We present an analysis of the long-term performance of the W. M. Keck observatory laser guide star adaptive optics (LGS-AO) system and explore factors that influence the overall AO performance most strongly. Astronomical surveys can take years or decades to finish, so it is worthwhile to characterize the AO performance on such timescales in order to better understand future results. The Keck telescopes have two of the longest-running LGS-AO systems in use today, and as such they represent an excellent test-bed for processing large amounts of AO data. We use a Keck-II near infrared camera 2 (NIRC2) LGSAO surve of the Galactic Center (GC) from 2005 to 2019 for our analysis, combining image metrics with AO telemetry files, multiaperture scintillation sense/differential imaging motion monitor turbulence profiles, seeing information, weather data, and temperature readings in a compiled dataset to highlight areas of potential performance improvement. We find that image quality trends downward over time, despite multiple improvements made to Keck-II and its AO system, resulting in a 9 mas increase in the average full width at half maximum (FWHM) and a 3% decrease in the average Strehl ratio over the course of the survey. Image quality also trends upward with ambient temperature, possibly indicating the presence of uncorrected turbulence in the beam path. Using nine basic features from our dataset, we train a simple machine learning (ML) algorithm to predict the delivered image quality of NIRC2 given current atmospheric conditions, which could eventually be used for real-time observation planning and exposure time adjustments. A random forest algorithm trained on this data can predict the Strehl ratio of an image to within 18% and the FWHM to within 7%, which is a solid baseline for future applications involving more advanced ML techniques. The assembled dataset and coding tools are released to the public as a resource for testing new predictive control and point spread function-reconstruction algorithms.
We present an analysis of the long-term performance of the W. M. Keck Observatory Laser Guide Star Adaptive Optics (LGS-AO) system and explore factors that influence the overall AO performance most strongly. Astronomical surveys can take years or decades to finish, so it is worthwhile to characterize the AO performance on such timescales in order to better understand future results. Keck Observatory has two of the longest-running LGS-AO systems in use today and represents an excellent test-bed for investigating large amounts of AO data. Here, we use LGS-AO observations of the Galactic Center (GC) from 2005 to 2019, all taken with the NIRC2 instrument on the Keck-II telescope, for our analysis. We combine image metrics with AO telemetry files, MASS/DIMM turbulence profiles, seeing information, and weather data in one cohesive dataset to highlight areas of potential performance improvement and train a simple machine learning algorithm to predict the delivered image quality given current atmospheric conditions. The complete dataset will be released to the public as a resource for testing new predictive control and PSF-reconstruction algorithms.
SOFIA, the Stratospheric Observatory for Infrared Astronomy, is a joint project between NASA and the German Aerospace Center DLR to provide infrared and sub-millimeter observing capabilities to the worldwide astronomical community. With a wide range of instruments that cover both imaging and spectroscopy, SOFIA has produced unique scientific results that could not be obtained with a ground-based facility. In the coming decade, SOFIA will be a critical complement to the other major facilities for astronomical research, the James Webb Space Telescope (JWST) and the Atacama Large Millimeter/submillimeter Array (ALMA) by filling in the otherwise unobservable wavelength range of 30–300 μm. SOFIA provides a wide range of instrumentation, and this paper will describe some of the new capabilities in heterodyne spectroscopy, direct detection spectroscopy, and polarimetry.
KEYWORDS: Stray light, Telescopes, Optical coatings, Infrared radiation, Mirrors, Reflectivity, Space telescopes, Neodymium, Infrared telescopes, System on a chip
Effective stray light control is a key requirement for wide dynamic range performance of scientific optical and infrared systems. SOFIA now has over 325 mission flights including extended southern hemisphere deployments; science campaigns using 7 different instrument configurations have been completed. The research observations accomplished on these missions indicate that the telescope and cavity designs are effective at suppressing stray light. Stray light performance impacts, such as optical surface contamination, from cavity environment conditions during mission flight cycles and while on-ground, have proved to be particularly benign. When compared with earlier estimates, far fewer large optics re-coatings are now anticipated, providing greater facility efficiency.
The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA), project has been operating airborne astronomy flights from Palmdale, California since 2011. The observatory consists of a modified 747-SP aircraft with a 2.5-meter telescope in its aft section. SOFIA has a suite of eight science instruments spanning visible to far-infrared wavelengths. For the majority of the year SOFIA operates out of the Armstrong Flight Research Center in Palmdale, California, giving access to Northern Hemisphere targets. SOFIA’s mobility also allows observations in the Southern Hemisphere (Christchurch, New Zealand), of objects such as the Large and Small Magellanic Clouds, the Galactic Center, and Eta Carinae In 2016, SOFIA added polarimetry capability on SOFIA, with HAWC+ commissioning flights. Selected science results, current instrument suite status, new capabilities, and some expectations of future instrument developments over the lifetime of the observatory will be discussed.
KEYWORDS: Point spread functions, Adaptive optics, Photometry, General relativity, Sensors, Data modeling, Stars, Optical transfer functions, Atmospheric modeling, Instrument modeling
General relativity can be tested in the strong gravity regime by monitoring stars orbiting the supermassive black hole at the Galactic Center with adaptive optics. However, the limiting source of uncertainty is the spatial PSF variability due to atmospheric anisoplanatism and instrumental aberrations. The Galactic Center Group at UCLA has completed a project developing algorithms to predict PSF variability for Keck AO images. We have created a new software package (AIROPA), based on modified versions of StarFinder and Arroyo, that takes atmospheric turbulence profiles, instrumental aberration maps, and images as inputs and delivers improved photometry and astrometry on crowded fields. This software package will be made publicly available soon.
We present a performance report for FLITECAM, a 1-5 μm imager and spectrograph, upon its acceptance and delivery to SOFIA (Stratospheric Observatory for Infrared Astronomy). FLITECAM has two observing configurations: solo configuration and “FLIPO” configuration, which is the co-mounting of FLITECAM with the optical instrument HIPO (PI E. Dunham, Lowell Observatory). FLITECAM was commissioned in the FLIPO configuration in 2014 and flew in the solo configuration for the first time in Fall 2015, shortly after its official delivery to SOFIA. Here we quantify FLITECAM’s imaging and spectral performance in both configurations and discuss the science capabilities of each configuration, with examples from in-flight commissioning and early science data. The solo configuration (which comprises fewer warm optics) has better sensitivity at longer wavelengths. We also discuss the causes of excess background detected in the in-flight FLITECAM images at low elevations and describe the current plan to mitigate the largest contributor to this excess background.
The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA), project has been operating airborne astronomy flights from Palmdale, California since 2011. The observatory consists of a modified 747sp aircraft with a 2.5meter telescope in the tail section. In addition to observing flights out of Palmdale, Ca. this airborne observatory has been able to take advantage of its mobility to observe in the southern hemisphere (New Zealand), to perform multi-wavelength observations of the Super Novae (SN 2014b) in 2014, and to intersect the track of a Pluto Occultation in the southern hemisphere just a few weeks prior to the New Horizons mission fly by of the planet in summer 2015. Science results, observatory operations, current instrument status and participation in future instrument developments, over the lifetime of the observatory will be discussed.
KEYWORDS: Exoplanets, Observatories, Photometry, Stars, Data modeling, Infrared astronomy, Rayleigh scattering, Signal to noise ratio, Point spread functions, Planets
Here, we report on the first successful exoplanet transit observation with the Stratospheric Observatory for Infrared Astronomy (SOFIA). We observed a single transit of the hot Jupiter HD 189733 b, obtaining two simultaneous primary transit lightcurves in the B and z′ bands as a demonstration of SOFIA’s capability to perform absolute transit photometry. We present a detailed description of our data reduction, in particular, the correlation of photometric systematics with various in-flight parameters unique to the airborne observing environment. The derived transit depths at B and z′ wavelengths confirm a previously reported slope in the optical transmission spectrum of HD 189733 b. Our results give new insights to the current discussion about the source of this Rayleigh scattering in the upper atmosphere and the question of fixed limb darkening coefficients in fitting routines.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) is the world’s largest airborne observatory, featuring a
2.5 meter effective aperture telescope housed in the aft section of a Boeing 747SP aircraft. SOFIA’s current instrument
suite includes: FORCAST (Faint Object InfraRed CAmera for the SOFIA Telescope), a 5-40 μm dual band
imager/grism spectrometer developed at Cornell University; HIPO (High-speed Imaging Photometer for Occultations), a
0.3-1.1μm imager built by Lowell Observatory; GREAT (German Receiver for Astronomy at Terahertz Frequencies), a
multichannel heterodyne spectrometer from 60-240 μm, developed by a consortium led by the Max Planck Institute for
Radio Astronomy; FLITECAM (First Light Infrared Test Experiment CAMera), a 1-5 μm wide-field imager/grism
spectrometer developed at UCLA; FIFI-LS (Far-Infrared Field-Imaging Line Spectrometer), a 42-200 μm IFU grating
spectrograph completed by University Stuttgart; and EXES (Echelon-Cross-Echelle Spectrograph), a 5-28 μm highresolution
spectrometer designed at the University of Texas and being completed by UC Davis and NASA Ames
Research Center. HAWC+ (High-resolution Airborne Wideband Camera) is a 50-240 μm imager that was originally
developed at the University of Chicago as a first-generation instrument (HAWC), and is being upgraded at JPL to add
polarimetry and new detectors developed at Goddard Space Flight Center (GSFC). SOFIA will continually update its
instrument suite with new instrumentation, technology demonstration experiments and upgrades to the existing
instrument suite. This paper details the current instrument capabilities and status, as well as the plans for future
instrumentation.
SOFIA is a joint project between NASA and DLR, the German Aerospace Center, to provide the worldwide astronomical community with an observatory that offers unique capabilities from visible to far-infrared wavelengths. SOFIA consists of a 2.7-m telescope mounted in a highly modified Boeing 747-SP aircraft, a suite of instruments, and the scientific and operational infrastructure to support the observing program. This paper describes the current status of the observatory and details the General Investigator program. The observatory has recently completed major development activities, and it has transitioned into full operational status. Under the General Investigator program, astronomers submit proposals that are peer reviewed for observation on the facility. We describe the results from the first two cycles of the General Investigator program. We also describe some of the new observational capabilities that will be available for Cycle 3, which will begin in 2015.
We present a status report and early commissioning results for FLITECAM, the 1-5 micron imager and spectrometer for
SOFIA (the Stratospheric Observatory for Infrared Astronomy). In February 2014 we completed six flights with
FLITECAM mounted in the FLIPO configuration, a co-mounting of FLITECAM and HIPO (High-speed Imaging
Photometer for Occultations; PI Edward W. Dunham, Lowell Observatory). During these flights, the FLITECAM modes
from ~1-4 μm were characterized. Since observatory verification flights in 2011, several improvements have been made
to the FLITECAM system, including the elimination of a light leak in the FLITECAM filter wheel enclosure, and
updates to the observing software. We discuss both the improvements to the FLITECAM system and the results from the
commissioning flights, including updated sensitivity measurements. Finally, we discuss the utility of FLITECAM in the
FLIPO configuration for targeting exoplanet transits.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) is an airborne observatory, carrying a 2.5 m telescope onboard a heavily modified Boeing 747SP aircraft. SOFIA is optimized for operation at infrared wavelengths, much of which is obscured for ground-based observatories by atmospheric water vapor. The SOFIA science instrument complement consists of seven instruments: FORCAST (Faint Object InfraRed CAmera for the SOFIA Telescope), GREAT (German Receiver for Astronomy at Terahertz Frequencies), HIPO (High-speed Imaging Photometer for Occultations), FLITECAM (First Light Infrared Test Experiment CAMera), FIFI-LS (Far-Infrared Field-Imaging Line Spectrometer), EXES (Echelon-Cross-Echelle Spectrograph), and HAWC (High-resolution Airborne Wideband Camera). FORCAST is a 5–40 μm imager with grism spectroscopy, developed at Cornell University. GREAT is a heterodyne spectrometer providing high-resolution spectroscopy in several bands from 60–240 μm, developed at the Max Planck Institute for Radio Astronomy. HIPO is a 0.3–1.1 μm imager, developed at Lowell Observatory. FLITECAM is a 1–5 μm wide-field imager with grism spectroscopy, developed at UCLA. FIFI-LS is a 42–210 μm integral field imaging grating spectrometer, developed at the University of Stuttgart. EXES is a 5–28 μm high-resolution spectrograph, developed at UC Davis and NASA ARC. HAWC is a 50–240 μm imager, developed at the University of Chicago, and undergoing an upgrade at JPL to add polarimetry capability and substantially larger GSFC detectors. We describe the capabilities, performance, and status of each instrument, highlighting science results obtained using FORCAST, GREAT, and HIPO during SOFIA Early Science observations conducted in 2011.
The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA), a program to develop and
operate a 2.5-meter infrared airborne telescope in a Boeing 747SP, has obtained first science with the FORCAST camera
in the 5 to 40 micron spectral region and the GREAT heterodyne spectrometer in the 130 to 240 micron spectral region.
We briefly review the characteristics and status of the observatory. Spectacular science results on regions of star
formation will be discussed. The FORCAST images show several discoveries and the potential for determining how
massive stars form in our Galaxy. The GREAT heterodyne spectrometer has made mapping observations of the [C II]
line at 158 microns, high J CO lines, and other molecular lines including SH. The HIPO high speed photometer and the
high speed camera FDC were used to observe the 2011 June 23 UT stellar occultation by Pluto.
The Stratospheric Observatory for Infrared Astronomy (SOFIA) has recently concluded a set of engineering flights for Observatory performance evaluation. These in-flight opportunities have been viewed as a first comprehensive assessment of the Observatory's performance and will be used to address the development activity that
is planned for 2012, as well as to identify additional Observatory upgrades. A series of 8 SOFIA Characterization
And Integration
flights have been conducted from June to December 2011. The HIPO science instrument in
conjunction with the DSI Super Fast Diagnostic Camera (SFDC) have been used to evaluate pointing stability,
including the image motion due to rigid-body and
flexible-body telescope modes as well as possible aero-optical
image motion. We report on recent improvements in pointing stability by using an Active Mass Damper system
installed on Telescope Assembly. Measurements and characterization of the shear layer and cavity seeing, as
well as image quality evaluation as a function of wavelength have been performed using the HIPO+FLITECAM
Science Instrument conguration (FLIPO). A number of additional tests and measurements have targeted basic
Observatory capabilities and requirements including, but not limited to, pointing accuracy, chopper evaluation
and imager sensitivity. This paper reports on the data collected during these
flights and presents current SOFIA
Observatory performance and characterization.
This paper describes the current status of FLITECAM, the near-infrared (1 - 5 μm) camera and spectrometer for
NASA’s Stratospheric Observatory for Infrared Astronomy (SOFIA). Due to a change in schedule FLITECAM’s
delivery was advanced, allowing it to be co-mounted with the HIPO instrument and used on four flights in October 2011
for observatory verification. Although not part of FLITECAM’s commissioning time, some preliminary performance
characteristics were determined. Image size as a function of wavelength was measured prior to the installation of active
mass dampers on the telescope. Preliminary grism spectroscopy was also obtained. In addition, FLITECAM was used to
measure the emissivity of the telescope and warm optics in the co-mounted configuration. New narrow band filters were
added to the instrument, including a Paschen alpha filter for line emission. Results are illustrated.
SOFIA, the Stratospheric Observatory for Infrared Astronomy, is an airborne observatory with a 2.7-m telescope that is
under development by NASA and the German Aerospace Center DLR. From late 2010 and through the end of 2011,
SOFIA conducted a series of science demonstration flights, Early Science, using FORCAST (the Faint Object InfraRed
Camera for the SOFIA Telescope), HIPO (the High-speed Imaging Photometer for Occultations), and GREAT (the
German REceiver for Astronomy at Terahertz frequencies). Flying at altitudes as high as 13.7 km (45,000 ft), SOFIA
operates above more than 99.8% of the water vapor in the Earth’s atmosphere, opening up most of the far-infrared and
sub-millimeter parts of the spectrum. During Early Science, 30 science missions were flown with results in solar system
astronomy, star formation, the interstellar medium, the Galactic Center, and extragalactic studies. Many of these
investigations were conducted by the first group of SOFIA General Investigators, demonstrating the operation of SOFIA
as a facility for the astronomical community. This paper presents some recent highlights from Early Science.
Anisoplanatism is a primary source of photometric and astrometric error in single-conjugate adaptive optics. We present initial results of a project to model the off-axis optical transfer function in the adaptive optics system at the Keck II telescope. The model currently accounts for the effects of atmospheric anisoplanatism in natural guide star observations. The model for the atmospheric contribution to the anisoplanatic transfer function uses contemporaneous MASS/ DIMM measurements. Here we present the results of a validation campaign using observations of naturally guided visual binary stars under varying conditions, parameterized by the r0 and θ0 parameters of the C2n atmospheric turbulence profile. We are working to construct a model of the instrumental field-dependent aberrations in the NIRC2 camera using an artificial source in the Nasmyth focal plane. We also discuss our plans to extend the work to laser guide star operation.
SOFIA, the Stratospheric Observatory for Infrared Astronomy, is a specially modified Boeing 747SP aircraft with a 2.7-
m telescope. Flying above more than 99% of the water vapor in the Earth's atmosphere, SOFIA will enable observations
of large regions of the infrared and submillimeter that are normally opaque to terrestrial observatories. A joint project of
NASA and DLR, SOFIA has completed a series of major flight tests leading up to the Initial Science Flights this year. In
particular, SOFIA has recently completed its first observations through the telescope. This paper gives an overview of
the facility and reports on the recent progress in the development of this major astronomical facility including the First
Light observations with the FORCAST infrared camera.
The joint U.S. and German SOFIA project to develop and operate a 2.5-meter infrared airborne telescope in a Boeing
747-SP is in its final stages of development. Flying in the stratosphere, SOFIA allows observations throughout the
infrared and submillimeter region, with an average transmission of greater than 80%. SOFIA's first generation
instrument complement includes high-speed photometers, broadband imagers, moderate resolution spectrographs
capable of resolving broad features due to dust and large molecules, and high resolution spectrometers suitable for
kinematic studies of molecular and atomic gas lines at km/s resolution. These instruments will enable SOFIA to make
unique contributions to a broad array of science topics. First science flights will begin in 2010, and the observatory is
expected to operate for more than 20 years. The sensitivity, characteristics, science instrument complement, future
instrument opportunities and examples of first light science will be discussed.
KEYWORDS: Infrared telescopes, Stars, Observatories, Space telescopes, Infrared astronomy, Galactic astronomy, Space operations, James Webb Space Telescope, Spectrometers, Planets
The joint U.S. and German Stratospheric Observatory for Infrared Astronomy (SOFIA) Project will operate a 2.5-meter
infrared airborne telescope in a Boeing 747SP. Flying in the stratosphere at altitudes as high as 45,000 feet, SOFIA
enables observations in the infrared and submillimeter region with an average transmission of 80%. SOFIA has a wide
instrument complement including broadband imaging cameras, moderate resolution spectrographs capable of resolving
broad features due to dust and large molecules, and high resolution spectrometers suitable for kinematic studies of
molecular and atomic gas lines at km/s resolution. The first generation and future instruments will enable SOFIA to
make unique contributions to a broad array of science topics. SOFIA began its post-modification test flight series on
April 26, 2007 in Waco, Texas and will conclude in winter of
2008-09. SOFIA will be staged out of Dryden's aircraft
operations facility at Palmdale, Site 9, CA for science operations. The SOFIA Science Center will be at NASA Ames
Research Center, Moffet Field, CA. First science flights will begin in 2009, the next instrument call and first General
Observer science call will be in 2010, and a full operations schedule of ~120 flights per year will be reached by 2014.
The observatory is expected to operate for more than 20 years. The sensitivity, characteristics, science instrument
complement, future instrument opportunities, and examples of first light and early mission science are discussed.
The joint U.S. and German SOFIA project to develop and operate a 2.5-meter infrared airborne telescope in a
Boeing 747-SP is now in its final stages of development. Flying in the stratosphere, SOFIA allows observations
throughout the infrared and submillimeter region with an average transmission of ≥ 80%. The SOFIA instrument
complement includes broadband imagers, moderate resolution spectrographs capable of resolving broad features
due to dust and large molecules, and high resolution spectrometers suitable for kinematic studies of molecular
and atomic gas lines at km/s resolution. These instruments will enable SOFIA to make unique contributions
to a broad array of science topics. First science flights will begin in 2009, and the observatory is expected to
operate for more than 20 years. The sensitivity, characteristics, science instrument complement, and examples
of first light science are discussed.
FLITECAM is a 1-5 micron infrared camera for NASA's Stratospheric Observatory for Infrared Astronomy (SOFIA).
A 1024 ×1024 InSb ALADDIN III detector and large refractive optics provide a field of view of almost 8 arc minutes
in diameter with a scale of just under 0.5 arc seconds per pixel. The instrument is cooled by a double liquid helium and
liquid nitrogen cryostat. Using a collimated beam of about 26 mm diameter, a low resolution spectroscopic mode is also
available using direct-ruled KRS5 grisms and fixed slits of either 1" or 2" width and 60" length to yield resolving
powers of R~1700 and 900 respectively. FLITECAM has been partially commissioned at the 3-m Shane telescope of
Lick Observatory where the f/17 optics of this telescope provides almost the same plate scale as SOFIA. Astronomical
observing requests (scripts) and a real-time data reduction pipeline (DRP) for dithered image patterns have been
demonstrated. The performance of the instrument during ground-based trials is illustrated.
We present an overview of the science instrument program for the Stratospheric Observatory for Infrared Astronomy (SOFIA). Funded for an initial suite of facility and PI instruments, the SOFIA instrument development program includes imagers and spectrometers from both U.S. and German development teams. With an emphasis on lessons learned, we review the development of the facility instrument suite. We conclude with the anticipated role for SOFIA as a new technology test bed for the latest far-infrared detectors.
Amanda Mainzer, Ian McLean, Ted Aliado, Eric Becklin, George Brims, John Goulter, Evan Kress, Nick Magnone, John Milburn, Gunnar Skulason, Michael Spencer
Preliminary test results are reported for FLITECAM, the First Light Camera for SOFIA. This instrument is designed to perform imaging from 1 to 5 μm over the entire 8 arcmin field of view of SOFIA with 0.47arcsec pixels. The detector is a 1024 × 1024 InSb array, and large refractive optics are used for collimation and re-imaging. FLITECAM also has a pupil-viewing mode optimized for 3.5 mm and can accommodate grisms for slit spectroscopy. The instrument has passed Critical Airworthiness Design Review and has received the first part of its certificate of conformity. Ground-based tests of the finished instrument are planned for later in 2002 at the Lick Observatory 3-m Shane Telescope to verify that the point spread function meets its required FWHM of 1 arcsec over the full field and wavelength range. FLITECAM will be used to test the image quality and background of the SOFIA telescope, as well as for science applications.
This paper describes the performance of NIRSPEC, the cryogenic cross-dispersed IR echelle spectrograph for the Keck II telescope on Mauna Kea. NIRSPEC employs a 1024 by 1024 InSb array, diamond-machined metal optics and closed- cycle refrigeration on achieve high throughput and low backgrounds. The instrument operates directly at the f/15 Nasmyth focus, but can also be used in conjunction with the Keck adaptive optics system. First Light was obtained on April 25, 1999. As expected, the performance is detector- limited at short wavelengths and background-limited at longer wavelengths. All of the design goals have been met and result illustrating the optical performance and sensitivity are reported.
We present diffraction limited 2-25 micrometers images, obtained with the W.M. Keck 10-m telescopes that spatially resolve the cool Galactic Center source IRS 21, an enigmatic object that has alluded classification. Modeled as a Gaussian, the azimuthally averaged intensity profile of IRS 21, an enigmatic object that has alluded classification. Modeled asa a Gaussian, the azimuthally averaged intensity profile of IRS 21 has a HWHM radius of 740 +/- 30 AU at 2.2 micrometers and an average HWHM radius of 1540 +/- 90 AU at mid-IR wavelength. These sizes along with its color temperature favor the hypothesis that IRS 21 is self-luminous rather than an externally heated dust clump. Based on the size alone, the remaining possible dust geometries are (1) an intrinsic inflow or outflow or (2) an extrinsic dust distribution, in which case IRS 21 could be simply embedded in the Northern Arm. A simple SED model of the IR photometry from the literature and our mid-IR images reveal that the near-IR radiation is scattered light from an unknown embedded source while the mid-IR radiation is the remaining re-radiated light. The agreement between the 2.2 micrometers polarization angle for IRS 21 and the 12.5 micrometers polarization angle at the position of IRS 21, the symmetric shape of its intensity profiles, as well as the similarity of the observed properties of all the Northern Arm sources, lead us to conclude that the scattering dust around IRS 21 is extrinsic to the central source and is associated with the Northern Arm.
We report NIRSPEC/Keck observations of the Galactic Center obtained in both low and high resolution modes under excellent seeing conditions. The data were obtained as part of the NIRSPEC commissioning program and will be used to determine: 1) the nature of the stars in the central 0.02 pc, 2) the velocities and accelerations of stars around the central black hole, 3) the velocities of ionized gas in the central parsec, 4) the extent of the main sequence population and star formation history in central parsec, 5) the mass magnitude relation and initial mass function in the Arches cluster, 6) the nature of the MIR sources in the central parsec and Quintuplet clusters, 7) the physical parameters of stellar atmosphere/winds of super luminous stars, and 8) the metallicity in the GC as inferred from observations of red supergiants, red giants, and hot stars. We present a sample of these data, including a high resolution slit scan movie of the central parsec, and show how they can be used to vastly improve the current state of the art in the related science topics. Further, we discuss preliminary results concerning the nature of the central cusp stars and the resultant implications for star formation near a supermassive black hole.
The NIRSPEC Brown Dwarf Spectroscopic Survey is a project to obtain a consistent set of high-quality near-IR spectra for each spectral class and sub-class of low-mass and/or sub- stellar objects to provide a new data base for models of the atmosphere of brown dwarfs and extra-solar giant planets. Most of the current targets are L-dwarfs and T-dwarfs discovered by the 2MASS. The survey is begin performed with the recently-commissioned near-IR spectrometer, NIRSPEC, a 1-5 micrometers cryogenic spectrograph at the WM Keck Observatory on Mauna Kea, using resolving powers of R equals 2,500-25,000. Preliminary results for four sources, three L-dwarfs and one T-dwarf, are presented here. Spectra from 1.13-2.33 micrometers at an average resolution of R equals 2,500 illustrate the development of deep steam bands and the weakening of FeH through the L-sequence, and the emergence of methane bands in the T-dwarfs. Complex detail in the spectra are the result of blending of numerous unresolved molecular transitions.
A study of the average upper atmospheric conditions has been carried out in order to optimize the scientific return from SOFIA. By examination of atmospheric data from satellite missions, we found that at typical SOFIA flight altitudes (between 37,000 and 45,000 ft), it can be an advantage to fly north, as the water vapor overburden and the frequency of cloud occurrence is less than if the flights were centered above Moffett Field, CA, which will be the base for SOFIA. It has also been shown that for certain science projects, the amount of time on target can be considerably extended.
As a facility class instrument on SOFIA, FLITECAM will be developed at the UCLA Infrared Imaging Detector Laboratory. Its primary purpose is to test the SOFIA telescope imaging quality from 1.0 to 5.5 microns, using a 1024 X 1024 InSb ALADDIN II array. Once the telescope test flights are finished, FLITECAM will be available to the science community. FLITECAM's field of view of 8' in diameter, with a plate scale of 0.47' per pixel, is one of the largest available for any facility camera. Grisms are available to produce moderate resolution of R approximately equals 1000 - 2000, depending on the slit width, with direct ruled ZnSe grisms. The detector readout electronics will be provided by Mauna Kea IR Inc. and is able to operate the detector array at all its planned operation modes, including occulations, telescope-nodding, high-speed shift-and-add, and optionally chopping at the longer wavelengths. Here we present our design approach to achieve those specifications. We also discuss the most important tests FLITECAM will carry out and give examples of science projects on SOFIA. For the latter, we present a preliminary list of filters which is expandable and open for discussions within the science community.
The joint US and German SOFIA project to develop and operate a 2.5 meter IR airborne telescope in a Boeing 747-SP is now in its second year. The Universities Space Research Association, teamed with Raytheon E-Systems and United Airlines, is developing and will operate SOFIA. The 2.5 meter telescope will be designed and built by a consortium of German companies led by MAN. Work on the aircraft and the primary mirror has started. First science flights will begin in 2001 with 20 percent of the observing time assigned to German investigators. The observatory is expected to operate for over 20 years. The sensitivity, characteristics and science instrument complement are discussed.
We describe the requirements, constraints, and goals for FLITECAM, the first light IR test experiment camera being built at UCLA for SOFIA. The camera must allow testing of the testing of the telescope/observatory and provide first- light images for public outreach and publicity. In addition, the camera should become a facility-class instrument for use by the general SOFIA user community. The camera is relatively simple and inherits many of the designs from previous instruments built in the IR Imaging Detector Laboratory at UCLA. It will offer wide-field imaging, high- resolution imaging for observing diffraction-limited images at >= 3 micrometers , low-resolution grism spectroscopy, and pupil-viewing. FLITECAM will be delivered for observatory tests in early 2001. The project will not formally start until NIRSPEC is delivered and commissioned at the Keck Observatory.
The joint US and German SOFIA project to develop and operate a 2.5 meter IR airborne telescope in a Boeing 747-SP is now in its second year. The Universities Space Research Association , teamed with Raytheon E-Systems and United Airlines, is developing and will operate SOFIA. The 2.5 meter telescope will be designed and built by a consortium of German companies led by MAN. Work on the aircraft and the preliminary mirror has started. First science flights will begin in 2001 with 20 percent of the observing time assigned to German investigators. The observatory is expected to operate for over 20 years. The sensitivity, characteristics, US science instrument complement, and operations concept for the SOFIA observatory, with an emphasis on the science community's participation are discussed.
The design and development of NIRSPEC, a near-IR echelle spectrograph for the Keck II 10-meter telescope is described. This instrument is a large, facility-class vacuum-cryogenic spectrometer with a resolving power of R equals 25,000 for a 0.4 inch slit. It employs diamond-machined metal optics and state-of-the-art IR array detectors for high throughput, together with powerful user-friendly software for ease of use.
NIRSPEC is a recently funded, high-resolution, 1 - 5 micrometers cryogenic spectrograph for the Keck II telescope. The design of this new instrument is based on 1024 X 1024 InSb arrays and provides resolving powers of R equals 2,000 in non-cross-dispersed mode and R equals 25,000 in echelle mode with typically 5 to 6 orders on the array covering 60 - 90% of the selected waveband, J, H, K, or L, in a single observation. Later, even higher resolution can be achieved by using the proposed adaptive optics facility at Keck II and replacing some of the internal modules of NIRSPEC. This paper gives a brief description of the proposed design concepts, and a discussion of the detector and system constraints required to achieve the scientific goals of the instrument.
This paper describes the performance of a unique new IR array camera system which provides simultaneous imaging at two wavelengths in the near IR. Two-color imaging is achieved with a dichroic beam splitter which yields two independent beams, one short-wave (SW) from 1 to 2.5 micrometers and one long-wave (LW) from 2 to 5 micrometers . A Rockwell NICMOS 3 256 by 256 HgCdTe array is used in the SW channel and the LW channel has an InSb 256 by 256 array from SBRC. The instrument, which is designed for the University of California's Lick Observatory 3-m telescope and for the f/15 focus of the 10-m W.M. Keck telescope, employs a closed cycle refrigerator and a compact array control/data acquisition system based on transputers with a host 486 PC. On the Lick 3-m telescope the pixel size is 0.7' which gives a field of view of about 180' by 180'. Facilities are also provided for spectroscopy and polarimetry. Recent observational results are reported to illustrate the performance of this system.
This paper describes a new infrared imaging system being developed at UCLA for use on both the Lick Observatory 3-m telescope and the W.M. Keck 10-m telescope. The instrument has a relatively wide field of view on each telescope and is intended for infrared surveys and deep imaging. To enhance efficiency, the new instrument incorporates a dichroic beam splitter to provide two simultaneous imaging systems, one short-wave (SW) from 1 - 2.5 micrometers and one long-wave (LW) from 2 - 5 micrometers . Each wavelength channel is independently optimized. The SW channel contains a Rockwell NICMOS3 256 X 256 HgCdTe array and the LW channel has an SBRC 256 X 256 InSb array. The thermal design employs a closed cycle cooler. A control and data acquisition system based on transputers and high speed analog electronics is being developed to handle the high data rates.
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