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Interpreting Short Gamma Ray Burst Progenitor Kicks and Time Delays Using the Host Galaxy-Dark Matter Halo Connection
Cosmology and Nongalactic Astrophysics · Submitted 30 Jan 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim For the best-fitting velocity distribution, one in five sGRB progenitors receives a natal kick above 150 km/s, consistent with merging neutron star models but not with merging white dwarf binary models.
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The abstract, sentence by sentence
Nearly 20% of short gamma-ray bursts (sGRBs) have no observed host galaxies. Combining this finding with constraints on galaxies' dark matter halo potential wells gives strong limits on the natal kick velocity distribution for sGRB progenitors. For the best-fitting velocity distribution, one in five sGRB progenitors receives a natal kick above 150 km/s, consistent with merging neutron star models but not with merging white dwarf binary models. This progenitor model constraint is robust to a wide variety of systematic uncertainties, including the sGRB progenitor time-delay model, the Swift redshift sensitivity, and the shape of the natal kick velocity distribution. We also use constraints on the galaxy-halo connection to determine the host halo and host galaxy demographics for sGRBs, which match extremely well with available data. Most sGRBs are expected to occur in halos near 10^12 Msun and in galaxies near 5x10^10 Msun (L_*); unobserved faint and high-redshift host galaxies contribute a small minority of the observed hostless sGRB fraction. We find that sGRB redshift distributions and host galaxy stellar masses weakly constrain the progenitor time-delay model; the active vs. passive fraction of sGRB host galaxies may offer a stronger constraint. Finally, we discuss how searches for gravitational wave optical counterparts in the local Universe can reduce followup times using these findings.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Nearly 20% of short gamma-ray bursts (sGRBs) have no observed host galaxies. | background 0.81 | 0.25 | 0.04 | asserted 1.00 |
| s1 | Combining this finding with constraints on galaxies' dark matter halo potential wells gives strong limits on the natal kick velocity distribution for sGRB progenitors. | result 0.47 | 0.68 | 0.38 | asserted 1.00 |
| s2 | For the best-fitting velocity distribution, one in five sGRB progenitors receives a natal kick above 150 km/s, consistent with merging neutron star models but not with merging white dwarf binary models. | result 0.92 | 0.90 | 0.54 | asserted 0.79 |
| s3 | This progenitor model constraint is robust to a wide variety of systematic uncertainties, including the sGRB progenitor time-delay model, the Swift redshift sensitivity, and the shape of the natal kick velocity distribution. | result 0.71 | 0.84 | 0.18 | asserted 1.00 |
| s4 | We also use constraints on the galaxy-halo connection to determine the host halo and host galaxy demographics for sGRBs, which match extremely well with available data. | result 0.87 | 0.95 | 0.12 | asserted 1.00 |
| s5 | Most sGRBs are expected to occur in halos near 10^12 Msun and in galaxies near 5x10^10 Msun (L_*); unobserved faint and high-redshift host galaxies contribute a small minority of the observed hostless sGRB fraction. | result 0.99 | 0.88 | 0.13 | asserted 0.58 |
| s6 | We find that sGRB redshift distributions and host galaxy stellar masses weakly constrain the progenitor time-delay model; the active vs. passive fraction of sGRB host galaxies may offer a stronger constraint. | result 0.78 | 0.93 | 0.05 | hedged possibility 0.53 |
| s7 | Finally, we discuss how searches for gravitational wave optical counterparts in the local Universe can reduce followup times using these findings. | future work 0.99 | 0.32 | 0.03 | hedged possibility 0.49 |
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The paper
Original abstract
Nearly 20% of short gamma-ray bursts (sGRBs) have no observed host galaxies. Combining this finding with constraints on galaxies' dark matter halo potential wells gives strong limits on the natal kick velocity distribution for sGRB progenitors. For the best-fitting velocity distribution, one in five sGRB progenitors receives a natal kick above 150 km/s, consistent with merging neutron star models but not with merging white dwarf binary models. This progenitor model constraint is robust to a wide variety of systematic uncertainties, including the sGRB progenitor time-delay model, the Swift redshift sensitivity, and the shape of the natal kick velocity distribution. We also use constraints on the galaxy-halo connection to determine the host halo and host galaxy demographics for sGRBs, which match extremely well with available data. Most sGRBs are expected to occur in halos near 10^12 Msun and in galaxies near 5x10^10 Msun (L_*); unobserved faint and high-redshift host galaxies contribute a small minority of the observed hostless sGRB fraction. We find that sGRB redshift distributions and host galaxy stellar masses weakly constrain the progenitor time-delay model; the active vs. passive fraction of sGRB host galaxies may offer a stronger constraint. Finally, we discuss how searches for gravitational wave optical counterparts in the local Universe can reduce followup times using these findings.
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References
How the literature uses it
4 arXiv papers cite this in 7 sentences
Papers citing it · 6 sentences without a confident label
Uses its data or values 1 paper
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Compact binaries are expected to receive large “natal kicks" due to asymmetries manifested by the mechanisms of NS/BH formation, resulting in mean velocities of $≈180$ km s$^-1$ for NS/NS binaries and $≈120$ km s$^-1$ for NS/BH binaries [ref] .
Diversity Of Short Gamma-Ray Burst Afterglows From Compact Binary Mergers Hosting Pulsars · Introduction · 0.87
What it cites · 10 sentences without a confident label
Uses data or values from 1 paper
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In this calculation, we have assumed the metallicity of stars formed at a given redshift tracks the gas-phase metallicity in [ref] , and have adopted a dust optical depth of $τ=0.1$ (calibrated to match CANDELS observations of the stellar mass – F160W relation from $z=0.6$ to $z≈6$, for $M_∗< 10^10$; [ref] ).
The Relation Between SFR and Stellar Mass for Galaxies at 3.5 $\le z\le$ 6.5 in CANDELS · Instrumental, Geometrical, and Observational Biases · 0.85
Cites as background 3 papers
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Finally, mergers which statistically trace the globular cluster distribution around galaxies [ref] would result in very different interpretations for the offsets than if mergers traced the galactic potential [ref] .
The Formation of Eccentric Compact Binary Inspirals and the Role of Gravitational Wave Emission in Binary-Single Stellar Encounters · Introduction · 0.86
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These include mergers of compact stellar remnants (i.e., combinations of neutron stars and black holes) via gravitational radiation, accretion-induced collapse of neutron stars, magnetar flaring, and magnetar formation through binary white dwarf mergers or white dwarf accretion-induced collapse [ref] .
Short-Duration Gamma-Ray Bursts · Introduction · 0.98
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Long gamma-ray bursts, with $T_90$ (the time for 90% of their photons to be received) greater than 2s, have been associated with Type Ic supernovae ( [ref] ; see also references in [ref] ).
The Host Galaxies of Long-Duration Gamma-Ray Bursts · Introduction · 0.87
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