IRMS Spectroscopically resolved Hα Sensitivity
1/5/2010 updated.

To investigage what star formation rates will be observable with IRMS,
we simulate Hα emission from z=1.5 galaxies with various integrated star formation rates.
A Kennicutt law is used to estimate the total luminosity of each source.

SFR [M_solar/yr] = 7.9 × 10-42 L(Hα) [erg/s]

We then derive the observed flux using cosmology parameters as below.

F(Hα) [erg/s/m2/μm] = L(Hα) / dλ 4 π dL2  (&lambda=[μm], dL=[m])
                               = SFR / dλ 4 π dL2 × 7.9 × 10-42

Instrument parameters are the same as S/N Sensitivity

Other Parameters
H&alpha Redshift H&alpha@z=1.5 (H-band) H&alpha@z=2.4 (K-band)
H&alpha Wavelength 1.65 um (&lambda0 of H-band) 2.20 um (&lambda0 of K-band)
Cosmology Parameter H0=71, &OmegaM=0.27, &OmegaV=0.73 Calculator
Lookback Time 9.5 Gyr 10.9 Gyr Calculator
Light Distance (dL) 35.906 Gly 64.218 Gly Calculator
Scale 8540 pc/arcsec 8257 pc/arcsec Calculator
Sampling Scale 0.06 arcsec (60 mas) 0.06 arcsec (60 mas)
Slit width 0.16 arcsec (160 mas) ~2.7pix 0.16 arcsec (160 mas) ~2.7pix MOSFIRE minimum slit width
Angular Diameter at each redshift 0.16 mas = 1366 pc 0.16 mas = 1321 pc
Assumed Encircled Energy inside Slit NFIRAOS wide-field mode for &Phi 120 arcmin
On-axis: 0.65@J, 0.75@H, 0.8@K
Average: 0.4@J, 0.5@H, 0.6@K
TMT Instrument Handbook(2010)
Exposure Time 18000 s (900s x 20) 18000 s (900s x 20)
[OII]3727 Wavelength 9317 A @z-band 1.27 um @J-band
Hβ4860 Wavelength 1.22 um @J-band 1.65 um @H-band
[OIII]5007 Wavelength 1.25 um @J-band 1.70 um @H-band
Estimated S/N vs Star Formation Rate for Hα emission line of z=1.5 and z=2.4 galaxy. Flux distribution size (angular diameter) is assumed 0.16 mas (the same with MOSFIRE minimum slit width). Compared to IRIS 50 mas sensitivity (below), NFIRAOS effect is poor, but coarse spatial scale is suit for observations of high-z galaxies. IRIS IFS(Integral Field Spectroscopy) sensitivity in case of 50 mas sampling. (from IRIS Homepage)