The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours

By Paul Hewett, Stephen J. Warren, S. Leggett, S. I. F. Astronomy, Cambridge, I. College, London, Jac, Hawaii. 2006

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The UKIRT Infrared Deep Sky Survey is a set of v e surveys of complementary combinations of area, depth, and Galactic latitude, which began in 2005 May. The surveys use the UKIRT Wide Field Camera (WFCAM), which has a solid angle of 0.21deg 2 . Here we introduce and characterise the ZYJHK photometric system of the camera, which covers the wavelength range 0:83 2:37 m. We synthesise response functions for the v e passbands, and compute colours in the WFCAM, SDSS and 2MASS bands, for brown dwarfs, stars, galaxies and quasars of dieren t types. We provide a recipe for others to compute colours from their own spectra. Calculations are presented in the Vega system, and the computed osets to the AB system are provided, as well as colour equations between WFCAM lters and the SDSS and 2MASS passbands. We highlight the opportunities presented by the new Y lter at 0:97 1:07 m for surveys for hypothetical Y dwarfs (brown dwarfs cooler than T), and for quasars of very{high redshift, z > 6:4.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/75758232cb1b08dc54402c0e7c3504aad6f38429

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Citations in the corpus

THE RED MSX SOURCE SURVEY: THE MASSIVE YOUNG STELLAR POPULATION OF OUR GALAXY (2013, methodology): “The photometric system of UKIDSS is described in Hewett et al (2006), and the calibration is described in Hodgkin et al. (2009).”
Empirical determination of the shape of dust attenuation curves in star-forming galaxies (2011, methodology): “UKIDSS uses the UKIRT Wide Field Camera (WFCAM, Casali et al. 2007), the photometric system is described in Hewett et al. (2006), the calibraton in Hodgkin et al. (2009) and the science archive in Hambly et al. (2008).”
THE z = 5 QUASAR LUMINOSITY FUNCTION FROM SDSS STRIPE 82 (2012, methodology): “UKIDSS magnitudes are Vega-based, but we convert all UKIDSS magnitudes to AB using the values given in Hewett et al. (2006).”
Analytical approximations of K-corrections in optical and near-infrared bands (2010, methodology): “…and computed the corresponding 3 arcsec aperture magnitudes for UKIDSS objects by linearly interpolating between the values provided for three apertures (2.0, 2.8, and 5.7 arcsec) applying zero-point corrections (Hewett et al. 2006) for converting UKIDSS magnitudes from the Vega into the AB system.”
THE PAN-STARRS1 DISTANT z > 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE (2016, methodology): “UKIDSS and UHS use the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007) and a photometric system described in Hewett et al. (2006).”
THE CANADA–FRANCE HIGH-z QUASAR SURVEY: NINE NEW QUASARS AND THE LUMINOSITY FUNCTION AT REDSHIFT 6 (2009, background): “A primary goal of LAS is to find z = 7 quasars (Hewett et al. 2006), and it so far has found two at z ≈ 6 (Venemans et al. 2007; Mortlock et al. 2009).”
The Absolute Magnitude of the Sun in Several Filters (2018, neutral): “…(2015); 2: Cohen et al. (2003); 3: Gunn et al. (1998); 4: NOAO (2015); 5: Tonry et al. (2012); 6: Gwyn (2012); 7: Nick Kaiser 2002, private communication; 8: Hewett et al. (2006); 9: https://github.com/lsst/throughputs/tree/master/baseline 10: Bessell & Murphy (2012); 11: Bessell & Brett (1988);…”
A comparison of chemistry and dust cloud formation in ultracool dwarf model atmospheres (2008, methodology): “We compare our synthetic Y − J and J − H UKRIT colours to Hewett et al. (2006), and we reproduce the spectral class of our test case models better than for the near-IR colours (see Table 7).”
Resolved stellar mass maps of galaxies. I: method and implications for global mass estimates (2009, methodology): “The UKIDSS photometric system is described in Hewett et al. (2006), and the calibration is described in Hodgkin et al. (2009).”
THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION, (2012, neutral): “…(62) Henry & Kirkpatrick (1990); (63) Henry & McCarthy (1993); (64) Henry et al. (2002); (65) Henry et al. (2004); (66) Henry et al. (2006); (67) Hewett et al. (2006); (68) Huélamo et al. (2010); (69) Ireland et al. (2008); (70) Janson et al. (2011); (71) Jayawardhana et al. (2003); (72)…”
FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME (2015, neutral): “…et al. (2004), (4) Leggett et al. (2010), (5) Naud et al. (2014), (6) Leggett et al. (1998), (7) Chiu et al. (2006), (8) Leggett et al. (2000), (9) Hewett et al. (2006), (10) Leggett et al. (2002b), (11) Lawrence et al. (2007), (12) Currie et al. (2013), (13) Golimowski et al. (2004), (14)…”
New members in the upper scorpius association from the UKIRT infrared deep sky survey early data release (2006, methodology): “The ZY JHK photometric system of the instrument has been characterised by Hewett et al. (2006), who provide the total system response curves for each broad band, as well as colour equations to translate to 2MASS JHK (see also Section 6.4) and SDSS z, and synthetic colours of a wide variety of…”
3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, background): “The photometric sys- 27 http://www.naoj.org/Science/SubaruProject/SXDS/ 28 http://www.roe.ac.uk/~ciras/Scientific_ Research.html 29 http://surveys.roe.ac.uk/wsa/dr8plus_release. html tem is described in Hewett et al. (2006), and the calibration is described in Hodgkin et al. (2009).”
The UKIDSS galactic plane survey (2007, methodology): “Since the 2MASS J, H and Ks filters are slightly different from the WFCAM filters (see Hewett et al.2006), photometric transformations are used to correct the zero points.”
Scaling Relations of Spiral Galaxies (2007, background): “A study of scaling relations based on deeper IR survey data (e.g. UKIDSS; Hewett et al. 2006) should recover shallower slopes, comparable to those measured here for I-band data, for the infrared RL and RV relations.”
The UKIRT wide field camera ZYJHK photometric system: calibration from 2MASS (2008, methodology): “The spectrum for Vega is the same used by Hewett et al. (2006), originally from Bohlin & Gilliland (2004).”
SUBARU HIGH-z EXPLORATION OF LOW-LUMINOSITY QUASARS (SHELLQs). I. DISCOVERY OF 15 QUASARS AND BRIGHT GALAXIES AT 5.7 < z < 6.9 (2016, neutral): “Because the model spectra redshifted to z > 6 do not extend beyond the J-band, we take the J −H and H −K colors from Hewett et al. (2006).”