z~3恒星形成活动的多波长观测
A Multi-wavelength View of the Star Formation Activity at z~3
摘要：
我们提出了一个多波长，紫外到无线电分析的样品大规模（M $_{\ast}$ $\sim$ 10 $^{10}$ M $_\odot$）IRAC和MIPS 24 $μ$ m-检测莱曼Break Galerkin（LBG）的光谱红移z $\sim$ 3在GOODS北场（L $_{\rm UV}$ $>1.8\times$ L $^{\ast}_{z=3}$）。对于没有单独的24 $μ$ m检测的LBG，我们采用24 $μ$ m，1.1mm和1.4GHz的堆叠技术，构造平均紫外-射电光谱能量分布，并发现它与一个亮红外星系（LIRG）的能量分布一致，该星系的L $\rm_{IR}$ =4.5 $^{+1.1}_{-2.3}$ $\times 10^{11}$ L $_{\odot}$和特定的恒星形成率（SSFR）4.3 Gyr $^{-1}$，对应于质量倍增时间$\sim$ 230 Myrs。另一方面，当考虑24个$μ$ m探测到的LBG时，我们发现其中有L $\rm_{IR}> 10^{12}$ L $_{\odot}$的星系，这表明$z\sim$ 3紫外选择超亮红外星系（ULIRGs）的空间密度为$\sim$（1.5 $\pm$ 0.5）$\times 10^{-5}$ Mpc $^{-3}$。我们比较测量的恒星形成率（SFR）的数据在不同的波长，发现有紧密的相关性（肯德尔的$τ>$ 99.7%）和良好的协议之间的值来自尘埃校正的紫外线，中红外，毫米和无线电数据的整个范围的L $\rm_{IR}$到L $\rm_{IR}$ $\sim$ 10 $^{13}$ L $_{\odot}$。这个范围是大于相关性是已知的，以保持在z $\sim$ 2，可能是由于缺乏显着的贡献，从多环芳烃的24 $μ$ m流量在$z\sim$ 3。事实上，这一协议是观察星系与L $\rm_{IR}$ $>$ 10 $^{12}$ L $_{\odot}$表明，恒星形成的紫外选择ULIRGs，以及大部分的恒星形成活动在这个红移，是不是嵌入在光学厚的地区所看到的本地ULIRGs和亚毫米选择星系在$z=2$。
英文摘要：
We present a multi-wavelength, UV-to-radio analysis for a sample of massive (M$_{\ast}$ $\sim$ 10$^{10}$ M$_\odot$) IRAC- and MIPS 24$μ$m-detected Lyman Break Galaxies (LBGs) with spectroscopic redshifts z$\sim$3 in the GOODS-North field (L$_{\rm UV}$$>1.8\times$L$^{\ast}_{z=3}$). For LBGs without individual 24$μ$m detections, we employ stacking techniques at 24$μ$m, 1.1mm and 1.4GHz, to construct the average UV-to-radio spectral energy distribution and find it to be consistent with that of a Luminous Infrared Galaxy (LIRG) with L$\rm_{IR}$=4.5$^{+1.1}_{-2.3}$$\times 10^{11}$ L$_{\odot}$ and a specific star formation rate (SSFR) of 4.3 Gyr$^{-1}$ that corresponds to a mass doubling time $\sim$230 Myrs. On the other hand, when considering the 24$μ$m-detected LBGs we find among them galaxies with L$\rm_{IR}> 10^{12}$ L$_{\odot}$, indicating that the space density of $z\sim$3 UV-selected Ultra-luminous Infrared Galaxies (ULIRGs) is $\sim$(1.5$\pm$0.5)$\times 10^{-5}$ Mpc$^{-3}$. We compare measurements of star formation rates (SFRs) from data at different wavelengths and find that there is tight correlation (Kendall's $τ>$ 99.7%) and excellent agreement between the values derived from dust-corrected UV, mid-IR, mm and radio data for the whole range of L$\rm_{IR}$ up to L$\rm_{IR}$ $\sim$ 10$^{13}$ L$_{\odot}$. This range is greater than that for which the correlation is known to hold at z$\sim$2, possibly due to the lack of significant contribution from PAHs to the 24$μ$m flux at $z\sim$3. The fact that this agreement is observed for galaxies with L$\rm_{IR}$ $>$ 10$^{12}$ L$_{\odot}$ suggests that star-formation in UV-selected ULIRGs, as well as the bulk of star-formation activity at this redshift, is not embedded in optically thick regions as seen in local ULIRGs and submillimeter-selected galaxies at $z=2$.
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