1. Naoyuki Tamura (University of Durham) Expected Performance of FMOS ~ Estimation with Spectrum Simulator ~ Introduction of simulators  Examples of calculations  Guidelines of detection limits through realisations  Summary 

2. Capability of FMOS Expected performance ? success rate ?? How detectable and measurable ? Effects of OH suppression masks ? Emission / Absorption How would the spectra look ? Line flux / centre / width    Spectral coverage : 0.9 ~ 1.8  m  R ~ 500 / ~ 2200  OH airglow suppression mechanism 

3. Let’s perform virtual observation ! Web-based Calculator (http://elvira.phyaig.dur.ac.uk/naoyuki.tamura/ simulator.html) Creates reduced and calibrated spectra. Quick look at feasibility of your observing program is allowed. Image Simulator Creates mock “raw” data (FITS file). Data reduction and calibration processes can be fully followed.

4. Inside the simulators SignalNoise ObjectSky background, Detector, …

5. Light is coming through … Atmosphere Fibre system Fibres Fibre connector Main mirror Prime focus corrector Spectrograph Mirrors Gratings Correctors Thermal cut filter Detector Camera Lenses Window Sky (Cont.+ OH lines) Object Seeing Energy input Fibre (1.”25  ) Absorption Reflection … Energy loss due to : sec z = 1.5 0.9  m1.8  m 20% 10% High R Low R (Calculation by Oxford & RAL for UK spectrograph) Total system throughput (w/o OH masks)

6. Inside the simulators Web-based Calculator Image Simulator Refer to talk by M. Akiyama for details. Calculates an S/N per pixel and adds fluctuations onto an input spectrum. SignalNoise ObjectSky background, Detector, … Counts the total number of electrons stored in each pixel and adds Poisson noise. Is ready to take into account : Fibre-to-fibre variation in throughput. PSF variation between spectra on the detector E.g., Plus

7. Calculations Performed with Image Simulator 1 hour exposure, 0.”5 seeing & sec z = 1.5 were assumed in all calculations. (All the reduction and calibration processes were followed with no failure.) How detectable and measurable ? Effects of OH suppression masks ? Emission / Absorption How would the spectra look ? Line flux / centre / width    Low R mode High R mode

8. No pix. binning H = 19.5 mag H = 18.0 mag Calculations (low R mode) Objects  Old stellar population (3.0 Gyr age) at z = 1.5 5 pixel binning Starburst galaxy at z = 1.5L-type star (L6V) 4000 A G-band HH [O II ] [O III ] H  + [N II ] [S II ] HH

9. Emission line  No continuum Line profile : Gaussian (  = 300 km/s) Line flux = 6.0 x 10 erg/s/cm  17 2 Calculations (low R mode) No pixel binning was performed. Line flux = 3.0 x 10 erg/s/cm  17 2

10. 20 realisations at every angstrom. Calculations (low R mode) Measured flux/Centre/width given values (Estimated flux) / (Given flux)  Estimated) /  (Given)  (Line centre) [A] 90 % 10 % Emission line flux = 6.0 x 10 erg/s/cm  17 2 [Emission line]

11. Summary for a few cases. Calculations (low R mode) (Estimated flux) / (Given flux)  Estimated) /  (Given)  (Line centre) [A] 90 % 10 % Horizontal : Line flux [10 erg/s/cm ]  17 2 50 %

12. Absorption line  Continuum = 1.1 x 10 erg/s/cm /A Line profile : Gaussian (  = 300 km/s)  18 2 or H = 20 mag (Vega system) Line flux = 3.0 x 10 erg/s/cm  17 2 (EW = 27 A) Calculations (low R mode) No pixel binning was performed. Line flux = 2.0 x 10 erg/s/cm  17 2 (EW = 18 A)

13. 20 realisations at every angstrom. Calculations (low R mode) (Estimated flux) / (Given flux)  Estimated) /  (Given)  (Line centre) [A] 90 % 10 % absorption line flux = 3.0 x 10 erg/s/cm (EW = 27A)  17 2 Measured flux/Centre/width given values [Absorption ion line]

14. Summary for a few cases. Calculations (low R mode)  Estimated) /  (Given) (Estimated flux) / (Given flux)  (Line centre) [A] Horizontal : Line flux [10 erg/s/cm ]  17 2 EW [A] 9 18 27 54 90 % 10 % 50 %

15. Flux Effects of OH masks Mask Original spectrum Sensitivity correction Flux calibration Blurring High R mode Low R mode Counts

16. Emission line  No continuum Line profile : Gaussian (  = 300 km/s) Line flux = 6.0 x 10 erg/s/cm  17 2 Calculations (high R mode) Black No pixel binning was performed. Red 3 pixel binning was performed (masked regions were avoided).

17. 20 realisations at every angstrom. Calculations (high R mode) (Estimated flux) / (Given flux)  Estimated) /  (Given)  (Line centre) [A] 90 % 10 % [Emission line] Emission line flux = 6.0 x 10 erg/s/cm  17 2

18. Summary Will be discussed tomorrow … (1 hour exposure, 0.”5 seeing, sec z = 1.5) Simulators for virtual observations with FMOS. Web-based Calculator Image Simulator Performance estimations Emission line : 6.0 x 10 erg/s/cm w/ no cont.  17 2 Treatment of masked regions in high R mode. Sensitivity correction / Flux calibration Absorption line : 3.0 x 10 erg/s/cm  17 2 w/ H = 20 mag cont. Sky subtraction Flat fielding w/ mask effect  (Flux) ~ 10 %  (Centre) ~ 5 A  (Width) ~ 20 %