SearcharxivSearch

arXiv subjects

David Huenemoerder

Publications and source records attributed to David Huenemoerder.

3 recordsLinked to original sources

CIAO: Chandra's Data Analysis System for X-Ray Astronomy and Beyond

The Chandra Interactive Analysis of Observations (CIAO) software, developed by the Chandra X-ray Center, has been the data analysis package for the Chandra X-ray Observatory since its launch in 1999. Over nearly three decades, CIAO has grown from a small software suite into a widely used system for X-ray data analysis and beyond. CIAO provides tools for calibration, spectral, imaging, and timing analysis, together with high-level scripts and the \sherpa\ modeling and fitting application. Its modular design and unified data model allow users to build flexible analysis workflows while maintaining consistency with the Chandra data processing pipeline. Visualization capabilities are provided through integration with SAOImageDS9 and Python-based tools, and simulation components such as ChaRT and MARX extend the analysis environment to include detailed modeling of instrumental effects. In this paper we describe CIAO's design, evolution, and capabilities after 25 years of Chandra operations. We also describe its core architecture, scripting environment, modeling, visualization tools, simulation components, and testing infrastructure, as well as the documentation and user support system that have contributed to its widespread use. CIAO's continued development and broad adoption highlight its important role in X-ray astronomy and its usefulness in multiwavelength astrophysical research.

astro-ph.IM

X-ray flare modeling in the single giant HR 9024

We analyze a Chandra-HETGS observation of the single G-type giant HR 9024. The high flux allows us to examine spectral line and continuum diagnostics at high temporal resolution, to derive plasma parameters (thermal distribution, abundances, temperature, ...). A time-dependent 1D hydrodynamic loop model with semi-length 10$^{12}$cm ($\sim R_{\star}$), and impulsive footpoint heating triggering the flare, satisfactorily reproduces the observed evolution of temperature and emission measure, derived from the analysis of the strong continuum emission. The observed characteristics of the flare appear to be common features in very large flares in active stars (also pre-main sequence stars), possibly indicating some fundamental physics for these very dynamic and extreme phenomena in stellar coronae.

astro-ph

X-ray Spectra and Light Curves of AR Lac: Temperature Structure, Abundances, and Variability

We observed AR Lac, an eclipsing RS CVn binary star, with the Chandra High Energy Grating Spectrometer for a total of 100 ks divided into six intervals covering both quadratures and eclipses. We repeated observations at each phase. At least two flares were seen, in which the flux increased by factors of two and four. The flares occurred near eclipse phases and compromised detection of eclipse modulation. The quadrature fluxes were the most stable, but they also show non-repeating trends. Quadrature line profiles are broadened relative to eclipse profiles, presumably due to orbital velocity Doppler shifted emission from each binary component. The spectrum appears to be iron poor and neon rich, similar to HR 1099, but not as extreme as II Pegasi. We will examine line strengths, widths, and positions vs. phase, and present preliminary differential emission measure models and abundance determinations using the APED emissivity database. This work is supported by NASA contract NAS8-38249 (HETG) and SAO SV1-61010 (CXC) to MIT.

astro-ph