EXCITATION MECHANISMS FOR HCN(1–0) AND HCO+(1–0) IN GALAXIES FROM THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY-猫眼课题宝

DOI：

10.1088/0004-637x/814/1/39

发表时间：

2015-09

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

G. Privon;G. Privon;G. Privon;R. Herrero-Illana;A. S. Evans;A. S. Evans;K. Iwasawa;M. Pérez-Torres;L. Armus;T. Díaz-Santos;T. Díaz-Santos;Eric J. Murphy;S. Stierwalt;S. Aalto;J. Mazzarella;L. Barcos-Muñoz;H. J. Borish;H. Inami;D. Kim;E. Treister;J. Surace;S. Lord;John E. Conway;D. Frayer;A. Alberdi

我们提出了新的射电天文研究所（IRAM） 30米光谱观测到的~ 88 GHz波段，包括来自CCH的发射（N = 1→0）？>多元，HCN (J = 1→0)？>, hco + （j = 1→0）>, HNC (J = 1→0)？>，以获取来自大天文台全天lig调查（GOALS）的58个本地发光和超发光红外星系的样本。通过将我们新的IRAM数据与文献数据和斯皮策/IRS光谱相结合，我们研究了这些假定的致密气体示踪剂与活动星系核（agn）和恒星形成对每个系统中红外光度的相对贡献之间的对应关系。我们发现HCN（1-0）发射在agn主导的系统中增强(⟨？HCN (1 - 0) ' ？> / l hco + (1 - 0) ' ？>⟩= 1.84 ？>)，与复合和星暴主导的系统(⟨？HCN (1 - 0) ' ？> / l hco + (1 - 0) ' ？>⟩= 1.14,？>和0.88)。然而，一些复合系统和星暴系统具有L HCN (1 - 0) ' ？> / l hco + (1 - 0) ' ？>比值与agn相当，表明HCN发射增强并不仅仅与能量优势agn相关。在从样本中去除agn主导的系统后，我们发现log10(L HCN (1 - 0) ' ？>)和log10(lir)，与之前的研究结果一致。L HCN (1 - 0) ' ？> /L IR通常被解释为致密气体耗尽时间，对于我们的发光和超发光红外星系样品，它似乎与L IR没有系统的趋势，并且具有显著的散射。星系积分L HCN (1 - 0) ' ？>和L HCO + (1 - 0) ' ？>的发射似乎不能简单地解释AGN的优势或恒星形成速率，而可能是由多种过程决定的，包括密度和辐射效应。

We present new Institut de Radioastronomie Millimétrique (IRAM) 30 m spectroscopic observations of the ∼88 GHz band, including emission from the CCH ( N = 1 → 0 ) ?> multiplet, HCN ( J = 1 → 0 ) ?> , HCO + ( J = 1 → 0 ) ?> , and HNC ( J = 1 → 0 ) ?> , for a sample of 58 local luminous and ultraluminous infrared galaxies from the Great Observatories All-sky LIRG Survey (GOALS). By combining our new IRAM data with literature data and Spitzer/IRS spectroscopy, we study the correspondence between these putative tracers of dense gas and the relative contribution of active galactic nuclei (AGNs) and star formation to the mid-infrared luminosity of each system. We find the HCN (1–0) emission to be enhanced in AGN-dominated systems ( ⟨ ?> L HCN ( 1 – 0 ) ′ ?> / L HCO + ( 1 – 0 ) ′ ?> ⟩ = 1.84 ?> ), compared to composite and starburst-dominated systems ( ⟨ ?> L HCN ( 1 – 0 ) ′ ?> / L HCO + ( 1 – 0 ) ′ ?> ⟩ = 1.14 , ?> and 0.88, respectively). However, some composite and starburst systems have L HCN ( 1 – 0 ) ′ ?> / L HCO + ( 1 – 0 ) ′ ?> ratios comparable to those of AGNs, indicating that enhanced HCN emission is not uniquely associated with energetically dominant AGNs. After removing AGN-dominated systems from the sample, we find a linear relationship (within the uncertainties) between log10( L HCN ( 1 – 0 ) ′ ?> ) and log10(L IR), consistent with most previous findings. L HCN ( 1 – 0 ) ′ ?> /L IR, typically interpreted as the dense-gas depletion time, appears to have no systematic trend with L IR for our sample of luminous and ultraluminous infrared galaxies, and has significant scatter. The galaxy-integrated L HCN ( 1 – 0 ) ′ ?> and L HCO + ( 1 – 0 ) ′ ?> emission do not appear to have a simple interpretation in terms of the AGN dominance or the star formation rate, and are likely determined by multiple processes, including density and radiative effects.

EXCITATION MECHANISMS FOR HCN(1–0) AND HCO+(1–0) IN GALAXIES FROM THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY

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