def loadEA(self, instrument = "VERITAS", **pars):
''' - Instruments -
These are the currently avaialble instruments.
'VERITAS': this is an array of IACTs located in Southern
Arizona and sensitive from about 100 GeV to tens of TeV. You
can choose a variety of zenith angles (0 is pointing straight
up) and noise levels (ie. night sky background), and expected
source spectrum. The default noise level is adequate for most
fields and the default expected source spectrum (-4) is
adequate for most sources at VHE.
'HESS': This is an array of IACTs located in Nambia and
sensitive from about 100 GeV to tens of TeV. You can choose
three zenith angles (20, 45 and 60). The effective areas are
from A&A 457, 899 (2006), Figure 13. The threshold is set to
150 GeV.
'HAWC': This is a water Cherenkov experiment located in
Mexico. The effective areas are from APh 35, 6412 (2012),
Figure 2. You can choose from a high trigger rate (nHit > 70)
or a low trigger rate (nHit > 30). You can also choose from
four zenith angle rages.
'CTA': this is a future IACT observatory that will be an order
of magnitude more sensitive then the current generation. The
Effective Area curve is from "Monte Carlo design studies for
the Cherenkov Telescope Array", Bernlohr et
al. arXiv:1210.3503, Figure 15 and assume the baseline/MPIK
curve. Note that this is for demonstration purposes only and
there are no modifiers for zenith angle, noise level or
anything else. The safe energy range is hardcoded from 100
GeV to 100 TeV and the threshold is set to 100 GeV.
'''
EAParamTemplates = {"VERITAS" : {"zenith":20, "azimuth":0, "noise":4.07},
"CTA" : {"zenith":0, "azimuth":0, "noise":0},
"HESS" : {"zenith":20, "azimuth":0, "noise":0},
"HAWC" : {"zenith":20, "azimuth":0, "noise":0}}
EffectiveAreas = {"VERITAS": self.loadVERITASEA,
"CTA": self.loadCTAEA,
"HESS": self.loadHESSEA,
"HAWC": self.loadHAWCEA}
try:
checkParams(EAParamTemplates[instrument],pars, self.logger)
except KeyError:
self.logger.critical("Unsupported instrument.")
return
try:
self.EASummary,self.EACurve,self.SensCurve,self.EAFile,self.EATable,self.crabRate = EffectiveAreas[instrument](**pars)
except KeyError:
self.logger.critical("Unsupported instrument.")
return
def loadEA(self, instrument="VERITAS", **pars):
''' - Instruments -
These are the currently avaialble instruments.
'VERITAS': this is an array of IACTs located in Southern
Arizona and sensitive from about 100 GeV to tens of TeV. You
can choose a variety of zenith angles (0 is pointing straight
up) and noise levels (ie. night sky background), and expected
source spectrum. The default noise level is adequate for most
fields and the default expected source spectrum (-4) is
adequate for most sources at VHE.
'HESS': This is an array of IACTs located in Nambia and
sensitive from about 100 GeV to tens of TeV. You can choose
three zenith angles (20, 45 and 60). The effective areas are
from A&A 457, 899 (2006), Figure 13. The threshold is set to
150 GeV.
'HAWC': This is a water Cherenkov experiment located in
Mexico. The effective areas are from APh 35, 6412 (2012),
Figure 2. You can choose from a high trigger rate (nHit > 70)
or a low trigger rate (nHit > 30). You can also choose from
four zenith angle rages.
'CTA': this is a future IACT observatory that will be an order
of magnitude more sensitive then the current generation. The
Effective Area curve is from "Monte Carlo design studies for
the Cherenkov Telescope Array", Bernlohr et
al. arXiv:1210.3503, Figure 15 and assume the baseline/MPIK
curve. Note that this is for demonstration purposes only and
there are no modifiers for zenith angle, noise level or
anything else. The safe energy range is hardcoded from 100
GeV to 100 TeV and the threshold is set to 100 GeV.
'''
EAParamTemplates = {
"VERITAS": {
"zenith": 20,
"azimuth": 0,
"noise": 4.07
},
"CTA": {
"zenith": 0,
"azimuth": 0,
"noise": 0
},
"HESS": {
"zenith": 20,
"azimuth": 0,
"noise": 0
},
"HESS2": {
"zenith": 0,
"azimuth": 0,
"noise": 0
},
"HAWC": {
"zenith": 20
}
}
EffectiveAreas = {
"VERITAS": self.loadVERITASEA,
"CTA": self.loadCTAEA,
"HESS": self.loadHESSEA,
"HESS2": self.loadHESS2EA,
"HAWC": self.loadHAWCEA
}
try:
checkParams(EAParamTemplates[instrument], pars, self.logger)
except KeyError:
self.logger.critical("Unsupported instrument.")
return
try:
self.EASummary, self.EACurve, self.SensCurve, self.EAFile, self.EATable, self.crabRate = EffectiveAreas[
instrument](**pars)
except KeyError:
self.logger.critical("Unsupported instrument.")
return
def Spectrum(self,spectralModel, EnergyBins, **pars):
''' - Spectral Functions -
The VOT code uses a spectrum (dN/dE) given an input array of
energy bins (in GeV). There are several available types
avaialble and these are the only ones you can use to create a
'custom' source. The parameters given must match the
parameters and units shown below. Most of these functions are
based on the functions in the Fermi LAT catalog except as
noted.
PowerLaw: a simple power law with normalization ('N0', cm^-2
s^-1 GeV^-1), index ('index', negative), pivot energy ("E0",
GeV).
PowerLaw2: same as the PowerLaw but defined by the integral
flux and not the differential flux. Parameters are the
integral flux ('N', cm^-2 s^-1 GeV^-1), index ('index',
negative), lower energy limit ('E1', GeV) and upper energy
limit ('E2', GeV).
BrokenPowerLaw: two component power law with normalization
('N0', cm^-2 s^-1 GeV^-1), low energy spectral index
('index1', negative), high energy spectral index ('index2',
negative) and break energy ('Eb', GeV).
LogParabola: curving function used to model blazars with
parameters Normalization ('N0', cm^-2 s^-1 GeV^-1), spectral
index ('alpha', negative), index ('beta, negative) and break
energy ('Eb', GeV).
HESSExpCutoff: power law with a cutoff used by the HESS
collaboration to model the Crab Nebula's spectrum. The
parameters are the normalization ('N0', cm^-2 s^-1 GeV^-1),
index ('index', negative), pivot energy ('E0', GeV) and cutoff
energy ('EC', GeV).
Band: basic band function used to model GRBs. The parameters
are the normalization ('N0', cm^-2 s^-1 GeV^-1), alpha
('alpha', negative), beta ('beta', negative) and the peak
energy ('Ep', GeV).
'''
spectralParameterTemplates = {"PowerLaw": {"N0":1e-9,"index":-2,"E0":700},
"PowerLaw2": {"N":1e-6,"index":-2,"E1":1,"E2":100},
"BrokenPowerLaw": {"N0":1e-9,"index1":-2,"index2":-1.5,"Eb":700},
"LogParabola": {"N0":1e-9,"alpha":-1.0,"beta":-2.0,"Eb":700},
"HESSExpCutoff": {"N0":1e-9, "index":-2, "E0":1000, "EC":14000},
"Band": {"N0":1e-9, "alpha":-1.5,"beta":-2.5,"Ep":0.001},
}
if (spectralModel == "PowerLaw2"):
'''Assumes a 1GeV Decorrelation energy and energies in GeV.'''
pars["E0"] = 1.0
X1 = pars["E1"]/pars["E0"]
X2 = pars["E2"]/pars["E0"]
pars["N0"] = (pars["N"]*(1 + pars["index"])/pars["E0"])/(X2**(1 + pars["index"]) - X1**(1 + pars["index"]))
spectralModel = "PowerLaw"
self.logger.warn("Calculated normalization: " + str(pars["N0"]) + " s^-1 cm^-2 GeV^-1")
spectralFunction = {"PowerLaw": lambda x: pars["N0"]*((x/pars["E0"])**pars["index"]),
"PowerLaw2": lambda x: ((pars["index"] + 1)*pars["N"]*x**pars["index"])/\
(pars["E2"]**(pars["index"]+1) - pars["E1"]**(pars["index"]+1)),
"BrokenPowerLaw": lambda x: x < pars["Eb"] and pars["N0"]*((x/pars["Eb"])**pars["index1"])\
or pars["N0"]*((x/pars["Eb"])**pars["index2"]),
"LogParabola": lambda x: pars["N0"]*((x/pars["Eb"])**(pars["alpha"]+pars["beta"]*np.log(x/pars["Eb"]))),
"HESSExpCutoff":lambda x: pars["N0"]*((x/pars["E0"])**pars["index"])*np.exp(-x/pars["EC"]),
"Band": lambda x: x < pars["Ep"]*(pars["alpha"]-pars["beta"])/(pars["alpha"]+2)\
and (x/0.1)**pars["alpha"]*np.exp(-(x/pars["Ep"])*(pars["alpha"]+2))\
or (x/0.1)**pars["beta"]*((pars["Ep"]/0.1)*(pars["alpha"]-pars["beta"])/(pars["alpha"]+2))**(pars["alpha"]-pars["beta"])*np.exp(pars["beta"]-pars["alpha"]),
"Band1": lambda x: (x/0.1)**pars["beta"]*((pars["Ep"]/0.1)*(pars["alpha"]-pars["beta"])/(pars["alpha"]+2))**(pars["alpha"]-pars["beta"])*np.exp(pars["beta"]-pars["alpha"]),
}
try:
checkParams(spectralParameterTemplates[spectralModel],pars, self.logger)
except KeyError:
return
dNdE = []
try:
for energy in EnergyBins:
dNdE.append(spectralFunction[spectralModel](energy))
return dNdE
except KeyError:
self.logger.critical("No such model.")
def Spectrum(self, spectralModel, EnergyBins, **pars):
''' - Spectral Functions -
The VOT code uses a spectrum (dN/dE) given an input array of
energy bins (in GeV). There are several available types
avaialble and these are the only ones you can use to create a
'custom' source. The parameters given must match the
parameters and units shown below. Most of these functions are
based on the functions in the Fermi LAT catalog except as
noted.
PowerLaw: a simple power law with normalization ('N0', cm^-2
s^-1 GeV^-1), index ('index', negative), pivot energy ("E0",
GeV).
PowerLaw2: same as the PowerLaw but defined by the integral
flux and not the differential flux. Parameters are the
integral flux ('N', cm^-2 s^-1 GeV^-1), index ('index',
negative), lower energy limit ('E1', GeV) and upper energy
limit ('E2', GeV).
BrokenPowerLaw: two component power law with normalization
('N0', cm^-2 s^-1 GeV^-1), low energy spectral index
('index1', negative), high energy spectral index ('index2',
negative) and break energy ('Eb', GeV).
LogParabola: curving function used to model blazars with
parameters Normalization ('N0', cm^-2 s^-1 GeV^-1), spectral
index ('alpha', negative), index ('beta, negative) and break
energy ('Eb', GeV).
HESSExpCutoff: power law with a cutoff used by the HESS
collaboration to model the Crab Nebula's spectrum. The
parameters are the normalization ('N0', cm^-2 s^-1 GeV^-1),
index ('index', negative), pivot energy ('E0', GeV) and cutoff
energy ('EC', GeV).
Band: basic band function used to model GRBs. The parameters
are the normalization ('N0', cm^-2 s^-1 GeV^-1), alpha
('alpha', negative), beta ('beta', negative) and the peak
energy ('Ep', GeV).
'''
spectralParameterTemplates = {
"PowerLaw": {
"N0": 1e-9,
"index": -2,
"E0": 700
},
"PowerLaw2": {
"N": 1e-6,
"index": -2,
"E1": 1,
"E2": 100
},
"BrokenPowerLaw": {
"N0": 1e-9,
"index1": -2,
"index2": -1.5,
"Eb": 700
},
"LogParabola": {
"N0": 1e-9,
"alpha": -1.0,
"beta": -2.0,
"Eb": 700
},
"HESSExpCutoff": {
"N0": 1e-9,
"index": -2,
"E0": 1000,
"EC": 14000
},
"Band": {
"N0": 1e-9,
"alpha": -1.5,
"beta": -2.5,
"Ep": 0.001
},
}
if (spectralModel == "PowerLaw2"):
'''Assumes a 1GeV Decorrelation energy and energies in GeV.'''
pars["E0"] = 1.0
X1 = pars["E1"] / pars["E0"]
X2 = pars["E2"] / pars["E0"]
pars["N0"] = (pars["N"] * (1 + pars["index"]) / pars["E0"]) / (
X2**(1 + pars["index"]) - X1**(1 + pars["index"]))
spectralModel = "PowerLaw"
self.logger.info("Calculated normalization: " + str(pars["N0"]) +
" s^-1 cm^-2 GeV^-1")
spectralFunction = {"PowerLaw": lambda x: pars["N0"]*((x/pars["E0"])**pars["index"]),
"PowerLaw2": lambda x: ((pars["index"] + 1)*pars["N"]*x**pars["index"])/\
(pars["E2"]**(pars["index"]+1) - pars["E1"]**(pars["index"]+1)),
"BrokenPowerLaw": lambda x: x < pars["Eb"] and pars["N0"]*((x/pars["Eb"])**pars["index1"])\
or pars["N0"]*((x/pars["Eb"])**pars["index2"]),
"LogParabola": lambda x: pars["N0"]*((x/pars["Eb"])**(pars["alpha"]+pars["beta"]*np.log(x/pars["Eb"]))),
"HESSExpCutoff":lambda x: pars["N0"]*((x/pars["E0"])**pars["index"])*np.exp(-x/pars["EC"]),
"Band": lambda x: x < pars["Ep"]*(pars["alpha"]-pars["beta"])/(pars["alpha"]+2)\
and (x/0.1)**pars["alpha"]*np.exp(-(x/pars["Ep"])*(pars["alpha"]+2))\
or (x/0.1)**pars["beta"]*((pars["Ep"]/0.1)*(pars["alpha"]-pars["beta"])/(pars["alpha"]+2))**(pars["alpha"]-pars["beta"])*np.exp(pars["beta"]-pars["alpha"]),
"Band1": lambda x: (x/0.1)**pars["beta"]*((pars["Ep"]/0.1)*(pars["alpha"]-pars["beta"])/(pars["alpha"]+2))**(pars["alpha"]-pars["beta"])*np.exp(pars["beta"]-pars["alpha"]),
}
try:
checkParams(spectralParameterTemplates[spectralModel], pars,
self.logger)
except KeyError:
return
dNdE = []
try:
for energy in EnergyBins:
dNdE.append(spectralFunction[spectralModel](energy))
return dNdE
except KeyError:
self.logger.critical("No such model.")
