SpeX: A Medium‐Resolution 0.8–5.5 Micron Spectrograph and Imager for the NASA Infrared Telescope Facility

Rayner, John; Toomey, Douglas W.; Onaka, Peter M.; Denault, Anthony J.; Stahlberger, Werner E.; Vacca, William D.; Cushing, M. C.; Wang, S.

doi:10.1086/367745

Cited by 1,140 publications

(689 citation statements)

References 9 publications

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“…These effects were previously reported by Hardersen et al (2006). The instrumental approach of Vacca et al (2004) and Rayner et al (2003) allows to establish a clear relation between the dynamical regime of the NIR detector and its non-linear response. As a consequence, the spectrograph users are strongly advised to operate it in the lower 50% of the usable detector well depth as long as this region has a quasi-linear response (counts ≤4000 DN).…”

Section: Spectroscopysupporting

confidence: 70%

Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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Aims. In the framework of the ground-based science campaign dedicated to the encounter with the Rosetta spacecraft, the mineralogy of the asteroid (21) Lutetia was investigated. Methods. Near-infrared (NIR) spectra of the asteroid in the 0.8−2.5 µm spectral range were obtained with SpeX/IRTF in remote observing mode from Meudon, France in March and April 2006. We analysed these data together with previously acquired spectra -March 2003, August 2004. I-band relative photometric data obtained on 20 January 2006 using the 105 cm telescope from Pic du Midi, France has been used to build the ephemeris for physical observations. A χ 2 test using meteorite spectra from the RELAB database was performed in order to find the best fit of complete visible + infrared (VNIR) spectra of Lutetia. Results. The new spectra reveal no absorption features. We find a clear spectral variation (slope), and a good correspondence between spectral variations and rotational phase. Two of the most different spectra correspond to two opposite sides of the asteroid (sub-Earth longitude difference around 180 • ). For the neutral spectra a carbonaceous chondrite spectrum yields the best fit, while for those with a slightly positive slope the enstatitic chondrite spectra are the best analog. Based on the chosen subset of the meteorite samples, our analysis suggests a primitive, chondritic nature for (21) Lutetia. Differences in spectra are interpreted in terms of the coexistence of several lithologies on the surface where the aqueous alteration played an important role.

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Section: Spectroscopysupporting

confidence: 70%

Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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“…NIR spectra were obtained with the SpeX instrument (Rayner et al, 2003), equipped with a Raytheon Aladdin 3 1024×1024 InSb array. Spectral data were acquired using Spex in its low resolution (R∼150) prism mode with a 0.8" slit width.…”

Section: Near-infrared Spectramentioning

confidence: 99%

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Sanchez

Michelsen

Reddy

et al. 2013

Icarus

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In the past, constraining the surface composition of near-Earth asteroids (NEAs) has been difficult due to the lack of high quality near-IR spectral data (0.7-2.5 µm) that contain mineralogically diagnostic absorption bands. Here we present visible (∼ 0.43-0.95 µm) and nearinfrared (∼ 0.7-2.5 µm) spectra of nine NEAs and five Mars-crossing asteroids (MCs). The YT1) as a V-type was made on the basis of its near-infrared spectrum since no visible spectrum is available for this asteroid. A mineralogical analysis was performed on six of the asteroids (those for which near-IR spectra were obtained or previously available). We found that three asteroids (241662 (2000 KO44), 19764 (2000 NF5), 138404 (2000) have mafic silicate compositions consistent with ordinary chondrites, while three others (4055 Magellan, 164121 (2003 YT1), 5407 (1992 AX)) are pyroxene-dominated basaltic achondrite assemblages. In the case of 5407 (1992 AX) we found that its basaltic surface composition contrasts its taxonomic classification as a S-type.

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“…An analogous grid was constructed that is composed of field (1-5 Gyr) template spectra of G and K stars (Rayner et al 2009) retrieved from the IRTF Spectral Library 1 , together with M and L dwarf optical standards (Burgasser et al 2004;Burgasser & McElwain 2006;Burgasser et al 2008) retrieved from the SpeX Prism Spectral Libraries 2 , all taken with the SpeX spectrograph (Rayner et al 2003) mounted on the 3 m NASA Infrared Telescope Facility. These are reddened in the same way as described for the grid of young objects, and the grid is smoothed by calculating intermediate spectral types from the averages of the templates.…”

Section: Empirical Grid Of Template Spectramentioning

confidence: 99%

Spectroscopy of new brown dwarf members ofρ Ophiuchi and an updated initial mass function

Oliveira¹,

Moraux²,

Bouvier³

et al. 2012

A&A

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Aims. To investigate the universality hypothesis of the initial mass function in the substellar regime, the population of the ρ Ophiuchi molecular cloud is analysed by including a new sample of low-mass spectroscopically confirmed members. To that end, we have conducted a large spectroscopic follow-up of young substellar candidates uncovered in our previous photometric survey. Methods. The spectral types and extinction were derived for a newly found population of substellar objects, and its masses estimated by comparison to evolutionary models. A thoroughly literature search was conducted to provide an up-to-date census of the cluster, which was then used to derive the luminosity and mass functions, as well as the ratio of brown dwarfs to stars in the cluster. These results were then compared to other young clusters. Results. It is shown that the study of the substellar population of the ρ Ophiuchi molecular cloud is hampered only by the high extinction in the cluster ruling out an apparent paucity of brown dwarfs. The discovery of 16 new members of ρ Ophiuchi, 13 of them in the substellar regime, reveals the low-mass end of its population and shows the success of our photometric candidate selection with the WIRCam survey. The study of the brown dwarf population of the cluster reveals a high disk fraction of 76 +5 −8 %. Conclusions. Taking the characteristic peak mass of the derived mass function and the ratio of brown dwarfs to stars into account, we conclude that the mass function of ρ Ophiuchi is similar to other nearby young clusters.

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SpeX: A Medium‐Resolution 0.8–5.5 Micron Spectrograph and Imager for the NASA Infrared Telescope Facility

Cited by 1,140 publications

References 9 publications

Near infra-red spectroscopy of the asteroid 21 Lutetia

Near infra-red spectroscopy of the asteroid 21 Lutetia

Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids

Spectroscopy of new brown dwarf members ofρ Ophiuchi and an updated initial mass function

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