JHK observations of faint standard stars in the Mauna Kea Observatories near‐infrared photometric system

By S. Leggett, M. Currie, W. Varricatt, T. Hawarden, A. Adamson, J. Buckle, T. Carroll, J. Davies, C. Davis, T. Kerr and 3 more. 2006

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JHK photometry in the Mauna Kea Observatories (MKO) near-infrared system is presented for 115 stars. Of these stars, 79 are United Kingdom Infrared Telescope (UKIRT) standards from Hawarden et al., and 42 are Las Campanas Observatory (LCO, or NICMOS) standards from Persson et al. The average brightness of the sample in all three bandpasses is 11.5 mag, with a range between 10 and 15. The average number of nights each star was observed is 4, and the average of the internal error of the final results is 0.011 mag. These JHK data agree with those reported by other groups to 0.02 mag, for stars in common, which is consistent with the uncertainties. The measurements are used to derive colour transformations between the MKO JHK photometric system and the UKIRT, LCO and Two Micron All-Sky Survey (2MASS) systems. The 2MASS–MKO data scatter by 0.05 mag for redder stars, which is consistent with a dependence on stellar luminosity: the 2MASS J bandpass includes H2O features in dwarfs and the MKO K bandpass includes CO features in giants. We stress that colour transformations derived for stars whose spectra contain only weak features cannot give accurate transformations for objects with strong absorption features within one, but not both, of the filter bandpasses. We find evidence of systematic effects at the 0.02 mag level in the photometry of stars with J < 11 and H, K < 10.5 presented here and in Hawarden et al. This is due to an underestimate of the linearity correction for stars observed with the shortest exposure times; very accurate photometry of stars approaching the saturation limits of infrared detectors which are operated in double-read mode is difficult to obtain. There are indications that four stars in the sample, GSPC S705-D, FS 116 (B216-b7), FS 144 (Ser-EC84) and FS 32 (Feige 108), may be variable. There are 84 stars in the sample presented here that have 11 < J < 15 and 10.5 < H, K < 15, are not suspected to be variable, and have magnitudes with an estimated error ≤0.027 mag; 79 of these have an error of ≤0.020 mag. These represent the first published high-accuracy JHK stellar photometry in the MKO near-infrared photometric system; we recommend these objects be employed as primary standards for that system.

Subfields: Astronomy and Astrophysics, Computational Mechanics

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Citations in the corpus

• THE CARNEGIE SUPERNOVA PROJECT: FIRST PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE (2009, methodology): “Table 6 contains the results, together with the values given by Leggett et al. (2006), – 15 – transformed according to their prescription, from their Mauna Kea Observatory (MKO) system to the LCO system.”
• LARGE-AMPLITUDE VARIATIONS OF AN L/T TRANSITION BROWN DWARF: MULTI-WAVELENGTH OBSERVATIONS OF PATCHY, HIGH-CONTRAST CLOUD FEATURES (2012, methodology): “Because we do not have enough reference stars to derive robust color-dependent corrections between our MKO J filter and 2MASS J filter, we first converted 2MASS J magnitudes of the reference stars to MKO magnitudes according to the color-dependent transformations provided by Leggett et al. (2006).”
• The UKIRT wide field camera ZYJHK photometric system: calibration from 2MASS (2008, methodology): “…of a larger sample of observations and more-accurate photometry, we conclude that the WFCAM photometric system is a Vega system (to within 2 per cent) and is in agreement with all three of the Hawarden et al. (2001), Cohen et al. (2003) and Leggett et al. (2006) systems to within 2 per cent.”
• NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES (2012, methodology): “The UKIRT faint standards FS 133 and 136 were used for photometric calibration;J and H were taken from Leggett et al. (2006), andY from the UKIRT online catalog (http://www.jach.hawaii.edu/UKIRT/astronomy/calib/phot cal/fs ZY MKO wfcam.dat).”
• Type Ia Supernovae Are Good Standard Candles in the Near Infrared: Evidence from PAIRITEL (2007, methodology): “Cohen et al. (2003) describe the 2MASS JHKs filter system in detail and Leggett et al. (2006) provide color transformations to put observations with the 2MASS filter system on other widely used photometric systems.”
• A comparison of chemistry and dust cloud formation in ultracool dwarf model atmospheres (2008, methodology): “Comparisons of the mid-IR colours of L dwarfs to models that include chemical mixing (Leggett et al. 2006) suggest Keddy ∼ 104 cm2 s−1.”
• Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, methodology): “These data were calibrated with images of standard stars for the MKO system (Leggett et al. 2006).”
• PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, methodology): “8+121622 B based on photometry of the primary, which was first converted from the 2MASS to MKO filter system for the J and H filters with the relations from Leggett et al. (2006).”