Planned Observation Schedule on PSR 1259-63 by the H.E.S.S. experiment in March, 2004

ATel #250; M. Beilicke, Universitaet Hamburg; M. Ouchrif, Laboratoire de Physique Nucleaire de Haute Energie, Universite Paris VI and VII; G. Rowell, Max-Planck-Institut fuer Kernphysik; and S. Schlenker, Humboldt-Universitaet, Berlin; on behalf of the H. E.S. S. (High Energy Stereoscopic System) Collaboration
on 13 Mar 2004; 18:28 UT
Credential Certification: Michael Punch (punch@in2p3.fr)

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Further to our preceding telegram (ATEL #249) on the discovery of very-high-energy gamma-ray emission from the binary millisecond pulsar PSR 1259-63 by the H.E.S.S. experiment above a threshold of about 200 GeV, we present here our planned programme for observations for March, 2004, in order to facilitate simultaneous observations. Periastron passage of the pulsar was expected on Mar. 7.43 UT, and the pulsar is now leaving periastron. It will traverse the the inclined Be disk for the second time on Mar. 20-25, and phenomona on time-scales of hours or days may be expected preceding and during this phase. Simultaneous or quasi-simultaneous observations in other wavelengths are important for understanding of the source. The next periastron passage will not take place for another 3.4 years.

Our planned observing schedule on this source in the coming days is:

• Mar. 14.90-14.97
• Mar. 15.90-16.01
• Mar. 16.90-17.06
• Mar. 17.90-18.09
• Mar. 18.90-19.09

For the following nights, the times below are planned:

• Mar. 20.00-20.09
• Mar. 21.00-21.09
• Mar. 22.00-22.09
• Mar. 23.00-23.09

These nights' times may be modified to begin 0.1 day earlier if the preliminary analysis of the preceding nights' data shows a high flaring state.

Observations on subsequent nights will be determined by the preliminary results of the preceding nights of this period, and may be the object of a further follow-up telegram. Observations in this dark-moon period may continue up to Mar. 27 (as a multiwavelength campaign on another source will preclude further observations).

An INTEGRAL Target of Opportunity observation has been obtained on this source. Observations in other wavelengths (radio, X-ray) are strongly encouraged.

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