Powered by OpenAIRE graph
Found an issue? Give us feedback
image/svg+xml art designer at PLoS, modified by Wikipedia users Nina, Beao, JakobVoss, and AnonMoos Open Access logo, converted into svg, designed by PLoS. This version with transparent background. http://commons.wikimedia.org/wiki/File:Open_Access_logo_PLoS_white.svg art designer at PLoS, modified by Wikipedia users Nina, Beao, JakobVoss, and AnonMoos http://www.plos.org/ ZENODOarrow_drop_down
image/svg+xml art designer at PLoS, modified by Wikipedia users Nina, Beao, JakobVoss, and AnonMoos Open Access logo, converted into svg, designed by PLoS. This version with transparent background. http://commons.wikimedia.org/wiki/File:Open_Access_logo_PLoS_white.svg art designer at PLoS, modified by Wikipedia users Nina, Beao, JakobVoss, and AnonMoos http://www.plos.org/
ZENODO
Dataset . 2024
Data sources: ZENODO
ZENODO
Dataset . 2024
Data sources: Datacite
ZENODO
Dataset . 2024
Data sources: Datacite
versions View all 2 versions
addClaim

Data release for "Consistent eccentricities for gravitational wave astronomy: Resolving discrepancies between astrophysical simulations and waveform models"

Authors: Vijaykumar, Aditya; Hanselman, Alexandra G.; Zevin, Michael;

Data release for "Consistent eccentricities for gravitational wave astronomy: Resolving discrepancies between astrophysical simulations and waveform models"

Abstract

This is a data release to accompany arXiv:2402.07892 "Consistent eccentricities for gravitational wave astronomy: Resolving discrepancies between astrophysical simulations and waveform models". See also https://zenodo.org/doi/10.5281/zenodo.10974974. Please cite the paper (https://ui.adsabs.harvard.edu/abs/2024arXiv240207892V/abstract) if you use this in a publication or any other scientific work. The file can be read in using```import pandas data = pandas.read_hdf("CMC_eccentricities_standardized.hdf5")```The description of the different keys in the file are as follows:- `m1`: source-frame mass of the primary object in the binary in units of Msun- `m2`: source-frame mass of the secondary object in the binary in units of Msun- `chi1`: dimensionless spin of the primary object in the binary- `chi2`: dimensionless spin of the secondary object in the binary- `z`: cosmological redshift- `a0`: Initial separation in AU. This typically corresponds to the stopping criterion in astrophysical simulations.- `e0`: The eccentricity at the initial separation `a0`- `f0`: 22 mode frequency corresponding to the initial separation.- `channel`: Takes values between 1 and 5. - 1: Ejected mergers - 2: In-cluster (two-body) mergers - 3: Binary-Single Encounters - 4: Binary-Binary Encounters - 5: Single-Single Encounters- `cluster_weight`: Weight given to each binary based on cluster properties (mass and metallicity), assuming some initial mass function for the cluster and metallicity evolution as a function of redshift.- `cosmo_weight`: Weight given to each binary based on the redshift, to account for cosmological volume.- `e_W03_*Hz`: Eccentricities extracted from the Wen 2003 prescription at the reference peak frequency specified.- `e_t_2PN_10Hz`: Eccentricities extracted from the prescription in Vijaykumar et. al. 2024 at reference 22 mode frequency of 10 Hz. - `e_t_2PN_Mf_1000HzMsun`: Eccentricities extracted from the prescription in Vijaykumar et. al. 2024 at reference 22 mode frequency corresponding to `M \times f = 1000 Hz Msun`. This ensures that eccentricity is defined at a fixed number of cycles before merger, independent of the cosmological redshift. We strongly recommend that all eccentricity estimates from astrophysical simulations are quoted at a reference frequency corresponding to fixed `M \times f`.- `total_weight`: `cosmo_weight \times cluster_weight`NOTE: For mergers belonging to `channel=1`, we straightaway set the `e_t_*` estimates to zero. This is because mergers from this channel will not be eccentric at `f>10 Hz`, and due to its large initial separation is computationally intensive to evolve using the PN evolution equations.

  • BIP!
    Impact byBIP!
    selected citations
    These citations are derived from selected sources.
    This is an alternative to the "Influence" indicator, which also reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).
    1
    popularity
    This indicator reflects the "current" impact/attention (the "hype") of an article in the research community at large, based on the underlying citation network.
    Average
    influence
    This indicator reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).
    Average
    impulse
    This indicator reflects the initial momentum of an article directly after its publication, based on the underlying citation network.
    Average
Powered by OpenAIRE graph
Found an issue? Give us feedback
selected citations
These citations are derived from selected sources.
This is an alternative to the "Influence" indicator, which also reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).
BIP!Citations provided by BIP!
popularity
This indicator reflects the "current" impact/attention (the "hype") of an article in the research community at large, based on the underlying citation network.
BIP!Popularity provided by BIP!
influence
This indicator reflects the overall/total impact of an article in the research community at large, based on the underlying citation network (diachronically).
BIP!Influence provided by BIP!
impulse
This indicator reflects the initial momentum of an article directly after its publication, based on the underlying citation network.
BIP!Impulse provided by BIP!
1
Average
Average
Average
Related to Research communities