... Here we will look at line plots. We will go through steps, such as changing linestyles and symbols, you can use to modify your line plots. ... IDL> plot, num, line . ... IDL> plot, num, line, psym = 1 . ... IDL> plot, num, line, linestyle = 1 . ... Line Style . ... IDL> plot, num, line, linestyle=2, thick=3 . ... IDL> plot, num, line, psym = 8, symsize = 2.0 . ... IDL> plot, num, line, charsize=2.0, title='GHRS spectrum . ... IDL> plot, num, line, charsize=2.0, xcharsize=0.8, xtitle='wavelength' . ...

... The active time at each angular bin is the sum over frames of the active time contributions from all CCD pixels, within the node-specific telemetry window, which overlap the surface of the bin. ... The active time, per frame, of a normal pixel is the full frame integration time multiplied by the node-specific fractional exposure; bad pixels contribute no active time. ... If an event is rejected for this reason only, then its pixels remain normal in the exposure map. ...

This diagram illustrates a floating image that overlaps the borders of two paragraphs in normal flow: the paragraph borders are clipped by the non-transparent parts of the image. ... A left-floating image causes the final three lines of the upper paragraph to float along its right side. It causes the first three lines of the following paragraph to do the same, and the remainder of that paragraph flows normally. The paragraph borders shine through the margin area of the image box. ...

... Do not warn when variables are not explicitly declared. ... Do not check if a variable has been initialized before being used. If a variable is not in a DATA, COMMON, PARAMETER or SAVE statement, and if it is not a dummy subroutine argument, then Flint normally attempts to check that the variable is initialized before it is used. ... By default Flint warns if subroutine or variable names are longer than 8 characters, or if they contain underline or dollar characters. ...

Next: Echelle Reduction Up: No Title Previous: CCD-Commands Summary . The reduction of CES spectra is, especially for point sources, very straightforward, and the general instructions given in Chapter 6 for the standard reduction of spectra are fully adequate. ... As far as the data reduction goes, the main difference between Reticon and CCD is the data format. Since the Reticon is a one-dimensional array, no attention has to (can) be paid to the extraction of the object spectra. ...

... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

... We propose to use sid (supernovae identificator) as a reference name instead of Zwicky's nomenclature, see [[sid_details ? ... Host galaxy ( galaxy ) - primary key (gid) . ... All info about supernovae discovered by SAI SN team: select s.*, g.* from sn s, galaxy g, team t, sn_team_map st, sn_galaxy_map sg where t.name = 'SAI' and st.tid = t.tid and s.sid = st.sid and sg.sid = s.sid and sg.gid = g.gid; . ... 0 Comments on sncat proposal This page is read-only View other revisions Administration . ...

... Suppose that a NS having a rotational magnetic   luminosity forms a binary system (with semi-major axis a ) with a normal star losing matter in the form of stellar wind (with a loss rate ). ... This means that while deriving the formula for a cavern in the general case, we must take into account the proximity of the normal star. ... It follows from the symmetry considerations that at the anterior point of the cavern (i.e. the point closest to the normal star), . ... If , the cavern is closed. ...

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

... Normal cloud bottoms are flat because moist warm air that rises and cools will condense into water droplets at a very specific temperature, which usually corresponds to a very specific height. ... Planetary Nebula Project . ... The North America Nebula in Infrared . ... Red stars are cool, with surface temperatures of around 3,000 kelvins (K), while blue stars are hotter and can have temperatures over 30,000 K. Our own lovely "yellow" Sun's temperature is a comforting 6,000 K. [ First page ] Prev. ...

Displays the current status of the Dual Imaging Spectrograph (DIS) and allows you to change the configuration. Normally only the most common status is displayed and the configuration controls are hidden. ... Pushing the "Config" button displays configuration controls (each to the right of its corresponding item of status). Select TUI:Save Window Positions to remember the state of this checkbutton. ... Turret : current position of the grating turret. ... Grating : name of the current grating. ...