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ZFOURGE

From Wikipedia, the free encyclopedia

ZFOURGE or the FourStar Galaxy Evolution Survey is a medium-band imaging survey that aims to establish an observational benchmark of galaxy properties at redshift z > 1. The survey uses an efficient near-infrared FOURSTAR instrument on the Magellan Telescopes, surveying in all three HST legacy fields: COSMOS, CDFS, and UDS.[1]

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Transcription

Aims

ZFOURGE aims to create a benchmark of properties at z > 1 by deriving 1-2% accurate redshifts of ~60,000 galaxies at 1 < z < 3.

The majority of L∗ galaxies are too faint for spectroscopy. This resulted in inaccurate broadband photometric redshifts in earlier studies. FourStar is equipped with innovative "medium-bandwidth" filters from 1 − 1.8μm, which enable redshifts to z = 3.5.

This allows ZFOURGE to observe galaxy samples from the low mass at z > 1, to measure the value of mass and environment in transformation of galaxies, measure galaxy scaling relations. It will also explore the shape of the stellar mass function to z = 3, find luminous galaxies at z = 6–9, and identify high-redshift 1.5 < z < 2.5 (proto)clusters.[2]

Instruments

The Fourstar ZFOURGE is conducted using the FourStar imager[3] on the 6.5m Magellan Baade telescope at Las Campanas Observatory. It uses medium-band filters in the near-IR[4] that allow for samplings at wavelengths that bracket the Balmer break of galaxies leading to more well-constrained photometric redshifts at 1 < z < 4 than with broadband filters alone. This dataset provides a comprehensive sampling of the 0.3 – 8 micron spectral energy distribution of galaxies.

ZFOURGE is composed of three 11′ x 11′ pointings with coverage in the CDFS,[5] COSMOS[6] and UDS.[7] The 5sigma depth in a circular aperture of D=0.6" in the Ks band is 26.2-26.5 in the CDFS, COSMOS and UDS fields respectively at a typical seeing of ~0.4″.[1][8]

References

  1. ^ a b "ZFOURGE – Fourstar Galaxy Evolution Survey". zfourge.tamu.edu.
  2. ^ "Science – ZFOURGE". zfourge.tamu.edu.
  3. ^ Persson et al. 2013
  4. ^ van Dokkum et al. 2009
  5. ^ Giacconi et al. 2002
  6. ^ Capak et al. 2007
  7. ^ Lawrence et al. 2007
  8. ^ Straatman et al. (2016)

External links

This page was last edited on 2 March 2024, at 01:49
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