... These Frontier Fields will combine the power of HST with the natural gravitational telescopes of high-magnification clusters of galaxies. ... We are soliciting gravitational lensing maps for the last four Hubble Frontier Fields clusters (MACSJ0717.5+3745, MACSJ1149.5+2223, AbellS1063, and Abell 370) based upon the exceptionally deep HST FF imaging and other new ancillary data. ... For the full set of proposal instructions and requirements, see the FY16 Frontier Fields Lensing Map Call for Proposals....

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• Flat Fields
• Polarizer Quad Filter
• PSF Variations with Field Position

... The improvement will be more pronounced in our crowded Wide Field Camera (WFC) images, and may be increased further through use of a more sophisticated method of combining the individual dithered images. Our analysis allows us to check for point spread function shape variations in the HST Planetary Camera (PC) field. ... In crowded field images, we are deriving information about the faint end of the luminosity function (LF) from the texture of the image background. ...

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• Filtering KPNO LaTeX Observing Proposals with Perl
• On the Need for Input Data Control in Pipeline Reductions
• ADASS 2003 Conference Proceedings

... Fields Observed . ... Data Archive . ... Complete Optical and X-ray data for all ChaMPlane fields are available through the DS9 VO interface . ... functionality of DS9 is available to manipulate the results in addition to those provided by the "Champlane tools" You can select images, compare . ... our region of interest has been selected by drawing a red square region on the image. at bottom left the high res optical image of that selected region, and on the right is the X-ray image. ...

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• ChaMPlane apj_appendix
• ChaMPlane
• Infrared Data

IBIS Data Analysis . ... IBIS . ... Flat Fielding - Introduction . The images obtained by IBIS will have intensity variations across the field of view that are not due to the solar image, but rather caused by instrumental effects that alter the observed intensity in each point of the field of view. ... IBIS Flat Fielding Techniques . ... Therefore, it is desirable to obtain the flat field measurements center on a point along the equator near the heliographic center of the solar disk. ...

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• Carlo Baffa
• Observing capabilities
• LonGSp: Optical Design

. An example of ULF electromagnetic fields detection by the IESP-2M instrument. The figure presented is the dynamic spectrogram. E and B components are measured in satellite coordinates. Observations were made in the auroral region. Electromagnetic turbulence, which was observed mostly in electric components, is typical for this phenomenon. Fig.1 .

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• Examples of the raw magnetic field information, obtained with the MIF-M
• HYPERBOLOID Results Page
• SKA-3 Results Page

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Many of the fields are spatially . ... These include a pulsating white dwarf which appears to have a hot companion, a number of stars with A-type spectra that vary on a period in the range 20 35 min. Our primary goal is the discovery of new AM CVn systems: we find 66 sources which appear to show periodic modulation on a time-scales less than 40 min and a colour consistent with the known AM CVn systems. ...

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• C.S. Jeffery, Research Astronomer

... The STECF IRAF layered package impol provides five tasks specifically aimed at reduction of HST imaging polarimetry data for ACS, FOC, NICMOS and WFPC2. ... Reduction of HST polarimetry data and simulation of raw polarimetry images, together with polarization vector plotting, are covered. ... hstpolsim -- Produce simulated polarization input data frames for HST instruments from images of the total signal, the linear polarization and the position angle of the polarization vectors. ...

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• FORS1 Photometric System Characterization
• ESO - Thesis Topic: Magnetic fields in massive stars
• Observed Fields in NGC 300 | ESO

... XMM-Newton SOC Home Page Conferences & Meetings . ... Data Analysis SAS News What is SAS? How to use SAS SAS Workshops SAS Version Changes Download and Install SAS Science Simulator (SciSim) . ... EPIC cameras optical loading . ... The PI is invited to cross-check the expected X-ray flux from the target source (and from any other potentially bright source in the target field of view), or to provide the SOC with her/his own estimate, if not originally specified in the proposal. ...

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• Generation from In-Orbit Data
• XMM-Newton OM Response Files Page
• XMM-Newton Trainee Project 2004

... Several HST instruments both current and decommisioned have provided imaging linear polarimetry capabilities. ... The STECF IRAF layered package impol provides five tasks specifically aimed at reduction of HST imaging polarimetry data. ... Reduction of HST polarimetry data and simulation of raw polarimetry images, together with polarization vector plotting, are covered. ... For reduction of data from imaging linear polarization instruments other than from HST, the instrument name is `SPECIAL'. ...

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• The Stellar Population in the NICMOS Parallel Fields
• NICMOS Science
• NICMOS Observes the Galactic Center

... Tpram - time of the PRAM instrument (aquisition computer) . ... Bx - DC magnetic field with a fixed amplitude calibration; X component . ... The color lines present FFT from the AC magnetic field (Waveform); Bwx, Bwy, Bwz - from the bottom. ...

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• Some results from Intmins
• FM-3I Instrument
• ASPI experiment

... These data were originally part of a PhD-thesis at Leiden Observatory by M.H. Wieringa (1991). 1 name Name of source (char8, example : '76W0771*') 2 freq MHz Frequency of source detection in MHz (int, example : 327 or 608 ) 3 ra_1950 radians B1950 Right Ascension (in radians) ( real , example : 2.328327) 4 ra_1950_deg degrees B1950 Right Ascension (in degrees) ( real , example : 133.403290) 5 ra_err seconds Error in RA ( ... 70W : Umi, 327 MHz only, one field. ... Columns 21 Rows 5850...

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• HyperLEDA documentation: compilation of cz measurements (a110)
• Descriptor NFILTCAR
• Combining Sky Frames

... The world standard in telescope oculars, Meade Series 4000 eyepieces yield the widest possible fields of view, consistent with pinpoint edge-of-field sharpness and long eye relief and yet with extremely low astigmatism, spherical aberration, and off-axis color. ... Your Series 4000 eyepieces are superb, with the Super Wide Angle 32mm and Ultra Wide Angle 14mm (two incredible eyepieces) being particular favorites of mine. ... Meade Series 4000 8mm - 24mm Zoom Eyepices (1.25") . ... about meade | ...

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• Telescopes - Products
• Products
• Meade Instruments Corporation - Pictor Manual Part 16

... Exposure Time Calculator (ETC) . Survey processing . ... VISTA is a 4-m class wide field survey telescope for the southern hemisphere, equipped with a near infrared camera (1.65 degree diameter field of view at VISTA's nominal pixel size) containing 67 million pixels of mean size 0.34 arcsec and available broad band filters at Z,Y,J,H,K s and a narrow band filter at 1.18 micron. A wide field visible camera, if constructed, could also be used on VISTA. ... Tile . ... ESO VISTA Public Surveys . ...

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• VISTA ETC - Exposure Time Calculator

Program: ROTCUR Purpose: ROTCUR derives the kinematical parameters from the observed velocity field by fitting tilted-rings to the velocity field. ... Maximum number of rings is 512. ... VSYS= Give initial estimate(s) of systemic velocity(ies) in km/s. If the number of systemic velocities is less than the number of rings, the last supplied systemic velocity will be used for the rest of the rings. ... SIDE= Which half of the velocity field should be used in the fitting [RECEDING and APPROACHING half]. ...

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• The high quality H interference filter
• Observing Plan
• Normal galaxies in the XMM-Newton fields: X-rays as a star formation indicator

... Bit Fields . Bit Fields: Practical Example . ... NOTE: The combination of pointers and bit-level operators makes C useful for many low level applications and can almost replace assembly code. ... To illustrate many points of bitwise operators let us write a function, Bitcount , that counts bits set to 1 in an 8 bit number ( unsigned char ) passed as an argument to the function. int bitcount(unsigned char x) { int count; for (count=0; x != 0; x>>=1); if ( x & 01) count++; return count; } . ...

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• SCORPIO: IFP Gallery
• Laboratory of spectroscopy and photometry of extragalactic objects : Vortex
• SCORPIO-2 project: description

I-GALFA Survey Fields . ... Most I-GALFA fields are observed by ``nodding'' the telescope north and south along the meridian to trace out a zig-zag pattern on the sky as the Earth rotates. ... The I-GALFA fields fill the AO DEC range and overlap with each other by 20', with one field 3 degrees wide at the zenith and four others 9.3 degrees wide covering the rest of the survey. ... The LST range of each field is shown in blue. ... Field . ... The I-GALFA fields are shown in Galactic coordinates below. ...

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• Making Maps: Example + Animation
• a2704
• HIPASS Results and Lessons

... As a result of BTA observations of 23 chemically peculiar stars with strong magnetic fields, it was found that in 22 of them the longitudinal magnetic field, measured from the hydrogen line cores are considerably lower (by about 1/3) than the value measured from metal lines in the same spectra. ... New approaches need to be developed in order to interpret the data. ... The Zeeman spectrum of a star with a strong magnetic field, 53 Cam. ...

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• Galaxy sector, archive 2012
• Galaxy sector, archive 2014
• Galaxy scientific results 2003

... Here are some tips on how to get the best guiding out of our current system. ... NA2 Guider Tips . ... Optical double stars, late-type galaxies, and bipolar PNs may pose a problem for guiding, as will objects where you desire to observe a position away from the bright center (e.g., SNs near bright galaxies). ... Field Star is good if your object is too faint or asymmetrical for Boresight guiding, or if you need the slit to be off-center. ... Use Field Star guiding almost always. ...

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• TUI:TUI Menu:Log Windows
• APO Job Announcements
• TUI:Tidbits:Entering Sexagesimal Positions

NMW survey overview . Access image archive . ... The New Milky Way survey aims to detect bright (V<13.5) optical transients near the Galactic plane using an automated wide-field (8x6 deg.) system capable of surveying the whole Milky Way area visible from the observing site in one night. ... All images obtained during the transient search survey are available online (please use the image archive access form ). ... Images per field: . ... Images per night: . ... Milky Way imaging time: . ...

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RTT150 . ... This search system is designed for generating the necessary information on series of pointings (observations of each source consist of sets of exposures with different filters and sometimes with different exposure times) for observed sources. Search results appear at the separate page as a table with the following data: . DATE - real (not evening!) observations date (in YYYY-MM-DD format); . ... Bin - minimal CCD binning mode (may vary during the observations); . ...

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• High Energy Astrophysics Department at IKI RAN