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This page is maintained by GB, CK, SL and the GISMO team This page is maintained by IH, CK, SL and the GISMO team
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|| || Pixels || '''Wavelength''' || '''Bandwidth''' || '''Sensitivity''' || '''HPBW''' || '''Field-of-View''' || '''Spacing''' ||
||         || || mm || '''[GHz]''' || '''[mJy sqrt(s)''' || || || ||
||GISMO    || 8x16 || 2      || 140-162         || 10 || 16.7" || 1.8'x3.7' || 13.75" ||		 || || '''Pixels''' || '''Wavelength''' || '''Bandwidth (FWHM)''' || '''Sensitivity (out of atmosphere)''' || '''HPBW''' || '''Field-of-View''' || '''Spacing''' ||
||GISMO since 2012 || 8x16 || 2.0 mm || 140-162 GHz || 14 mJy*s^1/2^ || 16.7" || 1.8' x 3.7' || 13.75" ||
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The Goddard-IRAM Superconducting 2mm Observer (GISMO) is a bolometer camera for the IRAM 30m telescope. It has been build by Goddard Space Flight Center, in Greenbelt, Maryland under the lead of Johannes Staguhn. GISMO consists of '''8x16 pixels''' with super conducting transition edge sensors (TES). The TES are read out by time domain SQUID multiplexers built at the National Institute for Standards (NIST), in Boulder, Colorado. The nominal bandwidth is 140-162 GHz (FWHM), pixels are spaced by '''13.75"''', the telescope HPBW is '''16.7"'''. The sensitivity has improved relative to the April 2011 run to about '''10 mJy sqrt(sec)''' (cf. report below). The field-of-view is ''' 1.8'x3.7' '''. Two standard observing modes are offered, Lissajous curves and on-the-fly scans. Both work in total power, without switching the secondary. An automated pipeline merges the GISMO data with the telescope data streams to create FITS files which are automatically processed by the reduction software crush to create logs, pointing results, and a first quick view of the data. Typical overheads for single science targets on the sky are 60%. The relative flux stability is about 8% (cf. report below). The Goddard-IRAM Superconducting 2mm Observer (GISMO) is a bolometer camera for the IRAM 30m telescope. It has been build by Goddard Space Flight Center, in Greenbelt, Maryland under the lead of Johannes Staguhn. GISMO consists of '''8x16 pixels''' with super conducting transition edge sensors (TES). The TES are read out by time domain SQUID multiplexers built at the National Institute for Standards (NIST), in Boulder, Colorado. The nominal bandwidth is 140-162 GHz (FWHM), pixels are spaced by '''13.75"''', the telescope HPBW is '''16.7"'''. The sensitivity has improved relative to the April 2011 run to a media value of about '''14 mJy sqrt(sec)''' (cf. reports below). The field-of-view is ''' 1.8'x3.7' '''. Two standard observing modes are offered, Lissajous curves and on-the-fly scans. Both work in total power, without switching the secondary. An automated pipeline merges the GISMO data with the telescope data streams to create FITS files which are automatically processed by the reduction software crush to create logs, pointing results, and a first quick view of the data. Typical overheads for single science targets on the sky are 60%. The relative flux stability is about 8% (cf. report below).
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== Call for proposals for the summer semester 2013 == == Call for proposals for the winter semester 2013/14 ==
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 * [[attachment:TimeEstimator_v2.pdf|Updated guidelines to estimate observing times (Billot et al. 2012)]].  * [[attachment:TimeEstimator_v3.pdf|Updated guidelines to estimate observing times (Billot et al. 2013)]].
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 * [[attachment:3rdGISMOpool_public_final.pdf|Report on GISMO performance based on the pool run in April-2013 (Hermelo et al. 2013)]].
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 * [[attachment:GISMOSoftwareOperationalManual_02nov2012.pdf|GISMO Software Operational Manual]] by Steve Maher and Johannes Staguhn, October 2012  * [[attachment:GISMO Software Operational Manual - May 2013]] by Steve Maher and Johannes Staguhn, May 2013
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== Observations ==


=== pako scripts ===

 * GismoObservingScripts provides examples and explanations about how to start !PaKo in order to run the telescope with GISMO, and about total power maps using Lissajous and On-the-fly patterns. Observations using the wobbler will not be offered for this run. The old page GismoHowToObserve is obsolete.

 * [[https://www.iram.es/IRAMES/mainWiki/GismoPakoNotes|Notes on paKo and NCS for GISMO 2012]]

=== Pointing Sources ===

[[http://www.iram.es/IRAMES/FluxMonitoring/PointingSources/plotPointingSources.html|Plots for Pointing Sources]] can be accessed within the IRAM network. These data are provided ONLY to help in the planning of observations, in particular to select pointing and focus sources at the IRAM 30-m telescope. They should not be used for any other purpose.


=== crush data reduction ===

 * CrushExamples
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=== April 2013 - 3rd pool run ===
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=== October 2013 - 4th pool run ===
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 * Winter semester 2012 observations will be carried out as pooled observations from a dedicated pool account. M.Gonzalez will provide login information.  * Summer semester 2013 observations will be carried out as pooled observations from a dedicated pool account. I. Hermelo will provide login information.
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 * [[http://www.iram.fr/php/rel_sched/bgfiles/13/Bolopool-w12.html|List of accepted projects.]]  * [[http://www.iram.fr/php/rel_sched/bgfiles/13/Bolopool-s13.html|List of accepted projects (Not yet available).]]
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 * Progress of observations can be followed via the [[https://herapool.iram.es|pool data base]].  * Progress of observations can be followed via the [[https://pools.iram.es|pool data base]]. 
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==== Observing scripts ==== === April 2013 - 3rd pool run ===
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 * GismoObservingScripts provides examples and explanations about how to start !PaKo in order to run the telescope with GISMO, and about total power maps using Lissajous and On-the-fly patterns. Observations using the wobbler will not be offered for this run. The old page GismoHowToObserve is obsolete. ==== Pool projects and observers ====
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 * [[https://www.iram.es/IRAMES/mainWiki/GismoPakoNotes|Notes on paKo and NCS for GISMO 2012]] gives additional information on Pakonew and Lissajou observing mode.  * Winter semester 2012 observations will be carried out as pooled observations from a dedicated pool account. M.Gonzalez will provide login information.
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 * [[http://www.iram.fr/php/rel_sched/bgfiles/13/Bolopool-w12.html|List of accepted projects.]]
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 * Progress of observations can be followed via the [[https://pools.iram.es|pool data base]].
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 * [[http://www.iram.es/IRAMES/mainWiki/PoolW12 |Pool observers for the April 2013 run]]
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GISMO

This page is maintained by IH, CK, SL and the GISMO team

Contents

  1. GISMO
    1. Overview
    2. Call for proposals for the winter semester 2013/14
    3. Documentation
    4. Publications
    5. Support teams
    6. Observations
      1. pako scripts
      2. Pointing Sources
      3. crush data reduction
    7. Observing Runs
      1. October 2013 - 4th pool run
        1. Pool projects and observers
      2. April 2013 - 3rd pool run
        1. Pool projects and observers
      3. November 2012 - 2nd pool run
        1. Pool projects and observers
        2. Daily reports
      4. April 2012 - 1st pool run
        1. Daily reports
        2. Test plan
      5. Test runs 2007-2012
        1. 5th alignment run, March 2012
        2. 4th test run, April 2011
        3. 3rd test run, April 2010
        4. 2nd test run, October 2008
        5. 1st test run, November 2007

Overview

Pixels

Wavelength

Bandwidth (FWHM)

Sensitivity (out of atmosphere)

HPBW

Field-of-View

Spacing

GISMO since 2012

8x16

2.0 mm

140-162 GHz

14 mJy*s1/2

16.7"

1.8' x 3.7'

13.75"

The Goddard-IRAM Superconducting 2mm Observer (GISMO) is a bolometer camera for the IRAM 30m telescope. It has been build by Goddard Space Flight Center, in Greenbelt, Maryland under the lead of Johannes Staguhn. GISMO consists of 8x16 pixels with super conducting transition edge sensors (TES). The TES are read out by time domain SQUID multiplexers built at the National Institute for Standards (NIST), in Boulder, Colorado. The nominal bandwidth is 140-162 GHz (FWHM), pixels are spaced by 13.75", the telescope HPBW is 16.7". The sensitivity has improved relative to the April 2011 run to a media value of about 14 mJy sqrt(sec) (cf. reports below). The field-of-view is 1.8'x3.7' . Two standard observing modes are offered, Lissajous curves and on-the-fly scans. Both work in total power, without switching the secondary. An automated pipeline merges the GISMO data with the telescope data streams to create FITS files which are automatically processed by the reduction software crush to create logs, pointing results, and a first quick view of the data. Typical overheads for single science targets on the sky are 60%. The relative flux stability is about 8% (cf. report below).

Call for proposals for the winter semester 2013/14

GISMO is offered again to the community:

Documentation

Publications

  1. Dwek, Staguhn et al. 2011 ApJ,
    Star and dust formation activities in AzTEC-3: A starburst galaxy at z = 5.3

  2. Arendt et al. 2011 ApJ,
    The Radio - 2 mm Spectral Index of the Crab Nebula Measured with GISMO

  3. Capack et al. 2011 Nature,
    A massive proto-cluster of galaxies at a redshift of z~5.3

  4. Dicker et al. 2009 ApJ,
    90GHz and 150GHz observations of the Orion M42 region. A sub-millimeter to radio analysis

  5. Benford, Moseley, Zmuidzinas 2009 Journal of Physics
    Direct detectors for the Einstein inflation probe

  6. IRAM Newsletter 2/2009
    GISMO - The Goddard-IRAM Superconducting 2 Millimeter Observer tested at the IRAM 30m observatory

  7. Staguhn et al. 2008 Journal of Low Temperature Physics, 151, 3, 709
    GISMO, a 2 mm Bolometer Camera Optimized for the Study of High Redshift Galaxies

Support teams

Observations

pako scripts

Pointing Sources

Plots for Pointing Sources can be accessed within the IRAM network. These data are provided ONLY to help in the planning of observations, in particular to select pointing and focus sources at the IRAM 30-m telescope. They should not be used for any other purpose.

crush data reduction

Observing Runs

October 2013 - 4th pool run

Pool projects and observers

April 2013 - 3rd pool run

Pool projects and observers

November 2012 - 2nd pool run

Two weeks of dedicated GISMO observations have been carried out during November 2012.

Pool projects and observers

Daily reports

April 2012 - 1st pool run

In September 2011, GISMO had for the 1st time been offered to the community. Two weeks of dedicated GISMO observations have been carried out during April 2012.

Daily reports

Test plan

Test runs 2007-2012

5th alignment run, March 2012

4th test run, April 2011

3rd test run, April 2010

2nd test run, October 2008

1st test run, November 2007

GoddardIramSuperconductingTwoMillimeterCamera (last edited 2014-03-31 13:30:45 by gra-lx17)