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From the Division Chief
With this inaugural edition of the electronic IRTF NEWS, we begin a biannual update of activities at our facility. Our main purpose is to improve communication with our users.
\n"; echo " We are presently considering new initiatives for the next 5–10 years. These initiatives will address upgrades, instrumentation, and new observing modes that will make the IRTF more relevant to the future needs of the planetary and ground–based infrared community. The planning section provides more information. Please give us your opinion if we have not already solicited it from you.\n"; echo "
\n"; } ?>Old–timers will recognize significant changes in our home page. We hope these changes will provide quicker access to the information you need to prepare your proposals. Please dont hesitate to let us know what you think of these changes.
You may contact our staff using name@irtf.ifa.hawaii.edu. See our contact list. If you are unsure who to contact, email kokua@irtf.ifa.hawaii.edu.
Fall 2001 Observing
The IRTF fall 2001 telescope schedule is available. Remote observing with NSFCAM and SpeX has been instituted on a trial basis.
Spring 2002 Call for Proposals (Due Date: Monday, 1 October 2001)
>Instructions and a list of >instruments are available. Note that our observing forms have been revised. Please use the >new forms.
Adaptive Optics
Work on the 36–element curvature–based natural guide star AO system is progressing. The lab version of the wavefront sensor package, consisting of deformable mirror, membrane mirror, lenslet array, avalanche photodiodes, and associated electronics, is working, and closed–loop operation is planned for September 2001.
Associated work includes removal of the heat from the Cassegrain focus area, better control of the dome temperature, and control of the primary mirror temperature. This work should lead to a reduction of the seeing from a typical 0.8" seeing to about 0.5". We will also install a new on–axis and off–axis guider.
NSFCAM Upgrade
The project to upgrade NSFCAM with a 1024x1024 1–5 µm array has been funded by the NSF. The $0.75 million received covers a new array controller, new optics, mechanical modifications to the cryostat, and a second wave–front sensor package. All the current filter, CVF, and grism capabilities will be preserved. First–light is expected in 2003.
Facility Instruments
>SpeX, >CSHELL, and >NSFCAM are working normally. About two weeks of observing time with SpeX was lost in April due to an array problem, which has since been fixed. A new version of the Spextool spectral reduction package was released in August. Note that SpeX will be unavailable during February 2002 due to maintenance.
MIRLIN is a 10–µm camera that is available for four months every semester. The MIRLIN team at JPL is fabricating a new mount to improve servicing on IRTF.
TEXES is a 10–µm spectrograph with a resolving power of 105. This instrument is available on a collaborative basis with the instrument team.
Science Highlights
T. Kostiuk et al. made the first direct measurement of wind velocity in the atmosphere of Titan with the Goddard 10 µm heterodyne spectrometer. This instrument was installed at the coudè focus of the IRTF 10 years ago and was recently decommissioned. A new instrument built by the same team is now in use at the Cassegrain focus. Named HIPWAC, it has a spectral resolving power of 106 at 10 µm. This is the highest resolution spectrograph in use at any observatory.
Staff News
Paul Jensen retired in December 2000 after serving as IRTF superintendent and as foreman for 21 years. George Koenig, previously the IRTF foreman, is now superintendent. The latest addition to the IRTF staff is Tim Bond, who replaced Doug Neill as mechanical engineer on 4 September. Tim is from Canada and worked at both the Dominion Astrophysical Observatory and at the Carnegie Observatories.
There were several major accomplishments in 2001:
We have several major goals for 2002:
Proposal deadline for Aug. 2002 – Jan. 2003
Fall 2002 semester observing proposals are due on Monday, April 1. See the >instructions, current application form, and list of >instruments.
Remote Observing available
We will accept proposals for >remote observing from Hilo, Hale Pohaku, or your office for the fall 2002 semester.
Bibliography & Science Highlights
Keeping NASA informed of the progress and success of observers is a very important part of operating the IRTF. The IRTF >bibliography is one method used to accomplish this. We ask observers to periodically check to see if their publications are listed and are up to date. A >submission form is provided for all new entries, or you can email your IRTF publication information to us. The IRTF Science Highlights are also vital for this purpose, and we welcome all to send us highlights, which may be sent to NASA.
Personnel
Lars Bergknut was selected as Foreman in October 2001. Charles Lockhart was hired as the Embedded Software Engineer in November 2001.
It is with sadness that we report Danley Lee (Observatory Maintenance Technician) passed away on February 17, 2002. We shall miss him.
From the Division Chief
For the past 6 months we have been working diligently on improving image quality. A major improvement was the replacement of a defective dome chiller. The dome air conditioning system has been improved as well. In addition, new racks were mounted on the telescope, which will house enclosures to remove heat from the instrument electronics. Other work planned includes sealing the dome skirt and shutter to reduce heat input during the day, installation of temperature sensors, and cooling the primary mirror. This work should be done by the end of the year and it should lead to a reduction of the dome seeing.
We have also made great progress on finishing the >Adaptive Optics system (AOS). During our May engineering run the AOS was installed, as well as a new instrument spool and new acquisition camera. First light was achieved during this first engineering run and the preliminary results were encouraging. We plan to make this exciting new capability available on a shared risk basis starting in Feb. 2003.
A new item has been added to facilitate the usage of our website. Click on the Site Index or Site Map and see the >Observers Manual with its Table of Contents, where you can find pertinent information for your observing run.
Proposal deadline for Feb. 1 – July 31 2003 due Tuesday, October 1, 2002
Changes have been made to the Time Application form. 1) Only ONE PAGE allowed for the Scientific Justification. 2) Format has been changed from TeX to LaTex. See our web site for >instructions. Submit your proposals using this latest version (rev. Aug. 2002).
Adaptive Optics System
We will allow the use of the AOS on a shared risk basis starting in April 2003. Please note the following restrictions: (1) Only one pixel scale with NSFCAM will be supported, the 0.05/pixel scale. (2) Only NSFCAM will be available for use. (3) There will be no guarantee of having an optimized instrument, and time may be taken away to conduct engineering work if necessary. (4) Only one user program per month can be supported. In spite of these restrictions, we feel working with users at an early stage will be very helpful to achieve good science as quickly as possible.
Information on the AO system may be found on our >AO web page.
Changes to NSFCAM
In order to maintain precise alignment between the AO sensor and NSFCAM, we have found it necessary to fix the position of the NSFCAM dichroic which feeds the AOS. Starting from February 1, 2003, the 0.95 µm IR–transmitting/visible reflecting dichroic will be left in the beam. No open position will be available. As a result the average throughput of NSFCAM will fall slightly from about 35% to 32%, and a 0.3% ghost will be created.
Tip–tilt Status
Tip–tilt is currently not available although we hope to fix it sometime within the next few months. Observers should submit proposals that do not require tip–tilt.
Remote Observing Available
Ten remote observing proposals were accepted for the fall 2002 semester. The IRTF probably has the most flexible remote observing policy of any observatory. Remote observing is available from Hale Pohaku, Hilo, or from your office on the mainland. Programs that can benefit from this are those that require frequent or short observations, and programs where one member of the observing team is on site and the other is at his or her home office.
SpexTool Extension
Users of SpeX are familiar with the IDL program names SpexTool that allows quick extraction of spectra from SpeX. Additional programs are now available to provide telluric correction, merging orders, editing and smoothing spectra. These programs can now be downloaded from the SpeX Web site. These programs were written by Mike Cushing and Bill Vacca.
Science Highlights
See the latest IRTF >science highlights:
1) IR Specroscopic Montoring of Pluto with SpeX (W. M. Grundy et al.)
2) FeH Absorption in the Spectra of Ultra-Cool Dwarfs (Cushing et al.)
3) Detection of Massive Water Ice Emission from the Nucleus of Comet C/1999 S4 (LINEAR) (C. . Lisse et al.)
4) Detection of H3+ In an HAeBe Star Using CSHELL (Brittain et al.)
5) Groundbased Infrared Detection of Ios SO2 Atmosphere (J. Spencer et al.)
From the Division Chief
Significant improvements have been made at the IRTF in the past year and I would like to acknowledge the work done by the IRTF day crew and the scientific, engineering, and technical staff. We all benefit from the work they do but rarely pause to acknowledge them. Thank you!
Major accomplishments in 2002 include:
Major goals for 2003 include:
Proposal deadline for Aug. 2003 – Jan. 2004
Fall 2003 semester observing proposals are due on Tuesday, April 1st. See the >instructions, current >application form, and list of >instruments.
Remote Observing in full swing
Please note that all programs utilizing the IRTF facility instruments can be used by >remote observing from Hale Pohaku, Hilo, Honolulu, or your office wherever it may be. You may also split your observing party with some at the summit and some at your home institution.
Adaptive Optics System Update
The AOS will be used for the first time in April on a shared-risk basis with restrictions. Information for observers can be found >here. If you wish to propose using AO and need further information, please contact John Rayner.
NSFCAM Upgrade
>NSFCAM upgrade is fully underway and is expected to be on the telescope in the summer of 2004.
Telescope Allocation Committee
Dr. William Cochran (McDonald Obs.) has rotated off the IRTF TAC after serving four semesters. Dr. Nancy Chanover (New Mexico State) has agreed to serve on the TAC as of this spring semester and through fall 2004. Full committee membership can be found >here.
Bibliography & Science Highlights
We thank observers who answered our call for IRTF papers and >science highlights throughout last year. Progress and success of the IRTF are measured by your papers, and we ask for your continued support of our >bibliography. Use our >submission form for all new entries, or you can e-mail your publication information to us.
If IRTF facility instruments have been used you should also cite the the instrument paper. Citations can be found on the relevant instrument webpage.
Personnel
The IRTF welcomes two new employees, Fred Keske, Electronics Engineer,
and Maury McQuat, Observatory Maintenance/Technician.
From the Division Chief
We are continuing to strive to improve the instrumentation on the IRTF, and as a result there are some important announcements you should read before proposing for time for the February–July 2004 semester.
First, we have brought the adaptive optics system back to Hilo for improvements, so it will not be available.
Second, we will be modifying NSFCAM for use with adaptive optics. It will not be available during April–August 2004, but SpeX will be available for imaging.
Third, MIRLIN will not be available. Instead, MIRSI, a new 10–micron camera, is being offered.
Fourth, a new visible CCD camera is available for observations (including proposals that use only this camera). See below for more details on these items.
We also have changes to our staff, and I would like to welcome new members to the IRTF. Eric Tollestrup joins us from Boston University as our new Deputy Division Chief. He will be responsible for operations in Hilo, and will work on the adaptive optics system and on improving image quality. I would like to thank John Rayner for his time and contributions as the Deputy Division Chief since 1997. John will focus on finishing the upgrade of NSFCAM and improving SpeX.
Another new staff member is Jim Pantaleo. He is working with Tony Denault to finish the software for the new Telescope Control System. Eric Volquardsen is our newest staff member. He is a Research Associate who will be a night assistant for remote observing and also assist with data analysis. Check out our >staff photo gallery to see their cheery faces
Major improvements to the facility are continuing. Our efforts to improve image quality are now concentrated on sealing the dome shutter and cooling the primary mirror. We are also implementing autofocus software that will allow convenient focusing of the telescope and quantitative seeing data. Another project is the replacement of our 24–year–old telescope control system. We plan to complete this work in 2 years.
\n"; echo "We are also making long–range plans in conjunction with the IRTF Management and Operations Working Group and members of the planetary community. We are asking what role will the IRTF play after the Cassini mission and how the IRTF fits within the Solar System Decadal Survey. Please send me your input on these matters. In the next newsletter I will describe our thoughts about them.\n"; echo " \n"; } ?>Finally, please note below our pleas for science highlights, updating our bibliography, and driving safely.
Proposal Deadline for February 2004 – July 2004
Spring 2004 semester observing proposals are due on Wednesday, October 1. See the >instructions, current >application form, and list of >instruments.
Instrumentation
Our adaptive optics system has been brought back to Hilo for improvements. We plan to return it to the telescope by February 2004 for further engineering tests. We are also upgrading NSFCAM with a 2048x2048 array with 40–milliarc pixels for use with adaptive optics. As a result, NSFCAM will not be available from April through August 2004. We plan for NSFCAM to be ready in September 2004 in time to support the Cassini mission.
While NSFCAM is off–line, imaging with SpeX is available. See the >Spex web site for further information.
MIRLIN, our facility 10–micron camera built by Mike Ressler (JPL), has been showing its age and has not been as reliable as is necessary for a facility instrument. We will therefore no longer support MIRLIN. We are grateful to Mike for making it available to IRTF users for the past several years.
We are now offering MIRSI, an 8–24 micron camera built at Boston University (Lynn Deutsch, PI), on a collaborative basis with the MIRSI team. Please check the >MIRSI web site for details, and contact Joe Hora (jhora@cfa.harvard.edu) regarding collaborations with the MIRSI team.
A visible CCD camera (Apogee) is now available. Although it was built to support nearly simultaneous visible–IR observations of asteroids, it can also be used as a stand–alone instrument. It is thermoelectrically cooled, and utilizes a Marconi 1024 x 1024 CCD that has 13–micron–square pixels and a measured read–noise of 12 electrons.
We operate the camera at –30 degrees C, which results in an average dark current of 2.7 electrons/sec. During readout, pixels are binned 2 x 2, producing 512 x 512 images with a pixel scale of 0.13 arcsec/pixel and a field of view of 66 arcsec. Initial sensitivity tests have shown that this camera can yield a 10–sigma detection of an R = 19.5 magnitude point source in 30 sec through a standard R–band filter. Contact Bobby Bus for more details (sjb@ifa.hawaii.edu).
Driving Hazard
Caution is required on the portion of the Saddle Road between the 12- and 14-mile markers. Comply with the speed limits and heed all "dangerous curve" warnings. Numerous accidents have occurred along this stretch of road.
Science Highlights
A list of IRTF >science highlights is maintained on our web site. Please notify your support astronomer of any exciting science that we may include there. We send these science highlights to NASA and the NSF, since they provide funding for our operations and instrumentation, respectively.
Bibliography
The importance of maintaining our IRTF bibliography cannot be overstated. Please keep us informed of all new papers through our online submission form, or you can e-mail us. Of course, please remember to acknowledge the IRTF.
Telescope Allocation Committee
Drs. Michael Simon and Faith Vilas have rotated off the IRTF TAC. Drs. Daniel Jaffe (U. Texas) and Daniel Britt (U. Central Florida) are the new members beginning this fall semester through spring 2005. Click >here for the full membership list.
Welcome to the new website for the NASA Infrared Telescope Facility. We are in the process of re–designing our site. Please note that we are still working in the transition process, so sections of the site may look different. We hope you enjoy the new website and send any comments, suggestions or bug reports to our web developer.
Mahalo!
If you are experiencing difficulties with the new site, please notify us and use the old version in the meanwhile.
NASA IRTF
Proposal Deadline for August 2004–January 2005
Fall 2004 semester observing proposals are due on Thursday, April 1. See >instructions, current >application form, and list of >instruments. The TAC will review telescope applications for the fall 2004 semester on May 12, and time awards will be announced by July 1. Remote observing from any location will be supported.
Telescope Allocation Committee
Many thanks to Drs. David Osip and William Graham, who served on the IRTF TAC for the last four semesters (spring 2002–fall 2003). Drs. Martha Hanner (U. Mass., Amherst) and Michael Brotherton (U. Wyoming) are the new members whose terms begin this spring. Click >here for the full membership list.
Instrumentation
The IRTF 36–element adaptive optics system will be available on a shared-risk basis from November 2004-January 2005. For details, please contact Eric Tollestrup or John Rayner. We are also upgrading NSFCAM with a 2048x2048 array. People planning to use either the adaptive optics system or NSFCAM should review the information >here.
\n";
echo " Tempel 1 observations at the IRTF to support Deep Impact Mission
\n";
echo " This mission is designed to probe the interior of a comet by crashing a 370 kg copper mass into comet Tempel 1 on July 4, 2005 (see Deep Impact Mission Website for more details). To support this mission, there will be an observing campaign two weeks before and four weeks after the impact. Time will be set aside for the campaign, and you are encouraged to apply for this time. Proposals for this campaign will be handled differently from the usual process. Click here to get more details. These proposals are due on October 1, 2004. If you have any questions, please contact Alan Tokunaga.\n";
echo "
Science highlights
NASA Headquarters requested 10–micron observations to support the flyby of the StarDust spacecraft past Comet Wild 2 to determine if dust production had changed since the last thermal observations in 1997. Observations were made December 13–15, 2004, and they showed that the dust production had not changed. The IRTF observations combined with astrometric observations made with one of the Keck telescopes enabled NASA to minimize the flyby distance on January 2, 2004. As a result, the flyby was very successful. (See the StarDust web site and the IRTF >science highlights for details.)
Image quality
Work continues on improving image quality under the direction of Eric Tollestrup and Tim Bond. Recent accomplishments include sealing the dome, turning on the environment monitoring system (temperature, wind, humidity), and completing the mirror cooling system. In addition, autofocus software has been developed and is being tested. After further testing, we will allow this software to be used by the telescope operators. They will focus the telescope for users and provide quantitative data on the seeing.
If you are experiencing difficulties with the new site, please notify us and use the old version in the meanwhile.
NASA IRTF
Proposal Deadline for February – July 2005
Spring 2005 semester observing proposals are due on Friday, October 1. See >instructions, current >application form, and list of >instruments. Application form, rev. Aug. 2004, must be used. The TAC will review telescope applications on November 18, and time awards will be announced before January 1. Note that remote observing from any location will be supported.
Tempel 1 Observations in Support of the Deep Impact Mission July 4, 2005
The Deep Impact mission is designed to probe the interior of a comet by crashing a 370 kg copper mass into the nucleus of comet Tempel 1 on July 4, 2005. To support this mission, there will be an observing campaign two weeks before and four weeks after the impact. Time will be set aside for the campaign, and you are encouraged to apply for this time. Click here for more details. If you have any questions, please contact Alan Tokunaga. Proposals are due on Friday, October 1 (same deadline as all other proposals).
Instrumentation
The IRTF 36–element adaptive optics system will be available. We are also upgrading NSFCAM with a 2048x2048 array. People planning to use either the adaptive optics system or NSFCAM2 should review the information >here. If you have further questions, please contact Eric Tollestrup.
MIRSI
Boston Universitys Mid-InfaRed Spectrometer and Imager will continue to be available for use on the IRTF for the Spring 2005 semester. To date, MIRSI has been on the telescope for about 15% of the time and has been used for a wide variety of observing programs. Those interested in using MIRSI can find more information >here and are encourage to contact a MIRSI team member.
Science
We have updated the >science highlights. Please inform us of any science highlights you may have. We distribute these to the NASA Headquarters and the NSF, so this is an excellent way to let our funding agencies know what you are doing. Also please help us keep our publications up to date by sending your recent publications or an email to us.
Image Quality
We are continuing to work on improving image quality. We have made progress recently in reducing the heat input into the dome, installing temperature and environmental sensors, eliminating heat infiltration from the outside, and improving the performance of the dome air conditioning system. We next plan to cool the primary mirror and to implement a method of actively controlling the dome and primary mirror temperatures.
Telescope Allocation Committee
Kevin Luhman (Harvard–Smithsonian CfA) has rotated off the TAC after having served from fall 2001 through spring 2004. New member, Joan Najita (NOAO), will serve from fall 2004 through spring 2006. See full membership >here.
IRTF Vehicles
To assure that only licensed drivers operate IRTF vehicles, observers requesting vehicles are required to provide complete information in the transportation section of the >Observing Requirements Form.
Proposal Deadline for August 1, 2005 – January 31, 2006
Fall 2005 semester observing proposals are due on Friday, April 1. See the >information and >application form in the sidebar under "Applications". The most current application form, rev. Aug. 2004, must be used. A summary of instruments can be found at >irtfweb.ifa.hawaii.edu/Facility/. The TAC will review telescope applications in May, and time awards will be announced before July 1. Remote observing from any location will be supported.
Tempel 1 Observations in Support of the Deep Impact Mission!
The Deep Impact mission is designed to probe the interior of a comet by crashing a 370 kg copper mass into the nucleus of comet Tempel 1 on July 3, 2005 HST. The solar system panel of the IRTF TAC (D. Britt, N. Chanover, M. Hanner) and two members from the Deep Impact Team, Karen Meech (U. of Hawaii) and Mike AHearn (U. of Maryland) evaluated the proposals and created a plan for the Deep Impact observations. Selected to observe this event are N. Dello Russo et al., "Volatile Chemistry of Comet 9P/Tempel 1 Pre– and Post–Impact" Kelley et al., "Imaging Polarimetry of 9P/Tempel 1 During the Deep Impact Encounter" C. Lisse et al., "IRTF Observations of the Deep Impact Encounter with Comet 9P/Tempel 1" M. Sitko et al., "0.4–13 Micron Spectrophotometry of the Comet Tempel 1–Deep Impact Event" and D. Wooden et al., "Temporal Evolution of the Post–Impact Dust Properties of Comet 9P/Tempel 1 Using MIRSI+NSFCAM2." We plan to make the data public 6 months after the event.
Instrumentation
The IRTF 36–element adaptive optics system will be available. We are also upgrading NSFCAM with a 2048x2048 array. People planning to use either the adaptive optics system or NSFCAM2 should review the information >here. If you have further questions, please contact Eric Tollestrup (tolles@ifa.hawaii.edu). Note that both NSFCAM2 and the adaptive optics systems are under development, so please check with us regarding the latest status of these instruments.
MIRSI
Boston Universitys Mid–InfraRed Spectrometer and Imager is available for use on the IRTF on a long–term basis due to an agreement between the Univ. of Hawaii and Boston University. Those interested in using MIRSI can find more information at irtfweb.ifa.hawaii.edu/Facility/ and are encouraged to contact either James Jackson (Boston Univ.) or Eric Tollestrup (IRTF).
Science
Our >Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. Please keep submitting your recent publications using the form provided at our web site, or send them to Ms. Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications following the information on our >acknowledgement page.
Image quality
We continue to work on improving image quality. The primary mirror cooling system is up and running, and characterization of the system has begun with promising preliminary results. The autofocus system is now in final testing before being installed at the facility.
Telescope Allocation Committee
Nancy Chanover (New Mexico State U.) has rotated off the TAC after serving from spring 2003 through fall 2004. New members, Henry Roe (NOAO) and Frederick Walter (SUNY–Stony Brook), will serve from spring 2005 through fall 2006. See full >membership here.
IRTF Vehicles
To improve safety, we now request that observers who wish to use an IRTF vehicle provide information requested in the transportation section of the >Observing Requirements Form. Each driver is required to submit a signed copy of the >>Drivers Clearance form to the Hilo IRTF office prior to arrival.
Proposal Deadline for February 1 – July 31, 2006
Spring 2006 semester observing proposals are due on Monday, October 3, 2005. See the >information and >application form in the sidebar under “Applications.” The most current application form, last revised August 2004, must be used. A summary of instruments can be found at >irtfweb.ifa.hawaii.edu/Facility/. The TAC will review telescope applications on November 7, and time awards will be announced before January 1, 2006. Remote observing from any location will be supported.
Telescope Allocation Committee
Daniel Britt (U. of Central Florida) and Daniel Jaffe (U. of Texas) have rotated off the TAC after serving from fall 2003 through spring 2005. New members, Ellen Howell (Arecibo Obs.) and Jeff Valenti (STScI), will serve from fall 2005 through spring 2007. See full membership >here.
9P/Tempel 1 Observations in Support of the Deep Impact Mission
The Deep Impact mission designed to probe the interior of a comet by crashing a 370 kg copper mass into the nucleus of comet Tempel 1 on July 3, 2005, (Hawaii time) was a success. An observing campaign at the IRTF was implemented using SpeX, MIRSI, CSHELL and visitor instruments HIFOGS and BASS. During the night of the impact, SpeX was used to obtain high time resolution spectroscopy at 1–2.5 microns. This provided unique data on color changes right after the impact. We plan to make all of the data public in about 6 months.
Instrumentation Update
(1) NSFCAM2, with a 2048x2048 array, is presently being readied for commissioning. We are preparing for the first commissioning run in September. For more information, please see the >NSFCAM web page or contact Eric Tollestrup (tolles@ifa.hawaii.edu).
(2) Adaptive Optics System. We have had to postpone work on the 36–element adaptive optics system due to problems with obtaining a suitable deformable mirror and a lack of sufficient manpower. We are currently planning to replace our secondary mirror with one that is configured to correct the spherical aberration of the primary mirror. This will eliminate the largest source of wave–front error that is limiting the performance of our AO system and provide improved images for all of our instruments. With our limited manpower, this work requires us to put current work on our AO system on hold.
(3) Boston Universitys Mid–InfraRed Spectrometer and Imager (MIRSI) is available for use on the IRTF for the next five years, effective July 2005, due to a Memorandum of Agreement between the University of Hawaii and Boston University. The agreement includes future work on MIRSI that will improve the sensitivity and operations. Those interested in using MIRSI can find more information >here and are encouraged to contact either James Jackson (Boston Univ.) or Eric Tollestrup (IRTF).
Science
Our >Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. Please keep submitting your recent publications using the form provided on our web site, or send them to Ms. Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications using the information on our >acknowledgement page.
Telescope Control System
Work on replacing the telescope control system is proceeding. We have installed some of the new hardware and software at the summit and are using it on a daily basis. Current work is focused on testing the servo system and finishing the remaining hardware.
Remote Observing
Spring 2005 was the first semester in which 50% of the total observing time scheduled on the IRTF was remote observing. Saving travel time and money makes remote observing an appealing choice, but first–time observers are required to be on–site for their run.
Proposal Deadline for August 1, 2006 – January 31, 2007
Fall 2006 semester observing proposals are due on Monday, April 3, 2006. See the >information and >application form in the sidebar under “Applications.” The most current application form, last revised February 2006, must be used. A summary of instruments can be found at >irtfweb.ifa.hawaii.edu/Facility/. The TAC will review telescope applications on May 22, and time awards will be announced before July 1, 2006. Remote observing from any location will be supported.
Telescope Allocation Committee
Martha Hanner (U. Massachusetts, Amherst) and Michael Brotherton (U. Wyoming) have rotated off the TAC after serving from spring 2004 through fall 2005. New members, Yan Fernandez (U. Central Florida), and Dean Hines (Space Science Inst.), will serve from spring 2006 through fall 2007. See full membership >here.
9P/Tempel 1 Observations in Support of the Deep Impact Mission
The Deep Impact mission designed to probe the interior of a comet by crashing a 370 kg copper mass into the nucleus of comet Tempel 1 on July 3, 2005, (Hawaii time) was a success. An observing campaign at the IRTF was implemented using SpeX, MIRSI, CSHELL and visitor instruments HIFOGS and BASS. During the night of the impact, SpeX was used to obtain high time resolution spectroscopy at 1–2.5 microns. This provided unique data on color changes right after the impact. We plan to make all of the data public within about 6 months. Questions about the archive should be sent to Bobby Bus (sjb@ifa.hawaii.edu)
Instrumentation Update
NSFCAM2, with a 2048x2048 array, is presently being readied for commissioning. We are preparing for the first commissioning run in March. For more information, please see the >NSFCAM web page or contact Eric Tollestrup (tolles@ifa.hawaii.edu).
Science Highlights and Publications
Our >Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. Please keep submitting your recent publications using the form provided on our web site, or send them to Ms. Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications following the information on our >acknowledgement page and include in your papers the name of the instrument used, as this helps to insure future funding of IRTF instruments.
Note that the MIT–IRTF Near–Earth Object spectral survey is underway with many spectra that are publicly available. See the side bar for more information or go to smass.mit.edu/minus.html
New Secondary Mirror
The initial phase in replacing the IRTF secondary mirrors with a new corrective, scatter compensating mirror are currently underway. We are designing a prime focus instrument called PhCS (pronounced 'fix'), or 'Phase Corrective Secondary', that will measure and characterize the optical properties of the primary mirror. PhCS will have a prime focus camera, a knife–edge tester, a Hartmann wavefront sensor, and a guide camera. The goal of this NSF funded project is to correct the major static aberrations (mostly spherical aberration) and reduce the scattering due to higher order aberrations (primarily the zonal rings and support–pad print–through) that are in the primary mirror by applying an appropriate phase compensating surface on secondary mirror. Currently there is approximately 0.3 microns rms of spherical aberration in the IRTF, which caused a significant degradation to the 36–element AO system. Correcting these aberrations will not only benefit the AO system, but will significantly improve the image quality for nearly all observations. The characterization of the the primary mirror will occur this fiscal year, while the corrective mirror is planned to be manufactured in FY2007, for delivery to the IRTF in the Spring of 2007. This project is part of a three–pronged program underway at the IRTF to improve the image quality of the telescope – this includes improving the optics, controlling dome seeing, and reducing the aberrations caused by dynamic aberrations. The dome seeing has been improving by controlling the dome thermal environment and cooling the primary mirror during the day, while the dynamic aberrations (caused by inadequate mirror support) will be reduced by implementing improvements to the primary mirror cell. For more information, please contact the P.I., Eric Tollestrup (tolles@ifa.hawaii.edu).
New Telescope Control System
Work on replacing the telescope control system is proceeding. We have installed some of the new hardware and software at the summit and are using it on a daily basis. Current work is focused on testing the servo system and finishing the remaining hardware. We will begin daytime testing in March.
Remote Observing
Spring 2006 is the first semester in which remote observing has reached up to 70% of the total observing time scheduled on the IRTF in a single month. Saving travel time and money makes remote observing an appealing choice, but first–time observers are required advised to be on–site for their run.
Last updated Oct. 26, 2006
Many of you have expressed some concern regarding the status of the IRTF, and I am pleased to announce that we are fine.
A 6.7 magnitude earthquake struck near the South Kohala Coast on Sunday, Oct. 15, at 7:07 AM. This was followed by a 6.0 magnitude earthquake at 7:14 AM. There were numerous aftershocks in the days after Oct. 15. The IFA facilities in Hilo did not suffer any significant damage, although the Waimea facilities of Keck and CFHT did have extensive damage. There were no injuries at home or at the observatory reported by our staff.
A visual inspection of the IRTF revealed no perceptible damage, although the earthquake had knocked over many small items. Quick action by George Koenig, Eric Tollestrup, Charles Lockhart, and Miranda Hawarden-Ogata on Sunday was crucial in minimizing problems with the facility and instruments. The air conditioning system and electronics were secured before the power was turned on. Electric power was restored at about 2:30PM on Oct. 15, and the instruments were nurtured back to health. NSFCAM2 has a large format array that had to be carefully watched to prevent large temperature excursions.
On the morning of Oct. 17, we opened for observations of Saturn and our systems performed normally. On the evening of Oct. 18, we did a pointing run and the pointing coefficients were typical. This indicates that the alignment of the polar axis did not shift significantly.
Here is a picture from the USGS website showing the earthquake and its many aftershocks. Here is a story from the Honolulu Advertiser and here are two stories from the Star Bulletin, from Oct 16th and Oct 18th.
NASA IRTFLast updated Nov. 02, 2006
Proposal Deadline for February 1 – July 31, 2007
Spring 2007 semester observing proposals are due on Monday, October 2, 2006. See the information and application form in the sidebar under “Applications.” Available instruments include (1) SpeX, a 1–5 micron cross–dispersed medium–resolution spectrograph (up to R = 2,500); (2) CSHELL, a 1–5 micron high–resolution spectrograph (up to R = 30,000); (3) MIRSI, a 5–25 micron camera and low–resolution spectrometer (R = 100 to 200), (4) NSFCAM2, a 2048x2048 pixel, 1–5 micron camera with a 0.04 arcsec/pixel scale and a complement of discrete filters, CVFs, and grisms; and (5) PI–instruments including a low–resolution 3–14 micron spectrograph and high–resolution spectrographs for 8–25 microns. Note that TEXES is available at the IRTF for this semester and at Gemini North in the fall semester. Information on available instruments can be found at irtfweb.ifa.hawaii.edu. Remote observing from any location will be supported.
Spectral Library Now Available!
The Spex spectral library for FGKMLT stars is now available. The papers by John Rayner, William Vacca, and Michael Cushing should be referenced when this library is used.
NEO Spectral Survey
Note that the MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra publicly available. See the side bar for more information or go to smass.mit.edu/minus.html
Science Highlights and Publications
Our >Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. Please keep submitting your recent publications using the form provided on our Web site, or send your reprints to Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications following the information on our >acknowledgement page and include in your papers the name of the instrument used, as this helps to ensure future funding of IRTF instruments.
Instrumentation Update
NSFCAM2, with a 2048x2048 array, is presently being readied for commissioning. We are still in the process of solving excess noise problems in the array. For status on this instrument, contact Eric Tollestrup (tolles@ifa.hawaii.edu) or see irtfweb.ifa.hawaii.edu/~nsfcam/.
New Secondary Mirror
The initial phase of replacing the IRTF secondary mirrors with a new corrective, scatter compensating mirror is now currently underway. We are designing a prime focus instrument called PhCS (pronounced 'fix'), or 'Phase Corrective Secondary', that will measure and characterize the optical properties of the primary mirror. The goal of this NSF funded project is to correct the major static aberrations (mostly spherical aberrations) and reduce the scattering due to higher order aberrations (primarily the zonal rings and support–pad print–through) that are in the primary mirror by applying an appropriate phase compensating surface on the secondary mirror. This project is part of a three-pronged program underway at the IRTF to improve the image quality of the telescope that also includes improving the optics, controlling dome seeing, and reducing the aberrations caused by dynamic aberrations. For more information, please contact the P.I., Eric Tollestrup (tolles@ifa.hawaii.edu).
Autofocus
We have implemented autofocus with SpeX. The telescope operator will obtain the focus for all users. This should save users much time each night with the focusing. The data obtained from the autofocus will be used to help analyze the image quality each night.
Remote Observing
Remote observing continues to be in demand at the IRTF. Saving travel time and money makes remote observing an appealing choice, but first–time observers are advised to be on–site for their run.
Roof Repair Completed
We have been suffering from a leaky roof for over a year. However, a completely new top layer has been added to the roof this summer, and the sides of the roof and dome skirt area have also been repaired. This should last for about 7 years and end the occasional water infiltration in the control room area, much to the relief of our telescope operators.
Take a Tour of the IRTF!
The recently installed virtual tour allows anyone to visit the IRTF. Step inside the dome and view
our telescope up close.
Last updated 01 March 2007
Proposal Deadline for August 1, 2007-January 31, 2008
Fall 2007 semester observing proposals are due on Monday, April 2, 2007. See the information and application form >here. The current application form, revised in February 2007, must be used. Available instruments include (1) >SpeX, a 1-5 micron cross-dispersed medium-resolution spectrograph (up to R = 2,500); (2) >CSHELL, a 1-5 micron high-resolution spectrograph (up to R = 30,000); (3) >MIRSI, a 5-25 micron camera and low-resolution spectrometer (R = 100 to 200), (4) >NSFCAM2, a 2048x2048 pixel, 1-5 micron camera with a 0.04 arcsec/pixel scale and a complement of discrete filters, CVFs, and grisms; and (5) PI-instruments including a low-resolution 3-14 micron spectrograph and high-resolution spectrographs for 8-25 microns. Note that >TEXES is not available at the IRTF during this semester. Information on available instruments can be found at >irtfweb.ifa.hawaii.edu/Facility/. Remote observing from any location will be supported.
Telescope Allocation Committee
The >current TAC members are Yan Fernandez (U. Central Florida), Dave Glenar (Goddard), Dean Hines (Space Science Inst.), Ellen Howell (Arecibo Observatory), James Muzerolle (U. of Arizona), and Jeff Valenti (STScI).
Spectral Library Now Available!
The SpeX spectral library for FGKMLT stars is now available >here. The spectra are provided in FITS and text formats. The papers by John Rayner, William Vacca, and Michael Cushing presented at this website should be referenced when this library is used.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF.
Please keep submitting your recent publications using the form provided on our website, or send your reprints to Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications following the information >shown here and include in your papers the name of the instrument used, as this helps to insure future funding of IRTF instruments.
Instrumentation Update
NSFCAM2, with a 2048x2048 array, has been used on a conditional basis because of the high read noise, which decreases the sensitivity in the low-background filters (including J, H, and K). Several causes of the excess noise have been identified, and solutions are being implemented. Once all the solutions are applied, the read noise is expected to be about 18 to 20 e-rms. Some of the solutions require custom replacement components, which has resulted in delays. For the status of this instrument, contact Eric Tollestrup (tolles@ifa.hawaii.edu).
New Secondary Mirror
Eric Tollestrup has obtained an NSF grant to measure the spherical aberration of the primary mirror and to fabricate a new secondary mirror with a surface figure that removes the spherical aberration and other high-order aberrations. This new secondary mirror is called the Phase Compensating Secondary, or PhCS. The first stage of this project is to fabricate a prime focus instrument package (including a prime focus camera, knife-edge test, Hartmann wavefront sensor, and a guide camera) to characterize and measure the aberrations of the primary mirror. The first engineering run with this new camera is planned for April.
Remote Observing
During the Fall 2006 semester, the percentage of telescope time that was used remotely grew to 60%. Observers find that saving travel time and money makes remote observing very appealing. First-time observers are advised to be on-site for their run. If you wish to change to remote observing, please inform your support astronomer as soon as possible, since we need to arrange for a second person to be at the summit with the telescope operator. If you are a new user of remote observing, we will also need time to test the network connections.
Last updated 06 September 2007
Proposal Deadline for February 1 - July 31, 2008
Spring 2008 semester observing proposals are due on Monday, October 1, 2007. See the information and application form >here. (The current application form, revised August 2007, must be used. Available instruments include (1) >SpeX, a 1-5 micron cross-dispersed medium-resolution spectrograph (up to R = 2,500); (2) >CSHELL, a 1-5 micron high-resolution spectrograph (up to R = 30,000); (3) >MIRSI, a 5-25 micron camera and low-resolution spectrometer (R = 100 to 200), (4) >NSFCAM2, a 2048 ? 2048 pixel, 1-5 micron camera with a 0.04 arcsec/pixel scale and a complement of discrete filters, CVFs, and grisms; and (5) PI-instruments including a low-resolution 3-14 micron spectrograph and high-resolution spectrographs for 8-25 microns. Information on available instruments can be found at >irtfweb.ifa.hawaii.edu/Facility/. Remote observing from any location will be supported.
Telescope Allocation Committee
The >current TAC members are Yan Fernandez (U. Central Florida), Dave Glenar (Goddard), Joshua Emery (SETI), Dean Hines (Space Science Inst.), James Muzerolle (U. of Arizona), and Russel White (U. Alabama).
Spectral Library Available
The SpeX spectral library for FGKMLT stars is available >here. The spectra are provided in FITS, text, PDF, and postscript formats. The papers by John Rayner, William Vacca, and Michael Cushing presented at this website should be referenced when this library is used.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. Please keep submitting your recent publications using the >form provided on our website, or send your reprints to Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications following the information >shown here and include in your papers the name of the instrument used, as this helps to insure future funding of IRTF instruments.
Instrumentation Update
NSFCAM2, with a 2048 x 2048 array, has been used on a conditional basis because of the high read noise, which decreases the sensitivity in the low-background filters (including J, H, and K). Several causes of the excess noise have been identified, and solutions are being implemented. Once all the solutions are applied, the read noise is expected to be about 18 to 20 e- rms. Some of the solutions require custom replacement components, which has resulted in delays. For the status of this instrument, contact Eric Tollestrup (tolles@ifa.hawaii.edu). NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns) since it is background limited and the image quality is excellentexcellent.
The SpeX guider can be used for 1-5 µm imaging. Although it is not optimum given its engineering grade array (used for acquisition and guiding), it is still better than the current NSFCAM2 array at JHK. Observers who wish to use SpeX rather than NSFCAM2 for JHK imaging should consult with John Rayner.
MIRSI Upgrade
CSHELL Upgrade
New Secondary Mirror
Remote Observing
New Cooperative Agreement
MIRSI is currently undergoing an upgrade, which should be completed around the end of 2007. The most obvious changes will be a new graphical user interface that will have the same look and feel as the facility instrument GUIs. In addition, various hardware, firmware, and software upgrades will make MIRSI more reliable and robust. Finally, new readout schemes will be implemented to improve the sensitivity, improve the fix pattern noise, and eliminated various readout artifacts. These upgrades are happening without taking MIRSI out of operation. When the new GUI is implemented, all MIRSI observers will need to get additional training on how to use MIRSI. Contact
The user GUI for CSHELL is being improved so that it has a format similar to that of SpeX.
Eric Tollestrup has obtained an NSF grant to measure the spherical aberration of the primary mirror and to fabricate a new secondary mirror with a surface figure that removes the spherical aberration and other high-order aberrations. The first stage of this project (to fabricate a prime focus instrument package and measure the aberrations) has been completed this past spring. The data are being analyzed to derive specifications for the new secondary mirror, which should be installed on the IRTF during the 2008B semester. With the new secondary mirror, the majority of the static aberrations will be substantially corrected, if not eliminated, resulting in significantly better image quality. Upon completion, the IRTF image quality should be primarily limited by atmospheric seeing and mirror cell induced astigmatism.
Interest in remote observing has continued to grow since it was first offered at the IRTF in August 2002. About 60% of the observing time is now being used remotely. We support remote observing from any location with broadband Internet access for any project that utilizes IRTF instruments. See >here for more information.
A Cooperative Agreement to fund IRTF operations for five years has been submitted to NASA. This new agreement will cover the period of February 2008 to January 2013. In addition to continuing operations, we plan to undertake work to improve the image quality of the telescope. Separate proposals will be submitted to the NSF to provide additional instrumentation, particularly to support NEO follow-up observations.
\n";
echo " At the last Management and Operations Working Group (MOWG) meeting, held in Hilo on January 31, 2007, it was announced that NASA will be seeking a new Cooperative Agreement to continue IRTF operations for another 5 years. The time period of the new Cooperative Agreement will be February 2008 through January 2013. We will contact some of you about how best to use the IRTF during this period. We also welcome any input you may have. Please contact Alan Tokunaga regarding this matter.\n";
echo "
Last updated 03 March 2008
Proposal Deadline for August 1, 2008 - January 31, 2009
Fall 2008 semester observing proposals are due on Tuesday, April 1, 2008. Information and the application form (rev. Aug. 2007) can be found >here. Available instruments are listed at >irtfweb.ifa.hawaii.edu/Facility/. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Please refer to the remote observing site.
Telescope Allocation Committee
The >current TAC members are Joshua Emery (SETI), Dave Glenar (New Mexico State U.), Eilat Glikman (Caltech), Michael S. Kelley (U. Central Florida), James Muzerolle (U. Arizona), and Russel White (U. Alabama).
New Cooperative Agreement
A cooperative agreement with NASA to fund IRTF operations from February 2008 to January 2013, has been approved. In addition to continuing operations, we are planning to undertake work to improve the image quality of the telescope. This will be pursued in two ways: One is to fabricate a new secondary mirror that will remove the spherical aberration in the primary mirror (see below). Another is that we will continue to improve the dome thermal environment by eliminating a major source of heat infiltration during the daytime through the dome skirt. In addition, we have submitted proposals to both NASA and the NSF to provide additional instrumentation. We are hoping to provide a replacement for CSHELL with NSF and NASA funding and to provide polarimetric observations of asteroids to obtain size estimates of NEOs.
Personnel Spotlight
 |
Sammy Pung, the first employee to be spotlighted in our online news, is a member of the IRTF day crew that works as a team to keep the dome, shutter and all mechanical equipment operating smoothly. Sammy also maintains the air conditioning system (critical for good seeing) and keeps the mirror clean with regular CO2 washing. |
| Sammy began work as a mechanical technician in June 1982, two days after receiving an honorable discharge from the Navy after completing two tours of duty in the Persian Gulf. Sammys personal time is mainly spent working on his 10-acre farm with his wife, Carrie. When he manages to find spare time, Sammy joins the RP Gang in volunteering to keep Big Island trails open and rides his Harley Davidson with his motorcycle club, Na Kane Oke Awawa. | |
Instrumentation Update
MIRSI Upgrade:
Eric Tollestrup and Charles Lockhart are upgrading MIRSI. This work should be completed in March 2008. The most obvious changes will be a new graphical user interface that will have the same look and feel as the facility instrument GUIs. In addition, various hardware, firmware, and software upgrades will make MIRSI more reliable and robust. Finally, new readout schemes will be implemented to improve the sensitivity, improve the fix pattern noise, and eliminate various readout artifacts. These upgrades are happening without taking MIRSI out of operation. When the new GUI is implemented, all MIRSI observers will need to get additional training on how to use MIRSI. Contact Eric Tollestrup for more details.
NSFCAM2 status:
NSFCAM2 status: This camera has been used on a conditional basis because of the high read noise, which decreases the sensitivity in the low-background filters (including J, H, and K). Several causes of the excess noise have been identified by Eric Tollestrup, and he will work on them after the MIRSI upgrade is finished. If the troubleshooting is successful, the read noise is expected to be about 18 to 20 e- rms. Some of the solutions require custom replacement components, which has resulted in delays. To check the status of this instrument before writing a proposal, contact John Rayner. NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 µm), since at these wavelengths it is background limited and the image quality is excellent.
The SpeX guider can be used for 1-5 µm imaging. Although it is not optimal given its engineering-grade array (used for acquisition and guiding), it is still better than the current NSFCAM2 array at JHK. Observers who wish to use SpeX rather than NSFCAM2 for JHK imaging should consult with John Rayner.
CSHELL Upgrade:
The user GUI for CSHELL is being improved so that it has a format similar to that of SpeX. Please note that the macros were changed recently. Users should test their macros before observing.
New Secondary Mirror:
Eric Tollestrup has obtained an NSF grant to measure the spherical aberration of the primary mirror and to fabricate a new secondary mirror with a surface figure that removes the spherical aberration and other high-order aberrations. The first phase of this project, fabricating a prime focus instrument package and measuring the aberrations, has been completed. The analysis and characterization of the primary mirror show that it is actually an oblate ellipsoid, not a paraboloid as required, and has a turned-down edge over a larger area than expected. This results in significant spherical aberration, which will be corrected by the new secondary mirror. We expect a request for quotation for a new secondary mirror to go out soon.
Target-of-Opportunity Observing
We currently have an approved target-of-opportunity proposal to observe Type 1 supernovae at an early stage (within days of being discovered). This has been noted in the letter informing you of your IRTF time allocation. Up to one hour may be requested to allow these observations.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. Please keep submitting your recent publications using the >form provided on our website, or send your reprints to Karan Hughes (hughes@ifa.hawaii.edu). Please acknowledge the IRTF in your publications following the information >shown here and include in your papers the name of the instrument used, as this helps to insure future funding of IRTF instruments.
Last updated 01 September 2008
Proposal Deadline for Semester 2009A (February 1, 2009 - July 31, 2009) is Wednesday, October 1, 2008.
 |
style='color: #0000FF;'>Please review the information and use our new ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Joshua Emery (U. of Tennessee), Gordon Bjoraker (Goddard), Eilat Glikman (Caltech), Michael S. Kelley (U. of Central Florida), James Muzerolle (U. of Arizona), and Russel White (U. of Alabama). This committee consists of three solar system and three non-solar system members.
Target of Opportunity Observing
We currently have an approved target-of-opportunity proposal to observe Type 1 supernovae at an early stage (within days of being discovered). This has been noted in the letter informing you of your IRTF time allocation. Up to one hour may be requested to allow these observations.
Spectral Library Available
The SpeX spectral library for FGKMLT stars is available >here. The spectra are provided in FITS, text, PDF, and postscript formats. The papers by John Rayner, William Vacca, and Michael Cushing presented at this website should be referenced when this library is used.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
Instrumentation Update
SpeX:
We are pleased to announce that John Rayner obtained an NSF grant to upgrade SpeX. The current 1024 x 1024 Aladdin 3 InSb array will be replaced by a 2048 x 2048 Hawaii-2RG array and a new array controller. The upgrade will improve sensitivity and increase pixel sampling and wavelength coverage while maintaining resolving power (optics unchanged). It is important that we replace the array controller, which is now a decade old and has limited spares. This work will start this fall and take about two years. Installation and testing will require downtime of up to one semester towards the end of this period.
MIRSI:
Eric Tollestrup and Charles Lockhart are upgrading MIRSI. This work should be completed by Oct. 2008. The most obvious change will be a new graphical user interface that will have the same look and feel as the facility instrument GUIs. In addition, various hardware, firmware, and software upgrades will make MIRSI more reliable and robust, as well as improve the sensitivity, improve the fix pattern noise, and eliminate various readout artifacts. Contact Eric Tollestrup for more details.
NSFCAM2:
This camera has been used on a conditional basis because of the high read-noise, which decreases the sensitivity at JHK. Eric Tollestrup and Eric Warmbier are presently tracking down the sources of excess noise. To check the status of this instrument before writing a proposal, contact Eric Tollestrup. NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns), since it is background limited and the image quality is excellent.
New Secondary Mirror:
Eric Tollestrup has obtained an NSF grant to fabricate a new secondary mirror with a surface figure that removes the spherical aberration and other high-order aberrations in the primary mirror. The first objective of this project, which is to fabricate a prime focus instrument package and measure the aberrations, has been completed and a new secondary mirror is presently being fabricated.
CSHELL:
The user GUI for CSHELL is being improved so that it has a format similar to that of SpeX. Please note that the macros were changed recently. Users should test their macros before observing.
CSHELL replacement:
Alan Tokunaga has obtained funding through the NSF Major Research Instrumentation program to build a 1-5 micron cross-dispersed spectrograph to replace CSHELL. There is also significant funding from NASA in support of this new initiative, as well as contributions from IRTF operations and cost sharing through the Univ. of Hawaii. The spectral resolving power of this instrument will be approximately 70,000. A PDF copy of the proposal can be downloaded here.
Contact Alan Tokunaga if you have any questions or comments about the proposal. We welcome input from the community on this new major instrument for the IRTF.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to Karan Hughes. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. See here for more information.
Last updated 04 March 2009
Proposal Deadline for Semester 2009B (August 1, 2009 - January 31, 2010) is Wednesday, April 1, 2009.
| style='color: #0000FF;'>Important Announcement for Applications of Observing Time. Please review the information and use our new ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Gordon Bjoraker (Goddard), Joshua Emery (U. of Tennessee), Eilat Glikman (Caltech), Luke Keller (Ithaca College), Michael S. Kelley (U. of Central Florida), and Russel White (Georgia State U.). This committee consists of three solar system and three non-solar system members.
Target of Opportunity Observing
We currently have an approved target-of-opportunity proposal to observe Type 1 supernovae at an early stage (within days of being discovered). This has been noted in the letter informing you of your IRTF time allocation. Up to one hour may be requested to allow these observations.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. The paper on Cool Stars has been submitted to ApJS and will be posted on the website when accepted for publication. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
Personnel Spotlight
 |
Imaikalani "Imai" Namahoe, IRTF Electronics Technician, is a member of the day crew who is responsible for maintaining and repairing the electrical systems on the telescope, which includes the telescope guide cameras and the observing instrumentation. |
| Before joining the IRTF in 1986, Imai worked as an electronic technician on Kauai for Bendix Field Engineering Corp., a subcontractor for NASA, at the top of the Waimea Canyon at Kokee State Park. After 22 years with the IRTF, Imai says he is still very happy to be working "at the top of the world" and to be involved in cutting-edge astronomy. Imai and his wife, Geldine, have three children and two grandchildren. At sea level, Imai enjoys spending time with his grandchildren, surfing, hiking, and working in his yard. | |
Instrumentation Update
SpeX:
SpeX is working normally. Improvements have been made to IR guiding algorithms, allowing guiding on fainter targets.
Work on upgrading SpeX with a 2048x208 Hawaii-2RG (H2RG) array and new array control electronics is underway. We have been able to pool the award money for ISHELL and the SpeX upgrade to fund a foundry run at Teledyne. We expect the foundtry run to yield two science-quality H2RG spectrograph arrays for ISHELL and SpeX, in addition to a very good engineering-quality H2RG array, which we are planning to use in NSFCAM2. The new array controller will be deployed first in NSFCAM2 in 2010 followed by SpeX one year later. Contact John Rayner for more details.
MIRSI:
Eric Tollestrup and Charles Lockhart have upgraded MIRSI, and it is now called MIRSI-2. The most obvious change is a new graphical user interface that has the same look and feel as the facility instrument GUIs. In addition, various hardware, firmware, and software upgrades have made MIRSI more reliable and robust. Phase II of the upgrade, which has the goal of improving the sensitivity, avoiding the fix pattern noise, and eliminate various readout artifacts, has begun. Contact Eric Tollestrup for more details.
NSFCAM2:
This camera has been used on a conditional basis because of the high read-noise, which decreases the sensitivity at JHK. After extensive evaluations, we have determined that the current array should be replaced, and a new array has been ordered. In addition, because of obsolete components, a new set of control electronics will be developed. To check the status of this instrument before writing a proposal, contact Eric Tollestrup. NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns), since it is background limited and the image quality is excellent, or where a wide field of view of 0.04 arcsec pixels is required.
New Secondary Mirror:
Eric Tollestrup has obtained an NSF grant to fabricate a new secondary mirror with a surface figure that removes the spherical aberration and other high-order aberrations in the primary mirror. Two new mirrors being figured by Optical Surface Technologies are expected to be delivered by the end of March. Evaluation of the wavefront errors of mirrors will occur on the IRTF in April. Based on these in situ wavefront errors, one mirror will have additional figuring by Ion Beam Polishing to remove as much of the residual wavefront as is practical. This highly corrected, new secondary mirror is scheduled to be commissioned on the IRTF by the Spring 2010 semester.
CSHELL:
CSHELL is working normally. The new user GUI is now in regular use. Observing macros written for the old GUI should be tested prior to observing.
CSHELL replacement:
Alan Tokunaga has obtained funding through the NSF Major Research Instrumentation program to build a 1-5 micron cross-dispersed spectrograph to replace CSHELL. There is also significant funding from NASA in support of this new initiative, as well as contributions from IRTF operations and cost sharing through the Univ. of Hawaii. The spectral resolving power of this instrument will be approximately 70,000. A PDF copy of the proposal can be downloaded here.
Contact Alan Tokunaga if you have any questions or comments about the proposal. We welcome input from the community on this new major instrument for the IRTF.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. See here for more information.
Last updated 29 September 2009
Proposal Deadline for Semester 2010A (February 1, 2010 - July 31, 2010) is Thursday, October 1, 2009, 5:00 P.M. Hawaii Standard Time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
All the best, Karan
 |
Many of you have had some contact with Karan Hughes. She has the distinction of working with all of the IFA and IRTF Directors since 1983 as well as working with many of you over the years. Generally speaking if something was wrong, we went to Karan for help. |
| The time finally came for her to retire and spend more time with her family and projects she never had time for, including some traveling. We at the IRTF who had the pleasure of working with Karan miss her joyful presence, competence, guiding hand, and storehouse of knowledge. | |
Telescope Allocation Committee
The >current TAC members are Gordon Bjoraker (Goddard), Eilat Glikman (Caltech), Michael S. Kelley (U.
of Maryland), Luke Keller (Ithaca College), Mark Buie (SWRI), and Tracy Beck (STSI). This committee consists of three solar system
and three non-solar system members. Members who have rotated off are Josh Emery (Univ. of Tennessee) and Russel White (Georgia
State University).
Recent Press Releases
See the sidebar for recent new items - a new impact on Jupiter imaged by G. Orton and collaborators and the discovery of a large cloud on Titan and possible cryo-volcano by E. Schaller and collaborators.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. Look here for more information.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. The paper on Cool Stars has been submitted to ApJS and will be posted on the website when accepted for publication. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
Photomixers Music Videos
In case you have not seen it yet, the up and coming astronomy music video group Photomixers have released four music videos. Lead singer Kelley Fast has a growing group of adoring fans in this largely unclassifiable genre of soft rock, folk music, and high altitude craziness.
Videos:
Hotel Mauna Kea (Parody)
Getting Lucky at the Cassegrain (Focus)
Born to Heterodyne
1994 (The Jupiter Impact of 2009)
Personnel Spotlight
 |
Working alone in the quiet seclusion of his office Eric Warmbier is using a CAD program called Protel to create schematics and to layout resistors, capacitors and various integrated circuits that will one day be turned into the electronic boards that will control the IRTF and its instruments. |
| Eric is one of our newest staff members, and he graduated with an electrical engineering degree from Michigan State University. Before joining the IRTF in September 2007, Eric spent five years designing electrical systems for weather and GPS satellites at ITT Space Systems Division. Part of the challenge of working at IRTF these past two years is installing and testing newly designed equipment while avoiding downtime of the telescope, says Warmbier, but working as a team member on the new Stargrasp infrared controller is something new for me, which makes it interesting. The new controller will be used in the planned upgrade of the SpeX instrument and in the brand new iSHELL instrument. When hes not building circuits for the IRTF, Eric enjoys attending his seven-year-old sons activities including football, basketball, baseball, golf and the Cub Scouts. | |
Instrumentation Update
SpeX:
Work on upgrading SpeX with a 2048x208 Hawaii-2RG (H2RG) array and new array control electronics is underway. We have been able to pool the award money for iSHELL and the SpeX upgrade to fund a foundry run at Teledyne. We expect the foundry run to yield two science-quality H2RG spectrograph arrays for iSHELL and SpeX, in addition to a very good engineering-quality H2RG array, which we are planning to use in NSFCAM2. The new array controller will be common to all three instruments. We expect the new array and array controller to be deployed first in NSFCAM2 in 2010 followed by SpeX one year later. Contact John Rayner for more details.
MIRSI:
Eric Tollestrup and Charles Lockhart have upgraded MIRSI, and it is now called MIRSI-2. The most obvious change is a new graphical user interface that has the same look and feel as the facility instrument GUIs. In addition, various hardware, firmware, and software upgrades have made MIRSI-2 more reliable and robust. Phase II of the upgrade, which has the goal of improving the sensitivity, avoiding the fix pattern noise, and eliminate various readout artifacts, has begun. Contact Eric Tollestrup for more details.
NSFCAM2:
This camera has been used on a conditional basis because of the high read-noise, which decreases the sensitivity at JHK. After extensive evaluations, we have determined that the current array should be replaced, and a new array has been ordered. In addition, because of obsolete components, a new set of control electronics will be developed. To check the status of this instrument before writing a proposal, contact Eric Tollestrup. NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns), since it is background limited and the image quality is excellent, or where a wide field of view of 0.04 arcsec pixels is required.
New Secondary Mirror:
Eric Tollestrup is currently testing two new secondary mirrors. The new mirrors are being figured by Optical Surface Technologies in New Mexico. One of the two mirrors will have additional figuring by Ion Beam Polishing to remove as much of the residual wavefront errors (primarily polishing error in the primary mirror) as is practical. The IRTF will be commissioning this highly corrected new secondary mirror during the Spring 2010 semester.
CSHELL:
CSHELL is working normally. The new user GUI is now in regular use. Observing macros written for the old GUI should be tested prior to observing.
iSHELL:
Alan Tokunaga has obtained funding through the NSF Major Research Instrumentation program to build a 1-5 micron cross-dispersed spectrograph to replace CSHELL. The spectral resolving power of this instrument will be approximately 70,000. A PDF copy of the proposal can be downloaded here.
Contact Alan Tokunaga if you have any questions or comments about the proposal. We welcome input from the community on this new major instrument for the IRTF.
Last updated 24 February 2010
Proposal Deadline for Semester 2010B (August 1, 2010 - January 31, 2011) is Thursday, April 1, 2010.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
IRTF Hartley 2 Campaign
We are pleased to announce a comet Hartley 2 observing campaign to be conducted in semester 2010B (Aug. 2010 - Jan. 2011). This comet will reach perihelion in Oct. 2010 and will be visited by the EPOXI spacecraft. Up to two weeks of time will be guaranteed for this campaign. All data obtained will be made public, and observing logs will be requested for archiving. We encourage observing groups to form collaborations to enhance the scientific return from the observations. When submitting a proposal, please note clearly that the proposal is submitted for the campaign. Groups with visitor instruments can participate in the campaign so long as the data and observing logs are allowed to be public. We require that the acquired data be submitted to the PDS and we will assist observers in doing this.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. Look here for more information.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. The paper on Cool Stars has been submitted to ApJS and will be posted on the website when accepted for publication. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF Headlines
The IRTF is making headlines for its detection of methane in an exoplanet using the SpeX instrument. See the articles below.
Articles:
Scientific American
BBC
Space.com
Christian Science Monitor
CBC
The Guardian
 |
Every day of the year the IRTFs Day crew must travel two hours with 4x4 vehicles to the top of Mauna Kea. For the past eight years Maury McOuat has been serving as IRTFs cargo master with the responsibility of driving the facilitys flat-bed truck, which carries the telescopes vital supplies and scientific instruments to the 13,803-foot summit. |
| Over the years McOuat has mastered the art of driving at high altitude through dust, rock-strewn roads and even through snow and ice during the winter months. The first two weeks upon working for IRTF were the hardest McOuat said, but ever since then he has adjusted to the altitude and making the daily trips. Once at the summit McOuat is responsible for cleaning and maintaining the building performing such tasks as changing out the HVAC filters, maintaining an inventory of the facilitys compressed gas and cryogen cylinders, and even re-painting the dome when necessary. McOuat says that working on the outside of the building can be harsh with winds gusting up to 40 miles an hour. But Mauna Kea can also be a place of great beauty, McOuat said, with spectacular views of every corner of the island. Prior to working for the IRTF McOuat spent 20 years working in the construction trades. McOuat said that the most challenging aspect of his job is juggling the many tasks of maintaining the facility along with its eight service vehicles. When he is not working at the IRTF, McOuat enjoys spending time with his family, working on his project vehicles and tending to the tangerine, avocado, lychee and tangelo trees on his three-acre orchard in Puna. | |
Instrumentation Update
SpeX:
Work on upgrading SpeX with a 2048x208 Hawaii-2RG (H2RG) array and new array control electronics continues. We have taken delivery from Teledyne Scientific & Imaging one science grade H2RG detector and one engineering grade H2RG detector has been received for the instrument. Engineering work continues on the new array controller that will be common to three instruments including the SpeX upgrade, iSHELL and NSFCAM2. We expect the new array and array controller to be deployed first in NSFCAM2 in 2010 followed by SpeX one year later. Contact John Rayner for more details.
MIRSI:
Thanks to Charles Lockhart MIRSI is now called MIRSI-2 due to the completed upgrades to the graphical user interface that give it the same look and feel as the facility instrument GUIs. In addition, various hardware, firmware, and software upgrades have made MIRSI-2 more reliable and robust. Future upgrades to the sensitivity, avoiding the fix pattern noise, and eliminating various readout artifacts continue. Contact Bobby Bus for more details.
NSFCAM2:
This camera has been used on a conditional basis because of the high read-noise, which decreases the sensitivity at JHK. After extensive evaluations, we have determined that the current array should be replaced, and a new array has been received. In addition, because of obsolete components, a new set of control electronics is currently being developed. To check the status of this instrument before writing a proposal, contact Bobby Bus. NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns), since it is background limited and the image quality is excellent, or where a wide field of view of 0.04 arcsec pixels is required.
New Secondary Mirror:
Eric Tollestrup continues to test two new secondary mirrors that have been fabricated for the IRTF. The new mirrors have been figured by Optical Surface Technologies in New Mexico. One of the two mirrors will have additional figuring by Ion Beam Polishing to remove as much of the residual wavefront errors (primarily polishing error in the primary mirror) as is practical. The IRTF will be commissioning this highly corrected new secondary mirror during the Spring 2010 semester.
CSHELL:
CSHELL is working normally. The new user GUI is now in regular use. Observing macros written for the old GUI should be tested prior to observing.
iSHELL:
Alan Tokunaga has obtained funding through the NSF Major Research Instrumentation program to build a 1-5 micron cross-dispersed spectrograph to replace CSHELL. Science and engineering grade H2RG infrared detectors have been received from Teledyne Scientific & Imaging and the engineering of the instrument itself is underway. The spectral resolving power of this instrument will be approximately 70,000. A PDF copy of the proposal can be downloaded here. Contact Alan Tokunaga if you have any questions or comments about the proposal. We welcome input from the community on this new major instrument for the IRTF.
Last updated 1 September 2010
Proposal Deadline for Semester 2011A (February 1, 2011 - July 31, 2011) is Friday, October 1, 2010.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. Look here for more information.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. The paper on Cool Stars has been submitted to ApJS and will be posted on the website when accepted for publication. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF Headlines
The IRTF is making headlines for its work on the outer planets and Mars. See the articles below.
Articles:
http://www.sciencedaily.com/releases/2010/03/100316174210.htm
http://www.hanahou.com/pages/magazine.asp?Action=DrawArticle&ArticleID=873&MagazineID=56&Page=6
 |
How do you use a telescope that is over 30 years old to conduct cutting edge astronomy? That was the question posed to one of our newest employees, Dr. Michael Connelley. As one of the IRTFs support astronomers, Connelley believes he has the answer. "Collecting valuable data comes from the proper alignment of the telescope," Connelley said. |
| With the help of the former IRTF Deputy Director Eric Tollestrup, Connelley has been tasked with commissioning two new secondary mirrors for the IRTF Telescope. Connelley is using this opporunity to study everything that goes into how the mirrors are mounted, aligned and how they interact with the rest of the telescope. Although he was recently hired by the IRTF in February of 2010, Connelley is no stranger to the facility having been a graduate student with IRTF from 2003 to 2007. Connelley grew up in Hawaii graduating from Iolani High School in 1996 and receiving his Ph.D. in astronomy from the University of Hawaii. Normally accustomed to working with other astronomers, Connelley said one of his biggest challenges is working with a diverse set of engineers, technicians and managers many of which have more experience at the IRTF and use different skills. Before coming to work with IRTF Connelley was a postdoctoral researcher at the NASA Ames Research Center working with Tom Greene on a spectroscopic survey with embedded protostars. On his own time Connelley enjoys amateur astronomy and has built several of his own telescopes. He also has a strong interest in photography and classic cars. | |
Instrumentation Update
SpeX:
Two significant milestones have been achieved in the program to upgrade SpeX. The H2RG infrared detectors have been received, and the new array controller has its first IRTF specific pre-amplifier electronics board. The new array controller draws from the Stargrasp controller originally designed for Pan-STARRS, but it will have special modified features that make it specific to the IRTF. This IRTF version of the Stargrasp controller will eventually be common to three instruments including the SpeX upgrade, iSHELL and NSFCAM2. The controller and its newly minted pre-amplifier board are presently undergoing bench testing at the Hilo IRTF laboratory. Cryogenic tests of the new low-noise cabling scheme for the H2RG have been successfully completed using the lab test dewar, together with plans to modify the SpeX cryostat to mount the Stargrasp controller. The IRTF Stargrasp controller will initially be deployed and tested in NSFCAM2. Once these tests are successful the IRTF Stargrasp will be used in the SpeX upgrade and in the iSHELL instrument once they have completed fabrication. Contact John Rayner for more details.
MIRSI:
Lars Bergknut is currently on a "Mission of MIRSI." That is, the MIRSI instrument has been removed from the telescope, and Bergknut has taken on the challenge of bench testing its performance prior to breaking it down for a total systems diagnostics and evaluation. The goal is to bring the instrument, which has been on loan to IRTF from Boston University, back to its original liquid helium consumption rate. When it was first received in 2005 from its manufacturer Infrared Labs in Arizona, it had a boil off rate of 16 liters a day. Over the years it has increased to 25 liters a day making the instrument costly to use and maintain. Bergknut and instrument technician Darryl Watanabe are excited to evaluate MIRSIs internal components to see if anything can be repaired or optimized. If MIRSI can be returned to its original opreating parameters or even improved upon, it will make it less expensive for observers to use. MIRSI is expected to be fully refurbished and back in service by October 30, 2010.
 |
| Lars Bergknut delves into the inner workings of the MIRSI Instrument. |
NSFCAM2:
This camera has been used on a conditional basis because of the high read-noise, which decreases the sensitivity at JHK. It has been determined that the current array should be replaced with a new H2RG array from Teledyne Scientific & Imaging. Because of obsolete components in NSFCAM2, a new set of control electronics is currently being developed called the IRTF Stargrasp controller (as mentioned above). The NSFCAM2 camera will be the first instrument to receive the IRTF Stargrasp controller, and it will act as a test bed for the new controller before its deployed in the SpeX upgrade and the iSHELL instrument both currently under fabrication. Be advised that the NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns), since it is background limited and the image quality is excellent, or where a wide field of view of 0.04 arcsec pixels is required. Please check the status of this instrument before writing a proposal by contacting Bobby Bus.
CSHELL:
CSHELL is working normally. The new user GUI is now in regular use. Please be advised that observing macros written for the old GUI should be tested prior to observing. This semester CSHELL is going to be used to demonstrate a calibrating technique that uses custom-made gas cells during an observation run in November 2010. If this proves successful, the resulting data could discover planets outside of our solar system, additionally this approach may also be used to calibrate the new iSHELL instrument, which is currently under development. Contact John Rayner for more details.
iSHELL:
Now that the science and engineering grade H2RG infrared detectors have been received from Teledyne Scientific & Imaging, the engineering of the instrument itself is switching into high gear. The preliminary optical design and scattered light analysis is complete. Optical and mechanical tolerance analysis is continuing. Lead mechanical engineer Tim Bond has already mapped out the different folds the light path will take. Dimensioning and placement of all the instruments various internal components is now currently underway. Bond has been assigned the critical task of translating the lofty science requirements, developed by Dr. John Rayner, into tangible engineering specifications. Another advancement in the iSHELL project is the base material for the Silicon Immersion Grating has been produced by the vendor Toppan Photomask Inc. This material is currently at the University of Texas (UT) where a special grating will be applied using micro-machining techniques that UT has perfected over the last decade. When completed the spectral resolving power of this instrument will be approximately 70,000 making it an exciting new tool in the Northern hemisphere for scientific discovery. A PDF copy of the proposal can be downloaded here. We welcome input from the community on this new major instrument for the IRTF. Contact Alan Tokunaga if you have any questions or comments about the proposal.
New Secondary Mirrors:
With the help of former IRTF deputy director Eric Tollestrup, Michael Connelley is now the primary lead investigator charged with commissioning the IRTFs two new secondary mirrors. The first of the two mirrors, figured by Optical Surface Technologies in New Mexico, received a special silver coating coupled with a protective AL203 overcoat by L&L Optical Services in Santa Ana California. Connelley will be testing the new mirrors performance during an engineering run from September 7th through September 10th, 2010. The commissioning process also presents the opportunity to re-evaluate everything surrounding the performance of the mirrors including the methods we are using to fasten the mirror to the telescope, how we are aligning it to the primary mirror, and how it works with the chopping secondary mechanism. The goal is to improve the telescopes image quality since the new secondary is figured to remove the spherical aberration in the primary mirror.
Last updated 8 March 2011
Proposal Deadline for Semester 2011B (August 1, 2011 - January 31, 2012) is Friday, April 1, 2011.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Thomas Greathouse (SWRI), Michael Gregg (Lawrence Livermore Nat. Lab.), Kevin Luhman (Penn. State), Susan Lederer (Johnson Space Center), Mark Buie (SWRI), and Tracy Beck (STScI). This committee consists of three solar system and three non-solar system members.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please send updates or reprints on your publications to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. Look here for more information.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity on Titan then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. The paper on Cool Stars has been submitted to ApJS and will be posted on the website when accepted for publication. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF Headlines
The IRTF is making headlines for its work on the outer planets and Mars. See the articles below.
Articles:
http://www.jpl.nasa.gov/news/news.cfm?release=2010-397
http://www.jpl.nasa.gov/news/news.cfm?release=2011-028
http://www.space.com/9714-strange-mini-asteroid-vesta.html
http://www.boston.com/news/local/massachusetts/articles/2011/02/27/local_scientists_study_asteroids_for_clues_potential_threats
Personnel Spotlight
 |
How do you take over a position that has been held by the same person for over 20 years? Karan kept copious notes. Ive kept those notes, and I treat them like gospel, said William Walters after taking over Karan Hughess position as the IRTFs Telescope Assistant. Walters has been working for the Institute for Astronomy |
| (IfA) since 2007. In April 2009 Hughes retired, and he began filling in her duties sending out calls for proposals, building the observation schedule, coordinating meetings and answering general questions about observing on IRTF. My biggest challenge is keeping up with all the various different tasks that Karen did and at the same time maintaining the vast array of professional contacts she had within the astronomy community, Walters said. Prior to working at IfA, Walters began working for the University of Hawaii in 2001 at the Hawai`i AIDS Clinical Research Program at the John A. Burns School of Medicine in Honolulu. Ive always enjoyed working with scientists and helping them reach their research goals, Walters said. When Walters is not working, he enjoys cycling, hiking and working in his garden at his home just outside of Hilo town. | |
Instrumentation Update
SpeX:
The effort to upgrade SpeX has made steady progress with the successful completion of the first round of testing of its new SGIR Stargrasp Array Controller. Additional tests are being designed with the final goal of preparing the controller to be hooked up to an actual H2RG infrared detector array.
Please be advised that we anticipate SpeX to be taken off line on Aug. 1, 2012, and it will be unavailable for the entire 2012B semester (Aug. 1, 2012 - Jan. 31, 2013) while it undergoes the scheduled detector upgrades. We strongly recommend observers to plan their observing accordingly. We also expect to accommodate key projects requiring large amounts of observing time using CSHELL, NSFCAM2, MIRSI, MORIS, and visitor instruments. Contact John Rayner for more details.
#
MIRSI:
The MIRSI instrument has been successfully returned to service after undergoing maintenance to remove cold shorts and to optimize its liquid Helium consumption. Since being retuned to service it is using less liquid Helium making it less costly to operate. Much thanks goes out to Lars Bergknut for spearheading the effort and to all those involved with taking it apart and carefully putting it back together again. Contact John Rayner for any questions regarding MIRSI.
#
NSFCAM2:
This camera has been used on a conditional basis because of the high read-noise, which decreases the sensitivity at JHK. Be advised that the NSFCAM2 is currently best suited for observations in the thermal infrared (3-5 microns), since it is background limited and the image quality is excellent, or where a wide field of view of 0.04 arcsec pixels is required. NSFCAM2 recently had its cryogenic coldhead and control computer replaced to keep it operational. Be advised that its scheduled to be taken off the telescope on October 1, 2011 to receive a new infrared detector and array controller. NSFCAM2 will act as a test bed for the new SGIR Stargrasp controller that eventually will be used on the SpeX upgrade and new iShell instrument, which are both under fabrication. Please check the status of this instrument before writing a proposal by contacting Bobby Bus.
CSHELL:
CSHELL is working normally. The new user GUI is now in regular use. Please be advised that observing macros written for the old GUI should be tested prior to observing. This past semester CSHELL has been used to demonstrate a calibrating technique that uses gas cells. Its resulting data is being analyzed, because a similar calibrating mechanism is being considered for use in the new iSHELL instrument. Contact John Rayner for more details.
iSHELL:
Fabrication of the new iSHELL instrument is fully underway. Lead mechanical engineer Tim Bond has reported much progress in designing the many folds the light path will take within the instrument, and he has produced three dimensional mechanical drawings of how the instrument will look and operate. Other components such as the optics, filters and filter/grating carousels are being designed and sourced. The immersion grating is currently being produced at the University of Texas (UT) using micro-machining techniques that UT has perfected over the last decade. When completed the spectral resolving power of the iSHELL instrument will be approximately 70,000 making it an exciting new tool to use in the Northern hemisphere for scientific discovery. A PDF copy of the proposal can be downloaded here. We welcome input from the community on this new major instrument for the IRTF. Contact Alan Tokunaga if you have any questions or comments about the proposal.
New Secondary Mirrors:
Michael Connelley has completed the secondary mirror project, and the new secondary Mirror "A" has been successfully used on the telescope since October 2010. The backup secondary Mirror "B" is currently undergoing silver coating with a protective AL203 overcoat by L&L Optical Services in Santa Ana California. Once coated Mirror "B" will undergo testing and eventual deployment during engineering runs planned this semester. As a result of everything he learned about the IRTF during the secondary mirror upgrade program, Connelley has developed an Image Quality Budget and a clear set of goals that he will be pursuing to improve the telescopes overall performance. This effort will begin with development of a refined Focus Assist Tool that incorporates real-time focus adjustments using temperature and telescope flexure variables. Connelleys long-term plans include using wavefront sensors to further refine the telescopes image quality.
Last updated 1 September 2011
Proposal Deadline for Semester 2012A (February 1, 2012 - July 31, 2012) is Monday, October 3, 2011, 5PM Hawaii time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Thomas Greathouse (Southwest Research Institute), Michael Gregg (Lawrence Livermore Nat. Lab.), Susan Lederer (Johnson Space Center), Kevin Luhman (Penn. State), Andy Rivkin (Johns Hopkins Applied Physics Lab), and Kris Sellgren (Ohio State Univ.). This committee consists of three solar system and three non-solar system members. The members who rotated off are Mark Buie (SWRI) and Tracy Beck (STScI).
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to ensure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX.
Please help us update our bibliography by checking your publications against our list of refereed and unrefereed publications at:
http://irtfweb.ifa.hawaii.edu/research/biblio/Refereed.html
http://irtfweb.ifa.hawaii.edu/research/biblio/Non_Refereed.html
Please send any missing references to William Walters
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity, then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. The papers on Cool Stars are published and are available here: The Infrared Telescope Facility (IRTF) Spectral Library: Cool Stars and An Infrared Spectroscopic Sequence of M, L, and T Dwarfs . Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
 | |
| One millimeter is not much for most people, but for IRTF Mechanical Engineer Morgan Bonnet it makes a big difference when designing astronomical instruments that are built to tolerances within a thousandth of an inch. Bonnet started working for the IRTF in March of 2010 and was immediately put to work designing a secondary mirror cover. The IRTF has two secondary mirrors that are periodically changed out depending on the needs of the observers. The day crew needed a handy and secure way to safely remove the mirror form the telescope and store it. Bonnets work involved interviewing the day crew to discuss their needs and researching how the mirror is handled and attached to the telescope. | |
| Then Bonnet created the mirror cover design using a CAD program and printed the results that were then reviewed then double checked and triple checked for measured accuracy before being sent to IfAs in-house machine shop for final fabrication. | |
 | |
| The results of his labor were immediately appreciated by the day crew who no longer had to worry about accidents while handling the mirror during change outs. | |
 | |
| Bonnets primary duties at the IRTF are to work on designing the cryogenic mechanisms within the iSHELL instrument. Bonnet obtained his mechanical engineering degree in France at the French Institute for Advanced Mechanics (IFMA) and first came to Hawaii by way of six-month internship at the Hawaii Natural Energy Institute where he researched lithium batteries for hybrid vehicles. Bonnet also worked in the automotive industry developing high-efficiency diesel injection systems. | |
| Bonnet said the biggest challenge of working at IRTF are the critical design decisions that go into making the iSHELL instrument. Bonnet said that developing the iSHELL involves merging the optical and mechanical designs together taking into account thermal and operational constraints and making sure the mechanisms can be controlled with an efficient and reliable strategy. The biggest challenge is also the biggest reward when you see it all come together Bonnet said. | |
| When Bonnet is not designing instruments for the IfA, he enjoys all the outdoor activities that Hawaii is famous for including surfing, sailing and hiking. | |
Instrumentation Update
SpeX:
SpeX is a 0.8-5.5 micron Medium-Resolution Spectrograph and Imager and continues to be the most popular instrument at the IRTF. We anticipate that SpeX will be taken offline on February 1st, 2013 and will be unavailable for the entire 2013A semester (Feb. 1, 2013 - Jul. 31, 2013). This is necessary to upgrade SpeX with new arrays and array controllers. The delay of one semester in SpeX downtime has become necessary to build and test the new array controller. We strongly recommend observers to plan their observing accordingly. We also expect to accomodate key projects requiring large amounts of observing time using CSHELL, NSFCAM2, MIRSI, and visitor instruments. For more information on SpeX contact John Rayner for all the details.
NSFCAM2:
Due to delays in the array controller development, we are planning to take NSFCAM2 offline on Feb. 1, 2012 to install a new infrared array. We expect it to be available starting in semester 2012B (Aug. 1, 2012 - Jan. 31, 2013). Due to the schedule uncertainties, proposals to use NSFCAM2 will be accepted provided the program can be also accomplished with the SpeX slit viewer which has a 0.12"/pixel and a 60"x60" field of view. For more information on when it will be returned to service please contact Michael Connelley.
CSHELL:
This is a 1-5.5 micron high-resolution echelle spectrometer. CSHELL has an ongoing observation program that uses a pioneering gas absorption cell in order to conduct the detection of exoplanets. Use of this technology will assist IRTF to identify what level of accuracy is needed in the development of the next generation of near-infrared spectrographs such as the iSHELL instrument that is currently under fabrication. Contact John Rayner for more details. Contact John Rayner for more details.
iSHELL:
The design of the iSHELL instrument continues. A design team including mechanical engineers Gary Mueller and Morgan Bonnet have very busy working under the direction of lead instrument engineer Tim Bond to bring the various components into one cohesive package. Mueller has been tasked to create the conceptual design for the cross-disperser grating and image rotator mechanisms while Bonnet has been tasked with the conceptual design of the filter, slit, and immersion grating changing mechanisms. As the lead instrument designer, Bond is creating the optical bench and fitting the rest of the components into a very compact package. Preliminary CAD drawings show that the final dimensions of the instrument will be smaller than the SpeX instrument. This is ideal for two reasons, Bond said, first because it will be easier to keep cool, and secondly the whole instrument will be less susceptible to flexure.
While the mechanical drawings are reaching completion, lead electronics engineer Peter Onaka is spearheading the effort to fine tune the IRTF Stargrasp array controller, which will eventually control all of information gathered by the iSHELLs infrared detector array. Once complete the IRTF Stargrasp controller will debut on the NSFCAM2 Instrument where it will be fully optimized before being deployed on the iSHELL Instrument.
MORIS:
The MIT Optical Rapid Imaging System (MORIS) is based on an Andor iXon 897 (512x512 pixel) camera, which has high quantum efficiency over the visible wavelength range (> 90% from 480 - 700 nm), low read noise (~6 e-/pixel in conventional 1-MHz readout), low dark current, and the capability to operate in electron-multiplying mode. The camera is thermoelectrically cooled. In addition, MORIS consists of a foreoptics box mounted to the side-facing, dichroic-fed window of the SpeX cryostat (60x60 field of view), and a GPS unit that can provide external triggering of exposures to several-nanosecond accuracy. A 10-slot filter wheel currently contains Sloan g, r, i, z, Johnson V, VR, two long-pass-red filters, an open slot, and one position that is reserved for a visitor filter (1 round). The Andor camera can be operated under either the Windows platform using the vendor supplied Solis program, or under Linux using an IRTF-standard GUI and data viewer (DV). When using the IRTF GUI, MORIS can be controlled simultaneously with SpeX through a single command-line macro, and MORIS provides the option for use as a visible-wavelength guider for SpeX. MORIS has been a PI instrument (PI - Amanda Gulbis, MIT and SAAO/SALT), but we are now making MORIS available to the general IRTF user community. For more information about MORIS, contact Bobby Bus.
Jumps, and things that go bump in the night:
After 30 years of operation some of the devices that move the telescope are beginning to wear. For example, after weeks of smoothly tracking objects in the sky the telescope will periodically jump without warning. Although these jumps are rare and affect few observation programs, staff Astronomer Michael Connelley has painstakingly analyzed recordings of these events and has developed a systematic plan to identify the cause. The plan calls for the use of 8 accelerometers stationed at key locations behind the secondary mirror. The goal is to observe which accelerometers record a jolt during a jump, and which dont in order to isolate the source of the jumps. Connelley estimates that it will require a month of data collection with computer time stamping while the telescope is tracking objects in the sky before a clear determination can be made.
In addition to the jumps occasionally the telescopes dome will refuse to move. For years telescope mechanic Sammie Pung has been able to make magical adjustments to the dome rollers and various moving parts to keep things moving smoothly. Lately these fixes seem to be less effective, and the dome has periodically burned out its control motors. A consultant from Geo Tech Industries has been called in to assist IRTF engineers to quickly identify a solution. Aside from making the dome move smoothly, their preliminary analysis suggests that modernizing the domes motors and electronic controllers may be required. Currently the dome uses three modestly powered DC motors with an older design that utilizes brushes making them susceptible to overheating. These motors could be replaced with modern powerful brushless motors that are less susceptible to over heating and use sturdy permanent magnets to generate more speed and torque.
Last updated 1 March 2012
Proposal Deadline for Semester 2012B (August 1, 2012 - January 31, 2013) is Monday, April 2, 2012, 5PM Hawaii time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Thomas Greathouse (Southwest Research Institute), Kris Sellgren (Ohio State University), Susan Lederer (Johnson Space Center), Andy Rivkin (Johns Hopkins Applied Physics Lab), Jason Surace (CalTech.) and Kevin Luhman (Penn. State Univ.) This committee consists of three solar system and three non-solar system members. Michael Gregg (Lawrence Livermore Nat. Lab.) rotated off this semester.
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. We have websites for refereed and unrefereed publications based on IRTF data: --- Please check these sites and inform William Walters of any missing references. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to ensure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity, then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
Personnel Spotlight
Charles Lockhart first made his presence known in the IRTF laboratory when he removed all the "caps lock" buttons from every keyboard in the lab, because the "caps lock" key causes havoc when using vi editor. Lockhart originally worked at IRTF as a student hire from 1996 to 1998 when he was studying electrical engineering at UH Manoa. He later returned in 2002 to his current position as IRTFs Embedded Software Engineer. Before working at IRTF Lockhart designed electronics and embedded software for use with satellite testing and control systems and embedded software for high-end broadband network testing equipment.
Lockhart is currently working on the IRTFs array controller, instrumentation and facility systems, and he especially enjoys working on technical solutions to accomplish science directed goals. Outside of work his interests vary from wooden canoe building, martial arts, and participating in Boy Scouts with his three sons. So if you ever need a "caps lock" button, dont ask Charles. He throws them away.
Instrumentation Update
SpeX:
SpeX is a 0.8-5.5 Micron Medium-Resolution Spectrograph and Imager and continues to be the premier facility instrument at the IRTF. Revised plans for the SpeX instrument are for it to be removed from the telescope on October 1, 2013 to undergo scheduled upgrades to its infrared arrays and control electronics. The most recent development is observers have been using SpeX in conjunction with the MORIS instrument acting as a guider. This has allowed for the collection of data on objects that were once too faint for the IRTF to guide on. For more information on this novel approach to using SpeX with MORIS contact Bobby Bus. For more information specifically concerning SpeX contact John Rayner for all the details.
CSHELL:
This instrument contains a 1-5.5 micron high-resolution echelle spectrometer (256 x 256 InSb array). IRTF engineer Tony Denault recently modified the instruments control software to include the ability to change the position angle when CSHELL is rotated into a non-standard rotation. Denault also added support for the focus collimation tool. Contact John Rayner for more details.
MORIS:
The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS has become the most talked about instrument on the IRTF. MORIS stands for MIT Optical Rapid Imaging System, and it was built by the Massachusetts Institute of Technology following on the successes of the POETS instrument. Amada Gulbis put a lot of care into refining its image quality over the course of several semesters, and its GUI has been developed to be familiar to anyone who has used any of the IRTFs facility instruments. MORIS can be used simultaneously with SpeX and can even guide SpeX in place of Guidedog. For more information on this exciting approach to using SpeX with MORIS contact Bobby Bus.
NSFCAM2:
This instrument has developed a level of high read-noise, which decreases the sensitivity at JHK. It will be removed from the telescope on October 1, 2012 for upgrades to its infrared detector and array controller. NSFCAM2 will act as a test platform for the newly designated ARC array controllers that will also be deployed on the SpeX and iShell instruments. Please note: due to unavailability of the instrument in the last quarter of 2012, proposals submitted to use NSFCAM2 will be accepted provided the program can be also accomplished with the SpeX instrument. For more information on NSFCAM2 please contact Michael Connelley.
MIRSI:
The MIRSI instrument has experienced significant problems with its control electronics and has been removed from the telescope for evaluation. At this time the IRTF is weighing the options of repairing the instrument and continuing to support it for scientific observations. For more information concerning the MIRSI instrument contact Bobby Bus.
iSHELL:
The year 2012 marks a new direction in the fabrication of the iSHELL instrument particularly with respects to its array controller electronics. It has been decided to use a commercially available array controller from Astronomical Research Cameras. This third generation controller has a growing user base and demonstrative ability to meet the engineering requirements of the iSHELL instrument. Fine-tuning the ARC controller to be used at IRTF is already underway at the IRTFs Hilo electronics laboratory. A Preliminary Design Review is scheduled for September 2012. Stay tuned for more developments.
Jumps, and things that go bump in the night:
Staff astronomer Michael Connelley has reduced the data collected from 8 accelerometers positioned on the telescope and concluded that the source of the periodic jumps is the chopping secondary mechanism. These jumps have been happening when the telescope slews in the East-West direction. The next phase of the repair will include resurrecting the hexapod from storage and modifying it for use with our current inventory of secondary mirrors. The hexapod will then be mounted onto the telescope and used for regular observations while the chopping secondary is brought down to the Hilo laboratory and refurbished.
If you have observed on the IRTF recently, you might have experienced our telescope operators disappearing from view to put a come-along winch on the dome. After 30 years of operation the dome has become prone to stalling. The IRTF engineers, day crew, and IFA machine shop head have made a number of improvements and have completed a long-term solution to this problem. Over the next 6 months a new set of brushless Baldor servo motors will be installed and the bottom of the dome rail will be resurfaced. The new motors will generate more torque, and the control electronics will allow the motors to move the dome more precisely.
Mirror Re-aluminizing:
Its been 10 years since the IRTFs primary mirror has been recoated with its reflective aluminum finish. Since then it has held up remarkably well. This is due in large part to the regularly scheduled cleaning by the day crew. In particular, Sammie Pung has been very meticulous with making sure this is done properly. Nevertheless its finally time for a re-coating, and this will begin in the last week of July 2012 and extend until the first week of August 2012. Since its likely the current day crew will have retired by the time it needs to be done again, Michael Connelley has taken on the task of documenting every detail of this process so that the years of knowledge and experience that the current day crew has can be passed on to the next generation.
Last updated 1 September 2012
Proposal Deadline for Semester 2013A (February 1, 2013 - July 31, 2013) is Monday, October 1, 2012, 5PM Hawaii time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Thomas Greathouse (SWRI), Andy Rivkin (Johns Hopkins Applied Physics Lab), Kris Sellgren (Ohio State University), Jason Surace (CalTech.), Leslie Young (SWRI) and Kevin Covey (Cornell Univeristy) This committee consists of three solar system and three non-solar system members. The members who rotated off are Kevin Luhman (Penn. State Univ.) and Susan Lederer (Johnson Space Center).
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. Look here for more information.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity, then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are reminded that the spectral library is available >here. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Personnel Spotlight
"As a young man growing up in New Jersey little did I know that on one especially freezing night while trying to raise a jammed window on a British sports car, that one day on an especially freezing night I would be on top of a telescope dome on Mauna Kea trying to close a stuck telescope shutter. A four year visit to Missouri for a degree in commercial art and a several year stint as a magazine art director in New York didnt bring forth any images of me transferring liquid helium into an infrared instrument used to detect volcanoes on one of Jupiters moons. Spending time as a Peace Corps volunteer in the Kingdom of Tonga setting up a facility to maintain and repair audio visual gear also didnt create any new occupational trends toward astronomy in my mind. Although it did bring me to Hilo for orientation training, and if I had chosen the daytrip hike to Mauna Kea over swim Hapuna Beach things may have turned out quite different as the hikers memories were much more painful than the snorkelers. Upon returning to Hilo after the 2 years in Tonga I was involved in selling and repairing both mechanical and electronic business equipment. Which, as a small business enterprise, is equivalent to working at least two jobs and paying yourself for something less than one. That’s when I imagined working on Mauna Kea, which became a reality in April 1983. What I never imagined was what a wonderful, intelligent, enthusiastic, and helpful group of co-workers, managers, engineers, and visiting astronomers I would encounter on a daily basis, all of who made me look like I knew what I was doing for the past 3 decades. I havent encountered any stuck windows around the house yet, but if I do Ill put on boots and a parka and get busy."
Since retiring, Koenig has been busy in his woodshop making Shoji Lamps. We wish him all the best and commend him for his 30 years of service to the IRTF.
Instrumentation Update
NSFCAM2:
After developing a high level of read-noise NSFCAM2 has been brought to the Hilo laboratory for upgrades to its H2RG infrared detector and array controller. NSFCAM2 will act as a test platform for Astronomical Research Cameras (ARC) array controllers that will eventually be utilized on the SpeX and iShell instruments. The new ARC controller is showing enormous potential as laboratory bench tests have already revealed them to be working at desirable specifications for infrared astronomy. NSFCAM2 is scheduled to be retuned to operation on the telescope in January 2013. For more information please contact Michael Connelley.
SpeX:
SpeX is a 0.8-5.5 micron medium-resolution spectrograph and imager. SpeX will not be available during Semester 2013B. It will be removed from the telescope on August 1 2013 for upgrade. SpeX will be back on the telescope at the start of Semester 2014A, February 1 2014. The upgrade involves involves replacing the 1024x1024 Aladdin 3 InSb array in the spectrograph with a 2024x2048 Hawaii-2RG array from Teledyne. We expect improved sensitivity and increased wavelength coverage in the standard observing modes. The resolving power and slit sizes will remain the same although pixel sampling will be increased. The current engineering quality 512x512 InSb array in the slit viewer will be replaced with the array to be removed from the spectropgraph, resulting in improved imaging sensitivity and cosmetics. The field of view and pixel scale of the slit viewer will be unchanged. The arrays will be run by new ARC controllers. The MORIS CCD camera (see below), which is fed by a selectable dichroic inside SpeX, is now available as a facility visible guider for SpeX. This has been particularly valuable for SpeX observations of small solar system objects where accurate guiding on targets as faint as V magnitude of 20 is now routinely possible. For more information about SpeX contact John Rayner.
MORIS:
The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was built by the Massachusetts Institute of Technology following on the successes of the POETS occultation systems. MORIS can be used simultaneously with SpeX and can even guide SpeX in place of Guidedog. For more information on this technique contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. The instrument GUI now includes the ability to change the position angle when CSHELL is rotated into a non-standard rotation (although CSHELL still has to be rotated manually). Support for the autofocus and collimation tool has also be added. We expect to replace CSHELL with iSHELL (see below) in about 2015. Contact John Rayner for more details.
MIRSI:
The MIRSI instrument has experienced significant problems and has been removed from the schedule. In the short term MIRSI will not be available; however, because of its niche capabilities it is being evaluated for repairs and possible upgrade of its array controller electronics. For more information concerning the MIRSI instrument contact Bobby Bus.
iSHELL:
iSHELL is 1-5 micron R=70,000 cross-dispersed spectrograph currently under construction at IRTF. It has about twice the resolving power and up to about 50 times the one-shot wavelength covererage of CSHELL, which it will replace. Like SpeX, iSHELL will employ an infrared slit viewer for efficient target acquisition and guiding. iSHELL will undergo a preliminary design review late this year. In order to meet its fabrication schedule IRTF will be enlisting the help of an engineering firm that will assist with the development of this instrument to the critical design review stage. A PDF copy of the 2008 proposal to NSF can be downloaded here. Contact Alan Tokunaga or John Rayner if you have any questions regarding iSHELL.
Dome Upgrade (update):
After 30 years of operation the IRTF’s dome has become prone to jamming. A replacement set of powerful brushless Baldor servo motors are being bench tested in the Hilo laboratory along with their electronic controllers. Once integrated into the telescope control software (TCS), the motors will be able to move the dome more precisely thereby allowing the next critical phase to begin, which is the grinding and smoothing of the dome’s rail surface.
Last updated 1 March 2013
Proposal Deadline for Semester 2013B (October 1, 2013 - January 31, 2014) is Monday, April 1, 2013, 5PM Hawaii time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Ted Kostiuk (Goddard), Andy Rivkin (Johns Hopkins Applied Physics Lab), Kris Sellgren (Ohio State University), Jason Surace (CalTech.), Leslie Young (SWRI-Boulder) and Kevin Covey (Cornell University) This committee consists of three solar system and three non-solar system members. Tommy Greathouse (SWRI-San Antonio) recently rotated off the TAC.
C/2012 S1 (ISON) observing campaign
We encourage proposals to observe comet C/2012 S1 (ISON), a recently discovered Oort Cloud comet with perihelion passage on Nov. 28, 2013. It is expected to become extremely bright with a significant amount of daytime availability while the comet is brightest (see link to additional information below). Approximately 170 hours of observing time will be set aside for this campaign. All data obtained will be made public (within one week), and observing logs will be requested for archiving. We encourage observing groups to form collaborations to enhance the scientific return from the observations. When submitting a proposal, please note clearly that the proposal is submitted for the campaign. Groups with visitor instruments can participate in the campaign so long as the data and observing logs are allowed to be public.
Additional information on comet ISON observing can be downloaded at:
dl.dropbox.com/u/12111886/additional_information_for_comet_ISON.pdf
Science Highlights and Publications
Our Science Highlights page is updated regularly as we receive the latest highlights from you. These highlights are sent to our funding agencies, NASA and NSF, to keep them abreast of the exciting and useful science obtained at the IRTF. See examples >here. Please continue to submit your new publications using the >form provided on our website, or send your reprints to William Walters. Please acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments. For AAS publications, please include the facility keyword and instrument, such as IRTF:SpeX. Look here for more information.
Non-standard Observing Programs
We have a program to observe Titan whenever it is up and SpeX is on the telescope "Titan's Methane Meteorology: Context for Cassini Titan Flybys T63-T66" (PI: E. Schaller). This program is aimed at discovering new cloud features on Titan (see the Press Release). If there is evidence for activity, then adaptive optics imaging is obtained at the Gemini or Keck observatories. The observing time is noted on the schedule and there is flexibility on when the observations are taken.
IRTF Spectral Library
Users are reminded that the spectral library is available >here. Citations for the papers that have been published can be found here. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Instrumentation Update
NSFCAM2:
The IRTF is pleased to announce recent upgrades to NSFCAM2. The instrument now has an additional filter, and tests in the Hilo laboratory have shown very low electronic read noise from its new H2RG infrared array and Astronomical Research Cameras (ARC) array controller. NSFCAM2 has been returned to the telescope for commissioning and will be available for observing in the 2013B semester. For more information on NSFCAM2 please contact Michael Connelley.
SpeX:
The SpeX instrument will available for the 2013B semester. SpeX is a 0.8-5.5 micron medium-resolution spectrograph and imager. Its scheduled upgrade has been pushed back to February 1, 2014 when it will be removed from the telescope to receive a new infrared array and array controller. SpeX is now routinely being used in conjunction with the MORIS instrument acting as a guider. This has allowed for the collection of data on 20th magnitude objects measured in the visible wavelengths. For more information on using SpeX with MORIS contact Bobby Bus. For more information specifically concerning SpeX contact John Rayner.
MORIS:
The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was built by the Massachusetts Institute of Technology following on the successes of the POETS occultation systems. MORIS can be used simultaneously with SpeX and can even guide SpeX in place of Guidedog. For more information on this technique contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. The instrument GUI now includes the ability to change the position angle when CSHELL is rotated into a non-standard rotation. Support for the focus collimation tool has also be added. Contact John Rayner for more details.
MIRSI:
Due to a failure of the array electronics, MIRSI continues to be unavailable in the 2013B semester. We are considering upgrading the MIRSI electronics, but this work has still not been scheduled. Please watch this site for future updates on the status of MIRSI, or contact the IRTF staff for more information.
Dome and Shutter Upgrades (update):
Three powerful brushless Baldor servo motors have been successfully tested on the dome, and control of the new motors has been integrated into the telescope’s control software (TCS). The next step will entail grinding and smoothing the dome’s rail surface. In addition, the dome’s shutter will be getting an upgrade to its electrical bus. The exposed open bar setup will be replaced by an insulated flexible cable and cable tray system. Both upgrades are scheduled to be completed by the second half of 2013.
Last updated 15 January 2014
Proposal Deadline for Semester 2014A (February 1, 2014 - July 31, 2014) is Tuesday, October 1, 2013, 5PM Hawaii time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Kevin Covey (Cornell University), Ted Kostiuk (Goddard Space Flight Center), Vishnu Reddy (Planetary Science Institute), Kris Sellgren (Ohio State University), Jason Surace (Caltech), and Leslie Young (SWRI). This committee consists of three solar system and three non-solar system members. The member who rotated off is Andy Rivkin (Johns Hopkins Applied Physics Lab).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments.
Non-standard Observing Programs
The C/2012 S1 (ISON) observing campaign will not be extended into semester 2014A. However we would like to continue archiving any additional comet ISON data on a voluntary basis. Information on comet ISON can be found at:
dl.dropbox.com/u/12111886/additional_information_for_comet_ISON.pdf
sungrazer.nrl.navy.mil/index.php?p=ison
The IRTF comet ISON data archive is online:
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. Citations for the papers that have been published can be found here. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Instrumentation Update
NSFCam:
On the night of January 10th, NSFCam suffered significant damage when the LN2 precharge can exploded due to an ice plug. Fortunately, no one was injured in this accident. Whereas the array appears undamaged and has passed a warm functionality test, many of the lenses are cracked and the cryostat was significantly damaged. NSFCam will be unavailable until further notice. For more information contact Michael Connelley.
SpeX:
SpeX will not be available in semester 2014A. It will be removed from the telescope and returned to Hilo on February 3 2014 for upgrade. Since the MORIS CCD imager is mounted on SpeX it will also be unavailable until SpeX is back. The upgrade involves replacing the now obsolete spectrograph and slit viewer array controllers (few spare boards remain) with new array controllers from ARC, Inc. The new controllers have been built and are currently being tested. The Aladdin 1024x1024 InSb array in the spectrograph will be replaced with a science grade 2048x2048 Hawaii 2RG array, which is already in-hand. The engineering grade 512x512 Aladdin InSb array in the slit viewer will be replaced by the science grade InSb array currently in the spectrograph. We expect improved sensitivity and increased simultaneous wavelength range in the spectrograph and improved sensitivity in the slit viewer/IR guider (same 60"x60" FOV). Resolving power will remain unchanged but with improved pixel sampling. A new version of Spextool will be available for the changed array format. For more information contact John Rayner.
MORIS:
Due to the SpeX upgrade, MORIS will not be available in the 2014A semester. The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was built by the Massachusetts Institute of Technology following on the successes of the POETS occultation systems. MORIS can be used simultaneously with SpeX and can even guide SpeX in place of Guidedog. For more information on this technique contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. CSHELL is working normally. The built-in CCD guider is less reliable when used under high background conditions (daytime guiding). Contact John Rayner for more details.
iSHELL:
Work on the Immersion Grating Echelle Spectrograph (iSHELL) continues. Design work on the mechanisms is almost finished, and machine shop drawings are being produced for the mechanisms. All of the optical components for the spectrograph and slit viewer have been ordered. The priority now is to finish the cryostat and calibration box design. We will have delivery of our science grade detector this month. A second science grade immersion grating has been fabricated by the University of Texas Austin group headed by Dan Jaffe. Our plan is to begin assembly of the mechanisms in the spring of 2014 and followed by the assembly of the cryostat during the summer.
MIRSI:
Due to a failure of the array electronics, MIRSI continues to be unavailable in the 2014A semester. We are considering upgrading the MIRSI electronics, but this work has still not been scheduled. Please watch this site for future updates on the status of MIRSI, or contact the IRTF staff for more information.
Dome and Shutter Upgrades Completed:
Upgrades to the IRTF’s dome and shutter mechanisms are complete. The dome drive system was refitted with three brushless servomotors from Baldor. The dome’s entire bottom rail was also machined to a smooth finish. This process required special programming to the telescope’s control system in order to move the dome at a very slow and controlled speed for the cutting tool. A slight angled profile was also restored to the bottom of the dome rail. This profile became worn away over the years but once restored proved vital to the way the dome centered itself with its guide wheels. The end result is that the now dome moves smoothly. Additional work to replace worn out dome supporting wheels and guide rollers are in progress.
The shutter mechanism was also upgraded to use power cables sheathed in a flexible plastic energy chain that is tucked neatly away in a curved trough that matches the arch of the dome. The present shutter power bus bar is prone to several types of failure modes. This upgrade, when completed, should eliminate these problems and make the shutter operate more reliably.
Last updated 14 March 2014
Proposal Deadline for Semester 2014B (August 1, 2014 - January 31, 2015) is Tuesday, April 1, 2014, 5PM Hawaii time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Sean Brittain (Clemson Univ.), Kevin Covey (Cornell University), Ted Kostiuk (Goddard Space Flight Center), Mark Lacy (NRAO), Vishnu Reddy (Planetary Science Institute), Kris Sellgren (Ohio State University), Diane Wooden (Ames Research Center) and Leslie Young (SWRI). This committee consists of four solar system and four non-solar system members. The member who rotated off is Jason Surace (IPAC).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments.
Non-standard Observing Programs
Comet C/2013 A1 Siding Spring will make a very close approach to Mars in 2014B and observations of this comet are of strong interest to NASA. Further information can be found here:
https://dl.dropboxusercontent.com/u/12111886/Comet_Siding_Spring.pdf
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Instrumentation Update
NSFCAM2:
On the night of January 10, 2014, NSFCAM suffered significant damage when the LN2 precharge can burst with great force due to the improper positioning of its pressure relief mechanism. Fortunately, no one was injured in this accident. The array and filter wheel appear undamaged and have passed a warm functionality test. Unfortunately many of the lenses are cracked and the cryostat was significantly damaged. NSFCAM will be unavailable until further notice and is undergoing evaluation for repair. For more information contact Michael Connelley.
SpeX:
SpeX will be available in semester 2014B. It is currently undergoing a scheduled upgrade. This upgrade involves replacing the now obsolete spectrograph and slit viewer array controllers with new array controllers from ARC, Inc. The new controllers have been built and are currently being tested. The Aladdin 1024x1024 InSb array in the spectrograph will be replaced with a science grade 2048x2048 Hawaii 2RG array, which is already in-hand. The engineering grade 512x512 Aladdin InSb array in the slit viewer will be replaced by the science grade InSb array currently in the spectrograph. We expect improved sensitivity and increased simultaneous wavelength range in the spectrograph and improved sensitivity in the slit viewer/IR guider (same 60"x60" FOV). Resolving power will remain unchanged but with improved pixel sampling. As part of the upgrade a new version of Spextool will be available for the revised array format. For more information contact John Rayner.
MORIS:
The MORIS instrument will be available in the 2014B semester. The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was built by the Massachusetts Institute of Technology following on the successes of the POETS occultation systems. MORIS can be used simultaneously with SpeX and can even guide SpeX in place of Guidedog. For more information on this technique contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. CSHELL is working normally. The built-in CCD guider is less reliable when used under high background conditions (daytime guiding). Contact John Rayner for more details.
iSHELL:
Work on the Immersion Grating Echelle Spectrograph (iSHELL) has accelerated. Its various metal components and optical bench are in the process of being machined. Assembly of its various slit and filter mechanisms is on schedule to begin soon followed by the assembly of the cryostat this summer.
MIRSI:
Due to a failure of the array electronics, MIRSI continues to be unavailable in the 2014B semester. We are considering upgrading the MIRSI electronics, but this work has still not been scheduled. Please watch this site for future updates on the status of MIRSI, or contact the IRTF staff for more information.
Last updated 4 September 2014
Proposal Deadline for Semester 2015A (February 1, 2015 - July 31, 2015) is Wednesday, October 1, 2014, 5PM Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Gerbs Bauer (JPL), Sean Brittain (Clemson Univ.), Kevin Covey (Western Washington Univ.), Catherine Espaillat (Boston Univ.), Ted Kostiuk (Goddard Space Flight Center), Mark Lacy (NRAO), Vishnu Reddy (Planetary Science Institute), and Diane Wooden (Ames Research Center). This committee consists of four solar system and four non-solar system members. The members who rotated off are Kris Sellgren (Ohio State) and Leslie Young (SWRI).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments.
IRTF Spectral Library
Users are encouraged to make use of the spectral library, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Instrumentation Update
SpeX:
SpeX is available for 2015A after successfully receiving upgrades to its infrared array and electronic array controllers. Improved sensitivity and increased simultaneous wavelength range in the spectrograph and improved sensitivity in the slit viewer/IR guider (same 60"x60" FOV) is evident. Resolving power is unchanged, but pixel sampling has been improved. As part of the upgrade, a new version of Spextool is being developed to take advantage of these improvements. For more information contact John Rayner.
MORIS:
The MORIS instrument will be available in the 2015A semester. The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was built by the Massachusetts Institute of Technology following on the successes of the POETS occultation systems. MORIS can be used simultaneously with SpeX and can even guide SpeX in place of Guidedog. For more information on this technique contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. CSHELL is working normally. The built-in CCD guider is less reliable when used under high background conditions (daytime guiding). Contact John Rayner for more details.
iSHELL:
Work on the Immersion Grating Echelle Spectrograph (iSHELL) has continued. The design and fabrication of nearly everything has been completed. The assembly process of the cryostat and mechanisms has started. For more information, contact Alan Tokunaga or John Rayner.
NSFCAM2:
NSFCAM suffered significant damage when the LN2 precharge can burst due to the improper positioning of its pressure relief mechanism, which led to an ice plug. NSFCAM will be unavailable until further notice and is undergoing evaluation for repair or modification for use with adaptive optics.
MIRSI:
Due to a failure of the array electronics, MIRSI continues to be unavailable in the 2015A semester. We are considering upgrading the MIRSI electronics, but this work has not been scheduled. Please watch this site for future updates on the status of MIRSI, or contact the IRTF staff for more information.
Last updated 2 March 2015
Proposal Deadline for Semester 2015B (August 1, 2015 – January 31, 2016) is Wednesday, April 1, 2015, 5PM Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are Gerbs Bauer (JPL), Chad Bender (Penn. State University), Sean Brittain (Clemson Univ.), Catherine Espaillat (Boston Univ.), Mark Lacy (NRAO), Vishnu Reddy (Planetary Science Institute), Michael Wong (UC Berkeley), and Diane Wooden (Ames Research Center). This committee consists of four solar system and four non-solar system members. The members who rotated off are Kevin Covey (Western Washington Univ.) and Ted Kostiuk (Goddard Space Flight Center).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments.
IRTF Cool Star Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, which is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Instrumentation Update
SpeX:
SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. For more information see the instrumentation page of the website or contact John Rayner.
MORIS:
The MORIS instrument is available in the 2015B semester. The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was made available to IRTF users by A. Gulbis. MORIS can be used simultaneously with SpeX and can be used as an optical guider. For more information contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. CSHELL is working normally. The built-in CCD guider is less reliable when used under high background conditions (daytime guiding). Contact John Rayner for more details.
iSHELL:
Assembly of the Immersion Grating Echelle Spectrograph (iSHELL) continues. Initial cool down testing has been completed, and the assembly process of the optics and internal mechanisms has begun. For more information, contact Alan Tokunaga or John Rayner.
Last updated 28 August 2015
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are
Gerbs Bauer (JPL),
Chad Bender (Penn. State University),
Sean Brittain (Clemson Univ.),
Peter Capak (IPAC),
Catherine Espaillat (Boston Univ.),
Nick Moskovitz (Lowell Observatory),
Michael Wong (UC Berkeley), and
Diane Wooden (Ames Research Center).
This committee consists of four solar system and four non-solar system members. The members who rotated off are Mark Lacy (NRAO) and Vishnu Reddy (Planetary Science Institute).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments.
IRTF Cool Star Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, which is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Instrumentation Update
SpeX:
SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. For more information see the instrumentation page of the website or contact John Rayner.
MORIS:
The MORIS instrument is available in the 2015B semester. The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was made available to IRTF users by A. Gulbis. MORIS can be used simultaneously with SpeX and can be used as an optical guider. For more information contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. CSHELL is working normally. The built-in CCD guider is less reliable when used under high background conditions (daytime guiding). Contact John Rayner for more details.
iSHELL:
Assembly of the Immersion Grating Echelle Spectrograph (iSHELL) continues. Initial cool down testing has been completed, and the assembly process of the optics and internal mechanisms has begun. We are planning for extensive laboratory testing during the next 7 months and for commissioning of the instrument to begin in semester 2016A. For more information, contact Alan Tokunaga or John Rayner.
Last updated 29 February 2016
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Note that we have a new instrument, the immersion grating echelle spectrograph (iSHELL), that will be available for general use starting on Oct. 1, 2016. A manual for preparation of proposals is available >here.
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF facility instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are
Gerbs Bauer (JPL),
Chad Bender (Penn. State University),
Adam Burgasser (UC San Diego),
Peter Capak (IPAC),
Catherine Espaillat (Boston Univ.),
Henry Hsieh (Planetary Science Institute),
Nick Moskovitz (Lowell Observatory), and
Michael Wong (UC Berkeley).
This committee consists of four solar system and four non-solar system members. The members who rotated off are Diane Wooden (Ames Research Center) and Sean Brittain (Clemson Univ.).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to insure future funding of IRTF instruments.
IRTF Cool Star Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, which is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
IRTF Data Archive:
Beginning with the 2016B semester, raw data taken with IRTF facility instruments will be made publicly available via an online archive following a proprietary period that begins at the end of the semester, and extends for 12 months. All data files obtained during the 2016B semester will be made available to the public through the archive beginning Feb. 1, 2018. Past users of the IRTF may notice small changes in observing procedures that are being made in preparation for the archive, and are necessary to produce more uniform data products that will be usable by other researchers in the future.
Instrumentation Update
SpeX:
SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. For more information see the instrumentation page of the website or contact John Rayner.
MORIS:
The MORIS instrument is available in the 2015B semester. The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for MIT Optical Rapid Imaging System, and it was made available to IRTF users by A. Gulbis. MORIS can be used simultaneously with SpeX and can be used as an optical guider. For more information contact Bobby Bus.
CSHELL:
CSHELL is a 1-5.5 micron high-resolution echelle spectrometer. It uses a 256 x 256 InSb array. CSHELL is working normally. The built-in CCD guider is less reliable when used under high background conditions (daytime guiding). Due to the start of iSHELL operation in the 2016B semester, CSHELL will be available only until Sept. 30, 2016. Contact John Rayner for more details.
iSHELL:
The immersion grating echelle spectrograph (iSHELL) is a 1.1-5.3 micron cross-dispersed spectrograph (up to a resolving power of R=70,000) and imager. The instrument has been assembled and is undergoing laboratory testing at IfA Manoa. Delivery of iSHELL to the telescope is now expected in June 2016, with a commissioning phase lasting until Sept. 30, 2016. iSHELL is expected to become available for public use starting Oct. 1, 2016 under shared risk. For more information see the instrumentation page of the website or contact Alan Tokunaga or John Rayner.
Last updated 07 September 2016
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Note that we have a new instrument, the immersion grating echelle spectrograph (iSHELL), which is available for general use in semester 2017A. A manual for preparation of proposals is available >here.
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF facility instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are
Chad Bender (Penn. State Univ.),
Adam Burgasser (UC San Diego),
Peter Capak (IPAC),
Henry Hsieh (Planetary Science Institute),
Serena Kim (Univ. of Arizona),
Nick Moskovitz (Lowell Observatory),
Silvia Protopapa (Univ. of Maryland), and
Michael Wong (UC Berkeley).
This committee consists of four solar system and four non-solar system members. The members who rotated off are Gerbs Bauer (JPL) and Catherine Espaillat (Boston Univ.).
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to ensure future funding of IRTF instruments.
IRTF Cool Star Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, and is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
IRTF Data Archive:
Effective August 1, 2016, raw data taken with IRTF facility instruments will be made publicly available via an online archive following a proprietary period of 18 months from the date of observation. Past users of the IRTF may notice small changes in observing procedures that have been made in preparation for the archive, and are necessary to produce uniform data products that will be usable by other researchers in the future.
Instrumentation Update
SpeX:
>SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. For more information see the instrumentation page of the website or contact Bobby Bus or Mike Connelley.
MORIS:
The MORIS instrument is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for >MIT Optical Rapid Imaging System, and was made available to IRTF users by A. Sickafoose. MORIS can be used simultaneously with SpeX and can be used as an optical guider. For more information contact Bobby Bus.
iSHELL:
The immersion grating echelle spectrograph (iSHELL) is a 1.1-5.3 micron cross-dispersed spectrograph (up to a resolving power of R=70,000) and imager. The instrument was designed and assembled at IfA Manoa, and delivered to the IRTF in late August 2016. >iSHELL is currently in the commissioning phase and is available for general use in semester 2017A. For more information see the instrumentation page of the website or contact John Rayner or Mike Connelley.
Last updated 21 February 2017
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF facility instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are
Adam Burgasser (UC San Diego),
Peter Capak (IPAC),
Henry Hsieh (Planetary Science Institute),
Serena Kim (Univ. of Arizona),
Nick Moskovitz (Lowell Observatory),
Lisa Prato (Lowell Observatory),
Silvia Protopapa (Univ. of Maryland), and
Constantine Tsang (SwRI).
This committee consists of four solar system and four non-solar system members. Chad Bender (Penn. State University) and Michael Wong (UC Berkely) rotated off the TAC effective .
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to ensure future funding of IRTF instruments.
IRTF Cool Star Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, and is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Staffing:
IRTF Director, Alan Tokunaga, and Observatory Manager, Lars Bergknut, both retired at the end of 2016, after decades of service to the telescope and IRTF community. We send them our sincere thanks and very best wishes (and, just in case, we know where you live). The new IRTF Director is John Rayner and the new Deputy Director is Bobby Bus. Imai Namahoe is acting Observatory Manager. We are hiring a new support astronomer.
Dome Resurfacing Project:
The reflective aluminum foil covering the rotating dome is now about 20 years old and has lost much of its reflectivity, which is required for optimum internal dome temperature control. Falling ice has also damaged the integrity of the surface resulting in water seepage and corrosion. We are therefore planning to resurface the dome with new aluminum foil. We expect to start resurfacing in late summer or early fall 2017 and for it to take a few months. Any daytime observing may be disrupted during resurfacing. An outside contractor will do the resurfacing work.
IRTF Data Archive:
Beginning with the 2016B semester, raw data taken with IRTF facility instruments will be made publicly available via an online archive following a proprietary period of 18 months from the date the observations were taken. Caltech’s Infrared Processing and Analysis Center (IPAC) will host the archive. Data files obtained during the 2016B semester will be made available to the public through the archive beginning Feb. 1, 2018. Past users of the IRTF may notice small changes in observing procedures that are being made in preparation for the archive, and are necessary to produce more uniform data products that will be usable by other researchers in the future.
Instrumentation Update
SpeX:
>SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. The current 0.8 micron cut-on dichroic will be replaced with a 0.7 micron dichroic during semester 2017A. This will increase the spectral wavelength grasp for optically guided solar system targets. For more information see the instrumentation page of the website or contact Mike Connelley.
MORIS:
MORIS is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for >MIT Optical Rapid Imaging System. MORIS was initially made available to IRTF through a grant obtained by Amanda Sickafoose. MORIS can be used simultaneously with SpeX and can also be used as an optical guider for SpeX. MORIS was upgraded during semester 2016B with a newer and more robust Andor camera system. For more information contact Bobby Bus.
iSHELL:
>iSHELL is a 1.1-5.3 micron cross-dispersed immersion grating spectrograph (up to a resolving power of R=75,000) and imager. The short wavelength limit will be lowered to cover the 1.08 micron He I line during semester 2017B. For more information see the instrumentation page of the website or contact John Rayner.
Last updated 6 September 2017
IRTF Future Directions Workshop
NASA IRTF will host a >Future Directions Workshop to seek input from the astronomical community on the future directions of the telescope. The workshop will be held at Biosphere 2 in Tucson on 12-14 February 2018.
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF facility instruments. Click >here for more information.
Telescope Allocation Committee
The >current TAC members are . This committee consists of four solar system and four non-solar system members. rotated off the TAC effective .
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to ensure future funding of IRTF instruments.
IRTF Cool Star Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, and is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Staffing:
Adwin Boogert was hired as a new support astronomer. He started work in June. Adwin is an expert in infrared observations of solid and gas phase molecules in molecular clouds. In addition to providing observing support Adwin will become responsible for the development and support of data reduction tools. Imai Namahoe is acting Observatory Manager while a formal recruitment is underway. Sean Lyons will join the IRTF day crew as the junior mechanical technician in October.
Dome Resurfacing Project:
The reflective aluminum foil covering the rotating dome is now about 20 years old and has lost much of its reflectivity, which is required for optimum internal dome temperature control. Falling ice has also damaged the integrity of the surface resulting in water seepage and corrosion. Work to resurface the dome with new aluminum foil started in late August and is expected to take about nine weeks. The telescope will remain operational throughout.
IRTF Data Archive:
Work continues on development of the IRTF Data Archive in collaboration with Caltech’s Infrared Processing and Analysis Center (IPAC) which will host the archive. Raw data taken with SpeX beginning Aug. 1, 2016 (the start of the 2016B semester) will become publicly available via the archive starting Feb. 1, 2018, after a proprietary period of 18 months from the date the observations were taken. Raw data taken with iSHELL beginning Feb. 1, 2017 will likewise become publicly available through the archive starting Aug. 1, 2018, after the 18-month proprietary period. Further information can be viewed on the >IRTF Data Archive Policy page.
Instrumentation Update
SpeX:
>SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. The 0.8 micron cut-on dichroic was replaced with a 0.7 micron dichroic during semester 2017A. This will increase the spectral wavelength grasp for optically guided solar system targets. SpeX will be off the telescope during January 2018 for maintenance and for work required to get sub-arrays working in the IR guider. For more information see the instrumentation page of the website or contact Mike Connelley.
MORIS:
MORIS is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). MORIS stands for >MIT Optical Rapid Imaging System. MORIS was initially made available to IRTF through a grant obtained by Amanda Sickafoose. MORIS can be used simultaneously with SpeX and can also be used as an optical guider for SpeX. MORIS was upgraded during semester 2016B with a newer and more robust Andor camera system. For more information contact Bobby Bus.
iSHELL:
>iSHELL is a1.1-5.3 micron cross-dispersed immersion grating spectrograph (up to a resolving power of R=75,000) and imager. The short wavelength limit has been lowered to 1.06 micron to enable coverage of the 1.08 micron He I line. Wedged order-sorting filters are being procured to remove slight fringing in the spectra but these will not be available until 2018B. For semester 2018A we are limiting the number of proposals requiring radial velocity precisions less than about 100 m/s since the results from commissioning runs are still being analyzed and the limiting precision is not yet know. Development of the data reduction tool for iSHELL has been delayed by some technical problems. These have now been resolved and the Spextool tool package, incorporating both iSHELL and SpeX should be available for download by October 2017. For more information see the instrumentation page of the website or contact John Rayner.
MIRSI:
We are delaying the availability of MIRSI by 6 months due to problems in the instrument's upgrade program. We anticipate commissioning no earlier than 2018A and open use in 2018B. MIRSI is being upgraded from being liquid helium cooled to a closed cycle cooler, and will have a simultaneous visible light imaging capability. For further information, please contact Mike Connelley.
Last updated 2 March 2018
Call for Proposals
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF facility instruments. Click >here for more information.
Comet 46P/Wirtanen Observing Campaign
The apparition of Comet Wirtanen in 2018 represents an excellent opportunity to characterise this potential spacecraft target. The comet will be close to opposition and near perihelion in mid-December 2018. Comet Wirtanen will be very favorably positioned for IRTF observations during 2018B and is predicted to be bright (V~6). A minimum of 150 hours of IRTF observing time will be allocated for this campaign. All data obtained will be made public (within one week), and observing logs will be requested for archiving. We encourage observing groups to form collaborations to enhance the scientific return from the observations. All Comet Wirtanen proposals will be considered part of the observing campaign. When submitting a proposal, please note clearly that the proposal is submitted for the campaign. Groups with visitor instruments can participate in the campaign so long as the data and observing logs are allowed to be public.
For more information on the 2018 apparition and community plans for observing Comet Wirtanen visit the website: http://wirtanen.astro.umd.edu/
IRTF Future Directions Workshop Update
We held a very successful workshop on the future of IRTF at the Biosphere 2 facility near Tucson on Feb 12-14. Input from the workshop will be used to explore possible future directions, to prepare white papers for input into the upcoming planetary and astrophysics decadal reviews, and to inform plans through and beyond the lease that ends in 2033 for operations of all the Maunakea telescopes. Workshop presentations are viewable here.
IRTF Data Reduction Update
A modified version of Spextool for the reduction of iSHELL spectra was made available by Mike Cushing and Bill Vacca. Please visit the >IRTF data reduction pages for download and user instructions, as well as sample data and other useful resources. In the near future we will make tools available to correct for telluric absorption lines using atmospheric models. Please contact Adwin Boogert for requests and questions about the reduction of IRTF data. We welcome software and calibration contributions by users as well.
Telescope Allocation Committee
The >current TAC members are . This committee consists of four solar system and four non-solar system members. rotated off the TAC effective .
Help Keep Our Publications List Current
Please continue to acknowledge the IRTF in your publications following the instructions >shown here. It is important that you include in your papers the name of the instrument used and the citation for the instrument, as this helps to ensure future funding of IRTF instruments.
IRTF Spectral Library
Users are encouraged to make use of the spectral library of FGKM stars, which is available >here. Citations for the papers that have been published can be found >here. An extended spectral library including non-solar metallicity and hotter stars will be available soon. Contact John Rayner for more details.
SpeX Prism Library
A library of more than 1000 prism spectra of low-mass stars and brown dwarfs is maintained by Adam Burgasser, and is available >here.
NEO Spectral Survey
The MIT-IRTF Near-Earth Object spectral survey is underway, and many spectra are publicly available. See the side bar for more information or go to >smass.mit.edu/minus.html.
IRTF News
Staffing:
Imai Namahoe was formally hired as Observatory Manager and a recruitment is underway for the Observatory Supervisor position he vacated. Morgan Bonnet has resigned as IRTF Mechanical Engineer to work on DKIST instrumentation at IfA. However, about fifty percent of Morgan’s time will still be available to IRTF until a replacement is recruited.
Dome Resurfacing Project:
Work on resurfacing the dome is about fifty percent complete but has suffered from significant interruptions due to precipitation and wind. Work was stopped in January and will resume in April when conditions improve. About four weeks of work remain. The telescope will remain operational throughout.
IRTF Data Archive:
The IRTF Data Archive is a collaborative effort between IRTF and Caltech’s Infrared Processing and Analysis Center (IPAC). The Archive webpage and beta version of the user interface are now open to the public via IPAC’s IRSA website. Raw data taken with SpeX beginning Aug. 1, 2016 (the start of the 2016B semester) and for which the time since date of observation has surpassed an 18-month proprietary period are now available for public download. Raw data taken with iSHELL beginning Feb. 1, 2017 will likewise become publicly available through the Archive starting Aug. 1, 2018, after the 18-month proprietary period. We are seeking people who are interested in testing the Archive user interface and providing feedback to Bobby Bus (sjb@ifa.hawaii.edu).
On Dec. 1, 2017 we announced that IRTF 'legacy' data for the years 2001 to 2016 would be made available upon request following a proprietary period of 18 months. Requests for data will be accepted beginning Jun. 1, 2019, must be made to IRTF staff, and will be handled as time permits.
Further information can be viewed on the >IRTF Data Archive Policy page or by contacting Bobby Bus (sjb@ifa.hawaii.edu).
Instrumentation Update
SpeX:
>SpeX is a 0.7-5.3 micron medium-resolution spectrograph and imager. The 0.8 micron cut-on dichroic was replaced with a 0.7 micron dichroic during semester 2017A. This will increase the spectral wavelength grasp for optically guided solar system targets. Sub-arrays are working again in the IR guider. For more information see the instrumentation page of the website or contact Mike Connelley.
MORIS:
MORIS is a 512x512 pixel Andor CCD camera mounted at the side-facing, dichroic-fed window of the SpeX cryostat (60"x60" field-of-view). For more information see the instrumentation page of the website or contact Bobby Bus.
iSHELL:
>iSHELL is a 1.06 – 5.3 micron cross-dispersed echelle spectrograph (up to R=75,000) and imager. Wedged order-sorting filters are being procured to remove slight fringing in the spectra but due to delays in procurement these will not be available until 2019A at the earliest (the vendor is not tax compliant with the IRS). For semester 2018B we are limiting the number of proposals requiring radial velocity precisions less than about 100 m/s since the results from commissioning runs are still being analyzed and the limiting precision is not yet know. Following the discovery that when operated at 80 K the silicon immersion grating is transparent down to 1.05 microns, a new observing mode (J0) has been added to cover the He I line at 1.08 microns. The data reduction tool for iSHELL is now available; it is part of the >Spextool package. For more information see the instrumentation page of the website or contact John Rayner.
MIRSI/MOC:
>MIRSI is a 5 – 20 micron camera and grism spectrograph. MIRSI was recently upgraded by IR Labs with a closed-cycle cooler to replace its liquid nitrogen and liquid helium cryostat. It is currently being further refurbished by IRTF with a new array controller and an optical channel similar to MORIS (MOC) with a 60"x60" field-of-view. For 2018B we are offering MIRSI and MOC in shared risk mode for the final two months of 2018B (December 2018 and January 2019). A new chopping secondary mirror should also be available for use with MIRSI. Remote observing will be available with MIRSI and MOC. For more information see the instrumentation page of the website or contact Mike Connelley.
Last updated DD MMMMMM YYYY
Proposal Deadline for Semester () is Hawaii Standard time.
| style='color: #0000FF;'>Please review the information and use our ONLINE application form |
Note that we have a new instrument, the immersion grating echelle spectrograph (iSHELL), which is available for general use in semester 2017A. A manual for preparation of proposals is available >here.
Available instruments are listed >here. Remote observing is offered from any location with broadband Internet access for any project that utilizes IRTF facility instruments. Click >here for more information.