Differences

This shows you the differences between two versions of the page.

--- ata_testing [2018/04/10 20:58] – jrseti
+++ ata_testing [2023/10/28 18:36] (current) – external edit 127.0.0.1
@@ Line 1: / Line 1: @@
-==ATA Testing==
+===ATA Testing===
-===Thoughts from Andrew and Griffin===
+==Feed Measurements==
+  * [[feed_measurements|Feed Measurements]]
+  * [[sefd_measurements|SEFD Measurements]]
+==Data Gathers==
+  * [[data_gathered|These sources have been observed with the Beamformer]]
+==Pulsar Finding==
+  * [[pulsar_finding|Pulsars]]
+==Handful of Sources==
+  * http://adsbit.harvard.edu//full/1994A%26A...284..331O/0000335.000.html
+  * [[http://www.atnf.csiro.au/people/pulsar/psrcat/|Pulsars]]
+  * [[https://github.com/UCBerkeleySETI/breakthrough/blob/master/doc/RAW-File-Format.md|GUPPI Raw format]]
+  * [[https://github.com/UCBerkeleySETI/gbt_seti/blob/master/src/filterbank_mkheader.c|Filterbank header]]
+  * [[http://astro.berkeley.edu/~davidm/rb-blgbt.git|Filterbank Ruby code from Dave]]
+  * [[http://sigproc.sourceforge.net/sigproc.pdf|Filterbank header spec (see section 3)]]
+  * [[https://github.com/UCBerkeleySETI/breakthrough/blob/master/GBT/voyager/voyager.ipynb|Filterbank Voyager1 Tutorial/Jupyter]]
+==Thoughts from Andrew and Griffin==
 Email from August 07, 2017 from Griffin:
@@ Line 47: / Line 71: @@
   I just wanted to restart this conversation.
   I think Griffin’s suggestions are great, here are a few other ideas.
@@ Line 57: / Line 81: @@
   http://adsbit.harvard.edu//full/1994A%26A...284..331O/0000335.000.html
-  Positions for these sources can be found on SIMBAD, e.g.: http://simbad.u-strasbg.fr/simbad/sim-id?
+  Positions for these sources can be found on SIMBAD, e.g.: http://simbad.u-strasbg.fr/simbad/sim-id?Ident=3C48&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id
- Ident=3C48&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id
   I would recommend cross scans at the nominal position in addition to the ON/OFF, as was done in the reference
   above.
   For the purposes of analyzing these observations, we will want to be able to produce coarsely channelized and
   integrated spectral data, e.g. ~1s time integration and 1 MHz frequency resolution.  This should keep the data rate
@@ Line 83: / Line 106: @@
+==Pulsars==
+PSR B0329+54
+  RA: 03h 32m 59.368s
+  Dec: +54° 34′ 43.57″
+  In hours,degrees: 3.5498244,54.5787694
+PSR B0531+21 (Crab Pulsar)
+  RA: 05h 34m 31.97s
+  Dec: +22° 00' 52.1"
+  In hours,degrees: 5.5755472,22.0144722
+PSR B0950+08
+  RA: 09h 53m 09.310s
+  Dec: +07° 55' 35.75"
+  In hours,degrees: 9.8859194,7.9265972