SCHED can set observing frequencies for spectral line observations based on velocities provided in the source catalog and rest frequencies provided in a separate type of input. This option is invoked by specifying DOPPLER and can be turned off with NODOP (DOPCAL is an obsolete form that was too easy to confuse with ``DO PCAL''). If DOPPLER is invoked, SCHED calculates the velocity of the center of the Earth with respect to the designated reference frame (VREF in the direction of the source at the time of the middle of the project. From this velocity, the source velocity from the source catalog, and the rest frequency, the required observing center frequency is calculated. The antennas need to know the LO settings so SCHED must know the bandwidth. The bandwidth will usually be obtained from the setup file. It may be provided for the scan with the BW parameter.
The reference frames supported by SCHED are the ``Local Standard of Rest'' or LSR VREF=L, heliocentric VREF=H, and geocentric VREF=G.
Note that channels assigned to the same BBC will be given the same frequency as the first channel on that BBC, no matter what velocities etc are given for the other channels. This will be the case when there are upper/lower sideband pairs. Their frequencies cannot be set independently. Because of the different sidebands, they will, however, cover different velocity ranges.
The frequencies derived from the doppler calculations have to be rounded off to a value that can be set on the available synthesizers. For the Mark III/IV and VLBA systems, frequencies can be set to the nearest 10 kHz. However other systems are different -- VSOP, for example, can only be set to the nearest 1 MHz. The parameter DOPINCR can be used to control the rounding.
The doppler calculations are for the center of the Earth for the middle of the project. This implies that the frequency for each source will be constant for the duration of the project. Experience over the years with spectral line VLBI has shown this to be the preferred observing mode since it minimizes the chances of mistakes at stations that do not have automatic frequency setting. The shifts of the resulting spectra of about a km per second that result from the rotation of the Earth can be removed in post-processing with the CVEL program in the NRAO spectral line software or with a task of the same name and with similar capability in AIPS.
The LO sum used when doppler calculations are requested are calculated by either the radio definition (VDEF=R in the source catalog ) or the optical definition (VDEF=O or VDEF=Z). With the radio definition, the LO sum is calculated as RESTFREQ * (1 - v/c) - BW/2 where RESTFREQ is the line rest frequency from the line initialization input, c is the speed of light, and BW is the bandwidth (appropriately signed according to the sideband). With the optical definition, the LO sum is RESTFREQ / (1 + v/c) - BW/2. Typically velocities for radio spectral lines in galactic sources are given in the radio definition in the LSR frame. Extragalactic velocities, on the other hand, are typically in the optical definition in the heliocentric frame. The differences in the radio and optical definitions only matter at large (typically extragalactic) velocities.
SCHED will accept redshifts if VDEF=Z in place of velocities, but be very careful that you have adequate accuracy to calculate proper frequencies - the bandwidths are typically very much smaller than the observing frequency so the velocities must be accurate.
Internally, if Doppler calculation is requested, SCHED calculates the desired observing frequencies and puts them in the same array that would be used if FREQ were used. This will override any FREQ specifications in the main schedule and any frequency specifications in the setup files. The frequencies of baseband converters will then be set properly based on the FIRSTLO for the station. Please note that the setup files must still contain a complete, valid frequency specification. This is to allow validity checking and to allow SCHED to pick up default parameters from the frequency catalog. The frequency in the setup should be close enough to the desired observing frequency that only final tuning of the BBCs is needed to get the exact desired frequency. For the VLBA with its 500 MHz IFs, this is not a serious concern. It might be for the VLA (50 MHz IFs) or other antennas with narrow IFs.
The number of channels desired is set with NCHAN in the setup file (NCHAN in the main schedule is an obsolete parameter and is not used.). To calculate a frequency, SCHED must have, for each channel, a bandwidth, a velocity from the source catalog, and a rest frequency from the line initialization input information. If a value is missing for any channel of any parameter, the value of that parameter for channel 1 will be used. This avoids the need, for example, of specifying lots of bandwidths when they are all the same.
For continuum sources mixed in with line sources, specify NODOP for that scan to avoid the Doppler calculations.
Often it is desired to observe a continuum source at the same frequency as a line source for bandpass calibration. This can be done by specifying the line source with DOPSRC in the continuum source's scan. The DOPSRC will be used for the Doppler calculation.
The important parameters in the SCHED keyin file for Doppler frequency calculation are listed below. Detailed descriptions are given with the descriptions of other SCHED parameters.
The rest frequencies are specified in separate keyin inputs in the SCHED keyin file following a ``/'' if LINEINIT was specified. There can be one rest frequency per channel, although any not specified default to the first which is often the desired behavior. There should be one velocity per channel in the source file for each source to be observed (other than continuum calibrators). Each group of lines has a name which is then refered to using LINENAME in the scan input. The group can change with each scan, but be careful to change the setup file, too, if necessary. Up to 10 groups of lines are allowed. The parameters in the LINEINIT group are:
A fairly extensive list of possible rest frequencies is given below. These frequencies are not guaranteed. If anyone finds an error, please notify Craig Walker (cwalkernrao.edu).
--------------------------------------------------------------- lineinit / ! Frequencies from Reid and Moran's Annual Reviews article preprint. ! Do not keep more than 10 lines in a SCHED input file. lineset='OH1612' restfreq=1612.231 / lineset='OH1665' restfreq=1665.402 / lineset='OH1667' restfreq=1667.359 / lineset='OH1720' restfreq=1720.530 / lineset='OH4660' restfreq=4660.42 / lineset='OH4765' restfreq=4765.562 / lineset='OH6030' restfreq=6030.747 / lineset='OH6035' restfreq=6035.092 / lineset='CH3OH' restfreq=6668.5192 / Breckenridge and Kukolich ApJ 438. lineset='CH3OH' restfreq=12178.597 / Breckenridge and Kukolich ApJ 438. lineset='OH13' restfreq=13441.417 / lineset='NH3' restfreq=18499.393 / Pratrap Preprint. lineset='CH3OH' restfreq=19967.3961 / Menton preprint. lineset='H2O' restfreq=22235.08 / lineset='CH3OH' restfreq=23121.0242 / Menton preprint. lineset='CH3OH' restfreq=25124.87 / lineset='SiO425' restfreq=42519.3 / lineset='SiO428' restfreq=42820.54 / lineset='SiO431' restfreq=43122.03 / lineset='SiO862' restfreq=86243.35 / lineset='SiO868' restfreq=86846.89 / lineset='CH3OH' restfreq=44069.43 / Bachiller preprint (SAO) lineset='CH3OH' restfreq=97980.97 / Plambeck preprint (SAO) lineset='SiO1293' restfreq=129363.26 / ! some more from VLA OBSERVE lineset='H' restfreq=1420.405752 / lineset='H2CO4830' restfreq=4829.656900 / lineset='H2CO145' restfreq=14488.475000 / lineset='NH3(1,1)' restfreq=23694.495500 / lineset='NH3(2,2)' restfreq=23722.633600 / lineset='NH3(3,3)' restfreq=23870.129600 / lineset='NH3(4,4)' restfreq=24139.416900 / lineset='NH3(5,5)' restfreq=24532.988700 / endlines / -----------------------------------------------------------------
The example below shows the SCHED input for a spectral line It is a modified version of the file used for a project by Phil Diamond in Dec 95. The modifications are to adjust for some of the new features of SCHED that were not available at the time the file was used. Note that it is not necessary to repeat the DUR and GAP specification every scan. However some users prefer to show these details and it certainly doesn't hurt. Also, the bandwidth specification is the same as the setup file so it is not required (it used to be).
! EXAMPLE - spectral line observations. ! ========================================================== ! ================= Cover Information ==================== ! ========================================================== EXPT = 'BD27 VLBA format 7mm line 1995 DEC 29 18:00 -> DEC 30 18:00 UT' EXPCODE = 'BD027' VERSION = 1 PINAME = 'P.J.Diamond' ADDRESS1 = 'NRAO' ADDRESS2 = 'P.O. Box O' ADDRESS3 = 'Socorro, NM 87801, USA' PHONE = '1-505-835-7365 (work) or 1-505-835-2095 (home)' OBSPHONE = '1-505-835-7365 (work) or 1-505-835-2095 (home)' FAX = '1-505-835-7027' EMAIL = 'firstname.lastname@example.org (internet)' OBSMODE = 'VLBA' OBSTYPE = 'VLBA' NOTE1 = 'At VLA use antenna 27' NOTE2 = 'its the standard VLBI antenna and has good Q band performance' ! ========================================================== ! ============== Correlator Information ================== ! ========================================================== correl = 'Socorro' coravg = 4 corchan = 256 cornant = 10 corpol = 'off' corwtfn = 'uniform' corsrcs = 'standard' cortape = DAT corship1 = 'Athol Kemball' corship2 = 'P. O. Box O' corship3 = 'Socorro NM 87801' ! ========================================================== ! ==================== Source Catalog ==================== ! ========================================================== ! This has sources with positions in mixed equinoxes. ! It is normally recommended to use J2000. ! Note most of the continuum sources below could be picked up ! from $SCHED/catalogs/sources.vlba SRCCAT / SOURCE='3C273' RA=12:26:33.2480 DEC= 02:19:43.290 EQUINOX='B1950' / SOURCE='3C279' RA=12:53:35.8380 DEC=-05:31:08.040 EQUINOX='B1950' / SOURCE='3C345' RA=16:41:17.6080 DEC= 39:54:10.820 EQUINOX='B1950' / SOURCE='3C454.3' RA=22:51:29.52 DEC= 15:52:54.35 EQUINOX='B1950' / SOURCE='OJ287' RA=08:51:57.2530 DEC= 20:17:58.440 EQUINOX='B1950' / SOURCE='1823+568' RA=18:23:14.9490 DEC= 56:49:18.050 EQUINOX='B1950' / SOURCE='1334-127' RA=13:34:59.8150 DEC=-12:42:09.900 EQUINOX='B1950' / SOURCE='1633+382' RA=16:33:30.6280 DEC= 38:14:10.050 EQUINOX='B1950' / SOURCE='0420-014' RA=04:20:43.5400 DEC=-01:27:28.660 EQUINOX='B1950' / SOURCE='1749+096' RA=17:51:32.8185 DEC= 09:39:00.728 EQUINOX='J2000' / SOURCE='RAQR' RA=23:41:14.269 DEC=-15:33:42.89 EQUINOX='B1950' VEL = -27.0, -27.0 / SOURCE='RLEO' RA=09:44:52.2 DEC= 11:39:40.8 EQUINOX='B1950' VEL = -2.0, -2.0 / SOURCE='VYCMA' RA=07:20:54.6 DEC=-25:40:12.2 EQUINOX='B1950' VEL = 20.0 / SOURCE='VXSGR' RA=18:05:02.9 DEC=-22:13:55.6 EQUINOX='B1950' VEL = 8.0 / SOURCE='UHER' RA=16:23:35.0 DEC= 19:00:18.0 EQUINOX='B1950' VEL = -15.0, -15.0 / SOURCE='IKTAU' RA=03:50:43.7 DEC= 11:15:31.8 EQUINOX='B1950' VEL = 34.0, 34.0 / SOURCE='TXCAM' RA=04:56:41.4 DEC= 56:06:29.9 EQUINOX='B1950' VEL = 9.0, 9.0 / SOURCE='NMLCYG' RA=20:46:25.59 DEC= 40:06:58.3 EQUINOX='J2000' VEL = -5.0, -5.0 / SOURCE='SPER' RA=02:19:15.1 DEC=+58:21:34.0 EQUINOX='B1950' VEL = -40.0, -40.0 / ENDCAT / ! ========================================================== ! ==================== Station Catalog =================== ! ========================================================== stafile = '$SCHED/catalogs/stations.dat' ! ========================================================== ! ============== Spectral line rest frequecies =========== ! ========================================================== LINEINIT / lineset='ccal' restfreq=43122.027, 43122.027, 43126.027, 43126.027, 43130.027, 43130.027, 43134.027, 43134.027 / lineset='prog' restfreq=43122.027, 43122.027 / ENDLINES / ! ========================================================== ! ==================== Observing setup =================== ! ========================================================== ! This is a fairly fully specified setup file. setinit = bd27.set / nchan = 8 samprate = 8.0 bits = 1 bbfilter = 4.0 ! 128 Mbps tpmode = 4 format = VLBA1:1 bbc = 1, 2, 3, 4, 5, 6, 7, 8 netside = U, U, U, U, U, U, U, U ifchan = R, L, R, L, R, L, R, L ! Radio Astronomy allocation: 42400-43500 pcal = 'off' freqref = 43150.99 freqoff = -8,-8,-4,-4,0,0,4,4 firstlo = 42400.00 fe(1) = '7mm' fe(3) = '7mm' synth(2) = 7.6 synth(3)= 11.6 ! LO = Syn(2) + 3*Syn(3) station = 'VLBA' rchan = A lchan = C / firstlo = 42489.9, 42489.9 vlaband = VQ vlabw = '0000' vlafeab = 51.6 vlafecd = 13.4 vlasyna = 3889.9 vlasynb = 3889.9 flukea = 100.0 flukeb = 200.0 pcal = 'off' ! Pulse cal tone can mess up spectra. station = 'VLA1' rchan = B lchan = D / endset / ! As a demonstration, the following is all that is needed ! to get an equivalent setup to the above. It uses A,C IFs at ! the VLA and a different VLA LO setup (better), but is otherwise ! the same. Note that both turn off the pulse calibration tones ! which can mess up spectral line observations. ! Neither setup uses the default 'format' because that would give a ! speedup factor on correlation and the correlator output data ! rate would be too high. Note that the format can be forced ! with either 'tpmode' or 'format'. setinit = bd27a.set / nchan = 8 bits = 1 bbfilter = 4.0 tpmode = 4 pol = dual pcal = 'off' band = '7mm' / endset / ! ========================================================== ! ================= Initial Scan Information ============= ! ========================================================== ! STATIONS = VLBA_SC, VLBA_HN, VLBA_NL, VLBA_FD, VLBA_LA, VLBA_PT, VLBA_KP, VLBA_OV, VLBA_BR, VLBA_MK, VLA1 VLAMODE 'VS' YEAR = 1995 MONTH = 12 DAY = 29 START = 18:02:00 ! ! LINENAME = 'ccal' DOPPLER SETUP = 'bd27a.set' ! ========================================================== ! ======================== The Scans ===================== ! ========================================================== SOURCE = '1749+096' GAP = 00:02:00 DUR = 00:11:00 DOPSRC 'SPER'/ ! SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / ! SOURCE = '3C454.3' GAP = 00:02:00 DUR = 00:11:00 DOPSRC 'SPER'/ ! SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / ! SOURCE = '3C454.3' GAP = 00:02:00 DUR = 00:11:00 DOPSRC 'SPER'/ ! SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'SPER' GAP = 00:02:00 DUR = 00:11:00 / ! ! __________________________________ ! | | ! | Many scans in the same style. | ! |__________________________________| ! SOURCE = '1749+096' GAP = 00:02:00 DUR = 00:11:00 DOPSRC 'UHER'/ ! SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / ! SOURCE = '1749+096' GAP = 00:02:00 DUR = 00:11:00 DOPSRC 'UHER'/ ! SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / SOURCE = 'UHER' GAP = 00:02:00 DUR = 00:11:00 / ! SOURCE = '1749+096' GAP = 00:02:00 DUR = 00:11:00 DOPSRC 'UHER'/ ! ---------------------------------------------------------------------