AO Photometry for NGAO

Transcription

1 AO Photometry for NGAO Dr. Matthew Britton, COO Dr. Richard Dekany, COO Dr. Ralf Flicker, WMKO Dr. Claire Max, UCSC Dr. Knut Olsen, NOAO January 19, Introduction Esslinger [1] In the remainder of this section we will briefly review astronomical applications that require photometric precision or high dynamic range. 1.1 Planetary Astronomy Io - [2, 3] Photometry of volcanoes. Uranus[4, 5] Photometry of transient features and rings. Titan [6] Photometry of clouds. Asteroid imaging [7, 8, 9]. Shape, size, multiplicity, composition. 1.2 Stellar Variability Imaging of crowded stellar fields. Variable stars in the galactic center [10] Flares of Sag A* [11]. Stellar populations in nearby galaxies [12, 13] Search and monitoring of variable stars in crowded fields, traditionally done with seeing limited instruments [14]. Stellar eclipses. [15]. Microlensing. [16] State of the art in AO photometry: Roberts [17] Britton [18] 1

2 Christou [19] 1.3 Extragalactic science CATS citation: [20] Max: NGC6240 [21] Cresci: SWAN [22, 23] Others? Note in particular photometric issues with AO corrected spatially resolved spectroscopy using integral field units. 2 Case Study: Stellar Populations in Nearby Galaxies Olsen s work. [12] In this particular application, detector effects are considered unimportant, as shot noise from fainter objects dominates the photometric error budget. 3 Effects on Photometry This is the table of effects that Rich wrote down: Atmospheric turbulence Other atmospheric effects Optical system Detector PSF evolution Scintillation Transparency waves Color correction Filter bandpass uncertainty Field dependent aberrations Read noise Flat fielding PSF sampling Nonlinear detector response Photon noise Table 1: xxx 2

3 3.1 Atmospheric Turbulence Effects PSF evolution - spatial, temporal functionality. NGS SCAO systems provide a PSF that varies with turbulence profile, field location, wavelength, zenith angle, and aperture diameter. The PSF evolves in time in response to evolution in the statistical properties of atmospheric turbulence. LGS SCAO systems share these dependencies, but also depend on the height of the beacon and the location of the tilt guide star within the field of view. MCAO systems aim to eliminate the field dependence of the PSF. The other dependencies remain. Scintillation - include excerpts from Palm 3000 scintillation writeup. 3.2 Other Atmospheric Effects Transparency waves - need citations. Color correction - need citations. 3.3 Optical System Effects Filter bandpass uncertainty seems to be of uncertain relevance for many applications. Field dependent aberrations may be a problem if we rotate the Cass ring or dither on a chip. 3.4 Detector Effects Shack Hartmann centroiding [24] Significant efforts mounted for HST images - must review this literature. intrapixel sensitivity variations - Lauer. Mighell s research [25] Effect of read noise on transiting planets [26] In particular, 4 PSF Estimation 4.1 PSF Estimation for the guide star PSF reconstruction from telemetry data. [27, 28, 29] Marois - angular differential imaging [30] 4.2 PSF Estimation over the field Steinbring [31, 32] Cresci and references therein. 3

4 Flicker [33] Fusco [34] Britton [35, 18] Sheehy [36] 5 Deconvolution Algorithms 5.1 Algorithms Employed in AO Mistral[37, 38, 39] is a myopic deconvolution code. The term myopic represents the notion that the PSF is unknown, but certain constraints such as positivity and band limited may be enforced in a solution. Applied to Keck observations of Io [2, 3]. Aida (E. F. Y. Hom et al., AIDA: An Adaptive Image Deconvolution Algorithm with application to multi-frame and 3D data, JOSA A, in press). Starfinder[40] is a code that performs deconvolution within the isoplanatic patch. Iterative blind deconvolution [41, 42] App Parameterized fit using a Lorentzian [43] or a Lorentzian plus an Airy function [44] 5.2 Comparisons Between Algorithms Christou [45] has compared IDAC, Starfinder, and Drummond s technique. [2] compares IDAC, Starfinder, and MISTRAL. de Pater [6] compares AIDA and MISTRAL. Deconvolution outside the isoplanatic patch. Britton[35] 6 Recommendations A few ways we might address the topic of photometry at Keck Observatory, in the near term and for NGAO. References [1] O. Esslinger and M. G. Edmunds. Photometry with adaptive optics: A first guide to expected performance. A&A SS, 129: , May [2] I. de Pater, F. Marchis, B. A. Macintosh, H. G. Roe, D. Le Mignant, J. R. Graham, and A. G. Davies. Keck AO observations of Io in and out of eclipse. Icarus, 169: , May

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