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            • Gemini as the Ultimate Time Domain Follow-up Machine: Understanding the Nearest Cosmic Explosions
            • SPECTRE-GHOST: Spectroscopically Probing Extremely (hot) Climates of TRansiting Exoplanets with GHOST
            • The GHOSTLy quasar sample
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            • Velocity-resolved Echo Mapping with Gemini
            • Deriving Reliable Fundamental Quasar Properties with Gemini Near-Infrared Spectroscopy
            • The First Large Census of Fast Radio Burst Host Galaxies with Gemini
            • Leverage the Past For A Future With High-res Spectroscopic Phase Curves of Hot Jupiters
            • Elemental Abundances via SpectroscopY of Exoplanet-hosting Cool Dwarfs
            • A MAROON-X radial velocity search for planets around the nearest stars
            • A Spectroscopically Complete Census of Faint Transients Observed by the Young Supernova Experiment
            • Roasting Marshmallows: Disentangling Composition & Climate in Hot Jupiter Atmospheres through High-Resolution Thermal Emission Cross-Correlation Spectroscopy
            • Investigating the Activity Drivers of Small Bodies in the Centaur-to-Jupiter-Family Transition
            • Subaru Intensive Program: g-band Imaging for Science with Euclid and UNIONS
            • Exploring the Diversity of Exoplanet Atmospheres at High Spectral Resolution
            • A High-Resolution Survey of Molecular Abundances in Transiting Exoplanet Atmospheres
            • Validation and Characterization of Exoplanets with Gemini High-Resolution Imaging
            • Monitoring Seasonal Reversal in Uranus' Upper Atmosphere
            • Observational Characterization of Recurrently Active Main-Belt Comets and Near-Earth Main-Belt Comet Candidates
            • ZF2K: The First Exploration of the K-Band Window and a Complete Census of Massive Galaxies at 4 < z < 6
            • Chemistry of new metal-poor stars found in the Pristine Survey
            • Validating TESS Exoplanet Candidates
            • Young Star & Protoplanetary Disk Evolution with High- Resolution IR Spectroscopy
            • Placing High-Redshift Quasars in Perspective: a Gemini Near-Infrared Spectroscopic Survey
            • MaDCoWS: The Massive and Distant Clusters of WISE Survey
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            • Addressing a Bias in the Relation Between Galaxies and Their Central Black Holes
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            • Characterizing Dusty Debris in Exoplanetary Systems
            • The First Survey Dedicated to the Detection and Characterization of Clouds in Exoplanet Atmospheres
            • Validating K2’s Habitable and Rocky Planets with AO Imaging
            • A GNIRS Near-IR Spectroscopic Survey of z>5.7 Quasars
            • Probing the dark halo of the Milky Way with GeMS/GSAOI
            • Where Accretion Meets Feedback: A Galaxy Redshift Survey in HST/COS Quasar Fields
            • Rapid Spectroscopy of Elusive Transients and Young Supernovae
            • Spectroscopic Confirmation of Dark Energy Survey Strong Lensing Systems and Spectra for Photometric Redshift Calibration
            • COL-OSSOS: COLours for the Outer Solar System Object Survey
            • The GOGREEN Survey of dense galaxy environments at 1<z<1.5
            • Followup of newly discovered Near-Earth objects from the NEOWISE survey
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Capability

Submitted by Anonymous on June 26, 2020
  • Read more about Capability
jQuery(function() { jQuery( "#lslow" ).click(function() { jQuery("#DivLSlow" ).toggle( "slow", function() { // Animation complete. }); }); }); function showDetailLSlow(objButton) { var x = document.getElementById("DivLSlow"); if (x.style.display === "block") { x.style.display = "none"; } else { x.style.display = "block"; } var elem = document.getElementById("LSlow"); if (elem.value=="Show Details") elem.value = "Hide Details"; else elem.value = "Show Details"; } function showDetailLSm

Spectroscopy

GNIRS has two spectroscopic modes:

Imaging

Observing proposals that involve infrared imaging should request NIRI, not GNIRS. If it is not known whether NIRI will be available, Phase 2 may involve creating observations for both instruments. For instance, GNIRS may be used to perform rapid Target of Opportunity (ToO) imaging programs when NIRI is unavailable. Prospective users should be aware that the Gemini IRAF package contains no dedicated support for GNIRS imaging reductions.

Sensitivity & Throughput

Spectroscopy

The following table provides estimated broadband magnitudes reached at 5 sigma (per spectral pixel) in 1 hour of integration, both without and with adaptive optics (AO).

Guiding Options

GNIRS can be used with the standard Gemini peripheral wavefront sensors, or with the Altair adaptive optics module (in both natural and laser guide star modes).

2020B programs and schedule announced

Submitted by achene on June 25, 2020
  • Read more about 2020B programs and schedule announced

Gemini 2020B observing programs and schedule have been announced. Notification emails were sent to successful PIs on June 25, 2020. Please check the schedules page for more information. Note that the latest version of the Observing Tool is required to access and update 2020B programs.

Experimental design performances (obsolete)

Submitted by Anonymous on June 8, 2020
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We present here measured sensitivity and throughput of GRACES in its experimental phase (phase I). No scientific data were obtained until GRACES was improved, and delivered to Gemini for routine operation. 

Proposal preparation

Submitted by Anonymous on June 8, 2020
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Observing Strategies (Phase I Set-up)

For questions about `Alopeke and/or Zorro, contact the support team. For questions about PIT or the proposal process in general, please file an helpdesk ticket.

Overheads

Acquisition overheads associated with setting up on each new target include time for slewing the telescope, configuring the guiding, and centering the target. These sum to ~5 minutes for most targets.

Every group of speckle targets within 15 degrees and/or every hour must include a point source standard. A photometric standard must be included once/night when doing photometry.

Proposal Preparation

Submitted by Anonymous on June 8, 2020
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Observing Strategies


MAROON-X has only one fixed instrument setting and currently one readout mode (100kHz, 1x1 binning). Observing strategies depend on the science case, i.e. whether general purpose echelle spectroscopy or high-resolution radial velocity observations are desired. The latter will require more careful planning of calibrations, both instrument stability tracking via the simultaneous calibration fiber as well as bracketing etalon exposures during the night.

Phase I Checklist for MAROON-X Proposals

  • Instrument configuration:
    • ​N/A (there is only one mode)
  • Telescope peripheral wavefront sensors:
    • PWFS1 and PWFS2 are used for MAROON-X. PWFS2 is the default.
  • Calibrations:
    • Are the baseline calibrations sufficient? If not, has sufficient observing time been requested for additional calibrations?
    • ​Is accurate removal of telluric lines needed?

Proposal preparation

Submitted by Anonymous on June 8, 2020
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Phase I Checklist

  • Instrument configuration
    • Did you choose the appropriate grating and filter?
  • Guiding configuration
    • Did you choose the appropriate guiding options with NIFS?
  • Observing time
    • Did you confirm the exposure time and S/N using the NIFS Integration Time Calculator?
    • Are

Proposal preparation

Submitted by Anonymous on June 8, 2020
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Understanding PIT

PIT, which is the acronym for Phase I Tool, is the software application that any PI has to use in order to submit a proposal for observing with GNIRS at Gemini North Telescope. In this section we aim to give a brief guideline of how to use efficiently this tool when preparing your proposal. There is a dedicated webpage of Phase I where you can find more detailed information about this first Phase of the proposal preparation.

How to estimate your program time

 At this early stage of the proposal preparation, that is Phase I, you only need to know an estimation of the program time that you will request for your science goals. That time must be set  in the PIT software ("Overview" section, "Time request" tag), as explained in the previous section.

The program time is not only the exposure time for your target, you also have to add other time consuming steps, such as the readout, the setup time, among others. 

Checklist for GNIRS Phase I proposals

In order to minimize the most common errors when creating a new program to observe with GNIRS, the PI is strongly encouraged to consider the following Phase I checklist before submitting the proposal.

  • Target visibility:

          ☐ Is your science object visible during the dates of the semester taken into account the observing time requested and the limits on elevation of the telescope?

Proposal preparation

Submitted by Anonymous on June 8, 2020
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Phase I Checklist

A number of common errors are made by PIs when creating phase I files writing their technical justifications. The PI should consider the following checklist when writing the Phase I proposal.

Proposal preparation

Submitted by Anonymous on June 8, 2020
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Phase I Checklist

  • Instrument configuration:
    • Is the filter (for imaging) and the filter, slit and grating (for spectroscopy) specified in the proposal instrument resource list?
    • Is the grating you need available?
    • Does your choice of slit and grating give appropriate spectral resolution and wavelength coverage?
  • Telescope peripheral wavefront sen

Proposal preparation

Submitted by Anonymous on June 8, 2020
  • Read more about Proposal preparation

Phase I Checklist

A number of common errors are made by PIs when creating phase I files writing their technical justifications. The PI should consider the following checklist when writing the Phase I proposal.

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The International Gemini Observatory  provides the astronomical communities in six participant countries with state-of-the-art astronomical facilities that allocate observing time in proportion to each country's contribution. In addition to financial support, each country also contributes significant scientific and technical resources. The national research agencies that form the Gemini partnership include: the US National Science Foundation (NSF), the Canadian National Research Council (NRC), the Chilean Agencia Nacional de Investigación y Desarrollo (ANID), the Brazilian Ministério da Ciência, Tecnologia e Inovação, the Argentinean Ministerio de Ciencia, Tecnología e Innovación, and the Korea Astronomy and Space Institute (KASI). The observatory is managed by the Association of Universities for Research in Astronomy, Inc. (AURA) under a cooperative agreement with the NSF. The NSF also serves as the executive agency for the international partnership.     


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