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| <<TableOfContents(5)>> == 3rd GISMO test run, April 2010 == === Staffing of the test run === * GSFC: J. Staguhn, D. Fixsen, A. Kovacs, S. Maher, E. Sharp, D. Benford * IRAM: S. Leclercq, A. Sievers, G. Quintana-Lacaci, R. Zylka === Test run schedule: 31.03. - 16.04.2010 === '''IRAM 30m schedule page: ''' [[http://www.iram.fr/IRAMFR/PV/sche/sche.html|Schedule]] '''T16-09''' in 30m schedule = GISMO has telescope time Participants presence dates: [[attachment:Schedule_GISMO_visitors_April2010.pdf]] || '''#''' || '''Dates''' || '''Main Task''' || '''Details''' || '''Lead (GSFC/IRAM)''' || '''Support''' || || || 31.03. Wednesday || || Arrival of ES, first GISMO visitor, in Granada || || || || || 01.04.-05.04. || Mount upgrades, close and cool down in the 30m workshop || Arrival of SM || || || || || 06.04. Tuesday || Turn on GISMO, and 1st tests in the 30m workshop || Arrival of JS, DF, AK, SL, AS. || Johannes / Samuel || Albrecht (AoD) || || || 07.04.-08.04. || Tests in the 30m workshop || Bias, Tuning, IV curves, internal LED, Computer... || Johannes / Samuel || Albrecht (AoD) || || || 09.04. Friday || Installation in the cabin, cool down, alignment, background noise || Arrival of RZ || Johannes / Samuel || Albrecht & Guillermo (AoD) || || || 10.04.-12.04. || Calibration on sky (alignment, pointing, focus, dips), observations '''T16-09''' || 12.04.: Arrival of DB, departure of AS, SL, RZ || Johannes / Samuel || Guillermo (AoD) || || || 13.04.-15.04 || Observations '''T16-09'''|| || Johannes || Guillermo (AoD) || || || 16.04. Friday || Dismounting || Departure of everybody || Johannes || Guillermo (AoD) || Compilation of the lists of sources that will possibly be observed (include few references to past runs): [[attachment:GISMOtestrun3_sources.pdf]]. Comments from Johannes about the proposed science grade sources: [[attachment:IRAM_Proposed_Sources_Comments.pdf]] === GISMO upgrades compared to previous runs === * 2 motorized neutral density filters allowing to compensate the restrained dynamic range of GISMO by reducing the optical transmission in case of poor weather conditions, their transmissions are 65% and 40% respectively. * A controllable shutter and a LED coupled to detectors through a fiber allowing to make optical internal calibration * Automated observing procedures usable via a dedicated GUI such as detector tunning, sky dips, I-V measurements for total power measurements * A reduction package (Crush) allowing near-to-real-time data processing * An observer's manual of the GISMO operating software: [[attachment:GISMO_Software_Operational_Manual.pdf]] === Daily reports === ==== 31.03. - 05.04. ==== Arrival of Elmer & Stephen. Mount GISMO in the 30m workshop. The pictures below show several elements of the optical stage of GISMO: the 4K motors controlling the neutral density filters, the neutral density filters in motion, the baffle with the NDF motors and the 3He sorption cooler, and a general view of GISMO mounted. ||{{attachment:GISMO_4K_NDfilters_motors.jpg}} {{attachment:GISMO_NDfilter_1_moves.jpg}} {{attachment:GISMO_NDfilter_2_moves.jpg}} {{attachment:GISMO_baffle_3He_cooler.jpg}} {{attachment:GISMO_recycle_in_workshop.jpg}} {{attachment:GISMO_IV_curves.jpg}}|| Start cooling down on Monday the 05.04. ==== 06.04. - 08.04. ==== Arrival of Johannes, Dale, Attila, and Samuel. GISMO is cold. Turn on the instrument, BIAS the SQUIDs, monitor the TESs responses, take IV curves: all 4 quadrants are working, about ~20 non-responsive pixels (mostly due to SQUID issues in the MUX). LED illumination not visible in the real time data, but appears finely in reduced curves. Problems of strange wiggles in the IV curves. Install the GISMO frame in the cabin, but keep everything else (GISMO & electronics) in the workshop. Find next morning that the problem with the IV curves was surely due to CPU overheating. A new power supply (with large fan) was installed and an external heat source (another computer) was removed. Subsequently things looks fine, frequency plots show 1/f^2 noise certainly due to thermal oscillations. We noted that the bars holding M5 are below it and wondered whether this position would block partially the FOV and whether they weren't above M5 in the past, in particular for previous runs. As the pictures show below they were already below M5 when MAMBO was reinstalled in December 2007 after the 1st GISMO run, and they were also in this position during the 2nd GISMO run in 2008: ||{{attachment:MAMBO_30m_table_12_2007.jpg}} {{attachment:GISMO_30m_table_10_2008.jpg}}|| So the bars supporting M5 have probably always been in that position and are not an issue concerning the FOV. ==== 09.04. Friday ==== Start moving GISMO in the 30m receiver cabin in the morning. Perform the laser alignment. ||{{attachment:GISMO_moving_in_Rx_cabin_2.jpg}} {{attachment:GISMO_installed_in_Rx_cabin.jpg}} {{attachment:GISMO_installed_in_Rx_cabin2.jpg}} {{attachment:GISMO_installed_in_Rx_cabin3.jpg}} {{attachment:Laser_alignment_1.jpg}} {{attachment:Laser_alignment_2.jpg}} {{attachment:Laser_alignment_3.jpg}} {{attachment:Laser_alignment_4.jpg}} {{attachment:Laser_alignment_5.jpg}} {{attachment:Laser_alignment_6.jpg}}|| A temperature jump occurred during the installation. The detectors reached their base temperature near diner time. IV curves with the cryostat shutter closed showed more than 100 bolometers respond with nice superconducting transitions. But once the shutter was open all the TESs saturated and couldn't reach the superconducting transition: impossible to align on the sky. Telescope shutter was closed... Redo all the alignment procedure. But saturation problem still there. Numerous procedures tried to diagnose the problem an fix it. The only way to get and optical alignment on the sky was to install a metallic disc with a small aperture (few cm in diameter) in front of the cryostat window. The most probable explanation is a broken filter in the cryostat. Once all the hypothesis and tests we could imagine were conducted the decision is taken near 5am to warm up the cryostat. ==== 10.04. - 11.04. ==== The 30m is used by a backup project. The cryostat reached room temperature in the evening, and was dismantled. No problem seen on the filters. Main hypothesis explaining the saturation at cold temperature when the window is open to the sky: some stray-lights can bounce at angles steep enough to be badly attenuated by the filters, but not too much so that they pass the baffle without touching its wall, then they bounce with many reflections in the Neutral Density filters box and are eventually absorbed by the TESs, deposing enough energy to saturate them. Hence it was decided to remove the ND box and replace it by the cylindrical spacer used in GISMO run #2. GISMO was remounted then pumped during the night, and the cool down started early Sunday morning. Base temperature expected Sunday after diner. ||{{attachment:Open_GISMO_77K_stage.JPG}} {{attachment:Open_GISMO_4K_stage.JPG}} {{attachment:Open_GISMO_baffle.JPG}} {{attachment:Open_GISMO_Si_lens.JPG}} {{attachment:Open_GISMO_ND_filters_box.JPG}} {{attachment:Open_GISMO_run2_spacer_no_ND_box.JPG}}|| ==== 12.04. Monday ==== ??? ==== 13.04. Tuesday ==== Elmer has left and Dominic has arrived. The observing started late after a careful but ultimately unsatisfying alignment that had been entered into to fix a point source coupling problem. The point source coupling had been measured by Attila using a sky noise correlation vs. source strength correlation, and showed that there was some slope across the array indicative of spilling off the secondary. After realignment, Venus appeared nicely and could be focused well. Unfortunately, the point source coupling was not obviously any better. Careful focusing and re-alignment on Mars resulted in a very good cold sky, but again no better point source coupling. Pointing again on Saturn (a few hours later) resulted again in good cold sky and more uniform illumination of M7. The lesson being learned is that optical alignment of a large field of view instrument is a nontrivial exercise; chief ray pointing solutions are not sufficient for this kind of instrument. However, the weather was decent and we decided to conduct a few science observations that would produce good results. M82 appeared as a bright, Jy-level resolved source. IC342 was weakly detected at about 20mJy, and is slightly extended. M87 is clearly detected in its core (S/N of around 500), but none of the filamentary structure seen in the 90cm maps was evident at the ~1% level. ||M82: [[attachment:GISMO_M82.jpg|{{attachment:GISMO_M82.jpg|alt M82|width=250}}]] IC342: [[attachment:GISMO_IC342.jpg|{{attachment:GISMO_IC342.jpg|alt IC342|width=250px}}]]|| ||M87 GISMO: [[attachment:GISMO_M87.jpg|{{attachment:GISMO_M87.jpg|alt M87_GISMO|width=250}}]] VLA: [[attachment:VLA_M87.gif|{{attachment:VLA_M87.gif|alt M87_VLA|width=250px}}]]|| ==== 14.04. Wednesday ==== Wednesday was almost completely shut out due to snow and high winds. As a demonstration of both, Dale went outside with the anemometer wearing only a light shirt. [[attachment:GISMO_Wiki_4.jpg|{{attachment:GISMO_Wiki_4.jpg|alt Dale in High Winds|width=500}}]] We were able to detect the T Tauri disk around GM Aur: [[attachment:GISMO_GMAur.jpg|{{attachment:GISMO_GMAur.jpg|alt GM Auriga|width=500}}]] We worked on processing data. Here's a skydip fit (from very unstable weather at high tau): [[attachment:skydip81_histogram.tiff|{{attachment:skydip81_histogram.tiff|alt Skydip|width=500}}]] Some representative data using the LED/shutter calibration have been taken, and we do see the system behaving as expected. Software to process this data automatically are in the works, but I'm too tired to finish it now. We also had a good fox sighting and took a panoramic photo of the snowy conditions during a brief sunny moment. [[attachment:GISMO_Wiki_3.jpg|{{attachment:GISMO_Wiki_3.jpg|alt Fox|width=250}}]] [[attachment:GISMO_Wiki_2.jpg|{{attachment:GISMO_Wiki_2.jpg|alt Panorama|width=500}}]] ==== 15.04. Thursday ==== ==== 16.04. Friday ==== ---- == 2nd GISMO Test run, October 2008 == In October 2008, the GISMO team Johannes Staguhn, Stephen Maher, Elmer Sharp, Dale Fixsen, and Dominic Benford spent two weeks at the 30m observatory to first install their GISMO bolometer in the lab and then in the receiver cabin to test its performance on the sky. GISMO consists of 8x16 pixels with transition edge sensors (TES). The super conducting TES are read out by SQUID multiplexers. The nominal bandwidth is 125-175GHz, pixels are spaced by 14", the telescope HPBW is 17" at 2mm. Data are taken while the telescope is performing Lissajous scan patterns, without switching the secondary, to increase the mapping efficiency. An automated pipeline merges the GISMO data with the telescope data streams to create FITS files, being triggered by the IRAM messaging system. Data are then further reduced using the Goddard data reduction package. The 2mm spectral range provides a unique terrestrial window enabling ground-based observations of the earliest active dusty galaxies in the universe and thereby allowing a better constraint on the star formation rate in these objects. Preliminary results from this second observing run at the 30m telescope look very promising. (CK, 28-Oct-2008) {{attachment:gismo-team.png}} <<BR>> The GISMO team in the control room at the 30m telescope, after one week of 24 hours observing time. From left to right: Stephen Maher, Elmer Sharp, Johannes Staguhn, Dale Fixsen, Dominic Benford (Photo by A.Sievers on October, 27, 2008) * [[attachment:Report_on_GISMO_Run2_Rev3.pdf]] * [[attachment:Atmospheric_Emission_Noise_at_Pico_Veleta.pdf]] * [[attachment:GISMO_run2_reply_to_J_Staguhn.pdf]] * [[attachment:GISMO_sensitivity_reply_to_D_Benford.pdf]] * [[attachment:Some_GISMO_reduced_images.pdf]] * [[http://www.submm.caltech.edu/~sharc/crush/index.htm|Crush]] ---- == 1st GISMO Test run, November 2007 == * [[http://esoads.eso.org/abs/2008JLTP..151..709S|Staguhn et al. 2008]] GISMO, a 2 mm Bolometer Camera Optimized for the Study of High Redshift Galaxies * [[attachment:SPIE_GISMO_Staguhn.pdf]] * [[attachment:Staguhn_GISMO_SPIE_08_Rev1.pdf]] * [[http://www.astro.umd.edu/people/staguhn.html|Johannes Staguhn]] * [[http://gsfctechnology.gsfc.nasa.gov/Detector.htm|(Goddard)]], * [[http://www.phys.ufl.edu/tes3/pdfs/Benford_TES_Bolometer_Arrays_Poster.pdf|Poster on TES Bolometers]] |
<<TableOfContents(2)>> ---- == 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*s^1/2^ || 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: * [[http://www.iram-institute.org/EN/content-page-169-7-57-169-0-0.html|Call for observing proposals with the 30m]] * [[attachment:TimeEstimator_v3.pdf|Updated guidelines to estimate observing times (Billot et al. 2013)]]. * [[attachment:3rdGISMOpool_public_v2.pdf|Report on GISMO performance based on the pool run in April-2013 (Hermelo et al. 2013)]]. * [[attachment:bruni-aug2012-gismo.pdf|Report on GISMO performance based on the pool run in April-2012 (Bruni et al. 2012)]]. ---- == Documentation == * [[attachment:GISMO Software Operational Manual - May 2013]] by Steve Maher and Johannes Staguhn, May 2013 * [[attachment:GISMONCSInterfaceandFITSFormatv0.5.pdf|GISMO NCS Software Interface and FITS File Description]] by Steve Maher, Attila Kovacs, Albrecht Sievers, April 2012 ---- == Publications == 1. [[http://arxiv.org/abs/1106.2092|Dwek, Staguhn et al. 2011]] ApJ, <<BR>> '''Star and dust formation activities in AzTEC-3: A starburst galaxy at z = 5.3''' 1. [[http://arxiv.org/abs/1103.6225|Arendt et al. 2011]] ApJ, <<BR>> '''The Radio - 2 mm Spectral Index of the Crab Nebula Measured with GISMO''' 1. [[http://arxiv.org/abs/1101.3586|Capack et al. 2011]] Nature, <<BR>> '''A massive proto-cluster of galaxies at a redshift of z~5.3''' 1. [[http://arxiv.org/abs/0907.1300|Dicker et al. 2009]] ApJ, <<BR>> '''90GHz and 150GHz observations of the Orion M42 region. A sub-millimeter to radio analysis''' 1. [[http://iopscience.iop.org/1742-6596/155/1/012001/pdf/jpconf9_155_012001.pdf|Benford, Moseley, Zmuidzinas 2009]] Journal of Physics <<BR>>'''Direct detectors for the Einstein inflation probe''' 1. [[http://www.iram.fr/IRAMFR/ARN/feb09/node12.html|IRAM Newsletter 2/2009]] <<BR>> '''GISMO - The Goddard-IRAM Superconducting 2 Millimeter Observer tested at the IRAM 30m observatory''' 1. [[http://esoads.eso.org/abs/2008JLTP..151..709S|Staguhn et al. 2008]] Journal of Low Temperature Physics, 151, 3, 709 <<BR>>'''GISMO, a 2 mm Bolometer Camera Optimized for the Study of High Redshift Galaxies''' ---- == Support teams == * Overall coordinator: '''Samuel Leclercq''' <leclercq@iram.fr> (IRAM/Grenoble) * GISMO support team: * '''Johannes Staguhn''' <johannes.g.staguhn@nasa.gov> (PI) * Elmer Sharp * Steve Maher * Dale Fixen * Attila Kovacs (crush) * IRAM/Granada support team: * '''Carsten Kramer''' (station manager, <kramer@iram.es>) * Israel Hermelo (bolometer pool manager, <hermelo@iram.es>) * Albrecht Sievers (friend of GISMO, <sievers@iram.es>) * Manuel Gonzalez (heterodyne pool manager, <gonzalez@iram.es>) * Nicolas Billot (30m scheduler, <billot@iram.es>) ---- == Observations == === How to observe === The [[http://www.iram.es/IRAMES/mainWiki/GISMOforDummies | Quick GISMO guide for dummies]] 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. ## [[http://www.iram.es/IRAMES/mainWiki/GismoObservingScripts | GismoObservingScripts ]] ## 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. === Data reduction === GISMO data are reduced using CRUSH (Comprehensive Reduction Utility for SHARC2 - and more). * [[http://www.submm.caltech.edu/~sharc/crush/ | CRUSH website]] * [[http://www.submm.caltech.edu/~sharc/crush/download.html | Download CRUSH]] * [[http://www.iram.es/IRAMES/mainWiki/CrushExamples | Quick introduction to CRUSH]] ---- == 4th GISMO pool (October/November 2013) == The 4th GISMO pool will take place from the 22nd of October to the 5th of November 2013. Observations will be carried from a dedicated pool account (I. Hermelo will provide login information). === Pool projects and observers === For information about the accepted projects and the observers at the 30m please go to: * [[http://www.iram.es/IRAMES/mainWiki/ProjectsPoolS13 | List of accepted projects.]] * [[http://www.iram.es/IRAMES/mainWiki/PoolS13 | Pool observers for the October/November 2013 run]] * [[http://www.iram.es/IRAMES/mainWiki/GISMO/4thPool/Rooms | Room occupancy.]] === Progress === The progress of the 4th GISMO pool can be followed via: * [[https://pools.iram.es | Pool data base]] * [[https://herapool.iram.es/GISMO/|External GISMO Nexus log]] with slow updates * [[https://mrt-lx1/Devices/GISMO/|Internal GISMO Nexus log]] with fast updates === Status === * ''' 2013.09.27 11:00 UT:''' Starting the observations. TAU(225GHz)~0.5 * ''' 2013.09.25 21:00 UT:''' The wind died down but it started to rain. * ''' 2013.09.24 23:00 UT:''' Stopped by strong wind. TAU(225GHz)~0.6 * ''' 2013.09.23 09:00 UT:''' Bad weather conditions. Testing new scripts on Mars * ''' 2013.09.22 14:00 UT:''' Stopped by bad weather conditions (strong wind and rain) ---- == Previous observing runs == === 3rd GISMO pool (April 2013) === ==== Pool projects and observers ==== * Winter semester 2012 observations will be carried out as pooled observations from a dedicated pool account. M.Gonzalez will provide login information. * [[http://www.iram.fr/php/rel_sched/bgfiles/13/Bolopool-w12.html|List of accepted projects.]] * Progress of observations can be followed via the [[https://pools.iram.es|pool data base]]. * [[http://www.iram.es/IRAMES/mainWiki/PoolW12 |Pool observers for the April 2013 run]] === 2nd GISMO pool (November 2012) === Two weeks of dedicated GISMO observations have been carried out during November 2012. ==== Pool projects and observers ==== * [[http://www.iram.fr/php/rel_sched/bgfiles/12/bolopool-S12.html|List of accepted projects.]] * [[http://www.iram.es/IRAMES/mainWiki/PoolS12 |Pool observers for the November 2012 run]] * [[attachment:GISMO_observations_summary.pdf|Observations summary]]. ==== Daily reports ==== * GismoRun7 === 1st GISMO pool (April 2012) === 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 ==== * GismoRun6 ==== Test plan ==== * TestPlan for the first days of the April run * GismoToDoList === 5th alignment run, March 2012 === [[GismoRun5|Go to the 5th run Wiki page]] (installation of GISMO at a permanent position with new optics, baffle and new filter) === 4th test run, April 2011 === [[GismoRun4|Go to the 4th run Wiki page]] (restricted access, please send an email to SL to obtain the login information) === 3rd test run, April 2010 === [[GismoRun3|Go to the 3rd run Wiki page]] === 2nd test run, October 2008 === [[GismoRun2|Go to the 2nd run Wiki page]] === 1st test run, November 2007 === [[GismoRun1|Go to the 1st run Wiki page]] |
GISMO
This page is maintained by IH, CK, SL and the GISMO team
Contents
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:
Updated guidelines to estimate observing times (Billot et al. 2013).
Report on GISMO performance based on the pool run in April-2013 (Hermelo et al. 2013).
Report on GISMO performance based on the pool run in April-2012 (Bruni et al. 2012).
Documentation
GISMO Software Operational Manual - May 2013 by Steve Maher and Johannes Staguhn, May 2013
GISMO NCS Software Interface and FITS File Description by Steve Maher, Attila Kovacs, Albrecht Sievers, April 2012
Publications
Dwek, Staguhn et al. 2011 ApJ,
Star and dust formation activities in AzTEC-3: A starburst galaxy at z = 5.3Arendt et al. 2011 ApJ,
The Radio - 2 mm Spectral Index of the Crab Nebula Measured with GISMOCapack et al. 2011 Nature,
A massive proto-cluster of galaxies at a redshift of z~5.3Dicker et al. 2009 ApJ,
90GHz and 150GHz observations of the Orion M42 region. A sub-millimeter to radio analysisBenford, Moseley, Zmuidzinas 2009 Journal of Physics
Direct detectors for the Einstein inflation probeIRAM Newsletter 2/2009
GISMO - The Goddard-IRAM Superconducting 2 Millimeter Observer tested at the IRAM 30m observatoryStaguhn 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
Overall coordinator: Samuel Leclercq <leclercq@iram.fr> (IRAM/Grenoble)
- GISMO support team:
Johannes Staguhn <johannes.g.staguhn@nasa.gov> (PI)
- Elmer Sharp
- Steve Maher
- Dale Fixen
- Attila Kovacs (crush)
- IRAM/Granada support team:
Carsten Kramer (station manager, <kramer@iram.es>)
Israel Hermelo (bolometer pool manager, <hermelo@iram.es>)
Albrecht Sievers (friend of GISMO, <sievers@iram.es>)
Manuel Gonzalez (heterodyne pool manager, <gonzalez@iram.es>)
Nicolas Billot (30m scheduler, <billot@iram.es>)
Observations
How to observe
The Quick GISMO guide for dummies 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.
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.
Data reduction
GISMO data are reduced using CRUSH (Comprehensive Reduction Utility for SHARC2 - and more).
4th GISMO pool (October/November 2013)
The 4th GISMO pool will take place from the 22nd of October to the 5th of November 2013. Observations will be carried from a dedicated pool account (I. Hermelo will provide login information).
Pool projects and observers
For information about the accepted projects and the observers at the 30m please go to:
Progress
The progress of the 4th GISMO pool can be followed via:
External GISMO Nexus log with slow updates
Internal GISMO Nexus log with fast updates
Status
2013.09.27 11:00 UT: Starting the observations. TAU(225GHz)~0.5
2013.09.25 21:00 UT: The wind died down but it started to rain.
2013.09.24 23:00 UT: Stopped by strong wind. TAU(225GHz)~0.6
2013.09.23 09:00 UT: Bad weather conditions. Testing new scripts on Mars
2013.09.22 14:00 UT: Stopped by bad weather conditions (strong wind and rain)
Previous observing runs
3rd GISMO pool (April 2013)
Pool projects and observers
- Winter semester 2012 observations will be carried out as pooled observations from a dedicated pool account. M.Gonzalez will provide login information.
Progress of observations can be followed via the pool data base.
2nd GISMO pool (November 2012)
Two weeks of dedicated GISMO observations have been carried out during November 2012.
Pool projects and observers
Daily reports
1st GISMO pool (April 2012)
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
TestPlan for the first days of the April run
5th alignment run, March 2012
Go to the 5th run Wiki page (installation of GISMO at a permanent position with new optics, baffle and new filter)
4th test run, April 2011
Go to the 4th run Wiki page (restricted access, please send an email to SL to obtain the login information)
3rd test run, April 2010
2nd test run, October 2008