... The Linear Ramp Filters provide a narrow band ( ) imaging capability which is continuously tunable from 3710 to 9762 . ... If it is necessary to know which CCD will be used, observers can consult Table 3.7 on page 48 or Table 3.8 on page 49 , or use the on-line LRF calculator tool on the WFPC2 WWW pages. It is possible to use POS TARGs with LRF observations; the offsets are made from the default pointing for the specified wavelength. ... POS TARG "X" = -0.09961 (235.7-414) = 17.76" , and . ...

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

HI spectral-line observations of galaxies (Karen O'Neil) . Measuring the width, flux, etc. of the HI profile of two galaxies, using some combination of : dwarf emission line, HVC emission line, spiral emission line, and spiral absorption line. This project was designed to demonstrate the fundamentals of spectral line observing and position switching. ... The types of galaxies observed in this project are being kept open and will be determined when the project LST is known. ...

Pulkovo NEO Page . ... NEA Accuracy Estimation . ... The estimation of accuracy of the current CCD observations of asteroids and comets is constantly performed at Pulkovo Observatory. ... The (O-C) values, so called "Observed" minus "Calculated" positions, characterize numerically the observations of any observatory, both professional and amateur, during a short period (one or several close nights). ... So the (O-C) values for these objects nearly entirely define the errors of observations. ...

Next: Observations Up: The Nuclear Region: HI Previous: The Nuclear Region: HI . There are mainly two questions to be addressed: 1) What causes the large velocity width (several hundred kms -1 ) of the absorption lines detected against the nuclear regions of galaxies? 2) Why are the absorption line widths observed against the nuclear radio continuum similar to those measured in emission over the whole extent of the galaxy? ...

True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR . ... Position of Central Source (J2000) : ( 23 01 08.3, 58 52 44.6 ) . ... Description: half shell, bright central AXP . ... Radio Images Page . ... Exposure uf . ... 4626 . ... Exposure uf Exposure time of unfiltered event file . Exposure f Exposure time of filtered event file . ... Central pulsar not in field. ... Event 2 FITS File . ... see fit detail page for more about the fit. see chandra spectrum page for region used. ...

... 67Lawrence+ Of the 3118 sources in the Arecibo 611 MHz survey, 2911 have been observed using the NRAO 300 ft transit telescope at 6 cm. ... 4 Mean 1950 RA (see col.3.) ... 6 Mean 1950 Decl. (see col.3.). if A appears in col.1, the Arecibo dec. is listed. 7 Dec error in arc seconds (see col.3.) ... 16 Number of observations, in the form abc, where a is the number of observations averaged in RA, b is the number of observations averaged Dec, c is the number of observations averaged in flux. ...

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

When entering Identification section user should open the file with observed positions of objects which are to be identified (the file may be first created). ... Format of observations must coincide with that of optic observations in which they are published by Minor Planet Center (observed position may be presented as “accurate” or “approximate” one): . ... observed right ascension (in hours, minutes, and seconds of time (“accurate position”) or in hours and minutes (“approximate position”) . ...

Next: Comments on Individual Sources Up: Sample Identification Previous: Sample Identification . In Figure 2, we show the spectra of the optical counterparts to 85 of 97 observed X-ray/radio sources. ... Positional information for all 85 sources for which we announce identifications herein are given in Table 3, including information from WGACAT, the PMN and Green Bank surveys, the NVSS and our ATCA survey. ... Of the 85 newly identified sources, 59 are FSRQs, and 22 are BL Lacs. ...

Left: An image in the near infrared (1.65 ЮМm) around RY Tauri, using a special mode of the Subaru HiCIAO coronagraph, the polarized intensity image. This type of observation is preferred for faint emissions associated with scattered light around planet-forming disks, as there is less light from the much brighter star. ... A white ellipse shows the position of the midplane of the disk, which is observed at millimeter wavelengths. ... Right: Schematic view of the observed infrared light. ...