STIS Instrument Handbook for Cycle 24 . ... Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 24 > Chapter 12: Special Uses of STIS > 12.3 Time-Resolved Observations . ... There are two ways to obtain time-resolved spectroscopic and imaging observations with STIS: . Use the MAMA TIME-TAG operating mode (described in Section 11.1.3 ) in the UV. ... If you wish to observe variability on second-or-less time-scales, observe in the UV using TIME-TAG mode. ... Time ( ? ... TIME-TAG 3 . ...

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• HST Spectral Maps of Accretion Disks in Cataclysmic Binaries
• Time resolved observations with STIS/MAMA (TIME-TAG mode)
• COS Spectroscopic Observing Strategies

... Up: Data Analysis and Processing Techniques . ... Also, a method for quality control of CCD observations is suggested. ... Everyone who observes a celestial object using a CCD detects moving celestial objects as a ``by product''. ... We hope that our investigations may be useful for near-Earth space control and also for searches of the moving celestial objects through analysis of old and new CCD frames obtained at any amateur or professional astronomical observatory. ...

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• NICMOS Software: An Observation Case Study
• Asteroseismology-Observing for a SONG
• The Co-Addition Technique Applied to Images of Galaxy Cores

We report here on those proposed UIT targets that, in fact, were successfully acquired. ... Note on Filters: . A1 centered at 2500 angstroms with a width of 1200 angstroms . ... Sextans A is a low mass dwarf companion to the Milky Way Galaxy. It is sufficiently close that it is easily resolved into its individual stars. ... An exposure of 1100 seconds through the A1 and B1 filters was obtained. NGC 2903 Is a relatively nearby mostly face-on galaxy with active star formation. ...

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... Data Analysis SAS News What is SAS? ... The main scientific objective of my project was a pulse phase resolved spectral analysis of observations of the Crab pulsar with XMM-Newton. Moreover, a new method would be developed into how to combine data from different camera modes in order to achieve a optimal phase and space resolved spectroscopy of the Crab pulsar and nebula. ... Fig. 2: pulse profile of the Crab pulsar (over two phases) in blue (Burst mode data); . ...

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• XMM-Newton OM Response Files Page
• Observing mode support
• LARGESCALESENS

... Maximum data output rate = 6.4 Mbyte/s. Output data files in PSRFITS format. ... spd: sel pp11 - pulsar phase vs amplitude . ... John Sarkissian starts the web-page checklist and writes report providing information on the last observing session and data processing. ... He produces a text file containing the processing commands required: /psr1/jms/processed.txt John Sarkissian copies the raw data files (DFB/WBC) from Lagavulin to Epping. > cd /data/LAGAVULIN_4/pulsar > cd DFB > rsync -av . ... Group ...

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• New HI Observations of the Prototype Polar Ring Galaxy NGC 4650A
• Programme - Abstract
• OH_maser

... We present 7mm observations of the dusty disk surrounding the 10 Myr old 1.5 Msun pre-main-sequence star CQ Tauri obtained at the Very Large Array with 0.8 arcsecond resolution and 0.1 mJy rms sensitivity. ... We find that the disk radius is constrained to the range 100 to 300 AU, depending on the steepness of the disk surface density distribution. The power law index of the dust opacity coefficient, beta, is constrained to be 0.5 to 0.7. ...

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• IBIS - Flat Fielding
• Cannibal Stars Cause Giant Explosions in Fornax Cluster Galaxy (ESO Press
• Procedures for Observations

... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

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• CIMA Auto-Observing
• Arecibo Observatory observations of 2005 YU55

Next: NICMOS/HST H-band (F160W) Images Up: NICMOS Science Previous: HST NICMOS Observations of . ... Observations of P . ... The NICMOS team has devised a comprehensive program of observations of the Galactic Center. ... Data in hand give a first look at variability and a detailed look at the search for the tip of the main sequence will be discussed where NICMOS has demonstrated adequate sensitivity and photometric precision to identify likely O8-B1 stars at the Galactic Center. ...

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• The Old Stellar Population of NGC 1569 from NICMOS data

... Public . ... Science Users Information > Science Publications > Science Announcements . ... Public Surveys . ... Published: 24 Feb 2014 . ... The Public ESO Spectroscopic Survey of Transient Objects ( PESSTO ) is one of the two on-going ESO public spectroscopic surveys . ... The first public data release ( DR1 ) of the VIDEO programme via the ESO Science Archive Facility, contained 97 individual (i.e. single-OB) tile images in the VIDEO-XMM3 field and their associated single-band source lists. ...

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• ESO - RASPUTIN: Resolved And unresolved Stellar PopUlaTIoNs
• FORS1 Photometric System Characterization
• ESO - UVES

Peremennye Zvezdy ( Variable Stars ) 32 , No. ... We report on a new episode of decretion disk formation in the IGR J06074+2205 system. ... From a study of three HeI lines, the rotational velocity of the star was determined as km/s. After five years of spectroscopic monitoring of IGR J06074+2205 (Reig et al. 2010), a reversion from emission to absorption of the H line and hence disappearance of the equatorial disk was reported. ... Reig P., 2011, Astrophys.& ...

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• Астронет > Supernova 1987a Fireball Resolved
• Supernova 1987a Fireball Resolved

... Contacts . 2012: . ... We refined the fundamental parameters of the components, the orbital periods, and the conditions of photospheric heating of the secondary component by the ultraviolet radiation of the hot component. ... The observations of the star clusters associated with ultra-luminous x-ray sources (ULXs) in four galaxies on the 6-meter and VLT telescopes have shown that all the ULXs are located within 200pc of very young star clusters (younger than 5 million years). ... Archive . ...

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• Solar eclipse 2015
• GRB090726
• RCJ0311+0507

... Frequency of wobble same as frequency of forcing mechanism (t) + i 2 (t) · Helmholtz Centre Potsdam ­ GFZ · Consistent estimates of AAM , OAM , HAM computed at GFZ · AAM computed from European Centre for Medium-Range Weather Forecasts · OAM computed from Ocean Model for Circulation and Tides (OMCT) · HAM computed from Land-Surface Discharge Model (LSDM) · Ocean and hydrology Sensitivity to Excitation Model GFZ ECMWF AAM OMCT OAM LSDM HAM 1962­2010 1971­2010 1981­2010 1991­2010 2001­2010! ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/perepelkin.pdf
• Pulkovo NEO Page: Ephemeris Support
• Pulkovo NEO Page: Estimation of Observational Accuracy

... January 24, 1997 . Supernova 1987a Fireball Resolved . Credit: C. S. J. Pun ( GSFC ) & R. Kirshner ( CfA ), WFPC2, HST , NASA . ... Supernova 1987a remains the closest supernova since the invention of the telescope . The explosion catapulted a tremendous amount of gas , light , and neutrinos into interstellar space. ... More recent HST observations shown in the inset, however, have uncovered something actually predicted : the expanding fireball from the exploding star. ... About APOD > . ...

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• SN 1989B Light Curve Analysis.
• Contributions by amateurs: SN1996X.
• Light Curve Templete/Observing Form For Visual SNe Observers.

... The x-ray spectral analysis consists of a comparison between the observed pulse height spectrum and a pulse height spectrum calculated using a given spectral model. ... To obtain the spectral parameters for an x-ray source, several steps need to be followed. For each source: . ... obtain the best fit parameters for a spectral model - repeated for each model of interest . obtain a 1-D or 2-D grid of values around the best fit values - this can be done for as many models as desired . ...

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• *qpspec* - Time Resolved Spectral Fitting
• Spectroscopic Data
• Period Criteria

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

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• The Radiopulsar PSRB1259-63 - a Probe in the Stellar Wind Plasma

... Assured of a reliable method of solving the normal equations, we now consider the equations of condition. The observed magnitude m of a star at M air masses with true instrumental magnitude is modelled as ([ 10 ], [ 28 ]) . ... The effective extinction coefficient depends on the effective spectral gradient [ 29 ] of the star, for which we use some color index, affected by half the atmospheric reddening ([ 26 ], [ 10 ]): . ... Thus, for the B band of UBV, we use the (U-V) color. ...

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• Missing bands
• Radio patrol survey by Gregory and Taylor
• VLA 360 compact sources

Ground-Based Mid Infra-Red Observations of Nearby Starburst and AGN Galaxies Bo jan Nikolic , Paul Alexander, Garret Cotter and Malcolm Longair Astrophysics Group, Cavendish Lab, Cambridge, U.K. Marcel Clemens Universita degli Studi di Padova, Italy Abstract. We present preliminary results of recent spatially resolved mid infrared (Mid-IR) spectroscopy with the MICHELLE instrument on UKIRT of NGC 7469, observed as part of a larger programme to study a sample of starburst and AGN in the Mid-IR. ...

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• Astrophysics Group COAST Astronomical Results
• Example of an OOF analysis for the GBT
• VLBI observations of the quasar 3C380

... Advises . Contact Advises . As an advise for amateurs we would like to underline: if it's possible, try to observe 3 asteroid positions per night and do not neglect to observe the Numbered Minor Planets in your telescope field of view as a "by product" of your observational programs. ... We think such estimations ought to be produced every morning after CCD observations of the moving celestial objects by observer himself. ...

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... In this paper we present the results of detailed B, V, R, I, and H study of the isolated nearby blue compact dwarf (BCD) galaxy NGC6789. Judging from the literature the observed galaxy has not been resolved into stars up to now. ... The distance of the galaxy, estimated from the tip of the red giant branch (TRGB) is 2.1 Mpc which places NGC6789 close to the Local Group. ... Key words: nearby galaxies: dwarf galaxies (NGC 6789): distance moduli: star content . ... Distance. ...

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• Linear polarization: wavelength dependence
• Introduction
• Project summary

... The comet 169P was first observed by the Near-Earth Asteroid Tracking system. In order to observe this comet we had to figure out if it was possible to view it from Faulkes Telescope South, a 2m reflecting telescope which is used for research as well as for use by school students around the world over the internet. ... Since 169P is such a bright object, we were able to use a red filter on some of our observations to provide a clearer image. ...

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• ULTRACAM Observations of Subdwarf B Stars
• Broadening of Si VIII lines observed in the Solar polar coronal holes
• Observations with the Faulkes Telescope North