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Papers by Joseph Adams
The Astrophysical Journal
We present the first spatially resolved mid-infrared (37.1 µm) image of the Fomalhaut debris disk... more We present the first spatially resolved mid-infrared (37.1 µm) image of the Fomalhaut debris disk. We use PSF fitting and subtraction to distinctly measure the flux from the unresolved component and the debris disk. We measure an infrared excess in the point source of 0.9 ± 0.2 Jy, consistent with emission from warm dust in an inner disk structure (Su et al. 2016), and inconsistent with a stellar wind origin. We cannot confirm or rule out the presence of a pileup ring (Su et al. 2016) near the star. In the cold region, the 37 µm imaging is sensitive to emission from small, blowout grains, which is an excellent probe of the dust production rate from planetesimal collisions. Under the assumptions that the dust grains are icy aggregates and the debris disk is in steady state, this result is consistent with the dust production rates predicted by Kenyon & Bromley (2008) from theoretical models of icy planet formation. We find a dust luminosity of (7.9 ± 0.8) × 10 −4 L ⊙ and a dust mass of 8-16 lunar masses, depending on grain porosity, with ∼ 1 lunar mass in grains with radius 1 µm-1 mm. If the grains are icy and highly porous, meter-sized objects must be invoked to explain the far-IR, submm, and mm emission. If the grains are composed of astronomical silicates, there is a dearth of blowout grains (Pawellek et al. 2014) and the mass loss rate is well below the predicted dust production values.
Journal of Astronomical Instrumentation, 2018
We describe the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST) which is presently... more We describe the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST) which is presently operating as a facility instrument on the Stratospheric Observatory For Infrared Astronomy (SOFIA). FORCAST provides imaging and moderate resolution spectroscopy capability over the 5–40[Formula: see text][Formula: see text]m wavelength range. In imaging mode, FORCAST has a 3.4[Formula: see text] field-of-view with 0.768[Formula: see text] pixels. Using grisms, FORCAST provides long-slit low-resolution ([Formula: see text]–300) and short-slit, cross-dispersed medium-resolution spectroscopic modes ([Formula: see text]–1200) over select wavelengths. Preceded by both Spitzer and Herschel, the discovery phase space for FORCAST lies in providing unique photometric bands and/or spectroscopic coverage, higher spatial resolution and exploration of the brightest sources which typically saturate space observatories.
The Astrophysical Journal, 2016
Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in natu... more Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in nature. Originally dubbed the "cocoon stars" due to their cool featureless spectra, high-resolution near-infrared imaging observations have shown that at least two of the objects exhibit "pinwheel" nebulae consistent with binary systems with a carbonrich Wolf-Rayet star and O/B companion. In this paper, we present 19.7, 25.2, 31.5, and 37.1 µm observations of the QPMs (with an angular resolution of 3.2-3.8") taken with the Faint Object Infrared Camera for the SOFIA Telescope (FORCAST) in conjunction with high-resolution (∼0.1-0.2") images at 8.8 and 11.7 µm from the Thermal-Region Camera Spectrograph (TReCS). DUSTY models of the thermal dust emission of two of the four detected QPMs, Q2 and Q3, are fitted by radial density profiles which are consistent with constant mass loss rates (ρ d ∝ r −2). For the two remaining sources, Q1 and Q9, extended structures (∼ 1") are detected around these objects in high-resolution imaging data. Based on the fitted dust masses, Q9 has an unusually large dust reservoir (M d = 1.3 +0.8 −0.4 × 10 −3 M) compared to typical dusty Wolf-Rayet stars which suggests that it may have recently undergone an episode of enhanced mass loss.
SPIE Proceedings, 2014
We describe the Short Wavelength Camera (SWCam) for the CCAT observatory including the primary sc... more We describe the Short Wavelength Camera (SWCam) for the CCAT observatory including the primary science drivers, the coupling of the science drivers to the instrument requirements, the resulting implementation of the design, and its performance expectations at first light. CCAT is a 25 m submillimeter telescope planned to operate at 5600 meters, near the summit of Cerro Chajnantor in the Atacama Desert in northern Chile. CCAT is designed to give a total wave front error of 12.5 µm rms, so that combined with its high and exceptionally dry site, the facility will provide unsurpassed point source sensitivity deep into the short submillimeter bands to wavelengths as short as the 200 µm telluric window. The SWCam system consists of 7 sub-cameras that address 4 different telluric windows: 4 subcameras at 350 µm, 1 at 450 µm, 1 at 850 µm, and 1 at 2 mm wavelength. Each sub-camera has a 6' diameter field of view, so that the total instantaneous field of view for SWCam is equivalent to a 16' diameter circle. Each focal plane is populated with near unit filling factor arrays of Lumped Element Kinetic Inductance Detectors (LEKIDs) with pixels scaled to subtend an solid angle of (λ/D) 2 on the sky. The total pixel count is 57,160. We expect background limited performance at each wavelength, and to be able to map > 35 (°)2 of sky to 5 σ on the confusion noise at each wavelength per year with this first light instrument. Our primary science goal is to resolve the Cosmic Far-IR Background (CIRB) in our four colors so that we may explore the star and galaxy formation history of the Universe extending to within 500 million years of the Big Bang. CCAT's large and high-accuracy aperture, its fast slewing speed, use of instruments with large format arrays, and being located at a superb site enables mapping speeds of up to three orders of magnitude larger than contemporary or near future facilities and makes it uniquely sensitive, especially in the short submm bands.
The Astrophysical Journal, 2013
We have imaged the bipolar planetary nebula M2-9 using SOFIA's FORCAST instrument in six waveleng... more We have imaged the bipolar planetary nebula M2-9 using SOFIA's FORCAST instrument in six wavelength bands between 6.6 and 37.1 µm. A bright central point source, unresolved with SOFIA's ∼ 4 ′′-to-5 ′′ beam, is seen at each wavelength, and the extended bipolar lobes are clearly seen at 19.7 µm and beyond. The photometry between 10 and 25 µm is well fit by the emission predicted from a stratified disk seen at large inclination, as has been proposed for this source by Lykou et al and by Smith and Gehrz. The principal new results in this paper relate to the distribution and properties of the dust that emits the infrared radiation. In particular, a considerable fraction of this material is spread uniformly through the lobes, although the dust density does increase at the sharp outer edge seen in higher resolution optical images of M2-9. The dust grain population in the lobes shows that small (< 0.1 µm) and large (> 1 µm) particles appear to be present in roughly equal amounts by mass. We suggest that collisional processing within the bipolar outflow plays an important role in establishing the particle size distribution.
The Astrophysical Journal, 2012
The Astronomical Journal, 2006
We present an analysis of thermal emission from comet 162P/Siding Spring (P/2004 TU 12) measured ... more We present an analysis of thermal emission from comet 162P/Siding Spring (P/2004 TU 12) measured during its discovery apparition in December 2004. The comet showed no dust coma at this time, so we have sampled emission from the comet's nucleus. Observations using the "Mid-Infrared Spectrometer and Imager" ("MIRSI") were performed at NASA's Infrared Telescope Facility, where the peak of the comet's spectral energy distribution was observed between 8 and 25 µm. In combination with the three near-infrared spectra presented by Campins et al. (2006, AJ, this issue) that show the Wien-law tail of the thermal emission, the data provide powerful constraints on surface properties of the nucleus. We find that the nucleus's effective radius is 6.0±0.8 km. This is one of the largest radii known among Jupiter-family comets, which is unusual considering the comet was discovered only recently. Its geometric albedo is 0.059 ± 0.023 in H-band, 0.037 ± 0.014 in R-band, and 0.034 ± 0.013 in V-band. We also find that the nucleus of 162P has little infrared beaming, and this implies the nucleus has low thermal inertia. Including all near-IR spectra yields a beaming parameter η of 1.01 ± 0.20. This result is in agreement with others showing that cometary nuclei have low thermal inertia and little infrared beaming. If confirmed for many nuclei, the interpretation of radiometry may not be as problematic as feared.
The Astrophysical Journal, 2012
The Astrophysical Journal, 2012
The Astrophysical Journal, 2015
We present mid-IR (19-37 µm) imaging observations of S106 from SOFIA/FORCAST, complemented with I... more We present mid-IR (19-37 µm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0
We used MIRSI on the IRTF to make 10 and 20 \micron images of four candidate high-mass protosetll... more We used MIRSI on the IRTF to make 10 and 20 \micron images of four candidate high-mass protosetllar objects (HMPOs) from the sample of Sridharan et al. (2002). These candidate HMPOs were selected from the IRAS database using FIR color criteria derived for UCHIIs. The HMPOs had been detected in CS, but not in 5 GHz radio continuum single dish surveys above 25 mJy. Most were detected in the MSX mid-IR survey. Beuther et al. (2002) presented maps of 1.2 mm dust emission of the sample of HMPOs. Our selection criteria were that the sources appear compact in MSX bands C (12.1 \micron) and E (21.3 \micron), and in the 1.2 mm maps. Three sources were detected by MIRSI at the IRTF at both 10 \micron (47% width 10.6 \micron, N band or a 10% width 11.6 \micron filter) and 20 \micron (42% width 20.9 \micron filter): IRAS 22134+5834, 23033+5951, and 23151+5912. Their sizes are marginally larger than the diffraction limited beams of about one arcsec. The MIRSI flux densities are significant fract...
Science (New York, N.Y.), Jan 19, 2015
Dust formation in supernova ejecta is currently the leading candidate to explain the large quanti... more Dust formation in supernova ejecta is currently the leading candidate to explain the large quantities of dust observed in the distant, early Universe. However, it is unclear whether the ejecta-formed dust can survive the hot interior of the supernova remnant (SNR). We present infrared observations of ~0.02 [Formula: see text] of warm (~100 K) dust seen near the center of the ~10,000 yr-old Sgr A East SNR at the Galactic center. Our findings signify the detection of dust within an older SNR that is expanding into a relatively dense surrounding medium (ne ~ 100 cm(-3)) and has survived the passage of the reverse shock. The results suggest that supernovae may indeed be the dominant dust production mechanism in the dense environment of early Universe galaxies.
The Astrophysical Journal, 2014
SPIE Proceedings, 2004
Four institutions are collaborating to design and build three near identical λ/∆λ ∼ 2700 cross-di... more Four institutions are collaborating to design and build three near identical λ/∆λ ∼ 2700 cross-dispersed nearinfrared spectrographs for use on various 5-10 meter telescopes. The instrument design addresses the common observatory need for efficient, reliable near-infrared spectrographs through such features as broad wavelength coverage across 6 simultaneous orders (0.8-2.4 µm) in echelle format, real-time slit viewing through separate optics and detector, and minimal moving parts. Lastly, the collaborators are saving money and increasing the likelihood of success through economies of scale and sharing intellectual capital.
SPIE Proceedings, 2008
We have designed and fabricated a suite of grisms for use in FORCAST, a mid-infrared camera sched... more We have designed and fabricated a suite of grisms for use in FORCAST, a mid-infrared camera scheduled as a first-light instrument on SOFIA. The grism suite gives SOFIA a new capability: low and moderate resolution spectroscopy from 5µm to 37µm, without the addition of a new instrument. One feature of the optical design is that it includes a mode using pairs of cross-dispersed grisms, providing continuous wavelength coverage over a broad range at higher resolving power. We fabricated four silicon (n = 3.44) grisms using photolithographic techniques and purchased two additional mechanically ruled KRS-5 (n = 2.3) grisms. One pair of silicon grisms permits observations of the 5 − 8µm band with a long slit at R∼ 200 or, in a cross-dispersed mode, at resolving powers up to 1500. In the 8 − 14µm region, where silicon absorbs heavily, the KRS-5 grisms produce resolving powers of 300 and 800 in long-slit and cross-dispersed mode, respectively. The remaining two silicon grisms cover 17 − 37µm at resolving powers of 140 and 250. We have thoroughly tested the silicon grisms in the laboratory, measuring efficiencies in transmission at 1.4 − 1.8µm. We report on these measurements as well as on cryogenic performance tests of the silicon and KRS-5 devices after installation in FORCAST.
SPIE Proceedings, 2010
Progress report on FORCAST grism spectroscopy as a future general observer instrument mode on SOF... more Progress report on FORCAST grism spectroscopy as a future general observer instrument mode on SOFIA", Proc. SPIE 7735, 77356N (2010).
The Astrophysical Journal, 2006
The Astrophysical Journal
We present the first spatially resolved mid-infrared (37.1 µm) image of the Fomalhaut debris disk... more We present the first spatially resolved mid-infrared (37.1 µm) image of the Fomalhaut debris disk. We use PSF fitting and subtraction to distinctly measure the flux from the unresolved component and the debris disk. We measure an infrared excess in the point source of 0.9 ± 0.2 Jy, consistent with emission from warm dust in an inner disk structure (Su et al. 2016), and inconsistent with a stellar wind origin. We cannot confirm or rule out the presence of a pileup ring (Su et al. 2016) near the star. In the cold region, the 37 µm imaging is sensitive to emission from small, blowout grains, which is an excellent probe of the dust production rate from planetesimal collisions. Under the assumptions that the dust grains are icy aggregates and the debris disk is in steady state, this result is consistent with the dust production rates predicted by Kenyon & Bromley (2008) from theoretical models of icy planet formation. We find a dust luminosity of (7.9 ± 0.8) × 10 −4 L ⊙ and a dust mass of 8-16 lunar masses, depending on grain porosity, with ∼ 1 lunar mass in grains with radius 1 µm-1 mm. If the grains are icy and highly porous, meter-sized objects must be invoked to explain the far-IR, submm, and mm emission. If the grains are composed of astronomical silicates, there is a dearth of blowout grains (Pawellek et al. 2014) and the mass loss rate is well below the predicted dust production values.
Journal of Astronomical Instrumentation, 2018
We describe the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST) which is presently... more We describe the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST) which is presently operating as a facility instrument on the Stratospheric Observatory For Infrared Astronomy (SOFIA). FORCAST provides imaging and moderate resolution spectroscopy capability over the 5–40[Formula: see text][Formula: see text]m wavelength range. In imaging mode, FORCAST has a 3.4[Formula: see text] field-of-view with 0.768[Formula: see text] pixels. Using grisms, FORCAST provides long-slit low-resolution ([Formula: see text]–300) and short-slit, cross-dispersed medium-resolution spectroscopic modes ([Formula: see text]–1200) over select wavelengths. Preceded by both Spitzer and Herschel, the discovery phase space for FORCAST lies in providing unique photometric bands and/or spectroscopic coverage, higher spatial resolution and exploration of the brightest sources which typically saturate space observatories.
The Astrophysical Journal, 2016
Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in natu... more Since their discovery, the Quintuplet proper members (QPMs) have been somewhat mysterious in nature. Originally dubbed the "cocoon stars" due to their cool featureless spectra, high-resolution near-infrared imaging observations have shown that at least two of the objects exhibit "pinwheel" nebulae consistent with binary systems with a carbonrich Wolf-Rayet star and O/B companion. In this paper, we present 19.7, 25.2, 31.5, and 37.1 µm observations of the QPMs (with an angular resolution of 3.2-3.8") taken with the Faint Object Infrared Camera for the SOFIA Telescope (FORCAST) in conjunction with high-resolution (∼0.1-0.2") images at 8.8 and 11.7 µm from the Thermal-Region Camera Spectrograph (TReCS). DUSTY models of the thermal dust emission of two of the four detected QPMs, Q2 and Q3, are fitted by radial density profiles which are consistent with constant mass loss rates (ρ d ∝ r −2). For the two remaining sources, Q1 and Q9, extended structures (∼ 1") are detected around these objects in high-resolution imaging data. Based on the fitted dust masses, Q9 has an unusually large dust reservoir (M d = 1.3 +0.8 −0.4 × 10 −3 M) compared to typical dusty Wolf-Rayet stars which suggests that it may have recently undergone an episode of enhanced mass loss.
SPIE Proceedings, 2014
We describe the Short Wavelength Camera (SWCam) for the CCAT observatory including the primary sc... more We describe the Short Wavelength Camera (SWCam) for the CCAT observatory including the primary science drivers, the coupling of the science drivers to the instrument requirements, the resulting implementation of the design, and its performance expectations at first light. CCAT is a 25 m submillimeter telescope planned to operate at 5600 meters, near the summit of Cerro Chajnantor in the Atacama Desert in northern Chile. CCAT is designed to give a total wave front error of 12.5 µm rms, so that combined with its high and exceptionally dry site, the facility will provide unsurpassed point source sensitivity deep into the short submillimeter bands to wavelengths as short as the 200 µm telluric window. The SWCam system consists of 7 sub-cameras that address 4 different telluric windows: 4 subcameras at 350 µm, 1 at 450 µm, 1 at 850 µm, and 1 at 2 mm wavelength. Each sub-camera has a 6' diameter field of view, so that the total instantaneous field of view for SWCam is equivalent to a 16' diameter circle. Each focal plane is populated with near unit filling factor arrays of Lumped Element Kinetic Inductance Detectors (LEKIDs) with pixels scaled to subtend an solid angle of (λ/D) 2 on the sky. The total pixel count is 57,160. We expect background limited performance at each wavelength, and to be able to map > 35 (°)2 of sky to 5 σ on the confusion noise at each wavelength per year with this first light instrument. Our primary science goal is to resolve the Cosmic Far-IR Background (CIRB) in our four colors so that we may explore the star and galaxy formation history of the Universe extending to within 500 million years of the Big Bang. CCAT's large and high-accuracy aperture, its fast slewing speed, use of instruments with large format arrays, and being located at a superb site enables mapping speeds of up to three orders of magnitude larger than contemporary or near future facilities and makes it uniquely sensitive, especially in the short submm bands.
The Astrophysical Journal, 2013
We have imaged the bipolar planetary nebula M2-9 using SOFIA's FORCAST instrument in six waveleng... more We have imaged the bipolar planetary nebula M2-9 using SOFIA's FORCAST instrument in six wavelength bands between 6.6 and 37.1 µm. A bright central point source, unresolved with SOFIA's ∼ 4 ′′-to-5 ′′ beam, is seen at each wavelength, and the extended bipolar lobes are clearly seen at 19.7 µm and beyond. The photometry between 10 and 25 µm is well fit by the emission predicted from a stratified disk seen at large inclination, as has been proposed for this source by Lykou et al and by Smith and Gehrz. The principal new results in this paper relate to the distribution and properties of the dust that emits the infrared radiation. In particular, a considerable fraction of this material is spread uniformly through the lobes, although the dust density does increase at the sharp outer edge seen in higher resolution optical images of M2-9. The dust grain population in the lobes shows that small (< 0.1 µm) and large (> 1 µm) particles appear to be present in roughly equal amounts by mass. We suggest that collisional processing within the bipolar outflow plays an important role in establishing the particle size distribution.
The Astrophysical Journal, 2012
The Astronomical Journal, 2006
We present an analysis of thermal emission from comet 162P/Siding Spring (P/2004 TU 12) measured ... more We present an analysis of thermal emission from comet 162P/Siding Spring (P/2004 TU 12) measured during its discovery apparition in December 2004. The comet showed no dust coma at this time, so we have sampled emission from the comet's nucleus. Observations using the "Mid-Infrared Spectrometer and Imager" ("MIRSI") were performed at NASA's Infrared Telescope Facility, where the peak of the comet's spectral energy distribution was observed between 8 and 25 µm. In combination with the three near-infrared spectra presented by Campins et al. (2006, AJ, this issue) that show the Wien-law tail of the thermal emission, the data provide powerful constraints on surface properties of the nucleus. We find that the nucleus's effective radius is 6.0±0.8 km. This is one of the largest radii known among Jupiter-family comets, which is unusual considering the comet was discovered only recently. Its geometric albedo is 0.059 ± 0.023 in H-band, 0.037 ± 0.014 in R-band, and 0.034 ± 0.013 in V-band. We also find that the nucleus of 162P has little infrared beaming, and this implies the nucleus has low thermal inertia. Including all near-IR spectra yields a beaming parameter η of 1.01 ± 0.20. This result is in agreement with others showing that cometary nuclei have low thermal inertia and little infrared beaming. If confirmed for many nuclei, the interpretation of radiometry may not be as problematic as feared.
The Astrophysical Journal, 2012
The Astrophysical Journal, 2012
The Astrophysical Journal, 2015
We present mid-IR (19-37 µm) imaging observations of S106 from SOFIA/FORCAST, complemented with I... more We present mid-IR (19-37 µm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0
We used MIRSI on the IRTF to make 10 and 20 \micron images of four candidate high-mass protosetll... more We used MIRSI on the IRTF to make 10 and 20 \micron images of four candidate high-mass protosetllar objects (HMPOs) from the sample of Sridharan et al. (2002). These candidate HMPOs were selected from the IRAS database using FIR color criteria derived for UCHIIs. The HMPOs had been detected in CS, but not in 5 GHz radio continuum single dish surveys above 25 mJy. Most were detected in the MSX mid-IR survey. Beuther et al. (2002) presented maps of 1.2 mm dust emission of the sample of HMPOs. Our selection criteria were that the sources appear compact in MSX bands C (12.1 \micron) and E (21.3 \micron), and in the 1.2 mm maps. Three sources were detected by MIRSI at the IRTF at both 10 \micron (47% width 10.6 \micron, N band or a 10% width 11.6 \micron filter) and 20 \micron (42% width 20.9 \micron filter): IRAS 22134+5834, 23033+5951, and 23151+5912. Their sizes are marginally larger than the diffraction limited beams of about one arcsec. The MIRSI flux densities are significant fract...
Science (New York, N.Y.), Jan 19, 2015
Dust formation in supernova ejecta is currently the leading candidate to explain the large quanti... more Dust formation in supernova ejecta is currently the leading candidate to explain the large quantities of dust observed in the distant, early Universe. However, it is unclear whether the ejecta-formed dust can survive the hot interior of the supernova remnant (SNR). We present infrared observations of ~0.02 [Formula: see text] of warm (~100 K) dust seen near the center of the ~10,000 yr-old Sgr A East SNR at the Galactic center. Our findings signify the detection of dust within an older SNR that is expanding into a relatively dense surrounding medium (ne ~ 100 cm(-3)) and has survived the passage of the reverse shock. The results suggest that supernovae may indeed be the dominant dust production mechanism in the dense environment of early Universe galaxies.
The Astrophysical Journal, 2014
SPIE Proceedings, 2004
Four institutions are collaborating to design and build three near identical λ/∆λ ∼ 2700 cross-di... more Four institutions are collaborating to design and build three near identical λ/∆λ ∼ 2700 cross-dispersed nearinfrared spectrographs for use on various 5-10 meter telescopes. The instrument design addresses the common observatory need for efficient, reliable near-infrared spectrographs through such features as broad wavelength coverage across 6 simultaneous orders (0.8-2.4 µm) in echelle format, real-time slit viewing through separate optics and detector, and minimal moving parts. Lastly, the collaborators are saving money and increasing the likelihood of success through economies of scale and sharing intellectual capital.
SPIE Proceedings, 2008
We have designed and fabricated a suite of grisms for use in FORCAST, a mid-infrared camera sched... more We have designed and fabricated a suite of grisms for use in FORCAST, a mid-infrared camera scheduled as a first-light instrument on SOFIA. The grism suite gives SOFIA a new capability: low and moderate resolution spectroscopy from 5µm to 37µm, without the addition of a new instrument. One feature of the optical design is that it includes a mode using pairs of cross-dispersed grisms, providing continuous wavelength coverage over a broad range at higher resolving power. We fabricated four silicon (n = 3.44) grisms using photolithographic techniques and purchased two additional mechanically ruled KRS-5 (n = 2.3) grisms. One pair of silicon grisms permits observations of the 5 − 8µm band with a long slit at R∼ 200 or, in a cross-dispersed mode, at resolving powers up to 1500. In the 8 − 14µm region, where silicon absorbs heavily, the KRS-5 grisms produce resolving powers of 300 and 800 in long-slit and cross-dispersed mode, respectively. The remaining two silicon grisms cover 17 − 37µm at resolving powers of 140 and 250. We have thoroughly tested the silicon grisms in the laboratory, measuring efficiencies in transmission at 1.4 − 1.8µm. We report on these measurements as well as on cryogenic performance tests of the silicon and KRS-5 devices after installation in FORCAST.
SPIE Proceedings, 2010
Progress report on FORCAST grism spectroscopy as a future general observer instrument mode on SOF... more Progress report on FORCAST grism spectroscopy as a future general observer instrument mode on SOFIA", Proc. SPIE 7735, 77356N (2010).
The Astrophysical Journal, 2006