The differential sensitivity shown below is defined as the minimum flux needed by CTAO to obtain a 5-standard-deviation detection of a point-like source, calculated in non-overlapping logarithmic energy bins (five per decade). Besides the significant detection, we require at least ten detected gamma rays per energy bin, and a signal/background ratio of at least 1/20.  The analysis cuts in each bin have been optimised to achieve the best flux sensitivity to point-like sources. The optimal cut values depend on the duration of the observation, therefore the performance curves are provided for three different observation times: 0.5, 5 and 50 hours.

CTAO Southern Array

CTAO Northern Array

CTAO Arrays Comparison

CTAO Southern Array vs Other Instruments

CTAO Northern Array vs Other Instruments

CTAO Arrays vs Other Instruments

Note that the curves for Fermi-LAT and HAWC are scaled by a factor 1.2 relative to the references (see below), to account for the different energy binning. The curves shown allow only a rough comparison of the sensitivity of the different instruments, as the method of calculation and the criteria applied are not identical. In particular, the definition of the differential sensitivity for HAWC is rather different due to the lack of an accurate energy reconstruction for individual photons in the HAWC analysis.

Sources:

ASTRI: https://pos.sissa.it/395/884/pdf

Fermi-LAT: public specifications webpage http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm

HAWC: arXiv:1701.01778
H.E.S.S.: Preliminary sensitivity curves for H.E.S.S.-I (stereo reconstruction), based on/adapted from Holler et. al 2015 (Proceedings of the 34th ICRC)
MAGIC: Astroparticle Physics 72 (2016) 76-94

LHAASO: https://arxiv.org/abs/1905.02773

SWGO (previously called SGSO): arXiv:1902.08429
VERITAS: public specifications webpage https://veritas.sao.arizona.edu/about-veritas/veritas-specifications

Differential flux sensitivity of CTAO-North at selected energies as function of observation time in comparison with the Fermi-LAT instrument (Pass 8 analysis, extragalactic background, standard survey observing mode). The differential flux sensitivity is defined as the minimum flux needed to obtain a 5-standard-deviation detection from a point-like gamma-ray source, calculated for energy bins of a width of 0.2 decades. An additional constraint of a minimum of 10 excess counts is applied. Note that especially for exposures longer than several hours, the restrictions on observability of a transient object are much stricter for CTAO than for the Fermi-LAT. CTAO will be able to observe objects above 20 degrees elevation during dark sky conditions. The differential flux sensitivity shown above are for observations near 70-degree elevation angles.

The angular resolution vs. reconstructed energy curve shows the angle within which 68% of reconstructed gamma rays fall, relative to their true direction. Gamma-hadron separation cuts are applied for the MC events used to determine the angular resolution. Dedicated analysis cuts can provide improved angular (or spectral) resolution at the expense of collection area, enabling e.g. a better study of the morphology or spectral characteristics of bright sources.

CTAO Southern Array

CTAO Northern Array

Other Instruments

The energy resolution ΔE / E is obtained from the distribution of (E_R – E_T) / E_T, where R and T refer to the reconstructed and true energies of gamma-ray events recorded by CTAO. ΔE/E is the half-width of the interval around 0 which contains 68% of the distribution. The plot shows the energy resolution as a function of reconstructed energy  (the result depends only weakly on the assumed gamma-ray spectrum; for the results here we use dNɣ/dE ~E^-2.62).

CTAO Southern Array

The effective collection area for gamma rays from a point-like source is shown below vs. E_T  for gamma/hadron cuts optimised for 0.5-, 5- and 50-h observations (no cut in the reconstructed event direction applied):

CTAO Southern Array

CTAO Northern Array

The effective collection area with cuts in the reconstructed event direction:

CTAO Southern Array

CTAO Northern Array

The (post-analysis) residual cosmic-ray background rate per square degree vs reconstructed gamma-ray energy E_R is shown below.

CTAO Arrays Comparison

The rate is the one integrated in 0.2-decade-wide bins in estimated energy (i.e. five bins per decade). Gamma-hadron separation cuts optimised for different observing times are applied to the selection of simulated cosmic-ray proton and electron events.

For details on the assumed cosmic-ray proton and electron spectra, see Bernlöhr et al 2013.

All performance parameters presented above are valid for a source located close to the centre of the CTA field of view (FoV). The differential sensitivity curves for a point-like source at increasing angular distances from the centre of the FoV are shown below.

CTAO Southern Array

CTAO Northern Array

Angular and energy resolution also degrade as one approaches the edge of the FoV. The provided IRFs contain the evolution of all performance parameters with off-axis angle.