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Journal articles on the topic 'IRTF'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 May 2024

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1

Ohikhena, Agele, Samuel. "Dry season Irrigation Regime Effects on Water Use, Rootzone Moisture and Yield of Cacao (Theobroma cacao L.) in a Rainforest Zone of Nigeria." International Journal of Plant & Soil Science 35, no. 18 (July 17, 2023): 302–20. http://dx.doi.org/10.9734/ijpss/2023/v35i183293.

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The humid tropics is characterized by wet-dry seasonal transitions, irrigation has the potential for building adaptation and resilience to climate stress for enhancing crop performance. A field trial was conducted to investigate the effects of dry season irrigation regimes on water use, root zone moisture dynamics and yield of cacao in a rainforest zone of Nigeria. Irrigation amounts computed as EPan x Pan coefficients were based on cumulative class A Pan evaporation. Irrigation treatments were coded as IrT1 (EPan x 1,0), IrT2 (EPan x 0.7) and IrT3 (EPan x 0.5). Irrigation water was applied 5-days interval and discharged via point source emitters (2.8 l/h discharge rate ) on drip lines laterally installed per row of trees. Mean irrigation requirements were 4.49 mm (9.81:9.6 l/tree/day), 3.14 mm (7.06:6.8 l/tree/day) and 2.44 mm (5.49: 4.8 l/tree/day) while total seasonal water applied were 121.19, 84.83 and 60.59 l/tree for IrT1, IrT2 and IrT3 respectively. Mean soil moisture contents and cacao evapotranspiration (ETc) were 52, 45 and 28 % and 4.54, 3.19 and 2.32 mm/day while evaporation from soil area wetted by emitters (EWz) were 5.65, 2.82 and 0.19 mm/day for respective IrT1, IrT2 and IrT3. The deficit irrigation strategies (IrT2 and 31 IrT3) imposed soil moisture deficit stress on cacao and produced lower pod and bean yields, it however enhanced water use efficiencies (25 and 44 %) and 30 and 50 % water savings. The study established suitable Pan coefficients for scheduling irrigation for cacao yield enhancement and drought (climate stress) amelioration.

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Kroustallas, Fotios G., Georgios A. Papadopoulos, Sofia Chalvatzi, Vasilis Skampardonis, Leonidas Leontides, and Paschalis Fortomaris. "Infrared Thermography Evaluation of Feet Temperature and Its Association with Claw Lengths and Anisodactylia in Purebred Sows of Three Greek Herds." Veterinary Sciences 8, no. 12 (December 6, 2021): 309. http://dx.doi.org/10.3390/vetsci8120309.

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The aim of the study was to investigate the associations of lower feet temperature with claw lengths measurements in purebred sows. In total 22, 19 and 45 multiparous sows in three herds A, B and C of PIC, DANBRED and TOPIGS genetic lines respectively participated in the study. Mean parity was 2.5, 2.3 and 3.0 for sows from herds A, B and C respectively. Measurements were made during the periparturient period. Infrared temperature distribution was measured in carpus/tarsus, upper-lower metacarpi/metatarsi and phalanges (IRT1, IRT2, IRT3 and IRT4 respectively). In addition, dorsal, diagonal, heel–sole and dew claw lengths of medial and lateral claw were measured and the difference in dorsal claw length between medial and lateral claw (anisodactylia) was calculated in all four feet. Differences between herds regarding IRT and claw length measurements were analyzed with one-way ANOVA with herds as a fixed factor. Correlations between IRT and claw length measurements in each foot including data from all herds were evaluated using the Pearson’s correlation test. Maximum IRT1 to 4 in almost all rear feet, differed significantly between herds, being lower in sows of herd C than A and B (p < 0.05). Claw lengths of all feet were lower in herd C than those of A and B (p < 0.05). Anisodactylia, differed significantly only in rear feet between herds been higher in herd A than C and B (p < 0.05). In all sows, claw lengths and rear feet anisodactylia were positively correlated with maximum IRT1 to IRT4 (p < 0.05). According to the results, IRT temperature distribution of lower feet of purebred sows of different genetic lines were positive correlated with claw lengths measurements and anisodactylia. Collectively, measuring IRT temperature of lower feet of sows with mobile IRT device could be used as an additional tool towards monitoring feet and claw health.

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3

Impey, C. D., C. G. Wynn-Williams, and E. E. Becklin. "Infrared Emission from Radio Galaxies." Symposium - International Astronomical Union 134 (1989): 404–5. http://dx.doi.org/10.1017/s0074180900141488.

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4

Kozlowski, Wojciech, and Rodney Van Meter. "Schrödinger's Internet at the IRTF." IEEE Communications Standards Magazine 4, no. 3 (September 2020): 4–6. http://dx.doi.org/10.1109/mcomstd.2020.9204590.

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5

Morales, Walter G., Alfredo Sequeira, Ester Chamorro, Mara Braga, Abilio Sobral, and Herminio De Sousa. "Termogravimetría y espectroscopía de infrarrojo para el control del rendimiento en la obtención de alquil esteres." Extensionismo, Innovación y Transferencia Tecnológica 2 (June 21, 2015): 35. http://dx.doi.org/10.30972/eitt.20278.

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En este trabajo se preparó zirconia modificada con sulfato de cerio al 5%, se evaluaron sus propiedades texturales y de acidez, y se han comparado bajo las mismas condiciones como catalizadores de las reacciones de esterificación y transesterificación de aceite de semilla de algodón con etanol y metanol. Las reacciones se llevaron a cabo en reactor bach bajo diferentes condiciones de tempe-ratura de reacción, relación molar aceite:alcohol, cantidad de catalizador y tiempo de reacción, la presión fue autogenerada de 30bar. Los productos de reacción fueron cuan-tificados por HPLC y posteriormente con análisis termogravimétrico (TGA) y espectroscopía infrarroja con transformada de Fourier (IRTF). Se halló que el análisis TGA es muy útil para seguimiento de reacciones de obtención de etil y metil ésteres, hallándose diferencias importantes hasta concentración del 96%, mientras que el IRTF es mucho menos sensible

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6

Marcq, E., I. Amine, M. Duquesnoy, and B. Bézard. "Evidence for SO2 latitudinal variations below the clouds of Venus." Astronomy & Astrophysics 648 (April 2021): L8. http://dx.doi.org/10.1051/0004-6361/202140837.

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Context. Sulphur dioxide (SO2) is highly variable above the clouds of Venus, yet no spatial or temporal variability below the clouds had been known until now. Aims. In order to constrain Venus’s atmospheric circulation and chemistry (including possible volcanic outgassing), more accurate SO2 measurements below the clouds are therefore needed. Methods. We used the high-resolution iSHELL spectrometer located at the NASA IRTF to record thermal night-side spectra, which we fitted using an updated forward radiative transfer model that was previously employed to process SpeX/IRTF and VIRTIS-H/Venus Express spectra. Results. We report, for the first time, an increase in SO2 with increasing latitude (+30% between the minimum near 15°S and > 35°N). This is consistent with the interaction between the Hadley-cell circulation and a postulated vertical profile in SO2 estimated to increase between 30 and 40 km in altitude, as previously suggested by in situ ISAV measurements. Conclusions. This SO2 variability challenges our current understanding of Venus’s tropospheric thermochemistry and underlines the high scientific return from high-resolution spectroscopy from, for example, future orbiters.

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Rayner, John, Alan Tokunaga, Daniel Jaffe, Timothy Bond, Morgan Bonnet, Gregory Ching, Michael Connelley, et al. "iSHELL: a 1–5 micron R = 80,000 Immersion Grating Spectrograph for the NASA Infrared Telescope Facility." Publications of the Astronomical Society of the Pacific 134, no. 1031 (January 1, 2022): 015002. http://dx.doi.org/10.1088/1538-3873/ac3cb4.

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Abstract iSHELL is a 1.06–5.3 μm high spectral resolution spectrograph built for the 3.2 m NASA Infrared Telescope Facility (IRTF) on Maunakea, Hawaii. Dispersion is accomplished with a silicon immersion grating in order to keep the instrument small enough to be mounted at the Cassegrain focus of the telescope. The white pupil spectrograph produces resolving powers of up to about R ≡ λ/δλ = 80,000 (0.″375 slit). Cross-dispersing gratings mounted in a tiltable mechanism allow observers to select different wavelength ranges and, in combination with a slit wheel and Dekker mechanism, slit widths ranging from 0.″375 to 4.″0 and slit lengths ranging from 5″ to 25″. One Teledyne 2048 × 2048 HAWAII-2RG array is used in the spectrograph, and one Raytheon 512 × 512 Aladdin 2 array is used in a 1–5 μm slit viewer for object acquisition, guiding, and scientific imaging. iSHELL has been in productive regular use on IRTF since first light in 2016 September. In this paper we discuss details of the science case, design, construction and astronomical use of iSHELL.

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Cesetti, M., A. Pizzella, V. D. Ivanov, L. Morelli, E. M. Corsini, and E. Dalla Bontà. "The Infrared Telescope Facility (IRTF) spectral library:." Astronomy & Astrophysics 549 (January 2013): A129. http://dx.doi.org/10.1051/0004-6361/201219078.

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Morelli, L., V. D. Ivanov, A. Pizzella, D. Gasparri, L. Coccato, E. M. Corsini, E. Dalla Bontà, P. François, and M. Cesetti. "The Infrared Telescope Facility (IRTF) spectral library." Astronomy & Astrophysics 641 (September 2020): A44. http://dx.doi.org/10.1051/0004-6361/202037505.

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Context. Stellar population studies in the infrared (IR) wavelength range have two main advantages with respect to the optical regime: they probe different populations, because most of the light in the IR comes from redder and generally older stars, and they allow us to see through dust because IR light is less affected by extinction. Unfortunately, IR modeling work was halted by the lack of adequate stellar libraries, but this has changed in the recent years. Aims. Our project investigates the sensitivity of various spectral features in the 1−5 μm wavelength range to the physical properties of stars (Teff, [Fe/H], log g) and aims to objectively define spectral indices that can characterize the age and metallicity of unresolved stellar populations. Methods. We implemented a method that uses derivatives of the indices as functions of Teff, [Fe/H] or log g across the entire available wavelength range to reveal the most sensitive indices to these parameters and the ranges in which these indices work. Results. Here, we complement the previous work in the I and K bands, reporting a new system of 14, 12, 22, and 12 indices for Y, J, H, and L atmospheric windows, respectively, and describe their behavior. We list the equivalent widths of these indices for the Infrared Telescope Facility (IRTF) spectral library stars. Conclusions. Our analysis indicates that features sensitive to the effective temperature are present and measurable in all the investigated atmospheric windows at the spectral resolution and in the metallicity range of the IRTF library for a signal-to-noise ratio greater than 20−30. The surface gravity is more challenging and only indices in the H and J windows are best suited for this. The metallicity range of the stars with available spectra is too narrow to search for suitable diagnostics. For the spectra of unresolved galaxies, the defined indices are valuable tools in tracing the properties of the stars in the IR-dominant stellar populations.

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10

Huitema, Christian, Geoff Huston, Dirk Kutscher, and Lixia Zhang. "Report of 2021 DINRG Workshop on Centralization in the Internet." ACM SIGCOMM Computer Communication Review 53, no. 2 (April 30, 2023): 31–39. http://dx.doi.org/10.1145/3610381.3610386.

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The Internet Research Task Force (IRTF) Research Group on Decentralizing the Internet (DINRG) hosted a workshop on Centralization in the Internet on June 3, 2021. The workshop focused on painting a broad-brush landscape of the Internet centralization problem space: its starting point, its driving force, together with an articulation on what can and should be done.

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11

Mezger, P. G., R. Zylka, C. J. Salter, J. E. Wink, R. Chini, E. Kreysa, and R. Tuffs. "Continuum Observations of Sgr A at mm/submm Wavelengths." Symposium - International Astronomical Union 136 (1989): 357–60. http://dx.doi.org/10.1017/s0074180900186735.

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We have mapped the source complex Sgr A (containing Sgr A West and East) at λ2.8mm, 1.3mm and 350μm using the IRAM 30m MRT (Pico Veleta, Spain) and the 3m IRTF (Mauna Kea, Hawaii) telescopes. Detailed results have been published or will be published elsewhere (Mezger et al., 1986, Paper I; Zylka and Mezger, 1988, Paper II; Mezger et al., 1988, Paper III).

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12

Meneses-Goytia, Sofia, and Reynier F. Peletier. "A first glance into the Spectral Energy Distributions of Single Stellar Populations in the Infrared range." Proceedings of the International Astronomical Union 7, S284 (September 2011): 32–34. http://dx.doi.org/10.1017/s1743921312008666.

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AbstractThe present work shows the Spectral Energy Distributions (SEDs) in the infrared using the IRTF stellar library, obtained using models based on Single Stellar population Models (SSP). We have focused on the K band in order to compare with observables of elliptical galaxies. We also present the comparisons of our models with velocity dispersions, ages and metallicities obtained with models in the optical range.

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13

Smith, C. H., D. K. Aitken, and P. F. Roche. "Spatially Resolved Observations of the Unidentified Dust Features in BD +30°3639." Symposium - International Astronomical Union 131 (1989): 203. http://dx.doi.org/10.1017/s0074180900138136.

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High resolution spatial scans through the planetary nebula BD +30°3639 have been made with the UCL cooled grating spectrometer at the IRTF. A spectral resolution of λ/Δλ = 50 was sufficient to resolve the unidentified dust features at 8.6 and 11.3 μm and separate them from the continuum emission. The scans were made in .7 arcsec steps across the nebula with a 1.8 arcsec diameter beam.

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14

Yang, Bin, Michael S. P. Kelley, Karen J. Meech, Jacqueline V. Keane, Silvia Protopapa, and Schelte J. Bus. "Searching for water ice in the coma of interstellar object 2I/Borisov." Astronomy & Astrophysics 634 (January 31, 2020): L6. http://dx.doi.org/10.1051/0004-6361/201937129.

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Aims. Interstellar objects passing through our Solar System offer a rare opportunity to probe the physical and chemical processes involved in solid body and planet formation in extrasolar systems. The main objective of our study is to search for diagnostic absorption features of water ice in the near-infrared (NIR) spectrum of the second interstellar object 2I/2019 Q4 (Borisov) and compare its ice features to those of the Solar System icy objects. Methods. We observed 2I in the NIR on three separate occasions. The first observation was made on 2019 September 19 UT using the SpeX spectrograph at the 3m IRTF and again on September 24 UT with the GNIRS spectrograph at the 8m GEMINI telescope; the last observation was made on October 09 UT with IRTF. Results. The spectra obtained from all three nights appear featureless. No absorption features associated with water ice are detected. Spectral modeling suggests that water grains, if present, comprise no more than 10% of the coma cross section. The comet consistently exhibits a red D-type like spectrum with a spectral slope of about 6% per 1000 Å, which is similar to that of 1I/’Oumuamua and is comparable to Solar System comets.

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Lacy, John H., J. M. Achtermann, and D. E. Bruce. "Observations of HI Br α, [Ne II], and [Ar III] from the Central Parsec of the Galaxy." Symposium - International Astronomical Union 136 (1989): 523–24. http://dx.doi.org/10.1017/s0074180900187017.

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H I Br α (4.05 μm), [Ne II] (12.8 μm), and [Ar III] (9.0 μm) emission lines from Sgr A West were mapped with ~100 km/s and 2″ resolution. The observations were made with the U. T. infrared echelle spectrometer (IRSHELL) on the IRTF in April 1988. The instrument simultaneously measures 10 64-point spectra along a 2 × 10″ slit. Data analysis is still in progress; preliminary results are presented here.

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Nagata, Tetsuya, Shuji Sato, A. R. Hyland, and Alan T. Tokunaga. "Bright Near-Infrared Sources Within 1° of the Galactic Center." Symposium - International Astronomical Union 136 (1989): 195. http://dx.doi.org/10.1017/s007418090018653x.

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A near-infrared survey has been conducted of 0.55 square degrees around the Galactic center with the 1 m telescope of Siding Spring Observatory, Australia. From the detected sources, 39 objects which are bright (K<7.6) and red (H-K>1.4) and 11 objects slightly fainter (K~8) have been selected. Subsequently, their 1–20 μm photometry and 2–3.5 μm spectra at a resolution of λ/Δλ∼150 have been obtained with the IRTF atop Mauna Kea, Hawaii.

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González-Cruz, Ricardo, Irma Idalia Rangel-Salas, Martín Martínez Ríos, and Gabriela Alejandra Flores Gómez. "Captura de iones Mercurio II con electrodos de PVA-Polianilina." Brazilian Journal of Development 9, no. 12 (December 14, 2023): 31246–58. http://dx.doi.org/10.34117/bjdv9n12-046.

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Se realizó electroadsorción de iones mercurio de forma exitosa aplicando un potencial de -1 V a películas de PVA-Polianilina empleadas como cátodos, además, el mismo material fue empleado como ánodo. La caracterización por IRTF muestra evidencia que el nitrógeno puede ser el elemento coordinante de los iones mercurio. Las mediciones de la concentración de las soluciones muestran que es posible captar la misma cantidad de iones en mucho menor tiempo si se aplica un potencial catódico al electrodo de trabajo.

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18

Blake, James S. D., Leigh N. Fletcher, Thomas K. Greathouse, Glenn S. Orton, Henrik Melin, Mike T. Roman, Arrate Antuñano, Padraig T. Donnelly, Naomi Rowe-Gurney, and Oliver King. "Refining Saturn’s deuterium-hydrogen ratio via IRTF/TEXES spectroscopy." Astronomy & Astrophysics 653 (September 2021): A66. http://dx.doi.org/10.1051/0004-6361/202038229.

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The abundance of deuterium in giant planet atmospheres provides constraints on the reservoirs of ices incorporated into these worlds during their formation and evolution. Motivated by discrepancies in the measured deuterium-hydrogen (D/H) ratio on Jupiter and Saturn, we present a new measurement of the D/H ratio in methane for Saturn from ground-based measurements. We analysed a spectral cube (covering 1151–1160 cm−1 from 6 February 2013) from the Texas Echelon Cross Echelle Spectrograph (TEXES) on NASA’s Infrared Telescope Facility (IRTF) where emission lines from both methane and deuterated methane are well resolved. Our estimate of the D/H ratio in stratospheric methane, 1.65−0.21+0.27 × 10−5 is in agreement with results derived from Cassini CIRS and ISO/SWS observations, confirming the unexpectedly low CH3D abundance. Assuming a fractionation factor of 1.34 ± 0.19 we derive a hydrogen D/H of 1.23−0.23+0.27 × 10−5. This value remains lower than previous tropospheric hydrogen D/H measurements of (i) Saturn 2.10(±0.13) × 10−5, (ii) Jupiter 2.6(±0.7) × 10−5 and (iii) the proto-solar hydrogen D/H of 2.1(±0.5) × 10−5, suggesting that the fractionation factor may not be appropriate for stratospheric methane, or that the D/H ratio in Saturn’s stratosphere is not representative of the bulk of the planet.

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Falk, Aaron. "The IETF, the IRTF, and the networking research community." ACM SIGCOMM Computer Communication Review 35, no. 5 (October 6, 2005): 69–70. http://dx.doi.org/10.1145/1096536.1096545.

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20

Lopez, D., and R. Krishnan. "The NFVRG Network Function Virtualization Research at the IRTF." Journal of ICT Standardization 3, no. 1 (2015): 57–66. http://dx.doi.org/10.13052/jicts2245-800x.313.

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21

Rayner, John T., Michael C. Cushing, and William D. Vacca. "THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS." Astrophysical Journal Supplement Series 185, no. 2 (November 17, 2009): 289–432. http://dx.doi.org/10.1088/0067-0049/185/2/289.

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Rivkin, Andrew S., Beth E. Clark, Maureen Ockert-Bell, Eric Volquardsen, Ellen S. Howell, Schelte J. Bus, Cristina A. Thomas, and Michael Shepard. "Asteroid 21 Lutetia at 3μm: Observations with IRTF SpeX." Icarus 216, no. 1 (November 2011): 62–68. http://dx.doi.org/10.1016/j.icarus.2011.08.009.

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23

Ramírez, S. V., K. Sellgren, D. M. Terndrup, J. S. Carr, S. Balachandran, and R. D. Blum. "Iron Abundances in AGB Stars and M Supergiant Stars at the Galactic Center." Symposium - International Astronomical Union 191 (1999): 529–34. http://dx.doi.org/10.1017/s0074180900203513.

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We are measuring Fe abundances of cool, luminous stars within 30 pc of the center of the Milky Way. Our sample contains both AGB stars and M supergiants. Low-resolution (λ/Δλ = 500) H and K band spectra are used to estimate temperatures and gravities. Stellar Fe abundances are determined from high-resolution (λ/Δλ = 40 000) K band spectra obtained on the IRTF using CSHELL. We find that Fe abundances of stars in the Galactic Center are consistent with the solar Fe abundance.

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Le Corre, Lucille, Juan A. Sanchez, Vishnu Reddy, Adam Battle, David C. Cantillo, Benjamin Sharkey, Robert Jedicke, and Daniel J. Scheeres. "Mineralogical Characterization and Phase Angle Study of Two Binary Near-Earth Asteroids, Potential Targets for NASA’s Janus Mission." Planetary Science Journal 4, no. 5 (May 1, 2023): 91. http://dx.doi.org/10.3847/psj/acd10d.

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Abstract Ground-based characterization of spacecraft targets prior to mission operations is critical to properly plan and execute measurements. Understanding surface properties, such as mineralogical composition and phase curves (expected brightness at different viewing geometries), informs data acquisition during the flybys. Binary near-Earth asteroids (NEAs) (35107) 1991 VH and (175706) 1996 FG3 were selected as potential targets of the National Aeronautics and Space Administration’s (NASA) dual spacecraft Janus mission. We observed 1991 VH using the 3 m NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, on 2008 July 26. 1996 FG3 was observed with the IRTF for seven nights during the spring of 2022. Compositional analysis of 1991 VH revealed that this NEA is classified as an Sq-type in the Bus–DeMeo taxonomy classification, with a composition consistent with LL ordinary chondrites. Using thermal modeling, we computed the thermally corrected spectra for 1996 FG3 and the corresponding best-fit albedo of about 2%–3% for the best spectra averaged for each night. Our spectral analysis indicates that this NEA is a Ch-type. The best possible meteorite analogs for 1996 FG3, based on curve matching, are two carbonaceous chondrites, Y-86789 and Murchison. No rotational variation was detected in the spectra of 1996 FG3, which means there may not be any heterogeneities on the surface of the primary. However, a clear phase reddening effect was observed in our data, confirming findings from previous ground-based studies.

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Faggi, Sara, Manuela Lippi, Maria Camarca, Camillus F. Buzard, Geronimo L. Villanueva, Gregory W. Doppmann, Geoffrey A. Blake, and Michael J. Mumma. "The Extraordinary Passage of Comet C/2020 F3 NEOWISE: Evidence for Heterogeneous Chemical Inventory in Its Nucleus." Astronomical Journal 162, no. 5 (October 5, 2021): 178. http://dx.doi.org/10.3847/1538-3881/ac179c.

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Abstract Upon its discovery in 2020 March, we requested Director Discretionary Time (DDT) at the NASA/IRTF facility to observe comet C/2020 F3 (NEOWISE), with the high-resolution spectrograph iSHELL. The comet approached the Sun, down to 0.3 au, in early 2020 July, providing a spectacular perihelion passage and revealing itself as one of the brightest comets that have appeared in the northern hemisphere in recent decades. Daytime observations with iSHELL/IRTF were performed to study the comet immediately after its perihelion passage, from 9 July to 1 August. In early August, a DDT at Keck Observatory was requested to continue following the comet with NIRSPEC 2.0. We acquired comprehensive high-resolution spectra of the comet as it progressively retreated from perihelion. We detected many cometary emission lines in the (2.8–5.3) μm range, identifying 12 molecular species: 9 primary volatiles (H2O, HCN, NH3, CO, C2H2, C2H6, CH4, CH3OH, and H2CO) and 3 product species (CN, NH2, OH). In this paper, we present the analysis and discussion of the molecular abundances found in this comet, and we compare them to reference median values for Oort Cloud Comets. Measured molecular mixing ratios showed drastic changes during our observing campaign, which spanned nearly one month from 2020 July 9 to August 6. Here, we provide a detailed discussion of the molecular spatial distributions and their role in identifying the presence of extended sources in the coma. Our investigations provided evidence for the heterogeneous chemical composition of the comet’s nucleus.

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Faggi, Sara, Manuela Lippi, Maria Camarca, Camillus F. Buzard, Geronimo L. Villanueva, Gregory W. Doppmann, Geoffrey A. Blake, and Michael J. Mumma. "The Extraordinary Passage of Comet C/2020 F3 NEOWISE: Evidence for Heterogeneous Chemical Inventory in Its Nucleus." Astronomical Journal 162, no. 5 (October 5, 2021): 178. http://dx.doi.org/10.3847/1538-3881/ac179c.

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Abstract Upon its discovery in 2020 March, we requested Director Discretionary Time (DDT) at the NASA/IRTF facility to observe comet C/2020 F3 (NEOWISE), with the high-resolution spectrograph iSHELL. The comet approached the Sun, down to 0.3 au, in early 2020 July, providing a spectacular perihelion passage and revealing itself as one of the brightest comets that have appeared in the northern hemisphere in recent decades. Daytime observations with iSHELL/IRTF were performed to study the comet immediately after its perihelion passage, from 9 July to 1 August. In early August, a DDT at Keck Observatory was requested to continue following the comet with NIRSPEC 2.0. We acquired comprehensive high-resolution spectra of the comet as it progressively retreated from perihelion. We detected many cometary emission lines in the (2.8–5.3) μm range, identifying 12 molecular species: 9 primary volatiles (H2O, HCN, NH3, CO, C2H2, C2H6, CH4, CH3OH, and H2CO) and 3 product species (CN, NH2, OH). In this paper, we present the analysis and discussion of the molecular abundances found in this comet, and we compare them to reference median values for Oort Cloud Comets. Measured molecular mixing ratios showed drastic changes during our observing campaign, which spanned nearly one month from 2020 July 9 to August 6. Here, we provide a detailed discussion of the molecular spatial distributions and their role in identifying the presence of extended sources in the coma. Our investigations provided evidence for the heterogeneous chemical composition of the comet’s nucleus.

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Farihi, J. "IRTF observations of white dwarfs with possible near-infrared excess." Monthly Notices of the Royal Astronomical Society 398, no. 4 (October 1, 2009): 2091–109. http://dx.doi.org/10.1111/j.1365-2966.2009.15250.x.

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Harrington, Joseph, Maren L. Cooke, William J. Forrest, Judith L. Pipher, Edward W. Dunham, and J. L. Elliot. "IRTF Observations of the Occultation of 28 Sgr by Saturn." Icarus 103, no. 2 (June 1993): 235–52. http://dx.doi.org/10.1006/icar.1993.1068.

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Roos-Serote, M., V. Coupé, P. Drossart, E. Lellouch, O. Saint-Pé, and Th Encrenaz. "Infrared imaging of Venus from IRTF/ProtoCAM observations in 1991." Planetary and Space Science 44, no. 6 (June 1996): 509–17. http://dx.doi.org/10.1016/0032-0633(95)00143-3.

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Lindau-Shepard, Barbara A., and Kenneth A. Pass. "Newborn Screening for Cystic Fibrosis by Use of a Multiplex Immunoassay." Clinical Chemistry 56, no. 3 (March 1, 2010): 445–50. http://dx.doi.org/10.1373/clinchem.2009.132480.

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Abstract Background: Since its beginnings, newborn screening for cystic fibrosis (CF) using an assay for immunoreactive trypsinogen (IRT) has been plagued by a high rate of false-positive results (screen positive, diagnosis negative), despite attempts to reduce this rate by use of altered cutoffs and second-tier DNA testing. IRT exists as 2 isoforms: IRT1 and IRT2, with IRT2 being more closely aligned with pancreatic disease, including CF. Assay standardization between programs is a continuing problem because the IRT assays currently in use variously recognize either 1 or both isoforms. Here we report the development of a multiplexed assay for both forms of IRT simultaneously. Methods: Using 2 different Luminex bead sets, we developed assays for each IRT isoform separately and then combined them. Using the sum of IRT1 and IRT2 values (IRT1+IRT2), we compared the results with a CF kit currently in use. Results: In a sample set consisting of 16 cases confirmed positive for CF, we established a cutoff at >97 μg/L total IRT. Seven of 8 carriers with 1 CF mutation screen-positive by the standard method were also screen-positive by IRT1+IRT2. Of 32 cases screen-positive by standard IRT, 11 were screen-negative by IRT1+IRT2. None of these 11 cases had CF mutations identified by the screening program. Conclusions: These data indicate that the multiplex method with specificity for 2 isoforms of IRT has performance comparable to that of a standard IRT method and the advantage of improved standardization by detection of the 2 isoforms.

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Plavchan, Peter, Peter Gao, Jonathan Gagne, Elise Furlan, Carolyn Brinkworth, Michael Bottom, Angelle Tanner, et al. "Precise Near-Infrared Radial Velocities." Proceedings of the International Astronomical Union 10, S314 (November 2015): 286–87. http://dx.doi.org/10.1017/s1743921315006468.

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AbstractWe present the results of two 2.3 μm near-infrared (NIR) radial velocity (RV) surveys to detect exoplanets around 36 nearby and young M dwarfs. We use the CSHELL spectrograph (R ~ 46,000) at the NASA InfraRed Telescope Facility (IRTF), combined with an isotopic methane absorption gas cell for common optical path relative wavelength calibration. We have developed a sophisticated RV forward modeling code that accounts for fringing and other instrumental artifacts present in the spectra. With a spectral grasp of only 5 nm, we are able to reach long-term radial velocity dispersions of ~20–30 m s−1 on our survey targets.

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Roth, Nathan X., Stefanie N. Milam, Michael A. DiSanti, Geronimo L. Villanueva, Sara Faggi, Boncho P. Bonev, Martin A. Cordiner, et al. "Molecular Outgassing in Centaur 29P/Schwassmann–Wachmann 1 during Its Exceptional 2021 Outburst: Coordinated Multiwavelength Observations Using nFLASH at APEX and iSHELL at the NASA-IRTF." Planetary Science Journal 4, no. 9 (September 1, 2023): 172. http://dx.doi.org/10.3847/psj/ace1e9.

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Abstract The extraordinary 2021 September–October outburst of Centaur 29P/Schwassmann–Wachmann 1 afforded an opportunity to test the composition of primitive Kuiper disk material at high sensitivity. We conducted nearly simultaneous multiwavelength spectroscopic observations of 29P/Schwassmann–Wachmann 1 using iSHELL at the NASA Infrared Telescope Facility (IRTF) and nFLASH at the Atacama Pathfinder EXperiment (APEX) on 2021 October 6, with follow-up APEX/nFLASH observations on 2021 October 7 and 2022 April 3. This coordinated campaign between near-infrared and radio wavelengths enabled us to sample molecular emission from a wealth of coma molecules and to perform measurements that cannot be accomplished at either wavelength alone. We securely detected CO emission on all dates with both facilities, including velocity-resolved spectra of the CO (J = 2–1) transition with APEX/nFLASH and multiple CO (v = 1–0) rovibrational transitions with IRTF/iSHELL. We report rotational temperatures, coma kinematics, and production rates for CO and stringent (3σ) upper limits on abundance ratios relative to CO for CH4, C2H6, CH3OH, H2CO, CS, and OCS. Our upper limits for CS/CO and OCS/CO represent their first values in the literature for this Centaur. Upper limits for CH4, C2H6, CH3OH, and H2CO are the most stringent reported to date, and are most similar to values found in ultra CO-rich Oort cloud comet C/2016 R2 (PanSTARRS), which may have implications for how ices are preserved in cometary nuclei. We demonstrate the superb synergy of coordinated radio and near-infrared measurements, and advocate for future small-body studies that jointly leverage the capabilities of each wavelength.

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Pérez Paolino, Facundo, Jeffrey S. Bary, Michael S. Petersen, Kimberly Ward-Duong, Benjamin M. Tofflemire, Katherine B. Follette, and Heidi Mach. "Correlating Changes in Spot Filling Factors with Stellar Rotation: The Case of LkCa 4." Astrophysical Journal 946, no. 1 (March 1, 2023): 10. http://dx.doi.org/10.3847/1538-4357/acbb61.

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Abstract We present a multi-epoch spectroscopic study of LkCa 4, a heavily spotted non-accreting T Tauri star. Using SpeX at NASA’s Infrared Telescope Facility (IRTF), 12 spectra were collected over five consecutive nights, spanning ≈1.5 stellar rotations. Using the IRTF SpeX Spectral Library, we constructed empirical composite models of spotted stars by combining a warmer (photosphere) standard star spectrum with a cooler (spot) standard weighted by the spot filling factor, f spot. The best-fit models spanned two photospheric component temperatures, T phot = 4100 K (K7V) and 4400 K (K5V), and one spot component temperature, T spot = 3060 K (M5V) with an A V of 0.3. We find values of f spot to vary between 0.77 and 0.94 with an average uncertainty of ∼0.04. The variability of f spot is periodic and correlates with its 3.374 day rotational period. Using a mean value for f mean spot to represent the total spot coverage, we calculated spot corrected values for T eff and L ⋆. Placing these values alongside evolutionary models developed for heavily spotted young stars, we infer mass and age ranges of 0.45–0.6 M ⊙ and 0.50–1.25 Myr, respectively. These inferred values represent a twofold increase in the mass and a twofold decrease in the age as compared to standard evolutionary models. Such a result highlights the need for constraining the contributions of cool and warm regions of young stellar atmospheres when estimating T eff and L ⋆ to infer masses and ages as well as the necessity for models to account for the effects of these regions on the early evolution of low-mass stars.

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Farihi, J., E. E. Becklin, and B. Zuckerman. "The Search for Brown Dwarfs around White Dwarfs." Symposium - International Astronomical Union 211 (2003): 289–92. http://dx.doi.org/10.1017/s0074180900210772.

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The infrared search for substellar companions to nearby white dwarfs has been going on for a little more than a decade. The most recent phase has been a wide field proper motion search carried out primarily at Steward Observatory, where we are complete down to J = 18. Earlier phases included near field searches at the IRTF and Keck Observatory. In the last year we have discovered ten previously unrecognized faint proper motion companions. Of the recent discoveries, most are white dwarfs and a few M dwarfs. GD165B, discovered in 1988 as part of our program, is still the only known companion to a white dwarf with spectral type later than M.

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Schmidt, Ricardo de O., Ramin Sadre, and Luuk Hendriks. "Flow-Based Network Management: A Report from the IRTF NMRG Workshop." Journal of Network and Systems Management 24, no. 3 (February 13, 2016): 746–53. http://dx.doi.org/10.1007/s10922-016-9365-0.

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Vernazza, P., F. DeMeo, D. A. Nedelcu, M. Birlan, A. Doressoundiram, S. Erard, and E. Volquardsen. "Resolved spectroscopy of Mercury in the near-IR with SpeX/IRTF." Icarus 209, no. 1 (September 2010): 125–37. http://dx.doi.org/10.1016/j.icarus.2009.12.010.

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Peralta, Javier, Juan A. Prieto, Pilar Orozco-Sáenz, Jesús González, Gonzalo Trujillo, Lucía Torres, Alberto Sánchez, and Manuel Arnedo. "Secondary School Students observe Venus with NASA Infrared Telescope Facility (IRTF)." Research Notes of the AAS 7, no. 3 (March 17, 2023): 53. http://dx.doi.org/10.3847/2515-5172/acc39e.

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Abstract Astronomy and astrophysics are regarded as highly motivating topics for students in primary and secondary schools, and they have been a recurrent and effective resource to inspire passion about science. In fact, during the last years we have witnessed a boost of facilities providing small robotic telescopes for teachers and students to remotely undertake their own observing projects. A step forward is presented here, where we describe the experience of secondary school students attending professional observations of Venus at NASA’s Infrared Telescope Facility and, in a second observing run, conducting the observations by themselves. In addition to quickly mastering the basic operation of the control software for the SpeX instrument, the students successfully performed different types of data acquisition, including drift scan imaging.

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Verro, K., S. C. Trager, R. F. Peletier, A. Lançon, A. Gonneau, A. Vazdekis, P. Prugniel, et al. "The X-shooter Spectral Library (XSL): Data Release 3." Astronomy & Astrophysics 660 (April 2022): A34. http://dx.doi.org/10.1051/0004-6361/202142388.

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We present the third data release (DR3) of the X-shooter Spectral Library (XSL). This moderate-to-high resolution, near-ultraviolet-to-near-infrared (350–2480 nm, R ∼ 10 000) spectral library is composed of 830 stellar spectra of 683 stars. DR3 improves upon the previous data release by providing the combined de-reddened spectra of the three X-shooter segments over the full 350–2480 nm wavelength range. It also includes additional 20 M-dwarf spectra from the ESO archive. We provide detailed comparisons between this library and Gaia EDR3, MILES, NGSL, CaT library, and (E-)IRTF. The normalised rms deviation is better than D = 0.05 or 5% for the majority of spectra in common between MILES (144 spectra of 180), NGSL (112/116), and (E-)IRTF (55/77) libraries. Comparing synthetic colours of those spectra reveals only negligible offsets and small rms scatter, such as the median offset(rms) 0.001 ± 0.040 mag in the (box1 − box2) colour of the UVB arm, −0.004 ± 0.028 mag in (box3 − box4) of the VIS arm, and −0.001 ± 0.045 mag in (box2 − box3) colour between the UVB and VIS arms, when comparing stars in common with MILES. We also find an excellent agreement between the Gaia published (BP − RP) colours and those measured from the XSL DR3 spectra, with a zero median offset and an rms scatter of 0.037 mag for 449 non-variable stars. The unmatched characteristics of this library, which combine a relatively high resolution, a large number of stars, and an extended wavelength coverage, will help us to bridge the gap between the optical and the near-IR studies of intermediate and old stellar populations, and to probe low-mass stellar systems.

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Gonneau, A., M. Lyubenova, A. Lançon, S. C. Trager, R. F. Peletier, A. Arentsen, Y. P. Chen, et al. "The X-shooter Spectral Library (XSL): Data release 2." Astronomy & Astrophysics 634 (February 2020): A133. http://dx.doi.org/10.1051/0004-6361/201936825.

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We present the second data release (DR2) of the X-shooter Spectral Library (XSL), which contains all the spectra obtained over the six semesters of that program. This release supersedes our first data release from Chen et al. (2014, A&A, 565, A117), with a larger number of spectra (813 observations of 666 stars) and with a more extended wavelength coverage as the data from the near-infrared arm of the X-shooter spectrograph are now included. The DR2 spectra then consist of three segments that were observed simultaneously and, if combined, cover the range between ∼300 nm and ∼2.45 μm at a spectral resolving power close to R = 10 000. The spectra were corrected for instrument transmission and telluric absorption, and they were also corrected for wavelength-dependent flux-losses in 85% of the cases. On average, synthesized broad-band colors agree with those of the MILES library and of the combined IRTF and Extended IRTF libraries to within ∼1%. The scatter in these comparisons indicates typical errors on individual colors in the XSL of 2−4%. The comparison with 2MASS point source photometry shows systematics of up to 5% in some colors, which we attribute mostly to zero-point or transmission curve errors and a scatter that is consistent with the above uncertainty estimates. The final spectra were corrected for radial velocity and are provided in the rest-frame (with wavelengths in air). The spectra cover a large range of spectral types and chemical compositions (with an emphasis on the red giant branch), which makes this library an asset when creating stellar population synthesis models or for the validation of near-ultraviolet to near-infrared theoretical stellar spectra across the Hertzsprung-Russell diagram.

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Sitko, Michael L., David K. Lynch, Ray W. Russell, and Carol A. Grady. "Mid-IR Spectroscopy of the Debris Disks in the TW Hydrae Association." Symposium - International Astronomical Union 202 (2004): 368–70. http://dx.doi.org/10.1017/s0074180900218287.

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Spectroscopic observation between 3-14 μm of 3 stars in the TW Hya Association were obtained using the Aerospace Corporation Broadband Array Spectrograph System (BASS) on the NASA IRTF telescope. The targets observed were TW Hya, HR 4796A, and HD 98800. Both of the late-type stars, TW Hya and HD 98800, exhibit a strong 10 μm silicate emission band. The strong emission indicates the presence of small dust grains close to the star, at angular distances not currently accessible to coronagraphic techniques. The spectral structure due to crystalline material that is present in some young early-type stars (HD 163296, HD 31648, etc.) is not apparent in these two objects. For HR 4796A, the dust emission is weak.

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Dayal, A., W. F. Hoffmann, J. H. Bieging, J. L. Hora, L. K. Deutsch, G. G. Fazio, M. Meixner, and C. J. Skinner. "Mid-infrared imaging of dust shells around young Planetary and Proto-Planetary Nebulae." Symposium - International Astronomical Union 180 (1997): 347. http://dx.doi.org/10.1017/s0074180900131237.

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The results presented here are from an ongoing mid-infrared imaging study of PPNe and PNe, using MIRAC2 the UA/SAO mid-IR camera. Our 8-21 μm observations have a spatial resolution of about 0.7″ to 1.5″, and a pixel scale of 0.25″/pixel (at UKIRT) or 0.34″/pixel (at IRTF). The high S/N and good spatial sampling in our images of IRAS 22272+5435 and IRAS 07134+1005 allow us to construct temperature and optical depth maps. Using our 11.7μm and 20.6μm images we also construct maps which isolate the 11.3μm (UIR) and 21μm emission features (Justannont et al. 1995). As a second part of this project, we are modelling the dust emission from PPNe and young PNe, using a axisymmetrical radiative transfer code.

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Estienne, J., and O. Cerclier. "Structural Characterization of Synthetic Boehmites by IRTF-Spectroscopy and X-Ray Diffractometry." Materials Science Forum 133-136 (January 1993): 721–26. http://dx.doi.org/10.4028/www.scientific.net/msf.133-136.721.

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Lisse, C. M., M. L. Sitko, and M. Marengo. "IRTF/SPEX OBSERVATIONS OF THE UNUSUAL KEPLER LIGHT CURVE SYSTEM KIC 8462852." Astrophysical Journal 815, no. 2 (December 17, 2015): L27. http://dx.doi.org/10.1088/2041-8205/815/2/l27.

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44

Guliano, M., G. Mille, J. Kister, and J. F. Muller. "Étude des spectres IRTF de charbons français déminéralisés et de leurs macéraux." Journal de Chimie Physique 85 (1988): 963–70. http://dx.doi.org/10.1051/jcp/1988850963.

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Kassis, Marc, Joseph D. Adams, Joseph L. Hora, Lynne K. Deutsch, and Eric V. Tollestrup. "MIRSI, A Mid-Infrared Spectrometer and Imager: Performance Results from the IRTF." Publications of the Astronomical Society of the Pacific 120, no. 874 (December 2008): 1271–81. http://dx.doi.org/10.1086/595711.

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Tice, Dane S., Patrick G. J. Irwin, Leigh N. Fletcher, Nick A. Teanby, Jane Hurley, Glenn S. Orton, and Gary R. Davis. "Uranus’ cloud particle properties and latitudinal methane variation from IRTF SpeX observations." Icarus 223, no. 2 (April 2013): 684–98. http://dx.doi.org/10.1016/j.icarus.2013.01.006.

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47

Hernández, Miguel Angel, Gabriela Itzel Hernández, Roberto Portillo, Martha Alicia Salgado, Fernando Rojas, and Vitalii Petranovskii. "Nanoporosity of MCM-41 Materials and Y-Zeolites Created by Deposition of Tournefortia hirsutissima L. Plant Extract." Journal of Nanomaterials 2017 (2017): 1–10. http://dx.doi.org/10.1155/2017/2783143.

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Hybrid materials based on MCM-41 silica and Y-zeolites with a variable Si/Al ratio and an appropriate countercationic composition were prepared by impregnating inorganic substrates with an organic extract. The organic phase was previously characterized by GC-MS and IRTF, while XRD, SEM, TEM, N2-physisorption, and TPD of NH3 were used to analyze the selected inorganic supports. The effect of size- and shape-selectivity was manifested in MCM-41 and Y-zeolites. Texture results confirm that the extract containing relatively large branched organic molecules is deposited in the internal voids of MCM-41 material and on the outer area of Y-zeolites. In the case of Y-zeolites, the results demonstrate the effect of the SiO2/Al2O3 molar ratio and countercations on the textural properties of the samples.

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Villaume, Alexa, Charlie Conroy, Benjamin Johnson, John Rayner, Andrew W. Mann, and Pieter van Dokkum. "The Extended IRTF Spectral Library: Expanded Coverage in Metallicity, Temperature, and Surface Gravity." Astrophysical Journal Supplement Series 230, no. 2 (June 20, 2017): 23. http://dx.doi.org/10.3847/1538-4365/aa72ed.

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Boukir, Abdellatif, Michel Guiliano, Pierre Doumenq, Abdelilah El Hallaoui, and Gilbert Mille. "Caractérisation structurale d'asphaltènes pétroliers par spectroscopie infrarouge (IRTF). Application à la photo-oxydation." Comptes Rendus de l'Académie des Sciences - Series IIC - Chemistry 1, no. 10 (October 1998): 597–602. http://dx.doi.org/10.1016/s1387-1609(99)80013-9.

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50

Weiland, J. J., R. Guyonnet, and R. Gibert. "Analyse de la pyrolyse menagee du bois par un couplage TG-DSC-IRTF." Journal of Thermal Analysis and Calorimetry 51, no. 1 (January 1998): 265–74. http://dx.doi.org/10.1007/bf02719028.

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