论文标题
星系光度在红移0.6至1.2的Chandra Deep Field South的功能
Galaxy luminosity functions at redshifts 0.6 to 1.2 in the Chandra Deep Field South
论文作者
论文摘要
我们介绍了RedShift范围z = 0.6-1.2，我们介绍了静止框架超紫（UV）星系光度函数（LF）和光度密度（LD）测量值（150 nm）波长。 UV LF使用XMM-Newton光学监视器（XMM-OM），紫外线（160-400 nm）观测到Chandra Deep South的观测值，位于396平方米的Arcmin面积上。使用CDF的深紫外成像，我们在样品中鉴定了2500多个星系，具有微弱的UVW1（AB）极限24.5 mag。该样本以及包含红移信息的其他各种目录，用于计算两个红移垃圾箱中Galaxy UV LF的binned代表，0.6-0.8和0.8-1.2，具有150 nm静止型UV尺寸的150 nm REST -FRAME范围，与以前的研究相比，在类似的Redshifts中，在1-1.5磁磁体上均与以前的研究相比。 BINNED LF通过Schechter函数形式很好地描述了。使用最大样本型Schechter函数拟合到未链接的数据中，以获得UV Galaxy LF参数的最佳拟合值。我们发现特征幅度从z = 0.7到z = 1的0.8 mag亮了0.8 mag，这意味着这些红移之间的恒星形成活性的增加，如过去的研究所报道。与先前的z = 0.7的研究相比，我们对微弱端斜率-1.10+0.19-0.18的估计是在较浅的一侧，而Z = 1.0估计的-1.56+0.19-0.18值同意了先前的结果。
We present the rest-frame Ultra-Violet (UV) galaxy luminosity function (LF) and luminosity density (LD) measurements in the far-UV (150 nm) wavelength, in the redshift range z = 0.6 - 1.2. The UV LF is derived using XMM-Newton Optical Monitor (XMM-OM), ultraviolet (160 - 400 nm) observations of the Chandra Deep Field South, over an area of 396 sq. arcmin. Using the deep UV imaging of the CDFS, we identified more than 2500 galaxies in our sample with faint UVW1(AB) limit 24.5 mag. This sample along with various other catalogues containing redshift information, is used to calculate the binned representation of the galaxy UV LF in the two redshift bins 0.6 - 0.8 and 0.8 - 1.2, having a wide range of 150 nm rest-frame UV magnitudes, reaching 1 - 1.5 magnitudes fainter than previous studies at similar redshifts. The binned LF is described well by the Schechter function form. Using maximum-likelihood the Schechter function is fitted to the unbinned data to obtain the best-fit values of the the UV galaxy LF parameters. We find that characteristic magnitude brightens by 0.8 mag from z = 0.7 to z = 1, implying an increase in the star formation activity between these redshifts, as reported by past studies. Our estimate of the faint-end slope -1.10+0.19-0.18 is on the shallower side compared with previous studies at z = 0.7, whereas a value of -1.56+0.19-0.18 estimated for z = 1.0, agrees with previous results given the uncertainties.
