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Last modified: 03/20/18

CXC/ACIS Operations

Welcome to our home page. ACIS, the Advanced CCD Imaging Spectrometer, is an instrument built by a team of scientists and engineers from the Massachusetts Institute of Technology's Center for Space Research and the Pennsylvania State University for the Chandra X-Ray Observatory. ACIS shares the Chandra focal plane with the High Resolution Camera. However, what you will find here is contact information and other resources relevant to the Chandra X-ray Observatory Center (CXC) ACIS Operations team members.

ACIS Operations Scientist On-Duty Schedule

Please consult the following table to determine the ACIS Operations scientist on-duty to contact for mission planning purposes or spacecraft emergencies:


Week Of Scientist Work Cell
Mar 19 - Mar 23 Paul Plucinsky 6-7726 617-721-4366
Mar 24 - Mar 24 Richard Edgar 5-7249 617-866-8615
Mar 25 - Mar 25 John ZuHone 6-1816 781-708-5004
Mar 26 - Mar 31 John ZuHone 6-1816 781-708-5004
Apr 1 - Apr 1 Paul Plucinsky 6-7726 617-721-4366
Apr 2 - Apr 8 Gregg Germain 6-1558 617-785-0976
Apr 9 - Apr 15 Richard Edgar 5-7249 617-866-8615
Apr 16 - Apr 21 John ZuHone 6-1816 781-708-5004
Apr 22 - Apr 22 Paul Plucinsky 6-7726 617-721-4366
Apr 23 - Apr 29 Catherine Grant 253-0797 617-584-2686
Apr 30 - May 6 Gregg Germain 6-1558 617-785-0976
May 7 - May 12 Richard Edgar 5-7249 617-866-8615
May 13 - May 13 Paul Plucinsky 6-7726 617-721-4366
May 14 - May 20 John ZuHone 6-1816 781-708-5004
May 21 - May 27 Catherine Grant 253-0797 617-584-2686
May 28 - Jun 3 Paul Plucinsky 6-7726 617-721-4366

Contact and Leave Information

Operations Memos, Documents and Links

Non-Load Event Tracking

ACIS Thermal Models

ACIS Procedures


ACIS Orbital Fluence

Real-Time Telemetry Links

Current MP Schedules


Shift Reports

Related ACIS and Chandra Web Sites:

Solar Cycle Info
Solar Cycle data and predictions

    Above: This image, courtesy of Dr. Judith Lean at the US Naval Research Laboratory, shows three extreme ultraviolet (EUV) pictures of the Sun captured by the ESA/NASA Solar and Heliospheric Observatory at different times during the current solar cycle. In 1996, near solar minimum, the EUV Sun was nearly featureless. Now, near the peak of the cycle, the Sun is dotted by fiery regions of hot gas trapped in magnetic fields above sunspots and plages. These active regions produce copious numbers of EUV and X-ray photons that are absorbed in outer layers of our atmosphere before they reach Earth's surface. The red curve in the image is a computer model of the solar EUV flux at 304 Angstroms derived from ground-based Ca K images made at the Big Bear Solar Observatory.

    Above: By combining data about geomagnetic activity during the previous solar cycle with sunspot counts for the current cycle, David Hathaway and collaborators are able to predict when the next sunspot maximum will occur. [Click here for details]. According to their results, the sunspot number will peak beginning in mid-2000. The dotted lines above and below the solid curve line indicate the prediction curve's range of error. The vertical bars indicate the full range of daily sunspot numbers that were averaged to obtain monthly data points. Large excursions, like the one on April 2 when the daily Boulder sunspot number reached 301, are not uncommon.

  • Sunspot Cycle Prediction
  • Solar Radio Monitoring Programme
  • 10.7cm Radio Flux Prediction

Spacecraft Constants
Standard Dither Pattern
Web Page Maintained by:
Gregg Germain, Paul Plucinsky, Richard Edgar, & Royce Buehler
(Please feel free to send us any comments or suggestions!)

The Chandra X-Ray Center (CXC) is operated for NASA by the Smithsonian Astrophysical Observatory.
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