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<H1 ALIGN=CENTER>Minutes of the Frascati meeting (16/12/1999)</H1>
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<STRONG>Subject: </STRONG>Minutes of the Frascati meeting (16/12/1999)<BR>
<STRONG>From: </STRONG>Germano Bonomi (<A HREF="mailto:bonomi@nppbs1.ing.unibs.it?subject=Re:%20Minutes%20of%20the%20Frascati%20meeting%20(16/12/1999)&replyto=Pine.LNX.4.04.9912200917460.19415-100000@nppbs1.ing.unibs.it"><EM>bonomi@nppbs1.ing.unibs.it</EM></A>)<BR>
<STRONG>Date: </STRONG>Mon Dec 20 1999 - 09:18:25 MET
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<P>
Minutes of the FINUDA OFF-LINE Software Meeting
<BR>
<BR>
Frascati, 16-December-199
<BR>
<P> ===========================================
<BR>
<P><P> I try to represent everybody as fairly as possible according to my
<BR>
understanding of the discussion. Let me know if you feel
<BR>
mis/under-represented and if you think I need to add anything.
<BR>
<BR>
G. Gomez
<BR>
<P><P><P><P>Present: G. Bonomi, A. Feliciello, G. Gomez, A. Panzarasa, A. Zenoni.
<BR>
=======
<BR>
<P><P>++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Current Status of the Code:
<BR>
==========================
<BR>
<P>It was decided that:
<BR>
<P>-> The FINUDA Software group will support two platforms: Digital Unix
<BR>
and Linux. Although the code presently runs on VMS systems as well,
<BR>
this platform will no longer be supported by the group.
<BR>
<P>-> A new version (4.00) of the MC and reconstruction code will be
<BR>
compiled and released. This version includes all the changes made
<BR>
to v 3.04 in order to make the code functional.
<BR>
<P>-> CERNLIB 2000 has been released. G. Bonomi and G. Gomez will verify
<BR>
that the new code release works on both platforms using either
<BR>
CERNLIB 99/2000 and add any linking options, if required, to be done
<BR>
automatically during code installation.
<BR>
<P>*** A little bit of good news for Friday 17:
<BR>
<BR>
Version 4.00 has already been released the morning of 17-December.
<BR>
We have checked that it runs on Linux and Digital Unix using either
<BR>
CERNLIB 2000 or CERNLIB 99. The Monte Carlo and reconstruction
<BR>
programs seem to run well for MC input and real data, interactive
<BR>
and non-interactive, on both platforms. The latest release, as well
<BR>
as all relevant information, can be found in the FINUDA Off-line
<BR>
Software WEB page:
<BR>
<P> <A HREF="http://fidabs.ing.unibs.it/finuda/rec_mc.html">http://fidabs.ing.unibs.it/finuda/rec_mc.html</A>
<BR>
<P>-> This version therefore becomes the common base from which code
<BR>
development will be done.
<BR>
<P><P>++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>FINUDA Off-line Group Mailing List
<BR>
==================================
<BR>
<P>It was decided that the group should have a mailing list to facilitate
<BR>
communication between group members. The task was assigned to G. Bonomi,
<BR>
who has already created such a mailing list. All integrants of this
<BR>
group should have received an e-mail with the relevant information.
<BR>
The mailing list can also be accessed through the WEB page above, and
<BR>
the address is:
<BR>
<P> <A HREF="mailto:Finuda.Offline@fidabs.ing.unibs.it?subject=Re:%20Minutes%20of%20the%20Frascati%20meeting%20(16/12/1999)&replyto=Pine.LNX.4.04.9912200917460.19415-100000@nppbs1.ing.unibs.it">Finuda.Offline@fidabs.ing.unibs.it</A>
<BR>
<P>Contact G. Bonomi if you have any requests for modification of this
<BR>
mailing list.
<BR>
<P>++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Examples of Remaining Problems
<BR>
==============================
<BR>
<P>A. Feliciello pointed out a few examples of problems which still need
<BR>
to be addressed in the code. It should be noted that this is in no way
<BR>
a comprehensive list of such problems.
<BR>
<P>-> Regarding the graphics, general conventions should be used.
<BR>
For example, an asterisk is used to mark a hit associated to a track,
<BR>
a cross marks a hit NOT associated to a track, warm colors denote
<BR>
associated hits, cold colors denote non-associated hits, etc...
<BR>
In particular, for the new pattern recognition of cosmics using the
<BR>
ISIM+OSIM+ITOF, this convention was not followed (by G. Gomez).
<BR>
People working in any graphics development should pay attention to
<BR>
the existing conventions.
<BR>
<P>-> The geometry of the ISIM Si micro-strips needs to be changed: the
<BR>
glass windows should be on the inside and the silicon on the
<BR>
outside, similar to the OSIM, which is modeled correctly.
<BR>
<P>-> For the reconstruction of Hyper-nucleus events, there are
<BR>
compilation warnings (at least on Digital Unix) which need to be
<BR>
looked at. They are "cern library error condition c205" and
<BR>
"cern 205 rzero ... F(A) and F(B) have the same sign". If anyone
<BR>
knows about these messages, advice is welcome.
<BR>
<P>-> The phi -> rho + pi generator might need some revision.
<BR>
<P>-> There are also warnings about the ISST and OSST structures missing.
<BR>
These structures (ISIM and OSIM support structures) were removed
<BR>
when the new ISIM geometry was implemented (G. Gomez), and indeed
<BR>
are no longer inside the detector.
<BR>
<P>-> The interactive reconstruction needs several corrections. In
<BR>
particular, Feliciello pointed out that the back-tracking feature
<BR>
exhibits some anomalous behavior.
<BR>
<BR>
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Cosmic Ray Data
<BR>
===============
<BR>
<P>A. Zenoni pointed out that one of the most urgent objectives is the
<BR>
analysis of cosmics, which are divided into 1) old cosmics taken for the
<BR>
study of the Straw Tubes (STRW) and Drift Chambers (DCH1/2), and 2) new
<BR>
cosmics being collected right now with the central detector
<BR>
(ISIM+OSIM+TOFINO). These data need to be reconstructed and analyzed
<BR>
in order to study the calibration, intrinsic resolution, and
<BR>
efficiency for each sub-detector.
<BR>
<P>1) STRW + Chambers:
<BR>
---------------
<BR>
<P> A. Panzarasa, A. Feliciello and A. Zenoni will be in charge of
<BR>
analyzing these cosmics and studying the DCH resolution. Their plan
<BR>
of action is to get the latest version of GARFIELD to model the DCH
<BR>
cell geometry, with the option to include the magnetic field. They
<BR>
hope to reproduce the current geometry and resolutions, and
<BR>
eventually to improve the DCH resolution to values comparable to
<BR>
those expected.
<BR>
<P>2) ISIM+OSIM+ITOF:
<BR>
--------------
<BR>
<P> V. Filippini will use the first cosmic ray data collected by the
<BR>
central detector to update the database. After that, G. Gomez will
<BR>
test the pattern recognition program for "central detector" cosmics.
<BR>
Once the reconstruction program is verified to work properly, G.
<BR>
Gomez will perform initial studies of Si micro-strip resolutions and
<BR>
ITOF efficiency.
<BR>
<P> A. Zenoni suggested that the task of using these cosmic ray data
<BR>
for testing of micro-strip reconstruction and alignment be given
<BR>
to L. Venturelli and S. Piano.
<BR>
<BR>
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Alignment + Detector Geometry
<BR>
=============================
<BR>
<P>The final detector alignment will require cosmic ray data taken with
<BR>
all sub-detectors. This alignment task will require some dedicated
<BR>
work, for which no one has yet been assigned. A. Zenoni pointed out
<BR>
that it is highly desirable to have an on-line, interactive alignment
<BR>
code.
<BR>
<P>The detector geometry should reflect, as closely as possible, that
<BR>
of the final aligned detector. To this effect, the Monte Carlo
<BR>
geometry description should include any "rigid body" displacement or
<BR>
rotation evidenced by the alignment procedure. It is hoped that this
<BR>
part of the code will be somewhat stable (as well as the detector
<BR>
geometry!).
<BR>
<P>In connection to the study of STRW + DCH cosmic ray data
<BR>
by A. Panzarasa and A. Zenoni, the DCH cell displacements need to be
<BR>
modeled correctly by displacing the entire cells, instead of using
<BR>
the temporary solution of displacing only the wires.
<BR>
<P>A. Feliciello and A. Panzarasa will try to insert into the
<BR>
reconstruction program the positions from photometric studies of the
<BR>
Drift Chambers.
<BR>
<P>++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Modeling of Bhabha Scattering
<BR>
==============================
<BR>
<P>Modeling of Bhabha scattering is altogether missing in the current
<BR>
off-line code. Some of the issues discussed were:
<BR>
<P>-> A Bhabha trigger has never been simulated or studied, and a
<BR>
trigger request should be made. A careful assessment of the Toushek
<BR>
background is needed.
<BR>
<P>-> Pattern recognition and reconstruction code for Bhabha events needs
<BR>
to be developed. A. Zenoni proposed to assign this task to
<BR>
P. Salvini, and offered to give her some help should she need it.
<BR>
<P>-> In connection to the alignment studies, Bhabha scattering events
<BR>
could be useful for final detector alignment, if Bremsstrahlung
<BR>
effects do not deteriorate the resolution too much.
<BR>
<BR>
-> Bhabha reconstruction can (and will) be used to monitor
<BR>
the machine luminosity as well as the transverse profile of the
<BR>
electron/positron beam .
<BR>
<BR>
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Integration of Existing Developments
<BR>
====================================
<BR>
<P>Mainly due to lack of time, Version 4.00 does not yet integrate
<BR>
important code developments. In particular, we need to include in
<BR>
future releases the work from:
<BR>
<P>-> P. Cerello: work on on-line/off-line connection and output for
<BR>
off-line analysis in C and root. He has kindly offered
<BR>
to give us a cradle with respect to the latest version,
<BR>
4.00/00.
<BR>
<P>-> M. Bertani: work on Straw Tube simulation and reconstruction.
<BR>
<P>-> S. Piano : work on micro-strip simulation and reconstruction and on
<BR>
background generator.
<BR>
<P>-> A. Olin : work on Monte Carlo studies of hyper-nuclear non-mesonic
<BR>
decays and nuclear muon capture.
<BR>
<P>Cradles with respect to version 4.00 would be greatly appreciated.
<BR>
Once these cradles are available, A. Zenoni and G. Gomez will certify
<BR>
them, and include them as soon as possible in future releases of the
<BR>
code.
<BR>
<P>++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
<P>Voices from Vancouver
<BR>
=====================
<BR>
<P>Unable to attend the Frascati meeting, A. Olin sent an e-mail which
<BR>
was considered and discussed. The issues raised were:
<BR>
<P>-> A. Olin pointed out that CMZ is no longer supported at CERN. He
<BR>
asked if the group should consider switching to another code
<BR>
management program, namely CVS. It was decided that we will stick
<BR>
to CMZ. The latest CMZ version, 1.50, can be downloaded from the
<BR>
CMZ WEB page (there is a link from our page).
<BR>
<P>-> A. Olin and Ed Auld (joining FINUDA) offer to work on the study of
<BR>
space-time relationships for the drift chambers. They would work in
<BR>
parallel to A. Panzarasa using the STRW + DCH cosmic ray data. It
<BR>
was deemed by the group a good idea to have people at Torino
<BR>
and Vancouver look at the data, and their offer is welcome.
<BR>
It might be a good idea for the Vancouver group to have their own
<BR>
local database. Copies of the CDs containing these cosmic ray
<BR>
data could be sent to them over the mail.
<BR>
<BR>
<P>++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
======================================================================
<BR>
++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
<BR>
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