THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS

By J. Rayner, M. Cushing, W. Vacca. 2009

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We present a 0.8–5 μm spectral library of 210 cool stars observed at a resolving power of R ≡ λ/Δλ ∼ 2000 with the medium-resolution infrared spectrograph, SpeX, at the 3.0 m NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii. The stars have well-established MK spectral classifications and are mostly restricted to near-solar metallicities. The sample not only contains the F, G, K, and M spectral types with luminosity classes between I and V, but also includes some AGB, carbon, and S stars. In contrast to some other spectral libraries, the continuum shape of the spectra is measured and preserved in the data reduction process. The spectra are absolutely flux calibrated using the Two Micron All Sky Survey photometry. Potential uses of the library include studying the physics of cool stars, classifying and studying embedded young clusters and optically obscured regions of the Galaxy, evolutionary population synthesis to study unresolved stellar populations in optically obscured regions of galaxies and synthetic photometry. The library is available in digital form from the IRTF Web site.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/48a08660d566f0802d70e0850baeedfa09130210

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Citations in the corpus

COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, methodology): “We make use of two separate libraries, the MILES library, which covers the wavelength range 0.35µm< λ < 0.74µm (Sánchez-Blázquez et al. 2006), and the IRTF library of cool stars, which covers the wavelength range 0.81µm< λ < 2.4µm (Cushing et al. 2005; Rayner et al. 2009).”
FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME (2015, neutral): “…(5) Kirkpatrick et al. (2000), (6) Burgasser et al. (2007), (7) Houck & Roellig (2004a), (8) J. Faherty et al. (2015, in preparation), (9) Rayner et al. (2009), (10) Cushing et al. (2005b), (11) Cushing et al. (2006), (12) Cushing et al. (2008a), (13) Liebert et al. (1999), (14) Cruz et…”
THE STELLAR INITIAL MASS FUNCTION IN EARLY-TYPE GALAXIES FROM ABSORPTION LINE SPECTROSCOPY. II. RESULTS (2012, methodology): “The core of the model is based on two empirical stellar libraries: MILES (Sánchez-Blázquez et al. 2006) in the optical and IRTF (Cushing et al. 2005; Rayner et al. 2009) in the near-IR, at solar metallicity.”
EARLY-TYPE GALAXY ARCHEOLOGY: AGES, ABUNDANCE RATIOS, AND EFFECTIVE TEMPERATURES FROM FULL-SPECTRUM FITTING (2013, methodology): “We make use of two separate libraries, the MILES library, which covers the wavelength range 0.35µm < λ < 0.74µm (Sánchez-Blázquez et al. 2006), and the IRTF library of cool stars, which covers the wavelength range 0.81µm < λ < 2.4µm (Cushing et al. 2005; Rayner et al. 2009).”
SPITZER OBSERVATIONS CONFIRM AND RESCUE THE HABITABLE-ZONE SUPER-EARTH K2-18b FOR FUTURE CHARACTERIZATION (2016, result): “This type is consistent with the derived stellar parameters and a visual comparison to late-type standards from the IRTF Spectral Library (Figure 5, Rayner et al. (2009); Cushing et al. (2005)).”
HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, methodology): “Rayner et al. (2009) noted that using the 0.3″ slit can lead to errors in the slope of the spectrum by 1%–3% due to changes in seeing, guiding, and differential atmospheric refraction between target and standard star observation.”
CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER (2011, background): “The templates are taken from the SpeX library (Cushing et al. 2005; Rayner et al. 2009).”
PROSPECTING IN LATE-TYPE DWARFS: A CALIBRATION OF INFRARED AND VISIBLE SPECTROSCOPIC METALLICITIES OF LATE K AND M DWARFS SPANNING 1.5 dex (2012, methodology): “The most likely explanation for this is a small difference in the RV templates used for our SpeX and SNIFS data, taken from Rayner et al. (2009) and Bochanski et al. (2007) respectively.”
LOW-MASS TERTIARY COMPANIONS TO SPECTROSCOPIC BINARIES. I. COMMON PROPER MOTION SURVEY FOR WIDE COMPANIONS USING 2MASS (2009, methodology): “The final reduced and calibrated spectra are then compared to spectral standards from the IRTF Spectral Library (Cushing et al. 2005; Rayner et al. 2009), and are displayed in Figures 4 - 9.”
NEAR-INFRARED METALLICITIES, RADIAL VELOCITIES, AND SPECTRAL TYPES FOR 447 NEARBY M DWARFS (2013, methodology): “IRTF spectral standards We initially used the M dwarfs in the IRTF spectral library (Rayner et al. 2009) as spectral standards, using the KHM spectral standards except for our M0V (HD19305), M3V (AD Leo/Gl 388) and M6V (CN Leo/Gl 406) spectral standards.”
THE NIRSPEC ULTRACOOL DWARF RADIAL VELOCITY SURVEY (2010, background): “With their cool temperatures, the atmospheres of UCDs contain a wide array of molecules, including TiO, VO, and CO, as well as dust particles, leading to complex NIR spectra (Rayner et al. 2009).”
UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS (2010, methodology): “The spectra of corresponding template stars were obtained from the IRTF Spectral Library (Cushing et al. 2005; Rayner et al. 2009)13.”
SPECTRO-THERMOMETRY OF M DWARFS AND THEIR CANDIDATE PLANETS: TOO HOT, TOO COOL, OR JUST RIGHT? (2013, methodology): “Following the technique of Rayner et al. (2009), for each photometric point we calculate the ratio of the photometric flux to the equivalent flux synthesized from the spectra, Ci; Ci = fzp,i × 10 −0.4mi ( ∫ λ Fλ × Sλ,idλ) , (4) where fzp is the band zero point, mi is the apparent magnitude, and…”
CHARACTERIZING THE COOL KOIs. VII. REFINED PHYSICAL PROPERTIES OF THE TRANSITING BROWN DWARF LHS 6343 C (2014, methodology): “To remove the system’s absolute radial velocity of -46 km s−1, we cross-correlated the spectrum with data from the IRTF spectral library (Cushing et al. 2005; Rayner et al. 2009), then applied an offset to the wavelength solution corresponding to the peak of the cross-correlation function.”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, background): “Of the stellar spectra observed with IRTF (Cushing et al. 2005; Rayner et al. 2009), the M8III red giant WX Piscium (IRAS 01037+1219; Ulrich et al. 1966; Decin et al. 2007) comes closest to matching the observed colors of MACS0647-JD.”
DISCOVERY OF SMALL-SCALE SPIRAL STRUCTURES IN THE DISK OF SAO 206462 (HD 135344B): IMPLICATIONS FOR THE PHYSICAL STATE OF THE DISK FROM SPIRAL DENSITY WAVE THEORY (2012, methodology): “Figure 1 also displays spectra obtained with the SpeX spectrograph (Rayner et al. 2009) on NASA’s Infrared Tele- scope Facility (IRTF).”
WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. I. THE TRANSIT (2014, methodology): “We calibrated the wavelength as a function of detector column by comparing the (unbinned) WFC3 spectrum of HD 189733 to the spectrum of a K1 V comparison star (Rayner et al. 2009).3.”
Systematic variation of the stellar initial mass function with velocity dispersion in early-type galaxies (2012, methodology): “For instance, in the region around the Na8190 feature, the MIUSCAT models use stellar spectra from the Indo-US library (Valdes et al. 2004), whereas the models of Conroy & van Dokkum (2012) use the IRTF library (Cushing et al. 2005; Rayner et al. 2009).”
AN EMPIRICAL CALIBRATION TO ESTIMATE COOL DWARF FUNDAMENTAL PARAMETERS FROM H-BAND SPECTRA (2014, methodology): “We supplement this sample with the five remaining: spectra for Gl 581 and Gl 892 are available in the IRTF spectral library (Cushing et al. 2005; Rayner et al. 2009)3 and we include spectra of Gl 876, Gl 649, and Gl 176 that were observed by Mann et al. (2013b).”