J-PLUS：揭开1000度范围内2.0<z<3.3时Lyα光度函数最亮端的面纱^2
J-PLUS: Unveiling the brightest-end of the Lyα luminosity function at 2.0<z<3.3 over 1000 deg^2
摘要：
在2.2<z<3.3的范围内，用光度计测定了Lya光度函数（LF）的亮端（LLya> 1043.5erg/s）。我们的工作是基于Javalambre测光局部宇宙巡天（J-PLUS）的首次数据发布，该数据提供了超过1000度^2的多个窄带测量，极限星等r~22。在如此广阔的区域内分析高z Lya发射源是前所未有的，并且允许选择总共约14，500个超亮（L_Lya>10^43.3 erg/s）Lya发射候选者。我们在GTC望远镜上用两个光谱跟踪程序测试了我们的选择，确认了约89%的目标是线发射源，其中约64%是真正的z~2.2类星体。我们首次将2.2<z<3.3 Lya的LF扩展到L_Lya~10^44 erg/s以上，密度降到~10^-8 Mpc^-3。我们的研究结果揭示了Lya LF最亮端的Schechter指数衰减的高度细节，补充了先前LF测定的43.3<Log_10（L_Lya / [erg/s]）<44的幂律分量。我们测量到φ ^*=（3.33+-0.19 x 10 ^-6），Log（L^*）=44.65+-0.65，α =-1.35+-0.84，作为我们探测的红移的平均值。这些值是显着不同的典型Schechter参数测量的Lya LF的高Z恒星形成LAEs。这表明z>2的活动星系核/类星体（在我们的样本中可能占主导地位）由结构上不同于z>2的恒星形成LAE的LF描述，即L^*_类星体约为100 L^*_LAE，而Phi^*_类星体约为10^-3 Phi^*_LAE。最后，我们的方法非常有效地识别出高z线发射源，而无需先前的光谱确认，目前被分类为恒星（平均每个红移仓中有约2000个物体）。假设在我们的样本中，发射Lya的活动星系核/类星体占很大的优势，这就支持了这样一种假设：在Lya>10^43.3 erg/s时，这些活动星系核/类星体是z>2的Lya发射体中最丰富的一类。
英文摘要：
We present the photometric determination of the bright-end (L_Lya>10^43.5 erg/s) of the Lya luminosity function (LF) within four redshifts windows in the interval 2.2<z<3.3. Our work is based on the Javalambre Photometric Local Universe Survey (J-PLUS) first data-release, which provides multiple narrow-band measurements over ~1000 deg^2, with limiting magnitude r~22. The analysis of high-z Lya-emitting sources over such a wide area is unprecedented, and allows to select a total of ~14,500 hyper-bright (L_Lya>10^43.3 erg/s) Lya-emitting candidates. We test our selection with two spectroscopic follow-up programs at the GTC telescope, confirming ~89% of the targets as line-emitting sources, with ~64% being genuine z~2.2 QSOs. We extend the 2.2<z<3.3 Lya LF for the first time above L_Lya~10^44 erg/s and down to densities of ~10^-8 Mpc^-3. Our results unveil with high detail the Schechter exponential-decay of the brightest-end of the Lya LF, complementing the power-law component of previous LF determinations at 43.3<Log_10(L_Lya / [erg/s])<44. We measure Phi^*=(3.33+-0.19)x10^-6, Log(L^*)=44.65+-0.65 and alpha=-1.35+-0.84 as an average over the redshifts we probe. These values are significantly different than the typical Schechter parameters measured for the Lya LF of high-z star-forming LAEs. This suggests that z>2 AGN/QSOs (likely dominant in our samples) are described by a structurally different LF than z>2 star-forming LAEs, namely with L^*_QSOs ~ 100 L^*_LAEs and Phi^*_QSOs ~ 10^-3 Phi^*_LAEs. Finally, our method identifies very efficiently as high-z line-emitters sources without previous spectroscopic confirmation, currently classified as stars (~2000 objects in each redshift bin, on average). Assuming a large predominance of Lya-emitting AGN/QSOs in our samples, this supports the scenario by which these are the most abundant class of z>2 Lya emitters at L_Lya>10^43.3 erg/s.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
