This is the online material accompanying the paper: 'Double neutron stars: merger rates revisited' by Chruslinska et al. (2018) For the description of the models please refer to the paper: https://ui.adsabs.harvard.edu/abs/2018MNRAS.474.2937C (Section 3 and Table 1). _________________________________________________________________________ Additional information: The models available on this site (full description in the paper): reference - standard StarTrack assumptions about the evolution up to ~2018 (described e.g. in Belczynski et al. 2016 https://ui.adsabs.harvard.edu/abs/2016Natur.534..512B/abstract) EC - as reference, but with wider range of the core masses at the beginning of the AGB stage that can lead to electron-capture supernova (ECS; NS forming in ECS are assumed to receive zero natal kick) BE1 - as reference, but CCSN natal kick magnitudes are assigned following Bray&Eldridge (2016) J1 - as reference, but with extreme angular momentum loss during the mass transfer with a non-degenerate accretor (j_loss=5 while in ref j_loss=1; see eq. 3 in the paper). J2 - as reference, but lower angular momentum loss during the mass transfer with a non-degenerate accretor (j_loss=0.2 while in ref j_loss=1; see eq. 3 in the paper). J5 - as reference, but assuming a fully conservative mass transfer with a non-degenerate accretor (ref: half conservative) NK2 - as reference, but modified distribution for the natal kicks - equal probability that the natal kick comes from a flat distribution at <50 km/s and Hobbs et al. (2005) at >50 km/s C - combined assumptions that favor the formation of double neutron stars; as in reference but with wider range of the core masses that can lead to electron-capture supernova (model EC), natal kicks following the CCSN assigned following Bray&Eldridge (2016) (model BE1) and lower angular momentum loss during the stable mass transfer with non-degenerate accretor (model J2). C+P - as in C but forcing thermal mass transfer instead of CE with HG donor and NS/BH accretor The distributions of initial binary parameters in the simulated models are based on Sana et al. (2012) and a Kroupa-like broken power-law IMF with the high-mass exponent of 2.3, used for the mass of the primary component. The number of simulated ZAMS binaries (Nsim) per metallicity in a given model: reference: 2*10^7 EC - 2*10^7 BE1 - 2*10^7 J1 - 2*10^7 J2 - 2*10^7 J5 - 2*10^7 C - 2*10^6 C+P - 2*10^6 NK2 - 2*10^6 The total mass of the simulations (Msim): This is the total mass of stars from the whole IMF mass range 0.08-150 Msun that would be created in order to obtain the simulated number of ZAMS binaries which were chosen from a narrower mass range (4 < Ma < 150 Msun for the primary and from 0.08 < Mb < 150 Msun for the secondary), assuming a particular IMF for the mass of the primary star, primordial mass ratio distribution and the binary fraction (fbin). Assuming fbin=1 in the entire mass range, Msim is ~1.14*10^9 Msun for the models with Nsim = 2*10^7 and ~1.13*10^8 Msun for the models with Nsim = 2*10^6. The data for the models: reference, C, C+P and NK2 were also used in Chruslinska, Nelemans & Belczynski (2019): https://ui.adsabs.harvard.edu/abs/2019MNRAS.482.5012C/abstract Note that the pair-instability pulsation supernovae (PPSN) and pair-instability supernovae (PSN) were not included in the calculations. This affects the maximum mass of BH forming in the simulations (see https://ui.adsabs.harvard.edu/abs/2016A%26A...594A..97B/abstract), but has no effect on the results concerning NS. __________________________________________________________________________ DESCRIPTION OF THE DATA (also contained within the downloadable archives): ARCHIVES: NAME: [model].tar.gz where the model specifies the set of assumptions about the evolution and formation of stars used in the simulations. Those models are described in the paper: https://ui.adsabs.harvard.edu/abs/2018MNRAS.474.2937C/abstract (Section 3 and Table 1). The names of the models are the same as in the paper. STRUCTURE: each [model].tar.gz contains three directories: NSNS, BHBH, BHNS Those directories contain the data for the systems which evolved into double compact objects of the type specified by their names. Each of those directories contains two sub-directories: B and HG_CE 'B' contains only binaries which did not evolve through the common envelope with the Hertzsprung Gap donors (sub model B from the paper) 'HG_CE' contains the binaries that evolved through the common envelope with the Hertzsprung Gap donors. FILES: FILE NAMES: [model]_[ZZ]_[HG CE treatment]_[DCO type].dat [model] - specific set of the assumptions about the evolution and formation of stars used in the simulations. [ZZ] - metallicity at which the stars were assumed to form; ZZ='02' corresponds to metallicity Z=0.02 (the assumed solar value), ZZ=002 to Z=0.002 etc. [HG CE treatment] - specifies whether the systems evolved through the common envelope with the Hertzsprung Gap donors (HG_CE) or not (B). Files with [HG CE treatment]=B correspond to sub-model 'B' discussed in the paper; sub-model 'A' can be recovered by combining the data from the files with [HG CE treatment]=B and [HG CE treatment]=HG_CE for the same model and metallicity. [DCO type] - type of double compact object (NSNS, BHBH or BHNS); files with DCO type = NSNS contain the data for the systems which evolved into double neutron stars only. STRUCTURE: Each line in each of the files corresponds to one system (binary that successfully evolved into a double compact object) The format of the lines is as follows: Ma Mb a e per Mchirp tdel tmer tms Vsm0,x Vsm0,y Vsm0,z Vsm,x Vsm,y Vsm,z ECSA ECSB Mzamsa Mzamsb a0 e0 k evol_hist - Ma is the mass of the stellar remnant from the primary star - initially (at Zero Age Main Sequence - ZAMS) more massive, in the units of Msun. - Mb is the mass of the stellar remnant from the primary star - initially (at ZAMS) less massive, in the units of Msun. - a is the semi-major axis of the system at the formation of the second compact object (supernova included) in units of Rsun. - e is the eccentricity of the system at the formation of the second compact object (supernova included). - per is the orbital period at the formation of the second compact object (supernova included) in days. - Mchirp is the chirp mass of the DCO system, in units of Msun. - tdel is the delay time of the DCO system, in units of Myr. The delay times is the sum of: the time to the formation of the last compact object measured from ZAMS, and the time to merger measured from the formation of the last compact object. - tmer is the merger time of the DCO system in units of Myr. It is measured from the formation of the second compact object until the merger. - tms is the time between supernova explosions in units of Myr. - Vsm0,i are the components of the velocity, of the center of mass after the first supernova. Units are Rsun day-1. - Vsm,i are the components of the velocity, of the center of mass after the second supernova. Units are Rsun day-1. - ECSA specifies whether the primary star underwent the electron-capture SN (ECS; 1-ECS; 0-no ECS) - ECSB specifies whether the secondary star underwent the electron-capture SN (ECS; 1-ECS; 0-no ECS) - Mzamsa is the initial mass of the primary component, in units of Msun. - Mzamsb is the initial mass of the secondary component, in units of Msun. - a0 is the initial (at ZAMS) separation (semi-major axis) of the components, in units of in units of Rsun. - e0 is the initial (at ZAMS) eccentricity of the binary. - k is an integer number of following string in the line, describing the evolutionary history of the system. - evol_hist is the evolutionary history of the system, presented in k number of strings. For example, a system with only two supernovae in its history will have the follwing k and evol_hist in its line: 2 SN1 SN2. EVOL_HIST - ADDITIONAL EXPLENATION: The list of events (strings) used by StarTrack to describe evolutionary history: MTx - stands for nonconservative mass transfer through Roche lobe overflow. "x" indicates the relative component: 1-primary, 2-secondary. SNx - stands for a supernovae explosion. CEx(a0-b0:a1-b1) - stands for a common envelope events. "x" indicates the donor star: 1-primary, 2-secondary or 12-both components are donors. "a0-b0" are integer numbers indicating stellar types (explained below) of the primary-secondary components, respectively, at the start of the CE. Analogously "a1-b1" indicate stellar types at the outcome of the CE. For example "CE2(14-2:14-7)" means that a CE was initiated by the secondary component ("CE2"), which was a Hertzsprung gap star ("-2:"), onto the primary, which was a black hole ("14-"). In the outcome, the secondary ejected its hydrogen envelope and became a Wolf-Rayet star ("-7"), while the primary remained a black hole (":14-"). AICtypex indicates an accretion induced core collapse. "type" describes the compact object to which the progenitor has collapsed and "x" - the relevant component: 1-primary, 2-secondary. For example "AICNS1" means that the accreting primary star ("1") has collapsed into a neutron star ("NS"). List of stellar types: 0 - main sequence star with M<=0.7 M☉ (deeply or fully convective) 1 - main sequence star with M>0.7 M☉ 2 - Hertzsprung gap star 3 - first giant brach star 4 - core helium burning star 5 - early asymptotic giant branch star 6 - thermally pulsing asymptotic giant branch star 7 - main sequence naked helium star (Wolf-Rayet star) 8 - Hertzsprung gap naked helium star 9 - giant branch naked helium star 10 - helium white dwarf 11 - carbon/oxygen white dwarf 12 - oxygen/neon white dwarf 13 - neutron star 14 - black hole