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Top > Suzaku > Proposal > AO2 > Announce

September 1, 2006

Announcement of Opportunity (AO-2) of Suzaku

1. Overview

The Japanese-US X-ray Astronomy satellite Suzaku was launched by ISAS/JAXA on 2005 July 10, and has since successfully carried out astronomical observations using the 4 X-ray CCD cameras (XISs) and Hard X-ray Detctor (HXD), although the X-Ray Spectrometer (XRS) is no longer operational. Between 2005 September and 2006 March ("SWG phase" - see below), observations were carried out for instrument calibration and performance verification, which confirm the wide-bandpass, high-sensitivity, moderate spectral resolution capabilities of Suzaku. In 2006 April, we entered the 1-year international AO-1 phase of the mission, performing observations based on proposals received from the astronomical community world-wide. We plan to start AO-2 observations in 2007 April, and hereby invite submission of observing proposals as follows.

US based scientists should consult the parallel announcement at

http://astroe.gsfc.nasa.gov/

while scientists in ESA member countries should consult the version at

http://www.rssd.esa.int/Suzaku

Present version is applicable to scientists based in all other countries.

2. Suzaku observatory

The Suzaku satellite carries four X-Ray Telescopes (XRTs) that focus X-rays up to 12 keV with a high efficiency, each with an XIS unit at its focus. The XIS has a high sensitivity particularly for extended sources, as well as good spectral resolution, for soft X-rays below 0.8 keV, a capability that is superior to those of Chandra and XMM-Newton. At the same time, the HXD, though non-imaging, has unprecedented sensitivity in the wide energy range up to several hundred keV. The wide bandpass coverage with the XIS and the HXD is an important characteristic of the Suzaku mission, so we invite observing proposals that make strong use of their sensitivities. The details of the instruments (Technical Description document), and a list of targets that have been observed or will be observed within the SWG (see below) time and AO-1 can be found at the

http://www.astro.isas.jaxa.jp/suzaku/

We plan to update the Technical Description document, as well as planning tools, with latest information in early October; existing versions should suffice for early planning of proposals, but may not give accurate results when detailed simulations are performed.

3. Mission phases and time allocation

The Suzaku mission has been developed as a Japanese-US collaboration, and the Science Working Group (SWG) that consist of researchers involved in the development and operation oversees the project overall. After the end of the SWG phase of the mission (through 2006 March), normal observations during AO-1 are entirely through open proposal process. Similarly, observing time during international AO-2 (1 year period starting 2007 April) is open. This, however, excludes the following categories.

  1. Observatory Time (4%) for satellite maintainance and related purposes
  2. Calibration time (3%) for routine calibration of instruments
  3. Director's Discretionary Time (5%) for any genuinely unpredictable events including gamma-ray bursts, and other important observations granted at the discretion of the mission director.

The remaining 88% of total time is available to proposers. This will be divided into (1) 50% for Japanese observations; (2) 37.5% for US observations; and (3) 12.5% for joint Japanese-US observations. The joint time will be used if proposals were received for the same target both in Japan and in the US, and if both PIs accept such merging (the proposal form will have a check box for the PI to indicate yes or no). This allocation is based on an ISAS-NASA agreement. Additionally, within the "Japanese" allocation, 8% of the observing time is reserved for proposals submitted to ESA as joint Japan-ESA observations, thus the purely Japanese time is 42%. The total time available to Japan researchers is 4923 ks, plus 1465 ks of joint time, assuming 37 ks of good time per day and 360 days of operation per year. Proposals from non-US, non-ESA countries will be accepted within the Japanese time up to the ESA portion (938 ks).

4. Observing Constraints

Over 200 objects will have been observed with Suzaku during the SWG and AO-1 peirods. A full listing can be found on the web.

http://www.astro.isas.ac.jp/suzaku/accept/

Observations of accepted priority A and B targets are guranteed, while those of priority C targets and Targets of Opportunity (TOOs) are not (see below for definitions of target priorities). Proposals for targets already observed are allowed, but must include a justification for an additional observation, such as a much longer exposure, different pointing within an extended object, or different observing window of a variable object. Proposers with an accepted C or TOO targets must re-propose if they wish to ensure that their observations are carried out (these targets are in principle open to competition). It must be noted that if the C target is observed in AO-1 with more than 70% of proposed time, it will not be observed in AO-2. If not, it will be observed until total time become 70% of proposed time of B proposal, while 90% for A proposal. In these cases, data should be shared by authors of AO-1 and AO-2.

The length of the observation should be justified based on the specific scientific objectives, preferably using simulations. However, we set the minimum observing time at 10 ksec, considering the efficiency of satellite operation. There is no upper limit to for the observing time, but longer observations will naturally require stronger scientific justifications.

It is possible to specify the time of observations (time critical (TC) observations) to observe specific phases or for simultaneous observations. The monitoring observations can be proposed with certain interval. You also able to chose the roll angle of the optical system. In all these cases, you have to put on the TC flag in the application form.

Target of opportunity (TOO) proposals are allowed for short-lived events on known objects whose timing is uncertain. The name and coordinates of the object(s) as well as the triggering conditions must be specified. We also require the estimated probability during AO-2 of such an event, as well as its duration. Generic TOOs without a specific target (such as "a nearby supernova") will not be accepted. The number of targets listed in a reserved TOO proposal should not exceed 5.

Any genuinely unpredictable events may be observed outside the proposal process, as part of the 5% Director's Time. Data from such observations will not have a proprietary period. Please make a contact to us (following e-mail address) for these cases, except for gamma-ray bursts.

Gamma-ray burst TOO observations will be planed by the Suzaku science working group.

5. Review process and schedule

Researchers based in Japan, and non-US, non-ESA countries should submit proposals to ISAS/JAXA. The deadline is 2006 December 1 at noon JST for proposals. All proposals from Japan and other countries will be reviewed in the same process in Japan. After the review in Japan together with the ESA proposals, a Japan-US merging committee will be convened in February, and the final observing program will be published soon thereafter.

Accepted proposal will be classified into three categories. Priority A targets will be preferentially observed during the AO-2 period (2007 Apr to 2008 Mar). Priority B targets will be scheduled in this period as far as possible, but may be carried over to the following AOs. Priority C targets will be used as fillers when there are gaps in the schedule. For the total available time T, we will accept 0.5T, 0.4T, and 0.5T as As, Bs, and Cs (for a total oversubscription by 40%). If the actual amounts of observatory, calibration, and director's times add up to less than 12% that is set aside, then the remainder will be used to observe additional C targets.

TOOs and time critical observations will be accepted only as priority A targets.

6. Data rights

Observers will have exclusive rights to the data for a 1 year period after receipt of data, after processing. This, however, does not apply to real time TOO observations and for Gamma-ray burst data. We will deem an observation complete if 90% (for A targets) or 70% (for B targets) of the proposed time is obtained.


Proposal Submission

1. Observations

X-ray observations with Suzaku observatory from April 2007 through March 2008.

2. Who may propose

Principal investigators (PI's) have to be affiliated with institutions and universities located in Japan and other countries than USA or ESA member states. PI's at USA institutions and those in ESA member states should submit to NASA or ESA, respectively. PI's in other countries should send proposals to ISAS/JAXA Japan.

3. Due date of proposals

12:00 JST (03:00 UT) on December 1, 2006. Printed material should be mailed with stamps dated on the day in Japan.

4. Proposal format

Following two materials are both necessary.
(1) RPS(Remote Proposal Submission system) submission : Note that the observation parameters in the electrical form should be accurate because they will be forwarded on-line to the satellite operation system.
(2) 7 sets of hard copy of the proposal has to be submitted to the following address,

Kazuhisa Mitsuda
Institute of Space and Astronautical Science
Japan Aerospace Exploration Agency
3-1-1, Yoshinodai, Sagamihara
Kanagawa,229-8510
Japan

The proposal form consists of
(1) Cover Page (1 page),
(2) General Form (1 page),
(3) Target Forms (1 page),
(4) Target Constraints (1 page),
(5) Target Remarks (1 page),
(6) Scientific Justification (scientific problem and technical feasibility) (maximum 4 pages; includes text, figures, charts, and tables).

5. Supplement Information

For the detail, mission description, especially technical description is available at the web page

http://www.astro.isas.jaxa.jp/suzaku/

We plan to update the Technical Description document, as well as planning tools, with latest information in early October; existing versions should suffice for early planning of proposals, but may not give accurate results when detailed simulations are performed.

If you have questions, please contact to

Institute of Astronautical Science/Japan Aerospace Exploration Agency
Kazuhisa Mitsuda, Tadayuki Takahashi and Hideyo Kunieda


ISAS/JAXA Department of High Energy Astrophysics

Last Modified: Friday, 01-Sep-2006 23:06:56 JST