PIMMS v3.9i now available

If you would like to be informed whenever a new version of PIMMS is released, please contact Koji Mukai, Koji.Mukai@nasa.gov.

V3.9i correctly treats the statistical errors in the Suzaku HXD background files provided to the users. It also includes updates of instrument-specific outputs when a limited energy range is specified.

V3.9h includes minor updates of the effective area curves for Suzaku suitable for Cycle 4 proposers.

In addition, PIMMS now outputs approximate time needed for 3-sigma and 5-sigma detection in standard HXD energy bands (1 for PIN and 2 for GSO), given the current level of systematic uncertainties in the background models.

This should be used as an initial guide; Cycle 4 proposers are encouraged to perform spectral simulation with background systematic uncertainties to establish the feasibility of the proposed observations.

PIMMS - Portable, Interactive Multi-Mission Simulator

Disclaimer

PIMMS, as described here, is software for high-energy astrophysicists, and has nothing to do with PIMMS, 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 this note.

Command-line version and World-Wide Web version

PIMMS had originally been written as a stand-alone, interactive program (the "command line PIMMS").

WebPIMMS implements a subset of the functionalities of the command line PIMMS. While allowing easy access, without the need to install the software, it probably will not have all the functionality of the command line versions in the foreseeable future.

Installation Guide

PIMMS is currently supported on several flavors of UNIX workstations, on Linux PCs, Macs running OS X/Darwin. It requires a Fortran77 compiler, and make on UNIX machines. Please consult the Installation Guide for details, then download the latest version.

Revision History

New in Version 3.9i (Released 2008 Nov 4)

This version correctly treats the statistical errors in the Suzaku HXD background files provided to the users.
It also crrects bugs for Swift XRT grade 0 count rates as well as ASCA count rates within the typical extraction regions, in cases when a limited energy range is specified.
Also when a limited energy range is specified for outputs, the message regarding the lack of instrument-specific extra information has been updated.

New in Version 3.9h (Released 2008 Oct 20)

The effective area curves for Suzaku XIS and HXD have been updated, although differences are minor compared with the previous version. In addition for the HXD, PIMMS now outputs approximate time needed for 3-sigma and 5-sigma detection in the standard energy bands (1 for PIN and 2 for GSO), given the current level of systematic uncertainties in the background models.

New in Version 3.9g (Released 2008 Sep 15)

Effective area curves for XMM-Newton EPIC/MOS and Swift XRT have been updated. For the MOS, a new warning regarding the loss of efficiency in MOS1 timing mode data has been included.

New in Version 3.9f (Released 2008 Apr 14)

Effective area curves for Constellation-X (under the new name "conx"), XEUS, as well as those for Swift UVOT (except grisms), have been updated.

New in Version 3.9e (Released 2007 Dec 18)

Effective area curves for the Chandra instruments have been updated. The new versions are appropriate for Cycle 10 proposers.

New in Version 3.9d (Released 2007 Oct 23)

Effective area curves for Suzaku XIS and HXD instruments have been updated. The new versions are appropriate for Cycle 3 proposers.

New in Version 3.9c (Released 2007 Sep 12)

Effective area curves for XMM-Newton EPIC instruments have been updated, reflecting very minor calibration changes. However, at the same time, PIMMS now predicts count rates for EPIC/pn for PATTERN=0 events only, to provide a more conservative estimates for proposers. This change reduces the predicted count rates typically by a third. There is a corresponding minor change in pile-up correction routine so it will continue using the total (all PATTERN) count rates internally.

New in Version 3.9b (Released 2006 Dec 26)

Updated Chandra effective area curves appropriate for Cycle 9 proposers.
A bug that affected energy flux calculations of redshifted, table-based models (including Raymond-Smith) has been fixed. Note that analytical models (power-law, blackbody, bremsstrahlung) were never affected by this bug; neither were table-based models when not redshifted; nor the photon flux calculations of redshifted, table-based models.

New in Version 3.9a (Released 2006 Oct 26)

Suzaku XIS and HXD effective area curves have been updated. The new calibration is appropriate for Cycle 2 proposers.

New in Version 3.9 (Released 2006 Sep 6)

A bug that affected command-line users on Linux platforms, causing a core dump under certain circumstances, has been fixed.
XMM-Newton EPIC effective area curves have been updated. The new calibration is appropriate for AO-6 proposers. However, the differences with previous versions are small.

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).

Users' Guide

Download the LaTeX, PDF, or PostScript 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 Koji Mukai, Koji.Mukai@nasa.gov.

This file was last modified on Tuesday, 04-Nov-2008 15:50:07 EST