WIYN One Degree Imager (ODI)

Jacoby, George H.; Tonry, J.; Burke, Barry E.; Claver, Charles F.; Starr, Barry Michael; Saha, Abhijit; Harmer, C. F. W.

doi:10.1117/12.457017

Cited by 21 publications

(10 citation statements)

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“…The operation of the OTA has been previously described 3,6 and will be briefly reviewed here with the help of Figure 2. All functioning cells are assigned to either image guide stars for measuring the local image translation or to acquire the science images.…”

Section: Device Architecture and Operationmentioning

confidence: 99%

“…6 WIYN is contributing to this device development by funding the design of a second source of OTAs at Semiconductor Technology Associates (STA) in San Juan Capistrano, CA and fabrication at Dalsa Semiconductor. The Lincoln and STA designs were jointly carried out to share common design features, be functionally compatible, and use a common package and pinouts.…”

Section: Introductionmentioning

confidence: 99%

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The orthogonal-transfer array: a new CCD architecture for astronomy

et al. 2004

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The orthogonal-transfer array (OTA) is a new CCD architecture designed to provide wide-field tip-tilt correction of astronomical images. The device consists of an 8 8 array of small (~500 500 pixels) orthogonal-transfer CCDs (OTCCD) with independent addressing and readout of each OTCCD. This approach enables an optimum tip-tilt correction to be applied independently to each OTCCD across the focal plane. The first design of this device has been carried out at MIT Lincoln Laboratory in support of the Pan-STARRS program with a collaborative parallel effort at Semiconductor Technology Associates (STA) for the WIYN Observatory. The two versions of this device are functionally compatible and share a common pinout and package. The first wafer lots are complete at Lincoln and at Dalsa and are undergoing wafer probing.

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Section: Device Architecture and Operationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The orthogonal-transfer array: a new CCD architecture for astronomy

et al. 2004

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“…The bi-directional nature of these links can be significant for some applications. For instance with QUOTA and ODI [4], the proposed processing methodology is that the PCs will be doing centroid calculation and determining the required image shifts in the OTACCD [4] cells. This high-speed bi-directional communication allows the OT correction data to pass to the Detector Head Electronics at the required rates, and off-load any significant processing from the Detector Head Electronics to the PC.…”

Section: System Communications Linksmentioning

confidence: 99%

“…As stated above, MONSOON is more than a controller, but rather an image acquisition system. MONSOON has been specifically designed to meet and exceed the requirements of ORION (2k x 2k) InSb Development [2], NEWFIRM (4k x4k) [3], QUOTA (8k x 8k) [4], ODI (32k x 32k) [4], and LSST (45k x 45k) [5].…”

Section: Integrated Systems Viewpointmentioning

confidence: 99%

MONSOON: Image Acquisition System or "Pixel Server"

et al. 2003

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The MONSOON Image Acquisition System has been designed to meet the need for scalable, multichannel, high-speed image acquisition required for the next-generation optical and infared detectors and mosaic projects currently under development at NOAO as described in other papers at this proceeding such as ORION, NEWFIRM, QUOTA, ODI and LSST. These new systems with their large scale (64 to 2000 channels) and high performance (up to 1Gbyte/s) raise new challenges in terms of communication bandwidth, data storage and data processing requirements which are not adequately met by existing astronomical controllers. In order to meet this demand, new techniques for not only a new detector controller, but rather a new image acquisition architecture, have been defined. These extremely large scale imaging systems also raise less obvious concerns in previously neglected areas of controller design such as physical size and form factor issues, power dissipation and cooling near the telescope, system assembly/test/ integration time, reliability, and total cost of ownership. At NOAO we have taken efforts to look outside of the astronomical community for solutions found in other disciplines to similar classes of problems. A large number of the challenges raised by these system needs are already successfully being faced in other areas such as telecommunications, instrumentation and aerospace. Efforts have also been made to use true commercial off the shelf (COTS) system elements, and find truly technology independent solutions for a number of system design issues whenever possible. The Monsoon effort is an full-disclosure development effort by NOAO in collaboration with the CARA ASTEROID project for the benefit of the astronomical community.

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“…Correlations could be induced by shared peculiar velocities if close enough to be influenced by the same over-density (e.g. galaxy cluster) or by lensing magnification if close to the same line CCAT (Radford et al, 2007), DES (Lin, 2006), EPIC (Bock et al, 2009), Euclid (Laureijs et al, 2011), HETDEX (Hill et al, 2008), JWST (Gardner, 2009), LiteBIRD (Hazumi, 2011), LSST (Ivezic et al, 2008), ODI (Jacoby et al, 2002), Pan-STARRS4 (Kaiser, 2004), SKA (Torres-Rodríguez & Cress, 2007), SNAP (Bebek, 2007), WFIRST (Spergel et al, 2013).…”

Section: Cosmic Microwave Background (Cmb)mentioning

confidence: 99%

Echo hunting: using reverberation mapping of active galactic nuclei to probe black hole growth and cosmic expansion

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Broad line active galactic nuclei (AGN) have been proposed as potential standardisable candles by Watson et al. (2011), using a technique called reverberation mapping. This thesis investigates whether AGN are useful high redshift standard candles and how to optimise the scientific output of the ongoing OzDES reverberation mapping survey.AGN are highly luminous, numerous, and are present over a huge range of cosmic history.Due to this, they can be used to probe unexplored regions in the Universe's expansion history and help constrain the properties of dark energy. To investigate the usefulness of AGN I consider whether a general high-redshift standard candle will be a powerful probe of dark energy, when compared to other types of planned dark energy measurements.I consider several models of how the dark energy equation of state, w(z), may evolve in time and assess the optimal redshift distribution that a high-redshift standard-candle survey could take to constrain these models. The more general the form of the dark energy equation of state w(z) being tested, the more useful high-redshift standard candles become.As part of the OzDES spectroscopic survey we are carrying out a large scale reverberation mapping study of ≥500 AGN over five years in the 30 deg 2 area of the Dark Energy Survey (DES) supernova fields. These AGN have redshifts ranging up to 4 and have apparent AB magnitudes between 16.8 < r < 22.5 mag. The aim of the survey is to measure time lags between fluctuations in AGN continuum and broad emission line fluxes of individual objects, in order to measure black hole masses for a broad range of AGN and constrain the radius-luminosity (R − L) relationship, which makes them viable standard candles. I investigate the expected efficiency of the OzDES reverberation mapping campaign and its ii iii possible extensions. We expect to recover lags for ∼ 35−45% of the AGN. AGN with shorter lags and greater variability are more likely to yield a lag and objects with lags ≲ 6 month or ∼ 1 year are expected be recovered the most accurately. I show that the baseline OzDES reverberation mapping campaign should produce an unbiased measurement of the radiusluminosity relationship for the emission lines: Hβ, Mg ii, and C iv. However, enhancing the baseline survey by either increasing the spectroscopic cadence, extending the survey season, or improving the accuracy of the emission line flux measurement will significantly improve the R − L parameter constraints for all lines.For the first two years of OzDES we have observed 989 AGN but in the following three years the number of targets we can continue to monitor will be reduced, possibly down to a minimum of 500 AGN. We chose to prioritise quasars that are likely to recover a lag and/or enhance the scientific output of the survey. I quantify the quality of the emission line flux measurements using the signal-to-noise ratio of the flux measurement, and select the year 3 (2015) targets based on this value and their scientific merit. I also perform preliminary reverbera...

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WIYN One Degree Imager (ODI)

Cited by 21 publications

References 0 publications

The orthogonal-transfer array: a new CCD architecture for astronomy

The orthogonal-transfer array: a new CCD architecture for astronomy

MONSOON: Image Acquisition System or "Pixel Server"

Echo hunting: using reverberation mapping of active galactic nuclei to probe black hole growth and cosmic expansion

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