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  • Instruments:
    • Chandra LETG + ACIS-S / HRC-S
    • XMM  EPIC-pn SW
    • SWIFT
    • Astrosat SXT
    • NICER
    • Hitomi
    • XRISM (new)
    • Einstein Probe FXT (new)
    • SVOM-MXT (Launch June 2024)
  • eROSITA calibration observations
    • 2019 09 13  80ksec to be done
    • 2019 09 24  80ksec to be done
    • 10 24  78 ksec
    • 2020 04 02  36 ksec
    • 2020 10 07  61 ksec2020 03 11 - 04 22  80ksec after survey #1
  • Chandra LETGS+HRC-S observations
    •  500ks OBS_IDs: 00113  03380  03381  03382  03399

    • 120ks  OBS_IDs: 14418  15293

    • 172ks  OBS_IDs: 21693 21896 (will be obvserved in the context of eROSITA calibration) 22282 22283 22284

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  • Chandra LETG + ACIS-S

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  • Models

RX J1856.5-3754 based on the CHANDRA LETGS + HRCS Data

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  • Missions
    EUVE, ROSAT, Chandra, XMM-Newton, Astrosat SXT
  • Data
    • Chandra
      • HZ 43

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      • Sirius B
      • GD 153
  • Results
    see papers

HZ43 Fitting Function

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Here the temperature of ~0.013 keV is the best-fit temperature using this fitting function, and does not represent the true white dwarf temperature.  The norm of ~0.039 is the best-fit norm, and again is physically meaningless other than as a fitting coefficient.  Using this model results in the following curve in the photon spectrum.  Solid is the Beuermann et al curve and dashed is the model.  The residual panel below demonstrates that the worst-case error in this fitting function approximation is 1%.

 

 

 

 




Papers

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Attachments:

Attachments