  COVER INFORMATION 

 Station:    GBT_VLBA  (Code Gb ) 
 Experiment: RadioAstron AGN polarization imaging
 Exp. Code:  gg081g  


Schedule Version:       1.00
Processed by SCHED version:  11.40  Release 11.4.  March 14, 2015

PI:       Jose L. Gomez

Address:  Instituto de Astrofisica de Andalucia-CSIC
          Glorieta de la Astronomia
          E-18008 Granada, Spain
 

Phone:    +79165452842
EMAIL:    jlgomez@iaa.es, alobanov@mpifr-bonn.mpg.de
Fax:
Phone during observation: +79165452842

Observing mode: K-band,Q-band, dual-pol

Notes:    K-band, Radioastron-compatible frequency setup
          P-CAL is ON
          Tsys is ON
          auto-level (AGC) is ON

Schedule for GBT_VLBA  (Code Gb )                                   Page   2
               RadioAstron AGN polarization imaging
  UP:  D => Below limits;  H => Below horizon mask;  W => still slewing at end;  blank => Up.
  Early: Seconds between end of slew and start.   Dwell: On source seconds. 
  Disk: GBytes recorded to this point.
  TPStart:  Recording start time.  Frequencies are LO sum (band edge).
  SYNC: Time correlator is expected to sync up.
----------------------------------------------------------------------------------------
Start UT  Source               Start / Stop                 Early    Disk   TPStart
Stop UT                  LST      EL    AZ   HA  UP   ParA  Dwell   GBytes    SYNC
----------------------------------------------------------------------------------------

 --- Thu   9 Mar 2017   Day  68 ---

 ---------- This is a 8-min scan for GBT to do POINTING ----------

 Next scan frequencies:  22220.00  22220.00  22252.00  22252.00  22284.00  22284.00  22316.00  22316.00
 Next BBC frequencies:     816.00    816.00    784.00    784.00    752.00    752.00    720.00    720.00
 Next scan bandwidths:      32.00     32.00     32.00     32.00     32.00     32.00     32.00     32.00

01 50 00  0823+033     07 38 27  53.0 159.7 -0.8     -15.8     0        0   Stopped 
01 58 00  ---          07 46 28  53.5 162.9 -0.7     -13.3   480        0           

 ---------- K-band VLBI scans. Space segment 01: 0823+033 with VLBA ----------

02 00 00  0823+033     07 48 28  53.6 163.8 -0.6     -12.7    98        0   02 00 00
02 10 00  ---          07 58 30  54.1 167.9 -0.5      -9.4   600       77   02 00 01

02 10 30  0823+033     07 59 00  54.1 168.1 -0.5      -9.3     8       77   02 10 30
02 20 00  ---          08 08 32  54.4 172.2 -0.3      -6.1   570      151   02 10 31

02 20 30  0823+033     08 09 02  54.4 172.4 -0.3      -6.0     8      151   02 20 30
02 30 00  ---          08 18 33  54.6 176.5 -0.1      -2.8   570      224   02 20 31

02 30 30  0823+033     08 19 03  54.6 176.7 -0.1      -2.6     8      224   02 30 30
02 40 00  ---          08 28 35  54.7 180.8  0.0       0.6   570      298   02 30 31

02 40 30  0823+033     08 29 05  54.7 181.0  0.0       0.8     8      298   02 40 30
02 50 00  ---          08 38 37  54.6 185.1  0.2       4.0   570      371   02 40 31

02 50 30  0823+033     08 39 07  54.6 185.3  0.2       4.2     8      371   02 50 30
03 00 00  ---          08 48 38  54.3 189.4  0.4       7.4   570      444   02 50 31


SETUP FILE INFORMATION:
   NOTE: If DOPPLER, FREQ, or BW were used, see the individual scans for the final BBC settings.


 ======== Setup file: ra1cm2.set
   Matching groups in ./gg081g_freq.dat:
     gbt1cm_a4       LO1=28.868, LO2=16.532, LO3=10.5

   Setup group:    1         Station: GBT_VLBA          Total bit rate:  1024
   Format: VDIF              Bits per sample: 2         Sample rate: 64.000
   Number of channels:  8    DBE type: RDBE_DDC         Speedup factor:   1.00

   Disk used to record data.

   1st LO=  23036.00  23036.00  23036.00  23036.00  23036.00  23036.00  23036.00  23036.00
   Net SB=         U         U         U         U         U         U         U         U
   IF SB =         L         L         L         L         L         L         L         L
   Pol.  =      RCP       LCP       RCP       LCP       RCP       LCP       RCP       LCP 
   BBC   =         1         2         3         4         5         6         7         8
   BBC SB=         L         L         L         L         L         L         L         L
   IF    =        B         D         B         D         B         D         B         D 

  The following frequency sets based on these setups were used.

   Frequency Set:   1  Setup file default.  Used with PCAL = 1MHz
   LO sum=   22220.00  22220.00  22252.00  22252.00  22284.00  22284.00  22316.00  22316.00
   BBC fr=     816.00    816.00    784.00    784.00    752.00    752.00    720.00    720.00
   Bandwd=      32.00     32.00     32.00     32.00     32.00     32.00     32.00     32.00
   VLBA legacy crd files using  4 channels based on RDBE channels:   3  4  5  6
   CRD fr=     776.01    776.01    744.01    744.01
   CRD bw=      16.00     16.00     16.00     16.00
    Matching frequency sets:   1

   Track assignments are: 
    track1=   1,  2,  3,  4,  5,  6,  7,  8
    barrel=roll_off 

 POSITIONS OF SOURCES USED IN RECORDING SCANS

   Source                         Source position (RA/Dec)                        Error
                        (B1950)             (J2000)             (Date)            (mas)

 * FAKERA            11 57 21.769299   * 12 00 00.000000     12 00 59.999094       0.00
                     85 16 41.77889    * 85 00 00.00000      84 54 13.39687        0.00
                     From catalog imbedded in main SCHED input file.
                     fake circumpolar target for a TS to look at

 * 0823+033          08 23 13.540326   * 08 25 50.338355     08 26 44.689444       0.00
   J0825+0309        03 19 15.40169    * 03 09 24.51995      03 05 47.49040        0.00
                     ./gg081g_sources.radioastron
                     AGN, MASIV, rfc_2013d Petrov, 2013, unpublished 57025 observations, RA-AO3-04, R



SOURCE SCAN SUMMARY FOR SOURCES LISTED ABOVE

     Scan hours are for recording scans only. 
     Baseline hours are only counted for scans above horizon at both ends.
  Source       Setup file             Frequency sets                  Observing hours
                                   (duplicates not shown)              Scan  Baseline
  FAKERA     ra1cm2.set            12                                0.958     0.000
  0823+033   ra1cm2.set            1 2                               0.958    52.708


EFFECT OF SOLAR CORONA

  The solar corona can cause unstable phases for sources too close to the Sun.
  SCHED provides warnings at individual scans for distances less than 10 degrees.
  The distance from the Sun to each source in this schedule is:
    Source         Sun distance (deg) 
   FAKERA              99.5
   0823+033           137.1

  Barry Clark estimates from predictions by Ketan Desai of IPM scattering sizes 
  that the Sun will cause amplitude reductions on the  longest VLBA baselines 
  at a solar distance of 60deg F^(-0.6) where F is in GHz. 
  For common VLBI bands, this is: 
       327 MHz        117. deg 
       610 MHz         81. deg 
       1.6 GHz         45. deg 
       2.3 GHz         36. deg 
       5.0 GHz         23. deg 
       8.4 GHz         17. deg 
      15.0 GHz         12. deg 
      22.0 GHz          9. deg 
      43.0 GHz          6. deg 

