snorer.event¶
snorer.event(mx,Rs,beta,Re=8.5,Tx_range=[5,30],
t_range=[10,1.1045e+09],sigxv0=1e-45,
is_spike=False,**kwargs)¶
The supernova-neutrino-boosted dark matter evnet per electron with DM-\(e\) cross section \(\sigma_{\chi e}\) normalized to 1 cm2 at Earth. The field-of-view \(d\Omega\) is integrated over entirely and the kinetic energy \(T_\chi\), exposure time \(t\) can be integrated within user-defined ranges. Precisely speaking, the event \(N_\chi\) is, using Eqs. (18) in BDM Physics,
and snorer.event
presumes \(N_e=1\) and \(\sigma_{\chi e}=1\) cm2.
One can restore the correct \(N_\chi^{\rm correct}\) for any detector by multiplying the true \(N_e^{\rm true}\) for that detector and \(\sigma_{\chi e}^{\rm true}\),
where we have set \(\sigma_{\chi \nu}=10^{-45}\) cm2 by default in the function.
mx
: float
Dark matter mass, MeV.
Rs
: floate
Distance from supernova to Earth, kpc.
beta
: floate
The off-center angle, characterizes how SN deviates from GC-Earth axis angularly, rad.
Re
: floate
The distance from GC to Earth, kpc. Default is 8.5 kpc.
Tx_range
: list
Integration range for BDM kinetic energy[Tx_min,Tx_max]
, MeV
t_range
: list
Integration range for exposure time[t_min,t_max]
, seconds
sigxv0
: float*
Total DM-\(\nu\) cross section, cm2. It will be multiplied by snorer.get_gx to account for the angular distribution and makes it cm2 sr−1.
is_spike
: bool
Is halo spike included? Default isFalse
.
**kwargs
Keyword arguments for characteristic parameters of NFW profile and spike halo, . Ifis_spike = False
, the parameters for configuring spiky halo will be deactivated. Default values assume Milky Way. See default arguments insnorer.params.min_distance
,snorer.params.halo
,snorer.params.spike
andsnorer.params.vegas
.
out
: scalar
Event number of supernova-neutrino-boosted dark matter per electron.
We also use vegas to evaluate \(N_\chi\). See Notes in snorer.flux
.