A Calibration of NICMOS Camera 2 for Low Count Rates
Gladders, M. D.; Lidman, C.; Amanullah, R.; Rubin, D.; Aldering, G.; Barbary, K.; Dawson, K. S.; Faccioli, L.; Fakhouri, H. K.; Fruchter, A. S.; Meyers, J.; Nordin, J.; Perlmutter, S.; Suzuki, N.; Koekemoer, A.; Deustua, S.; Fadeyev, V.; de Jong, R. S.; Ripoche, P.; Schlegel, D. J.; Spadafora, A.; Krechmer, E.
United States, Sweden, China, Germany, Australia, Japan
Abstract
NICMOS 2 observations are crucial for constraining distances to most of the existing sample of z\gt 1 SNe Ia. Unlike conventional calibration programs, these observations involve long exposure times and low count rates. Reciprocity failure is known to exist in HgCdTe devices and a correction for this effect has already been implemented for high and medium count rates. However, observations at faint count rates rely on extrapolations. Here instead, we provide a new zero-point calibration directly applicable to faint sources. This is obtained via inter-calibration of NIC2 F110W/F160W with the Wide Field Camera 3 (WFC3) in the low count-rate regime using z∼ 1 elliptical galaxies as tertiary calibrators. These objects have relatively simple near-IR spectral energy distributions, uniform colors, and their extended nature gives a superior signal-to-noise ratio at the same count rate than would stars. The use of extended objects also allows greater tolerances on point-spread function profiles. We find space telescope magnitude zero points (after the installation of the NICMOS cooling system, NCS) of 25.296\+/- 0.022 for F110W and 25.803\+/- 0.023 for F160W, both in agreement with the calibration extrapolated from count rates ≳1000 times larger (25.262 and 25.799). Before the installation of the NCS, we find 24.843\+/- 0.025 for F110W and 25.498\+/- 0.021 for F160W, also in agreement with the high-count-rate calibration (24.815 and 25.470). We also check the standard bandpasses of WFC3 and NICMOS 2 using a range of stars and galaxies at different colors and find mild tension for WFC3, limiting the accuracy of the zero points. To avoid human bias, our cross-calibration was “blinded” in that the fitted zero-point differences were hidden until the analysis was finalized.
Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, under programs SM2/NIC-7049, SM2/NIC-7152, CAL/NIC-7607, CAL/NIC-7691, CAL/NIC-7693, GO-7887, CAL/NIC-7902, CAL/NIC-7904, GO/DD-7941, SM3/NIC-8983, SM3/NIC-8986, GTO/ACS-9290, ENG/NIC-9324, CAL/NIC-9325, GO-9352, GO-9375, SNAP-9485, CAL/NIC-9639, GO-9717, GO-9834, GO-9856, CAL/NIC-9995, CAL/NIC-9997, GO-10189, GO-10258, CAL/NIC-10381, CAL/NIC-10454, GO-10496, CAL/NIC-10725, CAL/NIC-10726, GO-10886, CAL/NIC-11060, CAL/NIC-11061, GO-11135, GO-11143, GO-11202, CAL/NIC-11319, GO/DD-11359, SM4/WFC3-11439, SM4/WFC3-11451, GO-11557, GO-11591, GO-11600, GO/DD-11799, CAL/WFC3-11921, CAL/WFC3-11926, GO/DD-12051, GO-12061, GO-12062, GO-12177, CAL/WFC3-12333, CAL/WFC3-12334, CAL/WFC3-12341, GO-12443, GO-12444, GO-12445, CAL/WFC3-12698, CAL/WFC3-12699, GO-12874, CAL/WFC3-13088, and CAL/WFC3-13089.