The Pan-STARRS wide-field optical/NIR imaging survey

Kaiser, Nick; Burgett, W. S.; Chambers, K.; Denneau, L.; Heasley, J. N.; Jedicke, Robert; Magnier, E. A.; Morgan, J.; Onaka, Peter M.; Tonry, J.

doi:10.1117/12.859188

Cited by 427 publications

(173 citation statements)

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“…Regarding (iii), we have independently confirmed the reasonableness of the conversion scheme from B to K s magnitudes proposed by Karachentsev & Kutkin (2005) as far as can be monitored by available data, but the uncertainties are admittedly large. The situation could be vastly improved in the future with systematic incorporation of deep infrared or optical photometry from, for example, WISE, the Widefield Infrared Survey Explorer (Wright et al 2010) or Pan-STARRS (Kaiser et al 2010). Given an estimate of K s band flux with available information, the conversion to mass remains an issue; the concerns (ii) and (iv) emphasize separate aspects.…”

Section: The Group Mass Functionmentioning

confidence: 99%

Galaxy Groups Within 3500 km s⁻¹

Kourkchi¹,

Tully²

2017

ApJ

205

232

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A study of the group properties of galaxies in our immediate neighborhood provides a singular opportunity to observationally constrain the halo mass function, a fundamental characterization of galaxy formation. Detailed studies of individual groups have provided the coefficients of scaling relations between a proxy for the virial radius, velocity dispersion, and mass that usefully allows groups to be defined over the range 10 10 −10 15 M ⊙ . At a second hierarchical level, associations are defined as regions around collapsed halos extending to the zero velocity surface at the decoupling from cosmic expansion. The most remarkable result of the study emerges from the construction of the halo mass function from the sample. At ∼ 10 12 M ⊙ there is a jog from the expectation Sheth-Tormen function, such that halo counts drop by a factor ∼ 3 in all lower mass bins.

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Section: The Group Mass Functionmentioning

confidence: 99%

Galaxy Groups Within 3500 km s⁻¹

Kourkchi¹,

Tully²

2017

ApJ

205

232

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“…Large format, back-illuminated devices with high quantum efficiency and low noise form the basis for existing and planned large camera systems on astronomical telescopes such as the VLT Survey Telescope OmegaCAM 1 (268 Megapixels), the Dark Energy Survey camera 2, 3 (520 Megapixels), the Subaru HyperSuprime camera 4,5 (872 Megapixels), the University of Hawaii Pan-STARRS camera 6,7 (1.4 Gigapixels), and the camera for the planned Large Synoptic Survey Telescope 8 (LSST, 3.2 Gigapixels).…”

Section: Introductionmentioning

confidence: 99%

Design of low-noise output amplifiers for P-channel charge-coupled devices fabricated on high-resistivity silicon

et al. 2012

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We describe the design and optimization of low-noise, single-stage output amplifiers for p-channel charge-coupled devices (CCDs) used for scientific applications in astronomy and other fields. The CCDs are fabricated on highresistivity, 4000-5000 Ω-cm, n-type silicon substrates. Single-stage amplifiers with different output structure designs and technologies have been characterized. The standard output amplifier is designed with an n + polysilicon gate that has a metal connection to the sense node. In an effort to lower the output amplifier readout noise by minimizing the capacitance seen at the sense node, buried-contact technology has been investigated. In this case, the output transistor has a p + polysilicon gate that connects directly to the p + sense node. Output structures with buried-contact areas as small as 2 µm × 2 µm are characterized. In addition, the geometry of the source-follower transistor was varied, and we report test results on the conversion gain and noise of the various amplifier structures. By use of buried-contact technology, better amplifier geometry, optimization of the amplifier biases and improvements in the test electronics design, we obtain a 45% reduction in noise, corresponding to 1.7 e − rms at 70 kpixels/sec.

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“…As currently envisaged, the next generation of wide-field, time-domain surveys like Pan-STARRS (Kaiser et al 2010), PTF (Rau et al 2009), Skymapper (Keller et al 2007), and ultimately LSST (Ivezic et al 2008) is being designed to study the celestial sphere based dominantly on the variability of point sources. A mode in which whole images of the sky are preserved with a cadence of weeks or months is likely to reveal an abundance of additional LE features and the history and perspectives they carry in their scattered light.…”

Section: Discussionmentioning

confidence: 99%

“…These fairly common optically induced difference features make it difficult to identify faint LEs with software and most LE searches rely, at least in part, on visual inspection of the difference images. With the advent of the next generation of wide-field, time-domain surveys like the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS: Kaiser et al 2010), Palomar Transient Factory (PTF: Rau et al 2009), Skymapper (Keller et al 2007), and ultimately Large Synoptic Survey Telescope (LSST: Ivezic et al 2008), visual inspection will no longer be a viable option and software solutions for identifying true LEs will need to be developed.…”

Section: Finding Lesmentioning

confidence: 99%

Light Echoes of Transients and Variables in the Local Universe

Rest

Sinnott

Welch

2012

Publ. – Astron. Soc. Aust

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Astronomical light echoes, the time-dependent light scattered by dust in the vicinity of varying objects, have been recognized for over a century. Initially, their utility was thought to be confined to mapping out the three-dimensional distribution of interstellar dust. Recently, the discovery of spectroscopically useful light echoes around centuries-old supernovae in the Milky Way and the Large Magellanic Cloud has opened up new scientific opportunities to exploit light echoes.In this review, we describe the history of light echoes in the local Universe and cover the many new developments in both the observation of light echoes and the interpretation of the light scattered from them. Among other benefits, we highlight our new ability to classify outbursting objects spectroscopically, view them from multiple perspectives, obtain a spectroscopic time series of the outburst, and establish accurate distances to the source event. We also describe the broader range of variable objects with properties that may be better understood from light-echo observations. Finally, we discuss the prospects of new light-echo techniques not yet realized in practice.

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The Pan-STARRS wide-field optical/NIR imaging survey

Cited by 427 publications

References 0 publications

Galaxy Groups Within 3500 km s⁻¹

Galaxy Groups Within 3500 km s⁻¹

Design of low-noise output amplifiers for P-channel charge-coupled devices fabricated on high-resistivity silicon

Light Echoes of Transients and Variables in the Local Universe

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The Pan-STARRS wide-field optical/NIR imaging survey

Cited by 427 publications

References 0 publications

Galaxy Groups Within 3500 km s−1

Galaxy Groups Within 3500 km s−1

Design of low-noise output amplifiers for P-channel charge-coupled devices fabricated on high-resistivity silicon

Light Echoes of Transients and Variables in the Local Universe

Contact Info

Product

Resources

About

Galaxy Groups Within 3500 km s⁻¹

Galaxy Groups Within 3500 km s⁻¹