论文标题
探索$ \ rm {h}α$ -UV比和典型星系星系的爆发度之间的相关性
Exploring the Correlation between $\rm{H}α$-to-UV Ratio and Burstiness for Typical Star-forming Galaxies at $z\sim2$
论文作者
论文摘要
$ \ rm {h}α$ - to-uv光度比（$ l（\ rmhα）/l（\ rm uv）$）通常用于探测星形星系的SFHS，并且重要的是要对其对其他代理进行验证，这一点很重要。为了解决这个问题，我们对$σ_{\ rm {sfr}} $的解决分布进行统计分析，以及恒星年龄及其与全球测量的$ l（\ rmhα）/l（\ rmhα）/l（\ rm uv）$的相关性，用于两个310星级的$ 1.37 $ 1.37 <1.37 <1。 2.61 $由MOSDEF调查观察到。我们使用MOSDEF星系的多波带/3D-HST成像来构造$σ_ {\ rm {sfr}} $和恒星年龄地图。 We analyze the composite rest-frame far-UV spectra of a subsample of MOSDEF targets obtained by the Keck/LRIS, which includes 124 star-forming galaxies (MOSDEF-LRIS) at redshifts $1.4 < z < 2.6$, to examine the average stellar population properties, and the strength of age-sensitive FUV spectral features in bins of $L(\rm Hα)/L(\rm UV）$。我们的结果没有表明具有较高$ L（\ rmHα）/L（\ rm UV）$的单个星系$，基于$σ_ {\ rm {sfr}} $的分离分布的单个恒星形成星系的$σ_ {\ rm {sfr}} $的分布。我们将样品分离为低$ L（\ rmHα）/L（\ rm UV）$的子集。高$ l（\ rmhα）/l（\ rm UV）$子集平均表现出$ \ log [\ rm {age/yr}] $ = 8.0，与$ \ log [\ rm {age/yr}]相比仅以$2σ$级别。此外，我们发现SIIV $λ\ lambda1393，1402 $和civ $λ\ lambda1548，1550 $ p-cygni特征来自两个子样本之间的大型星星。
The $\rm{H}α$-to-UV luminosity ratio ($L(\rm Hα)/L(\rm UV)$) is often used to probe SFHs of star-forming galaxies and it is important to validate it against other proxies for burstiness. To address this issue, we present a statistical analysis of the resolved distribution of $Σ_{\rm{SFR}}$ as well as stellar age and their correlations with the globally measured $L(\rm Hα)/L(\rm UV)$ for a sample of 310 star-forming galaxies in two redshift bins of $1.37 < z < 1.70$ and $ 2.09 < z < 2.61$ observed by the MOSDEF survey. We use the multi-waveband CANDELS/3D-HST imaging of MOSDEF galaxies to construct $Σ_{\rm{SFR}}$ and stellar age maps. We analyze the composite rest-frame far-UV spectra of a subsample of MOSDEF targets obtained by the Keck/LRIS, which includes 124 star-forming galaxies (MOSDEF-LRIS) at redshifts $1.4 < z < 2.6$, to examine the average stellar population properties, and the strength of age-sensitive FUV spectral features in bins of $L(\rm Hα)/L(\rm UV)$. Our results show no significant evidence that individual galaxies with higher $L(\rm Hα)/L(\rm UV)$ are undergoing a burst of star formation based on the resolved distribution of $Σ_{\rm{SFR}}$ of individual star-forming galaxies. We segregate the sample into subsets with low and high $L(\rm Hα)/L(\rm UV)$. The high-$L(\rm Hα)/L(\rm UV)$ subset exhibits, on average, an age of $\log[\rm{Age/yr}]$ = 8.0, compared to $\log[\rm{Age/yr}]$ = 8.4 for the low-$L(\rm Hα)/L(\rm UV)$ galaxies, though the difference in age is significant at only the $2σ$ level. Furthermore, we find no variation in the strengths of Siiv$λ\lambda1393, 1402$ and Civ$λ\lambda1548, 1550$ P-Cygni features from massive stars between the two subsamples.
