pith. machine review for the scientific record. sign in

arxiv: 2605.14144 · v1 · submitted 2026-05-13 · 🌌 astro-ph.IM

Recognition: 2 theorem links

· Lean Theorem

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

Antonella Fruscione , Jonathan McDowell , Douglas Burke , Mark Cresitello Dittmar , Ian N. Evans , Janet D. Evans , Kenny Glotfelty , Hans Moritz Guenther
show 8 more authors
David Huenemoerder William Joye Nicholas P. Lee Warren McLaughlin Joseph B. Miller Melania Nynka David A. Principe Aneta Siemiginowska
Authors on Pith no claims yet

Pith reviewed 2026-05-15 01:45 UTC · model grok-4.3

classification 🌌 astro-ph.IM
keywords CIAOChandra X-ray ObservatoryX-ray data analysisSherpa modelingmodular softwareastronomical pipelinesspectral analysisimaging analysis
0
0 comments X

The pith

CIAO supplies modular tools for calibration, spectral, imaging and timing analysis of Chandra X-ray data while keeping workflows consistent with the observatory pipeline.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents CIAO as the primary analysis package for the Chandra X-ray Observatory, developed since the mission's 1999 launch and now in use for nearly three decades. It explains how the software combines individual tools for different analysis steps with high-level scripts and the Sherpa modeling application. The central argument is that a modular architecture and unified data model let users create their own analysis sequences without breaking compatibility with the original Chandra data processing. A reader would care because this design supports both routine observations and complex multiwavelength studies by reducing the need to rewrite basic processing steps each time.

Core claim

CIAO is a data analysis system for the Chandra X-ray Observatory that supplies 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 construct flexible analysis workflows while preserving consistency with the Chandra data processing pipeline. Visualization is handled through integration with SAOImageDS9 and Python-based tools, and simulation components such as ChaRT and MARX extend the system to model instrumental effects in detail. The paper reviews this architecture, the scripting environment, modeling capabilities, visualization tools, and the

What carries the argument

Modular design paired with a unified data model that supports custom workflows while enforcing pipeline consistency.

If this is right

  • Astronomers can combine individual analysis steps into reproducible custom scripts without reimplementing calibration or data format handling.
  • Integration with visualization and simulation packages lets users test instrumental effects directly inside the same workflow.
  • The same architecture supports both targeted observations and large survey processing while remaining aligned with official Chandra data products.
  • Continued updates to the core components have kept the system usable for multiwavelength studies that combine X-ray data with observations from other telescopes.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same modular-plus-unified-model pattern could be tested for new X-ray missions to shorten the time from raw telemetry to science-ready products.
  • Widespread scripting support may make it easier to embed CIAO steps inside automated pipelines for upcoming large-scale surveys.
  • Python-level integration opens a route to apply modern statistical or machine-learning methods to the same data objects already used by traditional spectral fitting.

Load-bearing premise

That the modular design and unified data model have actually delivered flexible workflows without introducing major inconsistencies or usability barriers across 25 years of operation.

What would settle it

A systematic review of user scripts or help-desk records that shows frequent cases where CIAO-derived products diverge from Chandra pipeline outputs or where users report repeated barriers when trying to combine tools.

Figures

Figures reproduced from arXiv: 2605.14144 by Aneta Siemiginowska, Antonella Fruscione, David A. Principe, David Huenemoerder, Douglas Burke, Hans Moritz Guenther, Ian N. Evans, Janet D. Evans, Jonathan McDowell, Joseph B. Miller, Kenny Glotfelty, Mark Cresitello Dittmar, Melania Nynka, Nicholas P. Lee, Warren McLaughlin, William Joye.

Figure 1
Figure 1. Figure 1: High-level schematic of the CIAO data analysis system. This simplified diagram illustrates, in an approxi￾mate way, the bidirectional connections between the central analysis core and the specialized modules for data acquisi￾tion, modeling, infrastructure, and user workflows. its role as a system designed to support Chandra users (A. Fruscione & A. Siemiginowska 2000). The initial CIAO concept was based on… view at source ↗
Figure 2
Figure 2. Figure 2: Annual number of CIAO downloads until the end of 2025, illustrating sustained usage over time, with thou￾sands of downloads per year. The increase observed since 2020 is likely related to the COVID-19 pandemic, when more researchers started working remotely and installing the soft￾ware on personal machines. These counts represent down￾loads, not unique users, so they cannot distinguish new users from exist… view at source ↗
Figure 3
Figure 3. Figure 3: Distribution of CIAO v4.18.0 downloads by op￾erating system and installation method, showing that ma￾cOS accounts for a slightly larger share of total downloads (∼52%) than Linux (∼46%). macOS users are distributed across both x86 and ARM architectures and multiple instal￾lation options, while Linux usage is concentrated in conda (24.1%) and script-based (21.9%) installations. Source code downloads account… view at source ↗
Figure 4
Figure 4. Figure 4: Event distribution at an intermediate stage of co￾ordinate transformations in an HETG spectrum. Top: each point represents a detected photon, plotted in “order-sort￾ing” coordinates. The x-axis shows the diffraction angle (set by where the photon lands on the detector), while the y-axis shows the CCD signal converted to an approximate energy. The gratings spread the incoming light into multiple diffraction… view at source ↗
Figure 5
Figure 5. Figure 5: Demonstration of several adaptive and alterna￾tive binning approaches available in CIAO. All images show a 620 ks observation of Abell 2052 in the 0.5–7.0 keV band. The top left panel shows the original image with standard pixel binning (each pixel is ∼ 1 ′′ on a side). The left col￾umn compares uniform tilings, including square pixels (top) and hexagonal bins (bottom, generated with hexgrid, side length ∼… view at source ↗
Figure 6
Figure 6. Figure 6: X-ray image of the supernova remnant RCW 103 using two methods of color representation: true color (left) and tri-color (right). The true color image was created using the energy hue map script, which combines the adaptively smoothed counts image with the median energy at each lo￾cation to create a true color image. Here, the color hues span a continuous range capped by red (median energies below 1.0 keV) … view at source ↗
Figure 7
Figure 7. Figure 7: A mosaic of 41 Chandra ACIS-I observations cen￾tered near η Carinae, processed using the merge obs script. (a) Integrated 0.5–7.0 keV counts image after all observations have been reprojected to a common tangent point. (b) The corresponding broadband monochromatic exposure map (in cm2 s count photon−1 ), used to account for spatial variations in instrument sensitivity and vignetting. (c) A fluxed true– col… view at source ↗
Figure 9
Figure 9. Figure 9: Example of two-dimensional modeling of the X-ray surface brightness of NGC 777 using Sherpa (E. O’Sullivan et al. 2024). Left: Chandra 0.5–2 keV expo￾sure-corrected image, smoothed with a 2.5 ′′ radius Gaus￾sian. Cyan contours indicate the 400 MHz radio emission. The dashed ellipse shows the approximate D25 contour of the galaxy. Right: Residual map after the removal of point sources and subtraction of the… view at source ↗
Figure 8
Figure 8. Figure 8: Schematic diagram of the srcflux script illustrat￾ing the complexity of the analysis pipeline. The procedure links multiple CIAO tools and intermediate data products, starting from an input event file, source position, and out￾put root, and proceeding through region definition, counts extraction in multiple energy bands, and background esti￾mation. Several alternative branches are used to compute PSF corre… view at source ↗
Figure 10
Figure 10. Figure 10: High-resolution LETG spectra of the blazar Mrk 421 showing absorption features from the warm–hot in￾tergalactic medium (WHIM) (F. Nicastro et al. 2005). The panels display selected wavelength regions with lines from highly ionized species (e.g., Ne X, O VII, O VIII). Black points represent the data; the model is obtained via for￾ward fitting with instrumental response folding, with the blue curve indicati… view at source ↗
Figure 12
Figure 12. Figure 12: An example of the capabilities of DAX show￾ing the Spectral Fit analysis task, which extracts a Chan￾dra spectrum, including response files, and fits the data with Sherpa. This task highlights many DAX features. The SAOImageDS9 window (left) displays source and back￾ground regions: a solid green circle for the source, a dashed annulus for the background, and a nearby source excluded from the background (d… view at source ↗
Figure 14
Figure 14. Figure 14: MARX simulations of Chandra HETG observa￾tions for two source models: a point source with a power-law spectrum (“plaw”, left) and an extended disk-like source (“pldisk”, right). In both cases, the zeroth-order image is accompanied by dispersed grating arms corresponding to multiple diffraction orders. The simulations reproduce the spatial distribution of photons along the dispersion direc￾tions, as well a… view at source ↗
Figure 13
Figure 13. Figure 13: Observed PSF of a bright off-axis Chandra calibration source (left; LMC X-1 observed ∼ 25′ off-axis with the ACIS detector), compared with simulations using MARX only (center) and SAOTrace+MARX (right). All three images show remarkably similar large-scale PSF struc￾ture, demonstrating the overall accuracy of both mirror mod￾els. A closer comparison reveals a subtle asymmetry just above and to the right of… view at source ↗
Figure 15
Figure 15. Figure 15: On-axis point-source simulation and PSF-based image reconstruction for τ Canis Major observed with the ACIS detector (ObsID 4469; ACIS-I, NGC 2362). Left: ob￾served image. Center: MARX-simulated PSF generated using simulate psf. Right: image restored via deconvo￾lution with the source PSF using the arestore tool and the Lucy–Richardson method. All three images are shown on the same angular scale. The over… view at source ↗
read the original abstract

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.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 2 minor

Summary. The manuscript is a descriptive overview of the CIAO (Chandra Interactive Analysis of Observations) software package developed by the Chandra X-ray Center. It recounts the system's history since the 1999 launch of the Chandra X-ray Observatory, its growth over 25 years, core modular architecture and unified data model, tools for calibration/spectral/imaging/timing analysis, the Sherpa modeling and fitting application, high-level scripts, visualization integration with SAOImageDS9 and Python, simulation components (ChaRT, MARX), testing infrastructure, documentation, and user support. The central claim is that the modular design and unified data model enable flexible user workflows while preserving consistency with the Chandra data processing pipeline.

Significance. If the descriptions hold, the paper provides a valuable reference document for the X-ray astronomy community on a long-running, widely used analysis system. It explicitly credits the modular architecture, unified data model, and integration with Sherpa and simulation tools as enabling flexible yet pipeline-consistent workflows. As a factual account rather than a novel empirical result, its significance rests on completeness and accuracy in documenting 25 years of evolution, which can aid both users and future software development in multiwavelength astrophysics.

minor comments (2)
  1. The abstract states 'nearly three decades' while the body refers to 'after 25 years of Chandra operations'; align the phrasing for consistency across the manuscript.
  2. The description of the unified data model and modular design would benefit from a simple schematic diagram showing data flow between core components, scripts, and Sherpa to illustrate the claimed flexibility.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript and for recommending acceptance. No major comments were raised in the report, so we have no specific revisions or responses to provide at this time.

Circularity Check

0 steps flagged

No significant circularity in descriptive software overview

full rationale

The paper is a purely descriptive account of the CIAO software system's design, architecture, tools, evolution, and usage over 25 years. It contains no derivations, equations, predictions, fitted parameters, or mathematical claims that could reduce to inputs by construction. Central statements about modular design enabling flexible workflows are presented as factual descriptions of implemented features and historical outcomes, not as results derived from prior assumptions within the paper. No self-citation load-bearing steps or ansatz smuggling appear; the text is self-contained as documentation of an established system.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a software description paper with no mathematical derivations, physical models, or new theoretical constructs; therefore no free parameters, axioms, or invented entities are introduced.

pith-pipeline@v0.9.0 · 5597 in / 1127 out tokens · 46020 ms · 2026-05-15T01:45:42.129378+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

66 extracted references · 66 canonical work pages · 1 internal anchor

  1. [1]

    2011, Handbook of X-ray Astronomy (Cambridge University Press)

    Arnaud, K., Smith, R., & Siemiginowska, A. 2011, Handbook of X-ray Astronomy (Cambridge University Press)

    work page 2011

  2. [2]

    Arnaud, K. A. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes, 17

    work page 1996

  3. [3]

    New Features in AST - a WCS Management and Manipulation Library

    Berry, D. S., & Jenness, T. 2012, in Astronomical Society of the Pacific Conference Series, Vol. 461, Astronomical Data Analysis Software and Systems XXI, ed. P. Ballester, D. Egret, & N. P. F. Lorente, 825, doi: 10.48550/arXiv.1210.5483

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1210.5483 2012

  4. [4]

    R., Chivvis, D

    Bouquin, D. R., Chivvis, D. A., Henneken, E., et al. 2020, ApJS, 249, 8, doi: 10.3847/1538-4365/ab7be6

    work page doi:10.3847/1538-4365/ab7be6 2020

  5. [5]

    S., Townsley, L

    Broos, P. S., Townsley, L. K., Feigelson, E. D., et al. 2010, ApJ, 714, 1582, doi: 10.1088/0004-637X/714/2/1582

    work page doi:10.1088/0004-637x/714/2/1582 2010

  6. [6]

    J., Fruscione, A., Galle, E., Milaszewski, R

    Burke, D. J., Fruscione, A., Galle, E., Milaszewski, R. M., & Stawarz, C. 2006, in Astronomical Society of the Pacific Conference Series, Vol. 351, Astronomical Data Analysis Software and Systems XV, ed. C. Gabriel, C. Arviset, D. Ponz, & S. Enrique, 674

    work page 2006

  7. [7]

    2003, in Astronomical Society of the Pacific Conference Series, Vol

    Beikman, S. 2003, in Astronomical Society of the Pacific Conference Series, Vol. 295, Astronomical Data Analysis Software and Systems XII, ed. H. E. Payne, R. I. Jedrzejewski, & R. N. Hook, 477

    work page 2003

  8. [8]

    2007, in Astronomical Society of the Pacific Conference Series, Vol

    Cresitello-Dittmar, M., Burke, D., Doe, S., et al. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw, F. Hill, & D. J. Bell, 519

    work page 2007

  9. [9]

    Davis, J. E. 2001, ApJ, 548, 1010, doi: 10.1086/319002

    work page doi:10.1086/319002 2001

  10. [10]

    E., Bautz, M

    Davis, J. E., Bautz, M. W., Dewey, D., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8443, Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray, ed. T. Takahashi, S. S. Murray, & J.-W. A. den Herder, 84431A, doi: 10.1117/12.926937 DePonte Evans, J., Cresitello-Dittmar, M., Doe, S., et al. ...

    work page doi:10.1117/12.926937 2012

  11. [11]

    T., Refsdal, B

    Doe, S., Nguyen, D. T., Refsdal, B. L., et al. 2009, in Chandra’s First Decade of Discovery, ed. S. Wolk, A. Fruscione, & D. Swartz, 88

    work page 2009

  12. [12]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Ebeling, H., White, D. A., & Rangarajan, F. V. N. 2006, MNRAS, 368, 65, doi: 10.1111/j.1365-2966.2006.10135.x

    work page doi:10.1111/j.1365-2966.2006.10135.x 2006

  13. [13]

    1993, PhRvE, 47, 704, doi: 10.1103/PhysRevE.47.704

    Ebeling, H., & Wiedenmann, G. 1993, PhRvE, 47, 704, doi: 10.1103/PhysRevE.47.704

    work page doi:10.1103/physreve.47.704 1993

  14. [14]

    N., Primini, F

    Evans, I. N., Primini, F. A., Glotfelty, K. J., et al. 2010, ApJS, 189, 37, doi: 10.1088/0067-0049/189/1/37

    work page doi:10.1088/0067-0049/189/1/37 2010

  15. [15]

    N., Evans, J

    Evans, I. N., Evans, J. D., Mart´ ınez-Galarza, J. R., et al. 2024, ApJS, 274, 22, doi: 10.3847/1538-4365/ad6319

    work page doi:10.3847/1538-4365/ad6319 2024

  16. [16]

    2001, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Freeman, P., Doe, S., & Siemiginowska, A. 2001, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 4477, Astronomical Data Analysis, ed. J.-L. Starck & F. D. Murtagh, 76–87, doi: 10.1117/12.447161

    work page doi:10.1117/12.447161 2001

  17. [17]

    E., Kashyap, V., Rosner, R., & Lamb, D

    Freeman, P. E., Kashyap, V., Rosner, R., & Lamb, D. Q. 2002, ApJS, 138, 185, doi: 10.1086/324017

    work page doi:10.1086/324017 2002

  18. [18]

    2010, Chandra News, 17, 37

    Fruscione, A. 2010, Chandra News, 17, 37

    work page 2010

  19. [19]

    2011, in The X-ray Universe 2011, ed

    Fruscione, A. 2011, in The X-ray Universe 2011, ed. J.-U. Ness & M. Ehle, 208

    work page 2011

  20. [20]

    2014, Chandra News, 21, 24

    Fruscione, A. 2014, Chandra News, 21, 24

    work page 2014

  21. [21]

    2015, Chandra News, 22, 31

    Fruscione, A. 2015, Chandra News, 22, 31

    work page 2015

  22. [22]

    2017, Chandra News, 24, 29

    Fruscione, A. 2017, Chandra News, 24, 29

    work page 2017

  23. [23]

    J., Joye, W., & McDowell, J

    Fruscione, A., Glotfelty, K. J., Joye, W., & McDowell, J. C. 2026, AAS Journals, submitted

    work page 2026

  24. [24]

    J., Lee, N

    Fruscione, A., Glotfelty, K. J., Lee, N. P., & CIAO Team. 2023, Chandra News, 34, 11

    work page 2023

  25. [25]

    2000, Chandra News, 7, 4

    Fruscione, A., & Siemiginowska, A. 2000, Chandra News, 7, 4

    work page 2000

  26. [26]

    C., Allen, G

    Fruscione, A., McDowell, J. C., Allen, G. E., et al. 2006, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 6270, Observatory Operations: Strategies, Processes, and Systems, ed. D. R. Silva & R. E. Doxsey, 62701V, doi: 10.1117/12.671760

    work page doi:10.1117/12.671760 2006

  27. [27]

    2024, Chandra News, 35, 15

    Fruscione, A., Burke, D., Cranmer, C., et al. 2024, Chandra News, 35, 15

    work page 2024

  28. [28]

    J., et al

    Gabriel, C., Denby, M., Fyfe, D. J., et al. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 314, Astronomical Data Analysis Software and Systems (ADASS) XIII, ed. F. Ochsenbein, M. G. Allen, & D. Egret, 759

    work page 2004

  29. [29]

    2003, Chandra News, 10, 20

    Galle, E., & Fruscione, A. 2003, Chandra News, 10, 20

    work page 2003

  30. [30]

    C., Anderson, C

    Galle, E. C., Anderson, C. S., Bonaventura, N. R., et al. 2011, in Astronomical Society of the Pacific Conference

    work page 2011

  31. [31]

    C., Burke, D

    Galle, E. C., Burke, D. J., Stawarz, C., & Fruscione, A. 2005, in Astronomical Society of the Pacific Conference

    work page 2005

  32. [32]

    2020, Chandra News, 28, 7

    Glotfelty, K., & Fruscione, A. 2020, Chandra News, 28, 7

    work page 2020

  33. [33]

    J., Joye, W., & Fruscione, A

    Glotfelty, K. J., Joye, W., & Fruscione, A. 2022, Chandra News, 32, 6 19

    work page 2022

  34. [34]

    2014, Simplifying Chandra Aperture Photometry with srcflux,, https://cxc.harvard.edu/symposium 2014/ ftp presentations/poster Glotfelty Kenny.pdf

    Lee, N. 2014, Simplifying Chandra Aperture Photometry with srcflux,, https://cxc.harvard.edu/symposium 2014/ ftp presentations/poster Glotfelty Kenny.pdf

    work page 2014

  35. [35]

    J., Miller, J., & Chen, J

    Glotfelty, K. J., Miller, J., & Chen, J. 2011, in Astronomical Society of the Pacific Conference Series, Vol. 442, Astronomical Data Analysis Software and Systems XX, ed. I. N. Evans, A. Accomazzi, D. J. Mink, & A. H. Rots, 629

    work page 2011

  36. [36]

    E., Evans, I

    Graessle, D. E., Evans, I. N., Glotfelty, K., et al. 2006, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 6270, Observatory Operations: Strategies, Processes, and Systems, ed. D. R. Silva & R. E. Doxsey, 62701X, doi: 10.1117/12.672876

    work page doi:10.1117/12.672876 2006

  37. [37]

    C., & Loredo, T

    Gregory, P. C., & Loredo, T. J. 1992, ApJ, 398, 146, doi: 10.1086/171844 G¨ uver, T., Bostancı, Z. F., Boztepe, T., et al. 2022, ApJ, 935, 154, doi: 10.3847/1538-4357/ac8106

    work page doi:10.1086/171844 1992

  38. [38]

    2019, in Astronomical Society of the Pacific Conference Series, Vol

    He, H., Cresitello-Dittmar, M., & Glotfelty, K. 2019, in Astronomical Society of the Pacific Conference Series, Vol. 523, Astronomical Data Analysis Software and Systems XXVII, ed. P. J. Teuben, M. W. Pound, B. A. Thomas, & E. M. Warner, 563

    work page 2019

  39. [39]

    Hunter, J. D. 2007, Computing in Science and Engineering, 9, 90, doi: 10.1109/MCSE.2007.55

    work page doi:10.1109/mcse.2007.55 2007

  40. [40]

    J., et al

    HyeongHan, K., Cho, H., Jee, M. J., et al. 2024, ApJ, 962, 100, doi: 10.3847/1538-4357/ad1bcc Ili´ c, D., Raki´ c, N., & Popovi´ c, L.ˇC. 2023, ApJS, 267, 19, doi: 10.3847/1538-4365/acd783

    work page doi:10.3847/1538-4357/ad1bcc 2024

  41. [41]

    H., Cohen, L., Edgar, R

    Jerius, D. H., Cohen, L., Edgar, R. J., et al. 2004, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 5165, X-Ray and Gamma-Ray Instrumentation for Astronomy XIII, ed. K. A. Flanagan & O. H. W. Siegmund, 402–410, doi: 10.1117/12.509378

    work page doi:10.1117/12.509378 2004

  42. [42]

    1999, in Astronomical Society of the Pacific Conference Series, Vol

    Joye, W., & Mandel, E. 1999, in Astronomical Society of the Pacific Conference Series, Vol. 172, Astronomical Data Analysis Software and Systems VIII, ed. D. M

    work page 1999

  43. [43]

    A., & Mandel, E

    Joye, W. A., & Mandel, E. 2003, in Astronomical Society of the Pacific Conference Series, Vol. 295, Astronomical Data Analysis Software and Systems XII, ed. H. E

    work page 2003

  44. [44]

    D., & Ciao Testing Team

    Karovska, M., Evans, J. D., & Ciao Testing Team. 2006, in Astronomical Society of the Pacific Conference Series, Vol. 351, Astronomical Data Analysis Software and Systems XV, ed. C. Gabriel, C. Arviset, D. Ponz, & S. Enrique, 563 Kov´ acs, O. E., Werner, N., Bogd´ an,´A., & de Plaa, J. 2025, A&A, 704, A196, doi: 10.1051/0004-6361/202555575

    work page doi:10.1051/0004-6361/202555575 2006

  45. [45]

    Lee, N. P. 2024, Getting the Most Out of the Chandra Helpdesk for Your Analysis,, Poster presented at the CXC Symposium 2024 https://cxc.cfa.harvard.edu/cdo/ symposium 2024/posters/CXC--HelpDesk--C25.pdf

    work page 2024

  46. [46]

    P., Karovska, M., Galle, E

    Lee, N. P., Karovska, M., Galle, E. C., & Bonaventura, N. R. 2011, in Astronomical Society of the Pacific Conference Series, Vol. 442, Astronomical Data Analysis Software and Systems XX, ed. I. N. Evans, A. Accomazzi, D. J. Mink, & A. H. Rots, 135

    work page 2011

  47. [47]

    M., Gallagher, S

    Leighly, K. M., Gallagher, S. C., Choi, H., et al. 2025, ApJ, 993, 129, doi: 10.3847/1538-4357/ae04df

    work page doi:10.3847/1538-4357/ae04df 2025

  48. [48]

    H., Prigozhin, G

    Li, J., Kastner, J. H., Prigozhin, G. Y., et al. 2004, ApJ, 610, 1204, doi: 10.1086/421866

    work page doi:10.1086/421866 2004

  49. [49]

    McDowell, J. C. 2006, in Astronomical Society of the Pacific Conference Series, Vol. 351, Astronomical Data Analysis Software and Systems XV, ed. C. Gabriel, C. Arviset, D. Ponz, & S. Enrique, 47

    work page 2006

  50. [50]

    2015, in Astronomical Society of the Pacific Conference Series, Vol

    McLaughlin, W. 2015, in Astronomical Society of the Pacific Conference Series, Vol. 495, Astronomical Data Analysis Software an Systems XXIV (ADASS XXIV), ed. A. R. Taylor & E. Rosolowsky, 111

    work page 2015

  51. [51]

    2005, ApJ, 629, 700, doi: 10.1086/431270

    Nicastro, F., Mathur, S., Elvis, M., et al. 2005, ApJ, 629, 700, doi: 10.1086/431270

    work page doi:10.1086/431270 2005

  52. [52]

    2022, A&A, 660, A18, doi: 10.1051/0004-6361/202142000

    Nigro, C., Sitarek, J., Gliwny, P., et al. 2022, A&A, 660, A18, doi: 10.1051/0004-6361/202142000

    work page doi:10.1051/0004-6361/202142000 2022

  53. [53]

    S., & Nowak, M

    Noble, M. S., & Nowak, M. A. 2008, PASP, 120, 821, doi: 10.1086/590324 O’Sullivan, E., Rajpurohit, K., Schellenberger, G., et al. 2024, ApJ, 970, 65, doi: 10.3847/1538-4357/ad4ed6

    work page doi:10.1086/590324 2008

  54. [54]

    P., Bogdan, A., & Marshall, H

    Plucinsky, P. P., Bogdan, A., & Marshall, H. L. 2022, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 12181, Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray, ed. J.-W. A. den Herder, S. Nikzad, & K. Nakazawa, 121816X, doi: 10.1117/12.2630193

    work page doi:10.1117/12.2630193 2022

  55. [55]

    A., & Kashyap, V

    Primini, F. A., & Kashyap, V. L. 2014, ApJ, 796, 24, doi: 10.1088/0004-637X/796/1/24

    work page doi:10.1088/0004-637x/796/1/24 2014

  56. [56]

    A., Houck, J

    Primini, F. A., Houck, J. C., Davis, J. E., et al. 2011, ApJS, 194, 37, doi: 10.1088/0067-0049/194/2/37

    work page doi:10.1088/0067-0049/194/2/37 2011

  57. [57]

    A., Connors, A., Kashyap, V

    Protassov, R., van Dyk, D. A., Connors, A., Kashyap, V. L., & Siemiginowska, A. 2002, ApJ, 571, 545, doi: 10.1086/339856

    work page doi:10.1086/339856 2002

  58. [58]

    L., Doe, S

    Refsdal, B. L., Doe, S. M., Nguyen, D. T., et al. 2009, in Proceedings of the 8th Python in Science Conference, 51

    work page 2009

  59. [59]

    1997, in Statistical Challenges in Modern Astronomy II, ed

    Siemiginowska, A., Elvis, M., Connors, A., et al. 1997, in Statistical Challenges in Modern Astronomy II, ed. G. J. Babu & E. D. Feigelson, 241

    work page 1997

  60. [60]

    M., et al

    Siemiginowska, A., Burke, D., G¨ unther, H. M., et al. 2024, ApJS, 274, 43, doi: 10.3847/1538-4365/ad7bab 20

    work page doi:10.3847/1538-4365/ad7bab 2024

  61. [61]

    2025, Nature Astronomy, 9, 1431, doi: 10.1038/s41550-025-02675-8

    Slane, P., Bogd´ an,´A., & Pooley, D. 2025, Nature Astronomy, 9, 1431, doi: 10.1038/s41550-025-02675-8

    work page doi:10.1038/s41550-025-02675-8 2025

  62. [62]

    2020, in Astronomical Society of the Pacific Conference Series, Vol

    Taghizadeh-Popp, M., Lemson, G., Kim, J.-W., Rippin, M., & Raddick, J. 2020, in Astronomical Society of the Pacific Conference Series, Vol. 522, Astronomical Data Analysis Software and Systems XXVII, ed. P. Ballester, J. Ibsen, M. Solar, & K. Shortridge, 279 van Dyk, D. A., Connors, A., Kashyap, V. L., &

    work page 2020

  63. [63]

    2001, ApJ, 548, 224, doi: 10.1086/318656

    Siemiginowska, A. 2001, ApJ, 548, 224, doi: 10.1086/318656

    work page doi:10.1086/318656 2001

  64. [64]

    C., Brinkman, B., Canizares, C., et al

    Weisskopf, M. C., Brinkman, B., Canizares, C., et al. 2002, PASP, 114, 1, doi: 10.1086/338108

    work page doi:10.1086/338108 2002

  65. [65]

    2019, The Chandra X-ray Observatory; Exploring the high energy universe, doi: 10.1088/2514-3433/ab43dc

    Wilkes, B., & Tucker, W. 2019, The Chandra X-ray Observatory; Exploring the high energy universe, doi: 10.1088/2514-3433/ab43dc

    work page doi:10.1088/2514-3433/ab43dc 2019

  66. [66]

    L., G¨ unther, H

    Wood, M. L., G¨ unther, H. M., Schneider, P. C., & Wolk, S. J. 2025, ApJ, 992, 49, doi: 10.3847/1538-4357/adf96a

    work page doi:10.3847/1538-4357/adf96a 2025