016

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Open clusters have been the focus of several exoplanet surveys, but only a few planets have so far been discovered. The Kepler spacecraft revealed an abundance of small planets around small cool stars, therefore, such cluster members are prime targets for exoplanet transit searches. Keplerʼs new mission, K2, is targeting several open clusters and star-forming regions around the ecliptic to search for transiting planets around their low-mass constituents. Here, we report the discovery of the first transiting planet in the intermediate-age ( and an orbital period of 10.134 days. We combined photometry, medium/high-resolution spectroscopy, adaptive optics/speckle imaging, and archival survey images to rule out any false-positive detection scenarios, validate the planet, and further characterize the system. The planet's radius is very unusual as M-dwarf field stars rarely have Neptune-sized transiting planets. The comparatively large radius of K2-95b is consistent with the other recently discovered cluster planets K2-25b (Hyades) and K2-33b (Upper Scorpius), indicating systematic differences in their evolutionary states or formation. These discoveries from K2 provide a snapshot of planet formation and evolution in cluster environments and thus make excellent laboratories to test differences between field-star and cluster planet populations.

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Section: Photometric Follow-upmentioning

confidence: 99%

K2 Discovers a Busy Bee: An Unusual Transiting Neptune Found in the Beehive Cluster

et al. 2016

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“…The WWFI camera has a f/7.8 optics and is equipped with a CCD mosaic from Spectral Instruments Tucson, mounting four 4k by 4k 15 μm 4port read-out e2V CCDs that provides a pixel size of 0.2 arcsec and covers 27 x 27 arcmin on the sky. Information on the observing site and the technical equipment used can be found in Kosyra et al (2014).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Mt. Wendelstein imaging of the post-perihelion dust coma of 67P/Churyumov–Gerasimenko in 2015/2016

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Riffeser

Kluge

et al. 2016

Mon. Not. R. Astron. Soc.

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“…in science verification data from the Dark Energy Camera (DECam), but also in many other cameras (e.g. MegaCam and LSST candidate sensors [2], Euclid candidate sensors [26] and the Wendelstein Wide Field Imager [20]).…”

Section: Introductionmentioning

confidence: 99%

Characterization and correction of charge-induced pixel shifts in DECam

et al. 2015

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Interaction of charges in CCDs with the already accumulated charge distribution causes both a flux dependence of the point-spread function (an increase of observed size with flux, also known as the brighter/fatter effect) and pixel-to-pixel correlations of the Poissonian noise in flat fields. We describe these effects in the Dark Energy Camera (DECam) with charge dependent shifts of effective pixel borders, i.e. the Antilogus et al. (2014) model, which we fit to measurements of flat-field Poissonian noise correlations. The latter fall off approximately as a power-law r −2.5 with pixel separation r, are isotropic except for an asymmetry in the direct neighbors along rows and columns, are stable in time, and are weakly dependent on wavelength. They show variations from chip to chip at the 20% level that correlate with the silicon resistivity. The charge shifts predicted by the model cause biased shape measurements, primarily due to their effect on bright stars, at levels exceeding weak lensing science requirements. We measure the flux dependence of star images and show that the effect can be mitigated by applying the reverse charge shifts at the pixel level during image processing. Differences in stellar size, however, remain significant due to residuals at larger distance from the centroid. KEYWORDS: Photon detectors for UV, visible and IR photons (solid-state). * Corresponding author. 12 −1 × Q 11 − Q 22 2Q 12 . (4.2) When second moments are measured with uniform weight as in Eqn. 4.1, deconvolution with the PSF can be performed by subtracting the observed and PSF second moments, 8 Q gal, dec ⋆ = Q gal, obs ⋆ − Q PSF ⋆ . (4.3)Observationally, one estimates Q PSF ⋆ from the second moments of star images. Since the stars

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The 64 Mpixel wide field imager for the Wendelstein 2m telescope: design and calibration

Cited by 23 publications

References 26 publications

K2 Discovers a Busy Bee: An Unusual Transiting Neptune Found in the Beehive Cluster

K2 Discovers a Busy Bee: An Unusual Transiting Neptune Found in the Beehive Cluster

Mt. Wendelstein imaging of the post-perihelion dust coma of 67P/Churyumov–Gerasimenko in 2015/2016

Characterization and correction of charge-induced pixel shifts in DECam

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