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Phase II Checklist

Checklist for FLAMINGOS-2 Phase II (OT) programs

 

GNIRS in the Observing Tool

The GNIRS team strongly recommends that users start from the automatically-generated OT templates and the GNIRS OT library when preparing GNIRS observations. The library contains detailed instructions for customising the template observations: changing targets, standard stars, slit widths, wavelengths, etc. This web page is intended to explain the various OT components in more depth:

Ultra-sharp Image Uncovers the Shocking Lives of Young Stars

Semester 2016B

This page provides instructions for completing Phase II Science Programs for all Gemini North and Gemini South instruments. It includes submission details and notes of any procedural changes. Please read this page carefully!

 


 

2016B Classical Schedule

Semester 2016B

The table below summarises the classically-scheduled programs that have been awarded time on Gemini North and South, as well as programs from the Gemini community awarded Exchange time on Subaru. Jump directly to the schedule for:

Guide Star Selection

The OT will automatically initiate a UCAC4 guide star query and select the brightest allowed guide star(s) in the current wavefront sensor (WFS) patrol field. The allowed WFS patrol field is the union of the patrol fields for all offset positions where the WFS is set to guide (not freeze or park).

2016B OT Released

The 2016B Gemini Observing Tool is now available for download. This update is required to access the Gemini Observing Databases.

The Installation Instructions are linked off of the Observing Tool web page, and we recommend that everyone download their programs from the databases rather than import from saved XMLs.

June Call for Proposals

Gemini North and South are accepting proposals for the Fast Turnaround (FT) program. Here, we give information specific to this proposal cycle. Please see the other FT pages - particularly the rules - for general information about the program. FT-specific proposal templates must now be used for all FT proposals; see the "PIT information" section below.

Resolving an Exoplanet’s Motion to Constrain a Young Planetary System

Figure 1. (Left:) Zoom-in images on HD 95086 b obtained with GPI at the first and last epochs. The magenta crosses show the measured positions (for clarity, the size of the symbol is not representative of the precision). Significant orbital motion is detected within the GPI data. (Right:) Deepest image obtained on HD 95086 with GPI at K1 on April 8, 2015.

Helium’s Role in the Pulsation of Early White Dwarfs

Before low-medium mass stars become white dwarfs they pulsate wildly and eventually spew their outer layers into space – often forming beautiful planetary nebulae. The same stars are predicted to continue pulsating during their transformation to a white dwarf, if they have helium in their atmospheres. A team from the University of Oklahoma used Gemini North, in conjunction with the 1.2-meter FLWO telescope in Arizona, to observe a much-sought-after link between these pulsations and helium in the star’s atmospheres.