Mapping the Galactic Halo IV. Finding Distant Giants Reliably with the Washington System

Details Mapping the Galactic Halo IV. Finding Distant Giants Reliably with the Washington System Mapping the Galactic Halo IV. Finding Distant Giants Reliably with the Washington System

2000-10-12

arxiv.org/abs/astro-ph/0010254v2

Astron.J. 121 (2001) 283-294

Astronomy and Astrophysics

Astrophysics

Accepted for publication in Jan. 2001 Astronomical Journal

Scientific paper

10.1086/318041

We critically examine the use of the Washington photometric system (with the 51 filter) for identifying distant halo giants. While this is the most powerful photometric technique for isolating G and K giant stars, spectroscopic follow-up of giant candidates is vital. There are two situations in which interlopers outnumber genuine giants in the diagnostic M-51/M-T2 plot, and are indistinguishable photometrically from the giants. (1) In deep surveys covering tens of square degrees, very metal-poor halo dwarfs are a significant contaminant. An example is our survey of the outer halo (Morrison et al. 2000, Dohm-Palmer et al. 2000), where these metal-poor dwarfs dominate the number of photometric giant candidates at magnitudes fainter than V = 18 and cannot be isolated photometrically. (2) In deep surveys of smaller areas with low photometric precision, most objects in the giant region of the color-color plot are dwarfs whose photometric errors have moved them there. Color errors in M-51 and M-T2 need to be smaller than 0.03 mag to avoid this problem. An example of a survey whose photometric errors place the giant identifications under question is the survey for extra-tidal giants around the Carina dwarf spheroidal of Majewski et al. (2000a). Accurate photometry and spectroscopic follow-up of giant candidates are essential when using the Washington system to identify the rare outer-halo giants.

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