JHK standard stars for large telescopes: the UKIRT Fundamental and Extended lists

By T. Hawarden, S. Leggett, M. Letawsky, D. Ballantyne, M. Casali. 2001

243 citations recorded by the source corpus.

We present high-precision JHK photometry with the 3.8-m UK Infrared Telescope (UKIRT) of 82 standard stars, 28 from the widely used preliminary list known as the ‘UKIRT Faint Standards’, referred to here as the Fundamental List, and 54 additional stars referred to as the Extended List. The stars have 9:4 , K , 15:0 and all or most should be readily observable with imaging array detectors in normal operating modes on telescopes of up to 10-m aperture. Many are accessible from the southern hemisphere. Arcsec-accuracy positions (J2000, epoch ,1998) are given, together with optical photometry and spectral types from the literature, where available, or inferred from the J 2 K colour. K-band finding charts are provided for stars with proper motions exceeding 0.3arcsecyr 21 . We discuss some pitfalls in the construction of flat-fields for array imagers and a method to avoid them. On 30 nights between late 1994 and early 1998 the stars from the Fundamental List, which were used as standards for thewhole programme, were observed on an average of 10 nights each, and those from the Extended List on an average of six nights. The average internal standard error of the mean results for the K magnitudes is 0.005mag; for the J 2 H colours it is 0.003mag for the Fundamental List stars and 0.005mag for those of the Extended List; for H 2 K the average is 0.004mag. The results are on the natural system of the IRCAM3 imager, which used a 256 � 256 InSb detector array with ‘standard’ JHK filters, behind gold-coated fore-optics and a gold- or silver-dielectric coated dichroic. We give colour transformations on to the CIT, Arcetri and LCO/Palomar NICMOS systems, and preliminary transformations on to the system defined by the new Mauna Kea Observatory near-infrared filter set.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/29a680777cbcfac549891e8765574260b8e76c7e

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Citations in the corpus

Colors and Spectra of Kuiper Belt Objects (2001, methodology): “Spectral calibration of the images was obtained from nearby stars on the UKIRT Faint Standards list (Hawarden et al. 2001).”
“The Mauna Kea Observatories Near‐Infrared Filter Set. III. Isophotal Wavelengths and Absolute Calibration” (PASP, 117, 421 [2005]) (2005, methodology): “The UKIRT photometric system (Hawarden et al. 2001; Leggett et al. 2003) is based on the Elias et al. (1982) standard stars, so it follows the convention that the magnitude of Vega is 0.0 mag.”
A Wide-Field Hubble Space Telescope Study of the Cluster Cl 0024+1654 at z=0.4. II. The Cluster Mass Distribution (2003, methodology): “Science observations were interspersed with observations of standards from the UKIRT list (Hawarden et al. 2001).”
Seventy-One New L and T Dwarfs from the Sloan Digital Sky Survey (2006, methodology): “United Kingdom Infrared Telescope (UKIRT) Faint Standards (Hawarden et al. 2001) were used to calibrate the data.”
Near-Infrared Photometry and Spectroscopy of L and T Dwarfs: The Effects of Temperature, Clouds, and Gravity (2004, methodology): “The JHK data were calibrated using the UKIRT Faint Standards of Hawarden et al. (2001),12 translated onto the MKO-NIR system using as yet unpublished observations carried out at UKIRT as part of an observatory project to provide calibrators in the MKO-NIR system.”
Low-Luminosity Companions to White Dwarfs (2005, methodology): “Optical and near-infrared standard stars were taken from Landolt (1983), Hunt et al. (1998), and Hawarden et al. (2001).”
The Mauna Kea Observatories Near‐Infrared Filter Set. I. Defining Optimal 1–5 Micron Bandpasses (2001, background): “…Observatory (ESO; van der Bliek et al. 1996), Las Companas Observatory (LCO; Persson et al. 1998), United Kingdom Infrared Telescope (UKIRT; Hawarden et al. 2001), Mount Stromlo and Siding Spring Observatory (MSSSO; McGregor 1994), and South Africa Astronomical Observatory (SAAO; Carter…”
The UKIRT wide field camera ZYJHK photometric system: calibration from 2MASS (2008, methodology): “For the H-band, an additional 3 per cent offset is required to bring the WFCAM photometry onto the same system as the UKIRT faint standards (as originally published by Hawarden et al. 2001).”
The Rest-Frame Optical Spectra of SCUBA Galaxies (2004, methodology): “To calibrate our data, we observed UKIRT faint photometric standards (Hawarden et al. 2001).”
Characterization of M, L, and T Dwarfs in the Sloan Digital Sky Survey (2002, methodology): “Some of the published near-infrared photometry was obtained with the Mauna Kea Observatory (MKO) system at UKIRT (Hawarden et al. 2001; Leggett et al. 2002).”
The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours (2006, methodology): “Since in the system of the UKIRT Faint Standards (Hawarden et al. 2001), that will be used to calibrate UKIDSS, Vega has zero magnitude in J , H , and K, whereas in the Johnson UBV system Vega has non–zero magnitudes, care must be taken in defining zero-points.”
JHK observations of faint standard stars in the Mauna Kea Observatories near‐infrared photometric system (2006, methodology): “The initial standard star catalogue consisted of UKIRT Faint Standard values transformed to the MKO system using the preliminary colour terms given in Hawarden et al. (2001).”
A Highly Complete Spectroscopic Survey of the GOODS-N Field (2008, methodology): “The MOIRCS images were calibrated by observing various UKIRT Faint Standards (Hawarden et al. 2001) at least every half night on each detector.”
Preliminary Parallaxes of 40 L and T Dwarfs from the US Naval Observatory Infrared Astrometry Program (2004, methodology): “…previously published USNO photometry (D02) which is on the CIT system (Guetter et al. 2003), UKIRT photometry for four objects (Leggett et al. 2000) transformed to the CIT system by the relations of Hawarden et al. (2001), and the small amount of new USNO CIT system photometry presented in Table 5.”
THE TAURUS SPITZER SURVEY: NEW CANDIDATE TAURUS MEMBERS SELECTED USING SENSITIVE MID-INFRARED PHOTOMETRY (2009, background): “042350.1+264006=FS 116: appears in Hawarden et al. (2001) as a UKIRT JHK standard.”
Spiral Structure in the Circumstellar Disk around AB Aurigae (2004, methodology): “FS 111 was observed immediately before AB Aur and was used as a photometric calibrator (Hawarden et al. 2001).”
The UKIRT Infrared Deep Sky Survey (UKIDSS) (2006, methodology): “Tests against observations of UKIRT faint standards (Hawarden et al. 2001) indicates that this procedure gives us a JHK photometric system accurate to 2%, which is the survey design requirement.”
Infrared Photometry of Late-M, L, and T Dwarfs (2001, methodology): “…the previous ““ UKIRT ÏÏ system Ðlters ; transformations between the UKIRT JHK system and the MKO-NIR system for stars as cool as L dwarfs are given by Hawarden et al. (2001).15 These transformations cannot be applied to the colors of T dwarfs because of their very structured Ñux distributions…”