2MASS photometry is quoted in the internal 2MASS photometric system. Conversions between the 2MASS and other popular near-infrared photometric systems were derived empirically by Carpenter et al. (2001, AJ, 121, 2851) using point source photometry from the 2MASS Second Incremental Data Release. Those transformations have been updated using the All-Sky Release PSC and are presented in VI.4b.
2MASS Survey observations did not enable a direct measurement of the absolute calibration of the 2MASS photometric system. Cohen et al. (2003, AJ, 126, 1090) have determined photon-counting relative spectral response curves (RSRs) for the 2MASS system by combining the transmission and QE curves provided in Section III.1.b1. Figures 1, 2, and 3 show these RSRs, with peaks renormalized to unity, and including atmospheric transmission as modeled by PLEXUS. These authors offer an absolute flux calibration for 2MASS based on the calibrated spectrum of Vega from Cohen et al. (1992 AJ, 104, 1650). Characteristic quantum efficiency curves for the NICMOS III detectors supplied by Rockwell were used in the computation, but have not been measured explicitly for each device in the 2MASS cameras.
The isophotal wavelengths, bandpasses, and fluxes for zero magnitude for the three 2MASS bands from Cohen et al. (2003) are listed in Table 1 below. Figures 21 and 22 in Section III.1.b1 show how the 2MASS J-band system response changes slightly with varying levels of atmospheric water vapor or atmospheric aerosols. The J-band values in Table 1 correspond to about 5.0 mm of water vapor, but are based on PLEXUS calculations, rather than the simpler ATRAN results shown in Figures 21 and 22 in III.3.b1.
|Band||Lambda (µm)||Bandwidth (µm)||Fnu - 0 mag (Jy)||Flambda - 0 mag (W cm-2 µm-1)|
|J||1.235 ± 0.006||0.162 ± 0.001||1594 ± 27.8||3.129E-13 ± 5.464E-15|
|H||1.662 ± 0.009||0.251 ± 0.002||1024 ± 20.0||1.133E-13 ± 2.212E-15|
|Ks||2.159 ± 0.011||0.262 ± 0.002||666.7 ± 12.6||4.283E-14 ± 8.053E-16|
3 present the 2MASS J, H and Ks
relative spectral response curves (RSRs),
peak-normalized to unity, derived by
Cohen et al. (2003).
As stated by these authors, these curves "are designed to be integrated
directly over stellar spectra
in Fλ form, in order to calculate synthetic photometric
magnitudes. The QE-based component was converted to yield photon-counting
RSRs by multiplying by wavelength and renormalized, as described
by Bessel (2000)."
These RSRs are consistent with the absolute calibration of 2MASS given in
Table 1 above.
J band RSR
H band RSR
Ks band RSR
|Data table||Data table||Data table|
[Last Updated: 2008 December 28; by R. Cutri]