Near-IR Wavefront Sensor - Planning Observations

If you want to use the AO3k/NIRWFS, you need to find a Natural Guide Star (NGS) that is bright enough at less than 14" separation from your target of interest. The target of interest can be the NGS itself if it is a bright enough stellar object. Non-sidereal tracking is currently not available with NIRWFS.

Read the following instructions carefully if you wish to apply for observing time with AO188. If technical details described in your proposal are incomplete, it may be rejected even if your science case is great.

• 1. Information you have to describe in your proposal
• 2. Selecting AO guide stars
• 3. Planning dates of observations
• 4. Overheads

1. Information you have to describe in your proposal

The following should be clearly stated in the proposal.

• H-band (or J-band if the Vis-HK Dichroic is used) magnitude of your AO guide stars (see section 2 for details).
• One or several choices for the dichroic beamsplitter used, depending on the brightness of the NGs (see section 2 for details).
• Separation between your targets and AO guide stars (see section 2 for details).
• Strehl ratio and/or FWHM of the point-spread function (PSF) required for your project.
• Whether the AO guide star is a point source or not. If you use an extended object, or a binary object, you must discribe the geometry of the source (size for extended objects, separation and contrast for binaries) (see section 2 for details).
• Schedule requirement to avoid the moon's glare which severely degrades the AO loop performance (see section 3 for details).
• Other usual requirements for the science instrument used (IRCS, SCExAO). Please check their respective webpages

2. Selecting AO guide stars

Throughput and Dichoic Choice

NIRWFS Dichroic transmission to the science instrument.

Transmission to the science instrument for the L-band dichroic.

Magnitude Limits

The values presented here were measured with the first design of the NIRWFS (hight-resolution or HR mode), and interpolated to include the optical binning (Low-resolution or LR) mode.

Guide star magnitude limit. The frequencies listed in the legend are the AO loop frequency. Correction at 500 Hz might be worst than at 1 kHz depending on the atmospheric conditions (seeing, coherence time). High-resolution modes (HR) were measured on-sky, and low-resolution modes (LR) were extrapolated from that.

Separation for off-axis NGS

If the science target is too faint, then you need to select a bright NGS that is no more than 14" away from it. This limitation is due to the capture field-of-view of the NIRWFS (See Performance for more details).

Extended objects and binaries

The pyramid WFS design is not ideal for extended objects and binaries. If the source is too extended (more than a few arcseconds), the loop cannot close. For smaller objects, we can close the loop, but with degraded performances. For binaries, results can vary depending on the separation and H-band contrast between the two stars. For separations below 2", a low-contrast binary will be difficult to observe, due to the added light of the companion inside the wavefront sensor. A field stop can be used for larger separations.

3. Planning dates of observations

• Elevation --- We recommend you to observe targets at an elevation of 45^o or larger. Strehl ratios and/or FWHMs can significantly be degraded at lower elevations. Please not that the atmospheric dispersion corrector (ADC) installed at the science path, or the wavefront sensor do not guarantee good correction for elevations below 30^o.
• Distance to the moon --- We cannot perform AO correction if the sky is very bright. We then recommend you to observe the target at least 10^o apart from the moon.

4. Overheads