PIMMS v4.7a now available
Version 4.7a contains an updated post-launch effective area curve file
for NuSTAR; the upper energy limit of NuSTAR has been updated form 80 keV
to 79 keV.
Version 4.7 newly supports HEAO-1 A1, MAXI SSC and GSC instruments. It also
contains updated effective area curves for the Chandra instruments, suitable
for Cycle 16 proposals. The APEC plasma model files have been updated using
ATOMDB version 2.0.2.
If you would like to be informed whenever
a new version of PIMMS is released, please contact
PIMMS - Portable, Interactive Multi-Mission Simulator
Command-line tool and the Web interface
PIMMS was originally written as a stand-alone,
interactive program (the "command line PIMMS").
implements a subset of the functionalities of the command line
PIMMS. While allowing easy access, without the need to
install the software, it does not have all the functionality
of the command line version.
PIMMS, as described here, is software for high-energy
astrophysicists, and has nothing to do with
the Project to Increase Mastery of Mathematics and Science.
The program was named quite independently of this
worthwhile project at Wesleyan University.
Time-Variable Instrumental Response
PIMMS currently does not support time-variable calibration
of instruments. Because it is primarily intended as a planning tool
for future observations, the responses in PIMMS is often
applicable for upcoming observations.
For example, if you are a Chandra user who wishes
to convert count rates in a past observation to flux, please see
PIMMS is currently supported on several flavors of UNIX
workstations, on Linux PCs, Macs running OS X/Darwin.
It requires a Fortran compiler, and make on UNIX machines.
Please consult the Installation Guide
for details, then
the latest version.
New in Version 3.8/3.8a/3.8a2 (Released 2006 May 1 - 2006 May 24)
New in Version 3.7/3.7a (Released 2005 Sep 13 - 2005 Dec 23)
New in Version 3.6/3.6a/3.6b/3.6c5 (Released 2004 Sep 15 - 2005 Feb 10).
New in Version 3.5 (Released 2004 Jul 9).
New in Version 3.4/3.4a (Released 2003 Sep - 2004 Jan 12).
New in Version 3.3/3.3a (Released 2002 Dec 16 - 2003 Mar 27).
New in version 3.2-3.2d (Released 2001 Sep 10 - 2002 Jan 29).
New in version 3.1 a-c (Released 2001 January 29 - May 03).
New in version 3.0 (Released 2000 April 28).
New in version 2.7 (Released 1999 July 9).
New in version 2.6 a-c (Released 1999 February 2 - May 4).
New in version 2.5 (Released 1997 December 15).
New in version 2.4/2.4b
(Released 1996 June 03).
New in version 2.3 (Released 1996 June 03).
New in version 2.2 (Released 1995 August 07).
New in version s2.1a (Released 1995 April 03).
- New in Version 4.7/4.7a (Released 2014 Mar 5/Jul 24)
- Version 4.7a contains an updated effective area curve and associated
information for NuSTAR, reflecting the post-launch understanding of the
mission. Although it was our intent to include the updated effective
area curves in Version 4.7, and our documentation claimed it did,
this was unfortunately not the case due to a configuration error.
Version 4.7a does contain the update; moreover, the upper energy limit
for the instrument has been updated from 80 keV to 79 keV.
- Version 4.7 newly includes effective area curves for MAXI SSC and GSC
all-sky monitor instruments.
- Version 4.7 also newly includes support for the HEAO-1 A1 instrument,
appropriate for a direct comparison with the HEAO-1 A1 X-ray Source
- Version 4.7 also contains updated effective area curves for the Chandra
instruments, appropriate for Cycle 16 proposals. Differences with Cycle
15 versions are minor.
- The set of APEC model files have been re-generated using ATOMDB
2.0.2 using xspec version 12.8.1g on 2013 Dec 9-11, with the
"solar" abundance values of Asplund et al. 2009. Previous APEC
model files were based on ATOMDB 1.3.1 and Anders & Grevesse
- New in Version 4.6/4.6a/4.6b (Released May 25/Sep 28/2013 Jan 25)
- New in Version 4.5 (Released 2012 Jan 30)
- New in Version 4.4 (Released 2011 Sep 19)
- New in Version 4.3 (Released 2011 Feb 15)
- New in Version 4.2/4.21 (Released 2010 Dec 20/Oct 27)
- New in Version 4.1/4.1a/4.1b (Released 2010 Jun 1 - Sep 21)
- New in Version 4.0 (Released 2010 Feb 17)
- New in Version 3.9 through 3.9k (Released 2006 Sep 6 - 2009 Oct 6)
- Sample Sessions
- Using Multi-component Models
- Extended Sources
- The User Interface
- PIMMS commands
version of the Guide.
Adding new missions and other future plans
At a very basic level, new missions can be added simply by
creating a set of effective area curve files: they need to
be two-column ASCII files, containing pairs of photon energy
in keV and effective area in cm2.
PIMMS source code and data files are distributed
freely, without restrictions. If you decide to add new
missions to PIMMS, we would like to be able to distribute
it from HEASARC.
We hope to have a programmers' guide some day to make it easier
to add mission-specific information.
Credits and Feedback
PIMMS is mostly written and maintained by Koji Mukai.
Effective area curves for current and future missions have been supplied
by the respective projects. XTE specific subroutines have been written
by Koji Mukai, with the help of Jim Lochner and Phil Blanco. The SAX
specific subroutine has been written by the SAX Data Center and
Lorella Angelini. Snowden R-band effective area curves for ROSAT
PSPC have been created by Richard West of Leicester.
The only published article on PIMMS is in the HEASARC journal:
Mukai, K. 1993, Legacy 3, 21-31.
Questions and comments on PIMMS can be sent to
HEASARC Home |
This file was last modified on Thursday, 24-Jul-2014 18:39:12 EDT