DCR_references.bib

@article{Stone1996,
author = {Stone, Ronald C.},
doi = {10.1086/133831},
file = {:Users/sullivan/Documents/Mendeley Desktop/Stone/1996/Stone - 1996 - An Accurate Method for Computing Atmospheric Refraction.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {nov},
number = {729},
pages = {1051},
title = {{An Accurate Method for Computing Atmospheric Refraction}},
note = {\url{http://www.jstor.org/stable/10.2307/40680838}},
url = {http://www.jstor.org/stable/10.2307/40680838},
volume = {108},
year = {1996}
}

@article{Filippenko1982,
	author = {Filippenko, Alexei V},
	doi = {10.1086/131052},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Filippenko/1982/Filippenko - 1982 - The importance of atmospheric differential refraction in spectrophotometry.pdf:pdf},
	issn = {0004-6280},
	journal = {Publications of the Astronomical Society of the Pacific},
	keywords = {instrumentation,observing techniques,spectrophotometry},
	mendeley-groups = {Astrometry},
	month = {aug},
	number = {August},
	pages = {715},
	title = {{The importance of atmospheric differential refraction in spectrophotometry}},
	note = {\url{http://www.jstor.org/stable/10.2307/40678026}},
	url = {http://www.jstor.org/stable/10.2307/40678026},
	volume = {94},
	year = {1982}
}

@inproceedings{Cuby1998,
	abstract = {The atmospheric refraction affects the position of objects in the sky in two ways: a chromatic effect and a field differential effect. The former is about the same in the field and can be, in principle, corrected using an Atmospheric Dispersion Compensator (ADC). The latter is dependent of the field size and cannot be corrected. For spectroscopy in wide fields, both effects have to be carefully considered because they affect the spectrophotometry in terms of signal to noise ratio and spectral distortions. The present study aims to evaluate the atmospheric effects in the case of the VIMOS instrument for the ESO VLT. It is shown that provided a careful operational mode the distortion of spectra can be kept at a level less than 15{\%} with reasonable constraints.},
	author = {Cuby, Jean Gabriel and Bottini, D. and Picat, Jean P.},
	booktitle = {Proc. SPIE Vol. 3355},
	doi = {10.1117/12.316769},
	editor = {D'Odorico, Sandro},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Cuby, Bottini, Picat/1998/Cuby, Bottini, Picat - 1998 - Handling atmospheric dispersion and differential refraction effects in large-field multiobject spectroscop.pdf:pdf},
	issn = {0277786X},
	keywords = {atmospheric refraction,operational mode,spectroscopy,vlt,wide field},
	mendeley-groups = {Astrometry},
	month = {jul},
	pages = {36--47},
	title = {{Handling atmospheric dispersion and differential refraction effects in large-field multiobject spectroscopic observations}},
	note = {\url{http://proceedings.spiedigitallibrary.org/proceeding.aspx?articleid=946150}},
	url = {http://link.aip.org/link/?PSI/3355/36/1{\&}Agg=doi$\backslash$nhttp://cdsads.u-strasbg.fr/abs/1998SPIE.3355...36C http://proceedings.spiedigitallibrary.org/proceeding.aspx?articleid=946150},
	volume = {3355},
	year = {1998}
}

@article{Chambers2005,
	abstract = {The potential of the Pan-STARRS project and the prototype PS1 telescope$\backslash$nfor new advances in ground based astrometry are discussed. In addition$\backslash$nwe provide a set of improved analytic expressions for atmospheric$\backslash$nrefraction and extinction accurate to 1 mas up to zenith angles of 75$\backslash$ndegrees using an extended set of meteorological data. The application of$\backslash$nthese expressions to wide field mosaic CCD imaging surveys at high air$\backslash$nmass is discussed. The results suggest that the absolute and relative$\backslash$nastrometric performace of such surveys may be significantly better than$\backslash$npreviously assumed, approaching and perhaps exceeding errors <= 1 mas to$\backslash$n21 magnitude.},
	author = {Chambers, K C},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Chambers/2005/Chambers - 2005 - Astrometry with Pan-STARRS and PS1 Pushing the limits of atmospheric refraction, dispersion, and extinction correction.pdf:pdf},
	isbn = {1-58381-205-9},
	note = {\url{http://adsabs.harvard.edu/abs/2005ASPC..338..134C}},
	journal = {Astrometry in the Age of the Next Generation of Large Telescopes},
	mendeley-groups = {Astrometry},
	number = {Vieira 2005},
	pages = {134--144},
	title = {{Astrometry with Pan-STARRS and PS1: Pushing the limits of atmospheric refraction, dispersion, and extinction corrections for wide field imaging.}},
	volume = {338},
	year = {2005}
}

@article{Meyers2015,
	abstract = {Current and future imaging surveys will measure cosmic shear with a statistical precision that demands a deeper understanding of potential systematic biases in galaxy shape measurements than has been achieved to date. We investigate the effects of using the point spread function (PSF) measured with stars to determine the shape of a galaxy that has a different spectral energy distribution (SED) than the star. We demonstrate that a wavelength dependent PSF size, for example as may originate from atmospheric seeing or the diffraction limit of the primary aperture, can introduce significant shape measurement biases. This analysis shows that even small wavelength dependencies in the PSF may introduce biases, and hence that achieving the ultimate precision for weak lensing from current and future imaging surveys will require a detailed understanding of the wavelength dependence of the PSF from all sources, including the CCD sensors.},
	archivePrefix = {arXiv},
	arxivId = {1409.6273v3},
	author = {Meyers, Joshua E. and Burchat, Patricia R.},
	doi = {10.1088/0004-637X/807/2/182},
	eprint = {1409.6273v3},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Meyers, Burchat/2015/Meyers, Burchat - 2015 - IMPACT OF ATMOSPHERIC CHROMATIC EFFECTS ON WEAK LENSING MEASUREMENTS.pdf:pdf},
	issn = {1538-4357},
	journal = {The Astrophysical Journal},
	mendeley-groups = {LSST/optical},
	month = {jul},
	number = {2},
	pages = {182},
	title = {{IMPACT OF ATMOSPHERIC CHROMATIC EFFECTS ON WEAK LENSING MEASUREMENTS}},
	note = {\url{http://arxiv.org/abs/1409.6273v3}},
	url = {http://arxiv.org/abs/1409.6273v3 http://arxiv.org/abs/1402.5101 http://stacks.iop.org/0004-637X/807/i=2/a=182?key=crossref.a90eaad6e0d123c53a25428d23895c0c},
	volume = {807},
	year = {2015}
}

@article{AlejandroPlazas2012,
	abstract = {The wavelength dependence of atmospheric refraction causes elongation of finite-bandwidth images along the elevation vector, which produces spurious signals in weak gravitational lensing shear measurements unless this atmospheric dispersion is calibrated and removed to high precision. Because astrometric solutions and PSF characteristics are typically calibrated from stellar images, differences between the reference stars' spectra and the galaxies' spectra will leave residual errors in both the astrometric positions (dr) and in the second moment (width) of the wavelength-averaged PSF (dv) for galaxies.We estimate the level of dv that will induce spurious weak lensing signals in PSF-corrected galaxy shapes that exceed the statistical errors of the DES and the LSST cosmic-shear experiments. We also estimate the dr signals that will produce unacceptable spurious distortions after stacking of exposures taken at different airmasses and hour angles. We also calculate the errors in the griz bands, and find that dispersion systematics, uncorrected, are up to 6 and 2 times larger in g and r bands,respectively, than the requirements for the DES error budget, but can be safely ignored in i and z bands. For the LSST requirements, the factors are about 30, 10, and 3 in g, r, and i bands,respectively. We find that a simple correction linear in galaxy color is accurate enough to reduce dispersion shear systematics to insignificant levels in the r band for DES and i band for LSST,but still as much as 5 times than the requirements for LSST r-band observations. More complex corrections will likely be able to reduce the systematic cosmic-shear errors below statistical errors for LSST r band. But g-band effects remain large enough that it seems likely that induced systematics will dominate the statistical errors of both surveys, and cosmic-shear measurements should rely on the redder bands.},
	archivePrefix = {arXiv},
	arxivId = {1204.1346},
	author = {{Alejandro Plazas}, Andr{\'{e}}s and Bernstein, Gary},
	doi = {10.1086/668294},
	eprint = {1204.1346},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Alejandro Plazas, Bernstein/2012/Alejandro Plazas, Bernstein - 2012 - Atmospheric Dispersion Effects in Weak Lensing Measurements.pdf:pdf},
	issn = {00046280},
	journal = {Publications of the Astronomical Society of the Pacific},
	mendeley-groups = {LSST/optical},
	month = {oct},
	number = {920},
	pages = {1113--1123},
	title = {{Atmospheric Dispersion Effects in Weak Lensing Measurements}},
	note = {\url{http://arxiv.org/abs/1204.1346}},
	url = {http://arxiv.org/abs/1204.1346$\backslash$nhttp://www.jstor.org/stable/10.1086/668294 http://www.jstor.org/stable/info/10.1086/668294},
	volume = {124},
	year = {2012}
}

@article{AlcockDiffIm1999,
abstract = {This is a preliminary report on the application of Difference Image$\backslash$nAnalysis (DIA) to Galactic bulge images. The aim of this analysis is to$\backslash$nincrease the sensitivity to the detection of gravitational microlensing.$\backslash$nWe discuss how the DIA technique simplifies the process of discovering$\backslash$nmicrolensing events by detecting only objects that have variable flux.$\backslash$nWe illustrate how the DIA technique is not limited to detection of$\backslash$nso-called ``pixel lensing{\{}''{\}} events but can also be used to improve$\backslash$nphotometry for classical microlensing events by removing the effects of$\backslash$nblending. We will present a method whereby DIA can be used to reveal the$\backslash$ntrue unblended colors, positions, and light curves of microlensing$\backslash$nevents. We discuss the need for a technique to obtain the accurate$\backslash$nmicrolensing timescales from blended sources and present a possible$\backslash$nsolution to this problem using the existing Hubble Space Telescope$\backslash$ncolor-magnitude diagrams of the Galactic bulge and LMC. The use of such$\backslash$na solution with both classical and pixel microlensing searches is$\backslash$ndiscussed. We show that one of the major causes of systematic noise in$\backslash$nDIA is differential refraction. A technique for removing this systematic$\backslash$nby effectively registering images to a common air mass is presented.$\backslash$nImprovements to commonly used image differencing techniques are$\backslash$ndiscussed.},
archivePrefix = {arXiv},
arxivId = {astro-ph/9903215},
note = {\url{http://iopscience.iop.org/article/10.1086/307567/pdf}},
author = {Alcock, C and Allsman, R A and Alves, D and Axelrod, T S and Becker, A C and Bennett, D P and Cook, K H and Drake, A J and Freeman, K C and Griest, K and Lehner, M J and Marshall, S L and Minniti, D and Peterson, B A and Pratt, M R and Quinn, P J and Stubbs, C W and Sutherland, W and Tomaney, A and Vandehei, T and Welch, D L and Collaboration, MACHO},
doi = {10.1086/307567},
eprint = {9903215},
file = {:Users/dreiss/Documents/Mendeley Desktop/Alcock et al. - 1999 - Difference image analysis of galactic microlensing. I. Data analysis.pdf:pdf},
issn = {0004-637X},
journal = {Astrophysical Journal},
keywords = {atmospheric effects; Galaxy : stellar content; gra},
number = {2, 1},
pages = {602--612},
primaryClass = {astro-ph},
title = {{Difference image analysis of galactic microlensing. I. Data analysis}},
volume = {521},
year = {1999}
}

@article{Hohenkerk1985,
	abstract = {The bending of a light ray as it passes through the atmosphere is cal- culated by numerical evaluation of the refraction integral, expressed in a form that avoids numerical difficulties at a zenith angle of 90 ◦ . A polytropic model atmosphere is used, and the parameters of the model are varied in order to determine the effect on the computed refraction value. Good agreement is obtained with other evaluations of refraction for zenith angles up to 75 ◦ . Beyond that it becomes sen- sitive to the values of the parameters used, particularly the pressure, temperature, temperature lapse rate, and wavelength of the light ray. Good agreement is obtained with other evaluations provided the same parameter values are used.},
	author = {Hohenkerk, C.Y. and Sinclair, A.T.},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Hohenkerk, Sinclair/1985/Hohenkerk, Sinclair - 1985 - NAO Technical Note The computation of angular atmospheric refraction at large zenith angles.pdf:pdf},
	number = {63},
	pages = {12},
	title = {{NAO Technical Note: The computation of angular atmospheric refraction at large zenith angles}},
	year = {1985},
	note = {\url{https://github.com/isullivan/LSST-DCR/blob/master/references/Hohenkerk%2C%20Sinclair%20-%201985%20-%20NAO%20Technical%20Note%20The%20computation%20of%20angular%20atmospheric%20refraction%20at%20large%20zenith%20angles.pdf}}
}

@article{Owens:67, 
	author = {James C. Owens}, 
	journal = {Appl. Opt.}, 
	keywords = {},
	number = {1}, 
	pages = {51--59}, 
	publisher = {OSA},
	title = {Optical Refractive Index of Air: Dependence on Pressure, Temperature and Composition}, 
	volume = {6}, 
	month = {Jan},
	year = {1967},
	note = {\url{http://ao.osa.org/abstract.cfm?URI=ao-6-1-51}},
	url = {http://ao.osa.org/abstract.cfm?URI=ao-6-1-51},
	doi = {10.1364/AO.6.000051},
	abstract = {The theoretical background and present status of formulas for the refractive index of air are reviewed. In supplement to Edl\'{e}n's recently revised formula for relative refractivity, the density dependence of refractive index is reanalyzed. New formulas are presented for both phase and group refractive index which are more useful over a wide range of pressure, temperature, and composition than any presently available. The application of the new formulas to optical distance measuring is briefly discussed.},
}

@article{Auer2000,
	author = {Auer, Lawrence H. and Standish, E. Myles},
	doi = {10.1086/301325},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Uer, Tandish/2000/Uer, Tandish - 2000 - Astronomical refraction computational method for all zenith angles l awrence h. a uer.pdf:pdf},
	issn = {00046256},
	journal = {The Astronomical Journal},
	keywords = {methods,numerical},
	mendeley-groups = {Astrometry},
	month = {may},
	number = {5},
	pages = {2472--2474},
	title = {{Astronomical Refraction: Computational Method for All Zenith Angles}},
	note = {\url{http://stacks.iop.org/1538-3881/119/i=5/a=2472}},
	url = {http://stacks.iop.org/1538-3881/119/i=5/a=2472},
	volume = {119},
	year = {2000}
}

@article{Mangum2015,
	author = {Mangum, Jeffrey G. and Wallace, Patrick},
	doi = {10.1086/679582},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Radio, Observatory, Oxford/2014/Radio, Observatory, Oxford - 2014 - Atmospheric Refractive Electromagnetic Wave Bending and Propagation Delay.pdf:pdf},
	issn = {00046280},
	journal = {Publications of the Astronomical Society of the Pacific},
	mendeley-groups = {Astrometry},
	month = {jan},
	number = {947},
	pages = {74--91},
	title = {{Atmospheric Refractive Electromagnetic Wave Bending and Propagation Delay}},
	note = {\url{http://www.jstor.org/stable/info/10.1086/679582}},
	url = {http://dx.doi.org/10.1086/679582 http://www.jstor.org/stable/info/10.1086/679582},
	volume = {127},
	year = {2015}
}

@article{Tomaney1996,
	abstract = {We present a new technique for monitoring microlensing activity even in highly crowded fields, and use this technique to place limits on low-mass MACHOs in the haloes of M31 and the Galaxy. Unlike present Galactic microlensing surveys, we employ a technique in which a large fraction of the stellar sample is compressed into a single CCD field, rather than spread out in a way requiring many different telescope pointings. We implement the suggestion by Crotts (1992) that crowded fields can be monitored by searching for changes in flux of variable objects by subtracting images of the same field, taken in time sequence, positionally registered, photometrically normalized, then subtracted from one another (or a sequence average). The present work tackles the most difficult part of this task, the adjustment of the point spread function among images in the sequence so that seeing variations play an insignificant role in determining the residual after subtraction. The interesting signal following this process consists of positive and negative point sources due to variable sources. The measurement of changes in flux determined in this way we dub "difference image photometry" (also called "pixel lensing" [Gould 1996]). - The matching of the image point spread function (PSF) is accomplished by a division of PSFs in Fourier space to produce a convolution kernel, in a manner explored for other reasons by Phillips {\&} Davis (1995). In practice, we find the application of this method is difficult in a typical telescope and wide field imaging camera due to a subtle interplay between the spatial variation of the PSF associated with the optical design and the inevitable time variability of the telescope focus. Such effects lead to complexities...(abstract continues)},
	archivePrefix = {arXiv},
	arxivId = {astro-ph/9610066},
	author = {Tomaney, Austin B. and Crotts, Arlin P. S.},
	doi = {10.1086/118228},
	eprint = {9610066},
	file = {:Users/sullivan/Documents/Mendeley Desktop/Tomaney et al/Unknown/Tomaney et al. - Unknown - EXPANDING THE REALM OF MICROLENSING SURVEYS.pdf:pdf},
	isbn = {9780874216561},
	issn = {00046256},
	journal = {Astronomical Journal},
	mendeley-groups = {Astrometry},
	number = {1995},
	pages = {2827},
	pmid = {15003161},
	primaryClass = {astro-ph},
	title = {{Expanding the Realm of Microlensing Surveys with Difference Image Photometry}},
	note = {\url{http://arxiv.org/abs/astro-ph/9610066}},
	url = {http://arxiv.org/abs/astro-ph/9610066},
	volume = {112},
	year = {1996}
}