... section 5.4 ) . If the detector map (a grid of positions used to calculate and flux weight the ARF: section 5.3 ) is either psf or flat , the map bounds and pixel size may be specified. ... The user can supply an external detector map instead (section 5.3.2 ), but the bounds must cover the regions. ... The following sub-sections show examples of usage. ... Example 4: Specifying an external detector map for an extended source . Example 5: Using an RMF dataset to specify the energy grid . ...

... Stellar Evolution . Nucleosynthesis in Stars . The Evolution of Star Clusters . JAVA Physics Lab . Alternative Energies Class . Steve Kevan's Physics 251 Class . ... Talk on Solid State Physics of CCD detectors . Talk on Cosmological Issues . ... Digital Spectra of Stars . NETexperts E-mail List . The Electronic Universe Project e-mail: nuts@moo.uoregon.edu ...

... The IRAF task rvcorrect is used to compute radial velocity corrections. rvcorrect is in the IRAF astutil package and it calls on task observatory , which is also found in astutil. The following steps are an example of its use for an HST dataset where the HST velocity around the Earth is ignored (maximum residual: +/- ~7.8 km/s): . ... Here is an example of file rvcor . ... Run the rvcorrect task: cl>rvcorrect f=rvcor.in > outputfile The above example produced the following output file. ...

... The input images are wlc , the wavelength calibration frame, and obj , the object. ... WRITE/OUT Copy test images -DELETE lndemo_*.* ... SAVE/LONG ses1 WRITE/OUT "Now calibrating another arc spectrum in GUESS mode" SET/LONG WLCMTD=GUESS GUESS=ses1 WLC=lndemo2 LINCAT=lndemo_thorium SET/LONG WIDTH=4 THRES=3. ... RADIUS=2 SKYFIT/LONG ext8 stdsky LOAD stdsky COMPUTE/IMAGE ext7 = ext8 - stdsky SET/LONG OBJECT = 199,203 EXTRACT/AVERAGE ext7 stda PLOT stda EXTRACT/LONG ext8 stde stdsky PLOT stde ! ...

... ESO for the Public > Doing Business with ESO > Technology Transfer > Examples of ESO developments that have been used for other similar projects in external institutions of firms . ... UVES (UV and Visual Echelle Spectrograph) was one of the first generation VLT instruments and was developed in-house at ESO. ... This has created pools of expertise within the ESO Member States that has allowed individual institutions to provide valuable contributions to the VLT observatory as well as other projects. ...

Each sequence of calls to one of the image I/O routines is associated with a unique identifier, the so called transfer identifier. Before the first call, 0 should be assigned to this identifier. When upon return the identifier has a value < 0, an error has occurred. ... These further calls must be made using the unmodified transfer identifier. ... With the help of this identifier, it is possible to handle subsets which contain more data than there is room for in your read/write buffer. ...

... Argument: C-Type: (char *) (IN) Desc: Pointer to the text which we parse 2. ... Argument: C-Type: (char **) (OUT) Desc: token text 3. ... LexDescr * descr = (LexDescr *) palloc(sizeof(LexDescr) * (2+1)); /* there are only two types in this parser */ descr [0].lexid = 3; descr [0].alias = pstrdup( word ); descr [0]. descr = pstrdup( Word ); descr [1].lexid = 12; descr [1].alias = pstrdup( blank ); descr [1]. descr = pstrdup( Space symbols ); descr [2].lexid = 0; PG_RETURN_POINTER( ...