“The Mauna Kea Observatories Near‐Infrared Filter Set. III. Isophotal Wavelengths and Absolute Calibration” (PASP, 117, 421 [2005])

By A. Tokunaga, W. D. V. I. F. Astronomy, U. Hawaii, Sofiausra, N. R. Center. 2005

194 citations recorded by the source corpus.

ABSTRACT The isophotal wavelengths, flux densities, and AB magnitudes for Vega (α Lyr) are presented for the Mauna Kea Observatories near‐infrared filter set. We show that the near‐infrared absolute calibrations for Vega as determined by Cohen et al. and Megessier are consistent within the uncertainties, so that either absolute calibration can be used.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Accurate fundamental parameters for lower main‐sequence stars (2006, unknown): “Also, Tokunaga & Vacca (2005) have shown the Vega absolute calibration of Cohen et al. (1992a) and the model-independent measurements of Megessier (1995) to be identical within the uncertainties in the range ∼1–4 µm.”
Bright OB stars in the Galaxy. III. Constraints on the radial stratification of the clumping factor (2006, background): “Note, however, that Tokunaga & Vacca (2005) have recently shown that the near-IR (1 to 5 µm) absolute flux densities of Vega derived by means of atmospheric models (e.g., Cohen et al. 1992) and by means of direct measurements (e.g., Megessier 1995) are actually indistinguishable within the…”
The UV continua and inferred stellar populations of galaxies at z ~7-9 revealed by the Hubble Ultra-Deep Field 2012 campaign (2012, background): “…definitions of ‘effective wavelength’ for broad-band filters, but the ‘pivot’ wavelength is the appropriate one for the present study, and in any case agrees with the alternative ‘mean’ (source independent) wavelength of the filter to within better than 1 per cent (see e.g. Tokunaga & Vacca 2005).”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “Although the mean value of the intrinsic flux is well defined, the determination of the isophotal wavelength becomes problematic because spectra contain absorption lines, and hence the definition of λ̃ can yield multiple solutions (e.g., Tokunaga & Vacca 2005; Rieke et al. 2008).”
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.”
LINE DERIVED INFRARED EXTINCTION TOWARD THE GALACTIC CENTER (2011, methodology): “…calibration of the Brackett γ line map: f = FλKs λiso Ks RλBr γ 10−0.4ZP (1) = FλKs λiso Ks RλBr γ 10 −0.4 ( ZPNACO+2.5 log FSINKs FNACOKs ) (2) Here, FλKs is the Ks calibration of Vega (Tokunaga & Vacca 2005), R the number of slices per µm and ZP the zero point in magnitudes of the SINFONI data.”
THE LOW-LUMINOSITY END OF THE RADIUS–LUMINOSITY RELATIONSHIP FOR ACTIVE GALACTIC NUCLEI (2013, background): “…hundredths of a magnitude for 18 A measure of the effective wavelength of a filter that is independent of the source spectral energy distribution (Tokunaga & Vacca 2005). all of our sample (median difference of −0.024 mag) except for 3C 120 where the new extinction value is 0.2 mag smaller than…”
LARGE-AMPLITUDE VARIATIONS OF AN L/T TRANSITION BROWN DWARF: MULTI-WAVELENGTH OBSERVATIONS OF PATCHY, HIGH-CONTRAST CLOUD FEATURES (2012, methodology): “New J-band filters closely matching the Mauna Kea Observatory (MKO) system (Tokunaga & Vacca 2005) were purchased and installed for our survey in order to minimize the effects of differential atmospheric extinction, by cutting off time-variable telluric water absorption bands red-ward of 1.35 µm…”
Colours and luminosities of z = 0.1 galaxies in the eagle simulation (2015, background): “All magnitudes are calculated as rest frame and absolute in the AB-system (Oke 1974) in which the apparent magnitude mAB is defined as mAB ≡ −2.5 log10(Fν) − 48.6 , (1) where Fν is the isophotal flux density (in cgs units) in a particular band (e.g. Tokunaga & Vacca 2005).”
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).”
NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES (2012, methodology): “The photometry is on the Mauna Kea Observatories system (Tokunaga & Vacca 2005).”
M dwarfs: effective temperatures, radii and metallicities (2008, methodology): “Although our adopted Vega absolute calibration has been thoroughly tested in both optical and infrared bands via ground (Tokunaga & Vacca 2005) and spaced based (Bohlin & Gilliland 2004; Price et al. 2004; Bohlin 2007) measurements, uncertainties at the level of a few percent are present and are…”
The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours (2006, methodology): “…work has been undertaken to determine the absolute flux-distribution of Vega from the ultraviolet through near-infrared wavelengths (e.g. Bohlin & Gilliland (2004); Cohen, Wheaton & Megeath (2003)) but uncertainty at the 2% level remains (see Tokunaga & Vacca (2005) for a recent discussion).”
PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, methodology): “When conditions were good (seeing below ∼1′′) we used the Mauna Kea Observatory (MKO) H-band filter (Simons & Tokunaga 2002; Tokunaga & Vacca 2005) as a compromise between higher Strehl and increased sky background levels at longer wavelengths.”
Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster (2009, methodology): “In order to facilitate comparison of our work, we have calculated the effective wavelengths for the photometry presented here, using equation (A3) of Tokunaga & Vacca (2005).”
The Absolute Magnitude of the Sun in Several Filters (2018, unknown): “The mean photon wavelength (Bessell & Murphy 2012), also called mean wavelength by (Tokunaga & Vacca 2005) and mean or effective wavelength Rieke et al. (2008) is defined as λmean = ∫ R(λ)λdλ ∫ R(λ)dλ (A1) The mean flux of a source within the band is defined as 〈fλ〉 = ∫ fλR(λ)λdλ ∫ R(λ)λdλ (A2) The…”