By continuing to use this website, you are giving consent to our use of cookies.
For more information on how ESO uses data and how you can disable cookies, please view our privacy policy.

Lyα sensitivities vs. redshift for MOSAIC compared with the expected fluxes and the deepest Lyα observations available at z>5

MOSAIC will measure Lyα line fluxes up to ~ 40 times deeper than current samples at z ~7 (blank fields), ~ 40 times deeper than current searches for Lyα emission from z~7-8.5 (lensed galaxies), and >100 times deeper than the current searches at z~8-10. It will also extend Lyα searches up to z~13, and undertake spectroscopy of large numbers of galaxies down to mAB~30, which are presumably the dominant population of reionisation sources, unachievable with other planned ELT instruments. Finally, it will reach an effective Lyα transmission (feff) of 10% for the faintest objects (and lower values for the brighter objects). Blue dashed lines: Expected fluxes for a range of SFR×feff, ranging from 10 to 0.01 M/yr, where feff is the effective Lyα transmissions. Green dash-dotted lines: Expected Lyα flux for star-forming galaxies, with their rest-frame UV continuum magnitudes (feff = 1). Filled circles: Observations from Shimasaku et al. (2006), Kashikawa et al. (2006), and Ota et al. (2008) at z = 5.7, 6.5, and 7, respectively. Crosses: Intrinsic fluxes for lensed candidates from Stark et al. (2007). Black spectrum: Flux limit from deep Keck-NIRSPEC spectroscopy (Richard et al. 2008). MOSAIC will provide a sensitivity gain of a factor of ≥40, potentially extending up to z~13. For galaxies lensed by clusters, we will be able to measure IGM transmissions down to even fainter physical limits.

Credit:

MOSAIC Consortium

About the Image

Id:science-galaxies-evolution3
Type:Simulation
Release date:16 September 2020, 16:56
Size:826 x 706 px

About the Object

Type:Unspecified
Category:ELT
Illustrations

Image Formats

Large JPEG
139.9 KB
Screensize JPEG
180.7 KB