The table below summarizes the Gemini North queue programs and their execution status. This page is updated once per day.
The columns in the table are:
Ref # Gemini reference number (note that this is different from any internal National TAC reference number). Click on it to see the proposal abstract (when available).
PI Name of Principal Investigator. (If a joint proposal, the name of the primary contact for the entire program is listed).
Partner Participant (AR, BR, CA, CL, KR, UH, US) to which time will be charged. If a joint proposal, all contributors are shown.
Title The title of the science program.
Instrument Name of the instrument(s) required.
Hours Allocated Time allocated to the program (if a joint proposal, this is the total time for the program). Semesters shown in square brackets e.g. [22B] indicate that the program can be carried over to the specified semester.
Execution Status Click on this hyperlink to see the current status of each observation in the program.
Data Taken The UT date(s) on which data were taken.
Completion Status This shows an estimate of the fraction of allocated time that has been used. Note that this is a preliminary estimate and is only an indication of the completion state of the program. The completion state may not reflect the formal time accounting. Also note that some programs may be completed in less than the allocated time (e.g. if conditions were better than requested or if the request was overestimated).
The assigned support staff (Gemini Contact Scientists and National Office staff) for each Gemini North ODB and Gemini South ODB program are listed in the interactive 'snapshots' of the Observing Database (ODB).
|GN Poor Weather Queue|
|GN-2022B-Q-401||Wang||GS||Investigating AGN Size-Luminosity Relation with Uniquely Selected High Luminosity Quasars||GMOS||4.00|
|GN-2022B-Q-402||Seccull||GS||A Search for Fainter Solar Calibrators||GMOS / GMOS-S||61.40|
|GN-2022B-Q-403||Tanaka||GS||NIR spectroscopy of chemically peculiar stars toward identification of lanthanide elements in kilonova spectra||GNIRS||1.90|