The Astronomical Society of Australia has been asked by STANDARDS AUSTRALIA to compile a list of "designated" optical observatories that are valuable resources for (i) research, (ii) education and (iii) community use. The ASA is the final arbiter of whether any particular observatory is so designated. ... Upon receipt of your application form, your observatory will be entered on a list of "Pending Designated Observatories" on the ASA Home Page. ... It will be emailed for you. ... Email . ...

... You are here: start €Ё lbaops €Ё lbaapr2011 €Ё v255n . ... VLBI Schedule . ... Observer's Wiki . ... lbaops:lbaapr2011:v255n . ... Setup v255n.5cm: . ... IFP#1-LO 6642 - 6658 MHz USB RCP . ... Setup v255n.5cm-icrf: . ... Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v255/v255n . ... For Hobart the LOs should be set to 468 MHz (IFP#1) and 810 MHz (IFP#2) for the 4 x 16 MHz setup and 810 MHz for the 2 x 16 MHz setup. ... lbaops/lbaapr2011/v255n.txt €§ Last modified: 2015/12/18 16:38 (external edit) . ...

October 30-31, 1992 . ... Modified images of the October 30-31, 1992 event. (a) - This NRH image is adapted to show a very bright loop-like source over AR 7321 near the SW-limb identified with the X1.7 soft X-ray LDE event peaked on 30d at 17:30 UT (see the GOES-7 soft X-ray plot also at the upper right corner). ... Here and hereafter, the white features are radio filaments. (c) - This modified NRH image shows some large scale microwave blob chains and structures. ...

do mod_pw (must be run from LRP account) . ... SU 0nnnn01 PC: xxxx cycle: 5 orb: 6 st.stat: scheduling in SPSS: Y cw_stat: S orient: Y type: GO/WFI pws.stat: planned S: Y proc_err: N lrp _state: ready LRP : 97073A ----------------------------------------------------------------------- QSP order_num: ( NONE ) week_id: ( NONE ) exe_time: ( NONE ) USC 1996.001:00:00:00 1997.054:00:00:00 M:c C:17-Feb-1997 N:FGS23GS Comment : Visit was unschedulable or had no FGS23 GSs when ...

. The page is under construction. Our table shows a classification of various light scattering methods, applicability to different scatterers and to their ensembles as well as the anzatz sources and recent reviews. In comments we briefly discuss different classifications, features, relationships, available codes, comparison works and recent reviews of the light scattering methods. To the top . Created by V.I. Last modified: 10/04/03, V.I.

. Comment on J2346+0930 . See Figure 4 for an image of each component. The source was detected at 2.3 GHz by Preston et al. (1985) (correlated flux density 40 mJy) with much higher resolution. VLBApls home page . Last modified: 16 Oct 2000

... The Figure shows the parallactic angle in relation to the source position at (RA,DEC), the zenith of the telescope at (LST,AoLatitude), the hour Angle HA, and the azimuth direction AZ (in the picture the source has already transitted). ... Now suppose that a second feed was placed 1 beam width away from the central horn parallel to the azimuth arm. ... Figure 1. shows the parallactic angle rate versus azimuth angle for declinations 8 through 28 (spaced 1 degree steps from Arecibo's latitude). ...

ChangeLog for omsource ====================== Version 1.9.5 - 2004-01-27 (CB) -------------------------------- Ammended code so that the logger list is cleared when delete list button clicked. (fixes SPR 3230). Version 1.9.4 - 2004-01-22 (CB) -------------------------------- Modified observation information display dialogue to show dates as a MJD. (fixes SPR 3226). ... Gui improved. ... Version 1.1.8 - 2002-12-05 (CB) -------------------- Fixed some minor bugs. ... Improved user interface. ...

... Galaxy Evolution home . ... The origin and evolution of radio sources . Radio sources and their environments . ... We are investigating how this interaction effects galaxy evolution in general as well as the feedback effect of the radio source on its host galaxy and AGN. ... One direct observational manifestation of this interaction is the existence of extended regions of emission-line gas which show a clear spatial relationship to the radio source itself. ...

... See also changes and comments in configure.in # prefix = @prefix@ exec_prefix = @exec_prefix@ DESTDIR = CFITSIO_LIB = ${DESTDIR}@libdir@ CFITSIO_INCLUDE = ${DESTDIR}@includedir@ INSTALL_DIRS = @INSTALL_ROOT@ ${CFITSIO_INCLUDE} ${ CFITSIO_LIB } ${ CFITSIO_LIB }/pkgconfig SHELL = / bin /sh RANLIB = @RANLIB@ CC = @CC@ CFLAGS = @ CFLAGS @ SSE_FLAGS = @SSE_FLAGS@ FC = @FC@ LDFLAGS = $( CFLAGS ) DEFS = @ DEFS @ LIBS = @ ...

... 13-Aug-2014 12:13 106K lk_20140815_0905.tar.. 15-Aug-2014 09:06 106K lk_20140901_0823.tar.. 01-Sep-2014 08:23 103K lk_20141016_1324.tar.. 16-Oct-2014 13:25 103K lk_20141211_1708.tar.. 11-Dec-2014 17:08 103K lk_20150430_0315.tar.. 30-Apr-2015 03:15 103K lk_20150430_0420.tar.. 30-Apr-2015 04:20 103K lk_20150818_1511.tar.. 18-Aug-2015 15:11 104K lk_20151113_1903.tar.. 13-Nov-2015 19:04 105K lk_20160314_0610.tar.. 14-Mar-2016 06:11 105K . ...

... The NVSS is being made as a service to the astronomical community, and the principal data products are being released into a directory accessible by anonymous FTP as soon as they are produced and verified. ... The large (4 deg x 4 deg) map cubes and total intensity only images and their associated multisource (u,v) data sets are stored as binary files in FITS format (see Grosbol et al. ... The source catalog derived from the available images is kept in directory CATALOG as CATALOG.FIT. ...