The Mauna Kea Observatories Near‐Infrared Filter Set. I. Defining Optimal 1–5 Micron Bandpasses

By D. Simons, A. Tokunaga. 2001

194 citations recorded by the source corpus.

A new Mauna Kea Observatories near‐infrared (MKO‐NIR) filter set is described, including techniques and considerations given to designing a new set of bandpasses that are useful at both mid‐ and high‐altitude sites. These filters offer improved photometric linearity and in many cases reduced background, as well as preserving good throughput within the JHKLM atmospheric windows. MKO‐NIR filters have already been deployed within a number of instruments around the world as part of a filter consortium purchase to reduce the unit cost of filters. Through this effort we hope to establish, for the first time, a single standard set of infrared filters at as many observatories as possible.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/fe4dabe32fbbd5a73d61ba8fb959c514907a9d98

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Michael C. Liu
2. A. Burgasser
3. M. Marley
4. J. D. Kirkpatrick
5. T. Dupuy
6. Kelle Cruz
7. K. Luhman
8. Jon Fortney

In Computational Mechanics

1. Michael C. Liu
2. A. Burgasser
3. J. D. Kirkpatrick
4. T. Dupuy
5. M. Marley
6. Kelle Cruz
7. D. Saumon
8. M. Cushing

Citations in the corpus

• JHK observations of faint standard stars in the Mauna Kea Observatories near‐infrared photometric system (2006, background): “For further discussion, see Simons & Tokunaga (2002) and Tokunaga et al. (2002).”
• A Unified Near-Infrared Spectral Classification Scheme for T Dwarfs (2005, methodology): “…(T7): Identified by B02 and selected as the T7 standard in that scheme (Knapp 4Near infrared photometry reported in the text are generally based on the Mauna Kea Observatory (MKO) filter system (Simons & Tokunaga 2002; Tokunaga, Simons & Vacca 2002), unless otherwise specified (e.g., Table 14).”
• Clouds and Chemistry: Ultracool Dwarf Atmospheric Properties from Optical and Infrared Colors (2001, methodology): “For J and K colors we use the Mauna Kea Observatory (MKO) near-infrared system (Simons & Tokunaga 2002; Tokunaga, Simons, & Vacca 2002), and for SDSS we use the i0 and z0 filter functions and the AB magnitude system (Fukugita et al. 1996).”
• A STUDY OF THE DIVERSE T DWARF POPULATION REVEALED BY WISE (2013, methodology): “We have separated the 2MASS and Mauna Kea Observatories Near-Infrared (MKO; Simons & Tokunaga 2002; Tokunaga et al. 2002) systems since care should be taken when making comparisons between the two filter systems whose different bandpasses produce slightly different magnitudes.”
• Subtle Signatures of Multiplicity in Late-type Dwarf Spectra: The Unresolved M8.5 + T5 Binary 2MASS J03202839–0446358 (2008, methodology): “2MASS J0320−0446 was observed in this setup us- 10 Mauna Kea Observatory (MKO) photometric system; Simons & Tokunaga (2002); Tokunaga, Simons & Vacca (2002). ing a two-point dither pattern, with five 50-second integrations at each dither position.”
• Hubble Space Telescope NICMOS Observations of T Dwarfs: Brown Dwarf Multiplicity and New Probes of the L/T Transition (2006, methodology): “To put our photometry into context with existing data, we compared F110W and F170M magnitudes to J and H photometry, respectively, on the 2MASS and Mauna Kea Observatory (MKO; Simons & Tokunaga (2002); Tokunaga, Simons & Vacca (2002)) systems.”
• BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, background): “In Figure 13, we show a MJ versus J −K CMD in the Mauna Kea Observatories NIR filter system (MKO; Simons & Tokunaga 2002) for low-gravity and field dwarfs.”
• SpeX SPECTROSCOPY OF UNRESOLVED VERY LOW MASS BINARIES. I. IDENTIFICATION OF 17 CANDIDATE BINARIES STRADDLING THE L DWARF/T DWARF TRANSITION (2009, methodology): “5Mauna Kea Observatory filter system; see Tokunaga et al. (2002) and Simons & Tokunaga (2002).”
• Planet Hunters IX. KIC 8462852-where's the flux? (2015, methodology): “We used the facility IR camera NIRC2 and the J (1.25 µm), H (1.64 µm), and K (2.20 µm) filters from the Mauna Kea Observatories (MKO) filter consortium (Simons & Tokunaga 2002; Tokunaga, Simons & Vacca 2002).”
• Seventy-One New L and T Dwarfs from the Sloan Digital Sky Survey (2006, methodology): “Candidates surviving our initial photometric screening were then imaged through the Mauna Kea Observatory (MKO) J, H, and K bands (Simons & Tokunaga 2002; Tokunaga et al. 2002) using the UKIRT Fast-Track Imager (UFTI; Roche et al. 2003) or the NASA Infrared Telescope Facility (IRTF) imager…”
• THE Pan-STARRS1 PHOTOMETRIC SYSTEM (2012, background): “Note that other definitions of JHKs such as the “MKO-NIR” set described by Simons & Tokunaga (2002) or the UKIDSS survey differ somewhat.”
• NEAR-INFRARED SPECTROSCOPY OF THE EXTRASOLAR PLANET HR 8799 b (2010, methodology): “…(e.g., Equation (5) of Tokunaga & Vacca 2005) from each prism spectrum of the field dwarf sample using the J, H, and KS bands from the Mauna Kea Observatory (MKO) filter consortium (Simons & Tokunaga 2002; Tokunaga et al. 2002) and the zero point Vega flux densities from Tokunaga & Vacca (2005).”
• The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours (2006, unknown): “2 THE WFCAM ZY JHK PHOTOMETRIC SYSTEM Extensive work on the specification of optimal passbands in the near-infrared has led to the development of the Mauna Kea Observatories (MKO) near-infrared filter set that includes JHKL′M ′ bandpasses (Simons & Tokunaga 2002; Tokunaga, Simons & Vacca 2002).”
• THE 0.8–14.5 μm SPECTRA OF MID-L TO MID-T DWARFS: DIAGNOSTICS OF EFFECTIVE TEMPERATURE, GRAIN SEDIMENTATION, GAS TRANSPORT, AND SURFACE GRAVITY (2009, unknown): “These color designations are based on the observed correlations between color and spectral type presented in Figure 3 of Knapp et al. (2004), which are defined on the Mauna Kea Observatory (MKO) photometric system (Simons & Tokunaga 2002; Tokunaga et al. 2002).”
• Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, methodology): “Imaging was performed through Mauna Kea Observatory (MKO) J , H , andK filters (Simons & Tokunaga 2002; Tokunaga et al. 2002; Tokunaga & Vacca 2005).”
• FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME (2015, methodology): “Additional magnitudes came from the Looper Near-Infrared Survey of the Southern Sky (DENIS; Epchtein et al. 1997) and the literature using the Mauna Kea Observatory Near-Infrared (Simons & Tokunaga 2002; Tokunaga et al. 2002), Spitzer Space Telescope IRAC and Johnson-Cousins V(RI)C filter sets.”
• THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, methodology): “We used the wide camera mode of NIRC2, with a pixel scale of 39.686 ± 0.008mas pixel−1 (H. Fu, priv. comm.), and standard Mauna Kea Observatories (MKO) filters J , H, and K (Simons & Tokunaga 2002; Tokunaga et al. 2002) in addition to the NIRC2 Y -band filter (see Appendix of Liu et al. 2012).”