论文标题
$ z <0.5 $的短期GRB的延迟无线电调查：中子星合并残留的新约束
A Late-time Radio Survey of Short GRBs at $z<0.5$: New Constraints on the Remnants of Neutron Star Mergers
论文作者
论文摘要
由于二进制中子星（BNS）合并而产生的大量，快速旋转的磁铁残留物可能会将其能量的一小部分沉积到周围的Kilonova弹出中，从而从射流与Circumburst培养基的相互作用中为同步射电信号提供动力。我们向6.0 GHz提出了非常大的阵列（VLA）观察结果，记录了9次，低红色的短伽马射线爆发（SGRBS; $ z <0.5 $）在$ \ 2.4-13.9 $ yr之后的REST-FRAME TIMESCALES上，yr the Burss爆发后。我们将$3σ$限制在$f_ν\ lyssim6-20 \，μ$ jy的无线电连续限制处在爆发位置，或$l_ν\ sillesim（0.6-8.3）\ times10^{28} $ erg s $ erg s $^s $^{-1} $ hz $ hz $^{ - 1} $ hz $^{ - 1} $。将这些限制与适当结合相对论效果的新的光曲线建模进行比较，我们获得了沉积在$ e_ {ej {ej} \ sillesim（0.6-6.7）\ times 10^{52} {52} $ erg（$ e_ {$ ej} \ silysim（ej} \ sims for）的能量限制$ 0.03 \，m _ {\ odot} $（$ 0.1 \，m _ {\ odot} $）。我们提出了27个SGRB的统一重新分析，$ 5.5-6.0 $ GHz观察结果，发现SGRB的$ \ gtrsim50 \％$并未在其合并中形成稳定的磁性残余物。假设SGRB是由BNS合并从银河BNS人口绘制的BNS合并产生的，以及在分数$ f_ {GW190425} $中的高质量GW194025的附加成分$ m_ {tov} \ sillsim2.23 \，m _ {\ odot} $ for $ f_ {gw190425} = 0.4 $;对于$ f_ {gw190425} $的较大值，此限制会增加。在不预定的调查（例如VLA Sky Survey（Vlass））中，对无线电残留物的检测（或缺乏）可以对产生稳定残余物的合并分数提供更严格的限制。如果在Vlass中发现了$ \ gtrsim30-300 $无线电残留物，则表明SGRB是偏见的BNS合并，就其产生的残留物的稳定性而言。
Massive, rapidly-spinning magnetar remnants produced as a result of binary neutron star (BNS) mergers may deposit a fraction of their energy into the surrounding kilonova ejecta, powering a synchrotron radio signal from the interaction of the ejecta with the circumburst medium. We present 6.0 GHz Very Large Array (VLA) observations of nine, low-redshift short gamma-ray bursts (SGRBs; $z<0.5$) on rest-frame timescales of $\approx2.4-13.9$ yr following the bursts. We place $3σ$ limits on radio continuum emission of $F_ν\lesssim6-20\,μ$Jy at the burst positions, or $L_ν\lesssim(0.6-8.3)\times10^{28}$erg s$^{-1}$Hz$^{-1}$. Comparing these limits with new light curve modeling which properly incorporates relativistic effects, we obtain limits on the energy deposited into the ejecta of $E_{ej}\lesssim(0.6-6.7)\times 10^{52}$erg ($E_{ej}\lesssim(1.8-17.6)\times10^{52}$erg) for an ejecta mass of $0.03\,M_{\odot}$ ($0.1\,M_{\odot}$). We present a uniform re-analysis of 27 SGRBs with $5.5-6.0$ GHz observations, and find that $\gtrsim50\%$ of SGRBs did not form stable magnetar remnants in their mergers. Assuming SGRBs are produced by BNS mergers drawn from the Galactic BNS population plus an additional component of high-mass GW194025-like mergers in a fraction $f_{GW190425}$ of cases, we place constraints on the maximum mass of a non-rotating neutron star (NS) ($M_{TOV}$), finding $M_{TOV}\lesssim2.23\,M_{\odot}$ for $f_{GW190425}=0.4$; this limit increases for larger values of $f_{GW190425}$. The detection (or lack thereof) of radio remnants in untargeted surveys such as the VLA Sky Survey (VLASS) could provide more stringent constraints on the fraction of mergers that produce stable remnants. If $\gtrsim30-300$ radio remnants are discovered in VLASS, this suggests that SGRBs are a biased population of BNS mergers in terms of the stability of the remnants they produce.
