T he Siding Spring Survey (SSS) is a Near-Earth Object search program that utilises the 0.5-m Uppsala Schmidt Telescope at Siding Spring Observatory, N.S.W., Australia. ... The mission of the Siding Spring Survey is to contribute to the inventory of near-earth objects (NEOs), or more specifically, the potentially hazardous asteroids (PHAs) and comets (PHOs) that may pose a threat of impact and thus harm to civilization. ... Based on the CSS Mission page . ... Siding Spring Survey Main Page . ...

... PUL VLBI Analysis Center . ... Pulkovo EOP and Reference Systems Analysis Center (PERSAC) is located at the Pulkovo Observatory . ... Processing of VLBI , GPS, and optical observations aimed at analysis of the Earth rotation, station displacement, and celestial reference system. ... Celestial Pole Offset (CPO) and Free Core Nutation (FCN) . Four daily updated CPO and FCN series (models) are provided. ... File fcn1.dat contains the ZM1 FCN model with variable amplitude and phase. ...

... region (region-7.9) [xmmsas_20070708_1801-7.1.0] . ... Local-background regions are in all cases annuli. ... Background regions of this shape should be chosen when there is no extended emission in the FOV, because OA-concentric regions are in general larger than source-concentric ones (thus offer better statisitics), yet sample everywhere approximately the same background level, because the value of the vignetting function is approximately the same at a given radius from the OA. fovbkgannulus =`no'....

Please enter the lightcurve file name and period search parameters: . Lightcurve file: . ... Apply the Heliocentric correction and convert all dates to Terrestrial Time (TT)? ... Also, the Heliocentric correction cannot be applied to such lightcurves. ... This period search service is also available at the mirror sites: Mirror 1 , Mirror 2 , Mirror 3 , Mirror 4 . You may download the latest source code distribution and install the period search service at your own web server. ...

Next: Photometry Up: Regions and Source Parameters Previous: *imcnts* - Find counts . This task (developed for use with optical images, but also useful with x-ray data) will quickly compute location, size, ellipticity, and position angle of sources. ... User can generate contour plots of any portion of the image and count rates in slices through the image. The program is advertised as ``quick [optical] photometry''. input file: rp110590_im1.imh . output file: logfile . ... Photometry . ...

... Tonight's Sky . ... The Magazine . ... Observing . ... Magazine . ... Gravitational wave search provides insights into galaxy evolution and mergers . ... The double star 54 Leonis, spiral galaxy NGC 3198, and emission nebula NGC 3199 . ... Open cluster NGC 2818, spiral galaxy NGC 2964, and spiral galaxy NGC 2976 . ... Astronomy for Kids . ... Cosmic Adventures . ... cosmic microwave background . ... Receive news, sky-event information, observing tips, and more from Astronomy's weekly email...

... HST . Using multiple FP-POS positions at new COS Lifetime Location. ... HST Overview . ... To minimize such local degradation at the new COS lifetime position and maximize COS FUV data quality, proposers are strongly encouraged to use all four FP-POS positions (FP-POS=ALL) at any given CENWAVE when planning their observations in Cycle 20 as well. ... STScI will keep monitoring the ongoing and planned usage of the different COS CENWAVE and FP-POS positions at the new COS lifetime position. ...

Next: Analysis Tools for Nebular Emission Lines . ... Extracting spectra from a large number of NICMOS grism images requires a convenient interactive tool which allows a user to manipulate direct/grism image pairs. ... The direct image is used to locate objects of interest, to find the position of the appropriate spectra in the grism image, to determine the optimal extraction technique to use, and to calibrate the wavelength range of the extracted spectra. ... Figure 1: The NICMOSlook User Interface . ...

Next: The STScI NICMOS Calibration Up: No Title Previous: CONICA: The high resolution . The STScI NICMOS Calibration Pipeline . Introduction . ... Dark Current Subtraction . ... Input Data . ... Scalar Background Subtraction . 2-D Background Subtraction . ... Status and Goals of the NICMOS Calibration Plan . ... Photometry . ... Photometric Performance of NICMOS . ... NICMOS Photometry. ... ST-ECF Grism Spectrum Software for NICMOS Grism Data . ... Analysis . ... STScI NICMOS Software . ...

Next: Related Table Commands Up: Multivariate Analysis Methods Previous: Discriminant Analysis . Correspondence Analysis may be described as a PCA in a different metric (the metric replaces the usual Euclidean metric). ... While PCA is particularly suitable for quantitative data, CA is recommendable for the following types of input data, which will subsequently be looked at more closely: frequencies, contingency tables, probabilities, categorical data, and mixed qualitative/categorical data. ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

... We can help students grasp the significance of Hubble's extremely keen eye, and learn a bit about angles and math in the process, with the following in-class activity. ... Looking through binoculars or telescopes allows us to magnify a small section of the sky. To measure sizes or distances in that small section, astronomers divide a degree into 60 smaller pieces called arcminutes, and further subdivide minutes into 60 smaller sections called arcseconds. ... 30 feet = . ... 36 seconds . ...

... The Earth orientation parameters UT1 and polar motion (x pol ; y pol ) are relat­ ed with the values of UT0 and VOL obtained from the LLR analysis for a station with geocentric longitude and latitude (–; OE) by the following expression: 7 UT0 \Gamma UTC = UT1 \Gamma UTC + (x pol sin – + y pol cos –) tan OE 15 V OL = x pol cos – \Gamma y pol sin – At least four normal points for each station--reflector pair at one day were accepted for the diurnal UT0 estimations. ...

... The units of N(S) are counts/Jy/steradian. The user also specifies N0, which is a cosmological normalization, usually a power law of S. This function is input via a power law and/or polynomial. ... Key: out Confusion noise (sigma) image (1/2 size of beam image) in Jy Key: flux 3 numbers (Jy). flux(1) and flux(2) define the range of flux densities for which the confusion noise is calculated. flux(3) is the break point below which the power law is used, and above which the polynomial is used. ...

... The dates are shown along the X axis, . The time on the orbit counted from ascending node of the each turn is shown along the Y axis. ... The geomagnetic local time is shown along the Y axis. ...

With the Phase I CGPS now complete at 21cm, we are in a position to examine the population of cold H I clouds over the entire range of the survey. Current methods of H I self-absorption (HISA) identification and analysis allow us to explore the properties and distribution of the portion of cold H I which appears as HISA shadows in the 21cm line data. Such studies are necessarily biased toward clouds with bright background emission. ...

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Time-resolved spectral analysis of the pulsating helium star V652 Her C.S. Je ery 1 , V.M.Woolf 1 and D.L.Pollacco 2 1. ... The most crucial measurement, how- ever, is that of radius, which may be measured using Baade's method. ... Analysis SFIT_SYNTH STERNE High resolution spectrograms UV + visual spectrophotometry Model flux grid Model structure grid High resolution model grid v_t, composition v_t Atomic data Teff, log g, v sin composition Teff, Eb-v q SPECTRUM LTE_LINES FFIT SFIT Figure 1. ...

Lessons learned from the Thirty Meter Telescope site testing Tony Travouillon Sebastian Els, Angel Otarola, Reed Riddle, Matthias Schoeck, Warren Skidmore TMT.XXX.PRE.05.0XX.DRF01 1 Introduction TMT and its Site testing. Important choice before going on site. ... Considerations during analysis of the data. TMT.XXX.PRE.05.0XX.DRF01 2 Some Background about the TMT Site Testing TMT is a 30m, segmented, RitcheyChretien telescope design. ... ASCA Cloud Cover Analysis So how do we do it in practice? ...

... Take a particularly simple signal: a cosine wave. ... Now, we are going to stretch and shrink the wavelet along the time axis (we assume the data is in the time domain), and at each time compare the shape of the signal to that of the wavelet. ... Figure 3: The wavelet (dotted line) is translated rela tive to the signal (solid line). ... Figure 4: The dashed line plots the `match' between the wavelets (dotted line) and the signal (solid line) as a function of time. ...