The Mauna Kea Observatories Near‐Infrared Filter Set. II. Specifications for a New JHKL′ M′ Filter Set for Infrared Astronomy

By A. Tokunaga, D. Simons, W. Vacca. 2001

362 citations recorded by the source corpus.

We present a description of a new 1–5 μm filter set similar to the long‐used JHKLM filter set derived from that of Johnson. The new Mauna Kea Observatories Near‐Infrared filter set is designed to reduce background noise, improve photometric transformations from observatory to observatory, provide greater accuracy in extrapolating to zero air mass, and reduce the color dependence in the extinction coefficient in photometric reductions. We have also taken into account the requirements of adaptive optics in setting the flatness specification of the filters. A complete technical description is presented to facilitate the production of similar filters in the future.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/94515e1ef0b49784c2663aae0a40213eb98ba38c

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In Astronomy and Astrophysics

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

In Instrumentation

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

Citations in the corpus

• “The Mauna Kea Observatories Near‐Infrared Filter Set. III. Isophotal Wavelengths and Absolute Calibration” (PASP, 117, 421 [2005]) (2005, methodology): “The measured filter response curves2 given by Tokunaga et al. (2002) were used for R(λ) (see their Fig.”
• Interstellar Extinction Law in the J, H, and Ks Bands toward the Galactic Center (2006, methodology): “The IRSF/SIRIUS system is similar to the MKO system (Tokunaga et al. 2002), and the effective wavelengths following equation (A3) of Tokunaga & Vacca (2005) are calculated for a typical bulge RC star when it suffers extinction of AKs ∼ 0.4−1.6 (the range of extinction in Fig.”
• SN 2003du: 480 days in the life of a normal type Ia supernova (2007, methodology): “The two telescopes use identicalJ andH filters, but the TNG uses aK′ while the NOT has aKs filter (Tokunaga et al., 2002).”
• FURTHER DEFINING SPECTRAL TYPE “Y” AND EXPLORING THE LOW-MASS END OF THE FIELD BROWN DWARF MASS FUNCTION (2012, methodology): “Our observation of WISE 2220−3628 used only the J filter, which is on the MKO-NIR system (Tokunaga et al. 2002).”
• An Infrared Spectroscopic Sequence of M, L, and T Dwarfs (2004, background): “This is not unexpected since the spectra are relatively featureless from 3.42 to 4.12 m, the wavelengths at which the MKO-NIR L0-band filter transmission is 50% of the peak (Tokunaga et al. 2002).”
• STELLAR POPULATIONS OF Lyα EMITTERS AT z ∼ 6–7: CONSTRAINTS ON THE ESCAPE FRACTION OF IONIZING PHOTONS FROM GALAXY BUILDING BLOCKS (2010, background): “For the z = 5.7 LAE, we set (m1,m2) = (mcon,mJ) and obtain β = −2.9 ± 1.0, where mcon is the continuum magnitude at 8303 Å (see Table 1) and λJc = 12500 Å (Tokunaga et al. 2002).”
• 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).”
• THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS (2009, methodology): “The Z and Y bands are custom filters designed for the UKIRT Infrared Deep Sky Survey (UKIDSS; Lawrence et al. 2007) centered at ∼0.88 and ∼1.03 µm while the JHK bands were constructed to the specifications of the Mauna Kea Observatories Near-Infrared (MKO-NIR) filter set (Tokunaga et al. 2002).”
• MASSES, RADII, AND CLOUD PROPERTIES OF THE HR 8799 PLANETS (2012, methodology): “The filter is the L′ filter in the MKO-NIR system, so we used the filter transmission profile from Tokunaga et al. (2002).”
• Binaries and the L Dwarf/T Dwarf Transition (2006, methodology): “8 Mauna Kea Observatory system; Simons & Tokunaga (2002); Tokunaga et al. (2002). derived by fitting an eighth-order polynomial toMK data 9 based on photometry (Geballe et al. 2002; Leggett et al. 2002; Knapp et al. 2004) and parallax data (Dahn et al. 2002; Tinney et al. 2003; Vrba et al. 2004)…”
• Seventy-One New L and T Dwarfs from the Sloan Digital Sky Survey (2006, methodology): “…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 /spectrometer…”
• The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs (2020, methodology): “The two filter systems employed by these nearinfrared surveys are those of 2MASS15 and the Maunakea Observatories (MKO; Tokunaga et al. 2002).”