Feasibility calculations for DAZLE

Linelam, ÅFline/FH-alpha Lline/Msolyr-1, 1040 erg s-1Plots
H-alpha6563111.2 PS
H-beta48610.350.39 PS
[OIII]50070.606.8 PS
[OII]37270.180.21 PS

F(Ly-a) vs z Plot (PS|gif) of Lyman-alpha flux against redshift, for SFR of 1 Msol yr-1, for three different cosmologies... [here for SI units]
...and again for two further cosmologies.

Plot (PS) of Ly-alpha photon count rate against redshift, for SFR=1Msolyr-1 and for three different cosmologies.

Plot (PS) of comoving survey volume, in Mpc3, against redshift, assuming a redshift slice dz = 0.1, and field of view 8.5'x8.5', for three different cosmologies.

Plot (PS) of angular scale, for the same three cosmologies.

Volume (xh-3Mpc3) surveyed by DAZLE (8.5'x8.5', 10<z<10.1), ALMA (10"x10", 5<z<15), and in HDF (5.3 sq', 2<z<3.5) :
1001.00.0880 402300
1000.20.86560 2651.4x104
1000.050.0 2.4x104925 1.2x104
650.040.01.0x105 37354.6x104
650.250.0 2.3x104900 2.6x104

LMA will detect massive starbursts (SFR > 100 Msolyr-1), containing large masses of dust (Mdust > 108Msol; c.f. SCUBA population, 2000 deg-2 with F850>2mJy, 1<z<3, gives space density of 10-3h1003Mpc-3, an order of magnitude smaller than phi*=1.4x10-2h3Mpc-3.

Density of Ly-alpha emitters at z=4, with SFR=1 Msolyr-1 is comparable to phi*, however. Hierarchical cosmogonies (CDM) lead us to expect low-mass systems to dominate at high z, so these objects are far more representative of the early stages of galaxy formation than the bright submm sources. DAZLE's detection rate, in a small (dz=0.1) redshift slice, in the low-SFR regime, should rival LMA's with bright objects over a much larger (hence uncertain) redshift range.

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Anthony Horton horton@ast.cam.ac.uk
Last modified: Sat Jun 8 13:04:34 2002