Chapter 1 | Chapter 2 | Chapter 3 | Chapter 4 | Chapter 5
Chapter 6 | Chapter 7 | Chapter 8 | Chapter 9
Appendix A | Appendix B
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Chapter 3
Offset Pointing, Visibility, and other Constraints

3.1  Introduction

This chapter gathers together several topics pertaining to observation planning, irrespective of focal-plane instrument and grating configuration, to serve as additional guidelines for the preparation of proposals. Many of these topics are automatically addressed by the target visibility interface webtool (ProVis; https://cxc.harvard.edu/cgi-bin/provis/provis_load.cgi) or the observation visualizer software (ObsVis; https://cxc.harvard.edu/obsvis/) available as part of the Chandra  Interactive Analysis of Observations (CIAO) software. The intention here is to familiarize the user with these various observation-planning topics.

3.2  Offset Pointing

The offset pointing convention for Chandra is that a negative offset of a coordinate moves the image to more positive values of the coordinate and vice-versa. Examples of offset pointings of the ACIS instrument are shown in Figure 3.1. Examples using the HRC are shown in Figures 3.2 and 3.3.
./images/ACISv4-1.png ./images/ACISv4-2.png
./images/ACISv4-3.png ./images/ACISv4-4.png
Figure 3.1: Image (1°x 1°) created with ObsVis shows the ACIS field-of-view overlaid on the optical image of the galaxy NGC 891. North is up and east is to the left. Roll is measured positive, west of north. The roll angle (the angle between celestial north and the spacecraft -Z axis projected on the sky, as measured from N through W) shown is 100°. Five chips are turned on (solid outlines, with dashed node boundaries shown) and five off (dashed chip outlines). The circle-in-a-square symbol shows the aimpoint. Upper left panel: Target is centered at the nominal ACIS-S aimpoint. The (dY,dZ) coordinate system used to define pointing offsets is also shown (refer to Figure 1.1 for a general view of Chandra spacecraft coordinates), as well as the SIM Z motion direction used to define the location of the aimpoint on the detector (see Figure 1.2). In the case shown, (dY,dZ)=(0,0). Upper right panel: The target has been offset by 1.5 arcmin in the negative Y direction, i.e., a (dY,dZ) target offset of (-1.5 arcmin, 0). Lower left panel: The target has been offset by 3 arcmin in the negative Z direction, i.e., (dY,dZ)=(0, -3 arcmin). Lower right panel: No target offset has been applied, i.e., (dY,dZ)=(0,0), but a SIM Z motion of +3 arcmin has been applied. Note that in the latter two cases (lower left and lower right) the target is in the same place on the detector, but in the lower right case the aimpoint moves with the target, keeping the target near the optical axis and the aimpoint for optimal imaging quality.
./images/HRCIv3-1.png ./images/HRCIv3-2.png
./images/HRCIv3-3.png ./images/HRCIv3-4.png
Figure 3.2: Offset pointing with HRC-I on a 2°x 2°image of NGC 891; orientation and roll angle are the same as in Figure 3.1. Upper left panel: Target is centered at the nominal HRC-I aimpoint. The (dY,dZ) coordinate system used to define pointing offsets is also shown, as well as the SIM Z motion direction used to define the location of the aimpoint on the detector. Upper right panel: The target has been offset by 5 arcmin in the negative Y direction, i.e., a (dY,dZ) target offset of (-5 arcmin, 0). Lower left panel: The target has been offset by 5 arcmin in the negative Z direction, i.e., (dY,dZ)=(0, -5 arcmin). Lower right panel: No target offset has been applied, i.e., (dY,dZ)=(0,0), but a SIM z motion of +5 arcmin has been applied. Note that in the latter two cases (lower left and lower right) the target is in the same place on the detector, but in the latter case the aimpoint moves with the target.
./images/HRCSv3-1.png ./images/HRCSv3-2.png
./images/HRCSv3-3.png ./images/HRCSv3-4.png
Figure 3.3: Offset pointing with HRC-S on a 2°x 2°image of NGC 891; orientation and roll angle are the same as in Figure 3.1. Upper left panel: Target is centered at the nominal HRC-S aimpoint. The (dY,dZ) coordinate system used to define pointing offsets is also shown, as well as the SIM Z motion direction used to define the location of the aimpoint on the detector. Upper right panel: The target has been offset by 5 arcmin in the negative Y direction, i.e., a (dY,dZ) target offset of (-5 arcmin, 0). Lower left panel: The target has been offset by 5 arcmin in the negative Z direction, i.e., (dY,dZ)=(0, -5 arcmin). Lower right panel: No target offset has been applied, i.e., (dY,dZ)=(0,0), but a SIM z motion of +5 arcmin has been applied. Note that in the latter two cases (lower left and lower right) the target is in the same place on the detector, but in the latter case the aimpoint moves with the target. Note also that, as shown in the lower two panels, it is quite possible to use offsets to move the target position entirely off a detector.

3.3  Visibility

There are a number of factors that limit when observations can be performed. These are discussed in the following subsections.

3.3.1  Radiation Belt Passages

High particle-radiation levels are encountered as the Observatory approaches perigee. Data acquisition ceases whenever certain particle-radiation thresholds are exceeded. A working number for the altitude at which this takes place is about 60,000 km. Cessation of observations and protection of the instruments in regions of high radiation results in approximately 25% of the 63.5 hour Chandra orbit being unusable.

3.3.2  Avoidances

The following constraints are necessary to ensure the health and safety of the spacecraft and science instruments. Proposals which violate these constraints may be rejected.
  1. Sun avoidance - cannot be overridden - viewing is restricted to angles larger than 46.4 deg from the center of the Sun. This restriction makes about 15% of the sky inaccessible on any given date, but no part of the sky is ever inaccessible for more than 3 months.
  2. Moon avoidance - viewing is restricted to angles larger than 6 deg from the limb of the Moon. This restriction makes less than 1% of the sky inaccessible at any time. This avoidance can be waived, but at the price of a reduced-accuracy aspect solution (see Chapter 5).
  3. Bright Earth avoidance - viewing is restricted to angles larger than 10 deg from the limb of the bright Earth. This restriction makes less than 5% of the sky inaccessible at any time, but there are certain regions which can only be viewed, continuously, for up to about 30 ks. The avoidance can be waived, but at the price of a reduced-accuracy aspect solution (see Chapter 5). Figure 3.4 illustrates the point that the Earth avoidance region is nearly stationary. This is a consequence of the combination of high elliptical orbit and radiation belt passages. This partially blocked region moves several deg per year, reflecting the evolution of the orbital elements.
    The greatest amount of observing time is available in the vicinity of apogee, when the satellite moves most slowly and the Earth and its avoidance zone occupy an approximately stationary location on the sky, visible in Figure 3.4 as the extension to the south of the Sun avoidance band.
  4. Roll angles - the spacecraft and instruments were designed to take advantage of the Observatory having a hot and a cold side. Thus, the spacecraft is preferentially oriented with the Sun on the −Z side of the X−Y plane, where +X is in the viewing direction, the Y-axis is parallel to the solar panel axes, and +Z is in the direction of the ACIS radiator (see Figure 1.1). In this orientation there is only one "roll angle" (rotation about the viewing- or X-axis - positive West of North) for which the solar panels can be rotated so that they are directly viewing the Sun - the nominal roll angle. Small deviations ( ∼ deg) from the nominal roll angle may be allowed depending on the viewing geometry. The roll-angle constraint imposes further visibility restrictions. These can also be evaluated with the ProVis tool.
./images/cycle26_vislite_7090.png
Figure 3.4: The Chandra visibility showing contours of fractional visibility averaged over the 12-month interval of Cycle 26. The darker the shade of gray, the lower the visibility. The three contour levels correspond to 70%, 80%, and 90% average visibility.

3.3.3  Thermal Constraints

As the spacecraft has aged, its thermal properties have gradually changed. Degradation of its reflective multilayer insulation means that the Sun-facing side of the satellite now heats more rapidly, and the spacecraft as a whole operates at higher temperatures than earlier in the mission. Steps have been taken to reduce internal sources of heating. However, the thermal limits of the various spacecraft subsystems are an increasingly important factor in planning operations.
The solar pitch angle (i.e., the angle between the viewing direction and the direction to the Sun) affects which subsystems heat or cool during any given observation. Figure 3.5 shows the solar pitch sensitivity of various spacecraft components. Restrictions on the operating temperatures of these components limit how long the spacecraft can maintain a given pitch angle, and it is often necessary to plan operations such that components heated during one observation can cool during (or in some cases before) the next. The thermal restrictions on the various subsystems evolve with time and are too complex to describe here in detail, but some of their impacts on observations are of direct interest to observers:
  1. Observations are possible across the full range of allowed solar pitch angles (46.4 to 178 degrees). However, balancing the thermal load across the whole spacecraft usually requires the breaking up of long observations into shorter exposures. The maximum continuous exposure depends on the solar pitch angle of the target, the instruments used, and the thermal history of the spacecraft. As of late 2022, observations are usually broken up into segments of duration ≤ 30ks for planning purposes, and these segments may be scheduled with significant periods of time separating them. It is expected that segments will be shorter as the spacecraft continues to age.
  2. The ACIS focal plane and electronics subsystems are particularly sensitive to heating at high solar pitch angles. The duration of ACIS exposures is limited to ensure that the instrument remains within its required operating temperature range. Observations which use fewer CCDs cause less heating. In Cycle 26, ACIS observers will be able to specify a maximum of 4 required chips; additional chips beyond those marked as required may be specified as optional, along with the order in which these may be turned off; this information will be used as needed during the mission planning process to control ACIS temperatures (see Section 6.22.1)
  3. The duration of HRC exposures is currently limited to 14.5ks, in order to meet new operational constraints on the temperature of the instrument electronics (see Section 7.12 for further details). This maximum duration may be reduced depending on external factors such as target pointing direction and may be subject to further review. Longer HRC observations will be broken into segments up to 14.5 ks in duration and scheduled with a minimum of 30 ks separating the segments. The required cooling time between segments means that including more than 2 HRC exposures in an orbit can be difficult, and no more than 4 will be scheduled.
  4. The increased operating temperature of the ACA has affected its ability to acquire faint guide stars. This can restrict observations of targets with difficult star fields to particular times of year since, if sufficiently bright guide stars occur only at the edges of the ACA field of view, they may only be visible at a limited range of roll angles. In future, some target fields may be unobservable owing to a lack of sufficiently bright guide stars.
  5. Simultaneous longer-duration observations with telescopes that have a limited range of accessible solar pitch angles such as the X-ray Multi-Mirror Mission (XMM; approximately 70-110 deg) may be difficult, or even impossible, to schedule.
Targets whose solar pitch angle varies through the year will generally be scheduled at times where these sensitivities are least restrictive. Targets for which the available solar pitch angles are always unfavorable may be broken up into smaller segments so as not to exceed the maximum dwell times for those pitch ranges. The specific impact of the various solar pitch angle sensitivities (Figure 3.5) on an observation's visibility and, therefore, scheduling difficulty is encapsulated by the resource cost of a given observation (see Section 4.3 of the Call for Proposals). Proposers concerned about resource cost and/or scheduling difficulty should contact the CXC HelpDesk (https://cxc.harvard.edu/helpdesk/) prior to submission.
images/timbre_protractor_plot_aphelion_2024.png
Figure 3.5: Illustration of the thermal impact of solar pitch angle on various spacecraft components with ACIS at the focus. Pale red arcs indicate pitch ranges in which it is more difficult to maintain the component within its thermal restrictions, gray arcs show where components are thermally neutral, and pale blue arcs indicate pitch ranges in which components can recover from time spent in thermally limited pitch regions. Dark red arcs indicate where a component represents the most limiting dwell time restriction at a given pitch angle; the MUPS at low pitch angles, ACA at mid-pitch, ACIS at high pitch, and the propulsion lines at the highest pitch angles. The HRC heats at all pitches while switched on, and only cools efficiently in a limited range of pitches while switched off. Note that the diagram represents the predicted status during 2024 with ACIS at the focus; thermal constraints will change over time so it should not be used as a guide for planning specific observations. For detailed inquiries regarding pitch sensitivity, please contact the CXC HelpDesk (https://cxc.harvard.edu/helpdesk/).

3.4  Other Instrument and Observation Considerations

Science instrument restrictions and limitations are discussed in the chapters devoted specifically to the instruments. User-imposed constraints are discussed in the instructions for the Chandra Proposal System (CPS). We summarize these here.

3.4.1  Instrument Considerations

For details on the following considerations that may be important in the planning of observations, please refer to Chapters 6 (for ACIS) and 7 (for HRC). (Note that we refer to restrictions when degradation of instrument capabilities may result, and to limitations when the science objectives of an observation may be jeopardized.)

3.4.2  User-Imposed Constraints

Chandra users may need to specify a number of observing constraints particular to their observations. In general, the specification of a user-imposed constraint decreases the efficiency of the observatory and therefore should be well justified in the proposal. Note that only a limited number of constrained observations can be accommodated (see the CfP for details). User imposed constraints are summarized here.
Time Constraints:
Time Windows - specific time intervals in which an observation must be scheduled. Such constraints are primarily for use in coordinated observing campaigns or for arranging an observation to coincide with some time-critical aspect of the target.
Monitoring Intervals - for observing a target repeatedly, with intervals and durations specified.
Phase Interval - specific phase intervals for observing sources with long, regular periods.
Unique Phase (split observations) - specifying that unique parts of the phase need to be covered if the observation is split.
Coordinated Observations - targets specified to be observed by Chandra and another observatory within a given time period.
Continuity of observation - specifying that an observation be performed in a single (or the fewest possible) segment(s).
Completion Time (split observations) - specifying relative time frame within which all the segments of a split observation must be completed.
Group Observation - a target which needs to be observed within a particular time range with other targets in the program.
Roll Constraints - specifying a particular roll angle and tolerance.
Roll-dependent Pointing - an observation for which the target coordinates and/or offsets require adjustment based on roll angle.
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