论文标题
检测H2O和OH+在Z> 3中> 3热灰尘的星系
Detection of H2O and OH+ in z>3 Hot Dust-Obscured Galaxies
论文作者
论文摘要
在本文中，我们介绍了Z> 3热尘的星系（热狗）中H2O和OH+发射的检测。使用ALMA BAND-6观察两只热狗，我们在W0149+2350中检测到H2O（2_02-1_11），以及H2O（3_12-3_03）和W0410-0913中的多重OH+（1_1-0_1）。我们发现，这两个源都具有L_H2O的线亮度> 2.2x10^8 LSOL和L_H2O = 8.7x10^8 LSOL分别为W0149+2350和W0410-0913。 H2O线曲线与相邻CO（9-8）线所看到的线路相似，线宽为FWHM〜800-1000 km/s。但是，H2O发射似乎比CO（9-8）更紧凑。在W0410-0913的发射中检测到OH+，fWHM = 1000km/s，L_OH+ = 6.92x10^8 LSOL的线发光度。对于两种热狗而言，观察到的H2O线光度与IR发光度的比率与先前观察到的恒星形成星系和AGN一致。 W0410-0913的热狗和OH+/H2O线比的H2O/CO线比与文献中的发光AGN相当。明亮的H2O（2_02-1_11）和H2O（3_12-3_03）发射线可能是由于这些来源的高星形形成水平和发光AGN所致。在发射中的OH+的存在，以及在文献中观察到的热狗具有发光AGN的线比的一致，这表明AGN发射主要主导了这些星系的辐射输出。但是，需要进行后续多转变观察以更好地限制这些系统的属性。
In this paper we present the detection of H2O and OH+ emission in z>3 hot dust-obscured galaxies (Hot DOGs). Using ALMA Band-6 observations of two Hot DOGs, we have detected H2O(2_02-1_11) in W0149+2350, and H2O(3_12-3_03) and the multiplet OH+(1_1-0_1) in W0410-0913. We find that both sources have luminous H2O emission with line luminosities of L_H2O > 2.2x10^8 Lsol and L_H2O = 8.7x10^8 Lsol for W0149+2350 and W0410-0913, respectively. The H2O line profiles are similar to those seen for the neighbouring CO(9-8) line, with linewidths of FWHM ~ 800-1000 km/s. However, the H2O emission seems to be more compact than the CO(9-8). OH+ is detected in emission for W0410-0913, with a FWHM=1000km/s and a line luminosity of L_OH+ = 6.92x10^8 Lsol. The ratio of the observed H2O line luminosity over the IR luminosity, for both Hot DOGs, is consistent with previously observed star forming galaxies and AGN. The H2O/CO line ratio of both Hot DOGs and the OH+/H2O line ratio of W0410-0913 are comparable to those of luminous AGN in the literature. The bright H2O(2_02-1_11), and H2O(3_12-3_03) emission lines are likely due to the combined high star formation levels and luminous AGN in these sources. The presence of OH+ in emission, and the agreement of the observed line ratios of the Hot DOGs with luminous AGN in the literature, would suggest that the AGN emission is dominating the radiative output of these galaxies. However, followup multi-transition observations are needed to better constrain the properties of these systems.
