###############OFF-AXIS GRB MODEL#############################

off-axis GRB models taken from the online repository
by van Eerten http://cosmo.nyu.edu/afterglowlibrary/index.html

LONG GRB
broadbandnu1.00e14obs0d30.txt
broadbandnu1.00e14obs0d60.txt

Off-axis models that are good to represent the case of a long bright
GRB: dataset ''broad-band long GRBs in ISM'', which corresponds to a
GRB of jet energy 2e51 erg, expanding in a uniform ISM medium of
density 1 cm^-3, select a frequency of 1e14 Hz (the closest to the
R-band central frequency among the ones available in this repository),
and an off-axis observer angle of 0.30 rad and 0.60 rad. The simulated
dataset has an assumed GRB opening angle of 0.2 rad.  The dataset
gives time in day, and fluxes in mJy at a distance of 1e28 cm.

LONG LOW-LUMINOSITY GRB (or BRIGHT SHORT GRB)  

sgrbEjets1e50n1thetajet0d2opticaltheta0d40.txt
sgrbEjets1e50n1thetajet0d2opticaltheta0d80.txt

Off-axis models that is good to represent the case of a long
low-luminosity GRB: dataset ''broad-band and off-axis low-energy
GRBs'', which select select a GRB of jet energy 1e50 erg, a uniform
ISM medium of density 1 cm^-3, a jet angle of 0.2rad, a frequency of
4.56e14 Hz (for R-band), and an off-axis observer's angle of 0.40 rad
and 0.80 rad.  The dataset gives time in day, and fluxes in mJy at a
distance of 1e28 cm.

SHORT GRB 
sgrbEjets1e50n1e-3thetajet0d2opticaltheta0d40.txt
sgrbEjets1e50n1e-3thetajet0d2opticaltheta0d80.txt

Off-axis models that is good to represent the case of a short GRB:
dataset ''broad-band and off-axis low-energy GRBs'' in the online
repository select a GRB of jet energy 1e50 erg, select a uniform ISM
medium of density 1e-3 cm^-3, select a frequency of 4.56e14 Hz (for
R-band), a jet angle of 0.2 rad, and an off-axis observer's angle of
0.40 rad and 0.8 rad. The dataset gives time in day, anf fluxes in mJy
at a distance of 1e28 cm.

130603B_2thj_r.txt
130603B_4thj_rSDSS.txt

Off-axis models which use the intrinsic estimated properties of the 
on-axis GRB 130603B (Stratta et al. in prep) for an obsever angle twice
the beaming angle and 4 times the beaming angle.

###############KILONOVA MODEL##########################
BB_R_1e-2.dat
Fe_R_1e-2.dat

The kilonova models by Metzger et al. 2010, BB_R_1e-2.dat assumes a blackbody emission and an ejecta mass 10^-2Mo and outflow speed v= 0.1c. Fe_R_1e-2.dat thermalization efficiency = 1, iron opacity. 

NS14_14.txt 
BH14_NS14.txt 

The kilonova models by Piran et al. 2013 
Approximation that all the bolometric luminosity goes in R band assuming a NS-NS merger with NS=1.4Mo and BH-NS merger with NS=1.4Mo and BH mass of 10Mo. 
Barnes & Kasen (2013), assuming low velocity 0.1 c and low mass 10^-3Mo ejecta. 

lv_l.dat
Barnes & Kasen (2013), for the case of low-velocity (0.1 c) and low-mass (M = 10^-3 Mo) ejecta, lanthanides opacity

Kasen15_t0.dat
Kilonova model by Kasen, Fernandez & Metzger 2015 (r band). In the file day, nu L_nu / 1e40  erg/s, model which considers that the BNS directly collapses in a BH

%Kasen15_t100.dat
%kilonova model by Kasen, Fernandez & Metzger 2015 (r band). In the file day, nu L_nu / %1e40  erg/s, model which considers that the BNS gives rise to an hypermassive NS which %survives for 100 ms before collapsing into a BH

Kasen15_tinf.dat 
kilonova model by Kasen, Fernandez & Metzger 2015 (r band). In the file day, nu L_nu / 1e40  erg/s, model which considers that the BNS gives rise to a NS surviving for t=inf