ASTRO-F - The next generation of mid-infrared surveys

By C. Pearson, H. Matsuhara, H. Watarai, T. Matsumoto, T. Onaka. 2000

142 citations recorded by the source corpus.

We present basic observational strategies for ASTRO-F (also known as the Imaging Infra Red Surveyor (IRIS)) to be launched in 2004 by the Japanese Institute of Space and Astronautical Science (ISAS). We examine 2 survey scenarios, a deep ~1sq.deg. survey reaching sensitivities an order of magnitude below than the deepest surveys performed by ISO in the mid-IR, and a shallow \~18sq.deg mid-infrared (7-25um in 6 bands) covering an area greater than the entire area covered by all ISO mid-IR surveys. Using 2 cosmological models the number of galaxies predicted for each survey is calculated. The first model uses an enhancement of the pure luminosity evolution model of Pearson&Rowan-Robinson while the new models incorporate a strongly evolving ULIG component. For the deep survey, between 20,000-30,000 galaxies should be detected in the shortest wavebands and ~5000 in the longest (25um) band. The shallow survey would be expected to detect of the order of 100,000 - 150,000 sources.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/925755824add1d348a5732cf47eb311971ac52da

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Citations in the corpus

The binary fraction of extreme horizontal branch stars (2001, unknown): “Maxted et al. (2000); 4.”
The Progenitors of Type Ia Supernovae (2012, background): “The only likely SN Ia progenitor in this sample is not a double WD system, but the WD + sdB binary KPD 1930+2752 (Maxted et al., 2000).”
The origin of subdwarf B stars – II (2003, background): “…1998; Koen, Orosz & Wade 1998; Saffer, Livio & Yungelson 1998; Kilkenny et al. 1999; Moran et al. 1999; Orosz & Wade 1999; Wood & Saffer 1999; Maxted, Marsh & North 2000a; Maxted et al. 2000b, 2001; Napiwotzki et al. 2001; Drechsel et al. 2001; Heber et al. 2002; Morales-Rueda et al. 2002, 2003).”
The origin of subdwarf B stars – I. The formation channels (2002, background): “…has been the identification of many sdB stars as short-period binaries (Saffer, Livio & Yungelson 1998; Koen, Orosz & Wade 1998; Jeffery & Pollacco 1998; Wood & Saffer 1999; Orosz & Wade 1999; Moran et al. 1999; Maxted et al. 2000; Maxted, Marsh & North 2000; Maxted et al. 2001; Heber et al. 2002).”
The frequency of planetary debris around young white dwarfs (2014, background): “…are confirmed double-degenerate binaries with periods of 1.12 d and 5.08 d (Marsh et al. 1995; Nelemans et al. 2005), WD 0341+021 is a suspected double-degenerate (Maxted et al. 2000), and WD 1229-013 and WD 1353+409 show no radial velocity variations (Maxted & Marsh 1998; Maxted et al. 2000).”
Supernova Type Ia progenitors from merging double white dwarfs - Using a new population synthesis model (2012, background): “An immediate precursor of a DW that is possibly a progenitor candidate for a SN Ia via the DD channel has also been observed; a subdwarf with a white dwarf companion, KPD 1930+2752 (Maxted et al. 2000; Geier et al. 2007).”
The helium star donor channel for the progenitors of Type Ia supernovae (2009, background): “(1) Maxted et al. (2000) suggested that KPD 1930+2752 is likely to eventually result in a merger and produce an SN Ia (see also Geier et al. 2007).”
COMPREHENSIVE PHOTOMETRIC HISTORIES OF ALL KNOWN GALACTIC RECURRENT NOVAE (2009, background): “For example, even the star KPD 1930+275 with a white dwarf in a binary of total mass 1.47±0.01 M (Maxted et al. 2000, but see Geier et al. 2007) will lose enough mass so as to avoid exceeding the Chandrasekhar mass (Ergma et al. 2001).”