ALMA 26 arcmin(2) Survey of GOODS-S at One-millimeter (ASAGAO): X-Ray AGN Properties of Millimeter-selected Galaxies

作者：Ueda Y; Hatsukade B; Kohno K; Yamaguchi Y; Tamura Y; Umehata H; Akiyama M; Ao Y; Aretxaga I; Caputi K; Dunlop J S; Espada D; Fujimoto S; Hayatsu N H; Imanishi M; Inoue A K; Ivison R J; Kodama T; Lee M M; Matsuoka K; Miyaji T; Morokuma Matsui K; Nagao T; Nakanishi K; Nyland K; Ohta K; Ouchi M; Rujopakarn W; Saito T; Tadaki K; Tanaka I; Taniguchi Y; Wang T; Wang W H; Yoshimura Y; Yun M S

来源：Astrophysical Journal, 2018, 853(1): 24.

DOI：10.3847/1538-4357/aa9f10

<jats:title>Abstract</jats:title>
<jats:p>We investigate the X-ray active galactic nucleus (AGN) properties of millimeter galaxies in the Great Observatories Origins Deep Survey South (GOODS-S) field detected with the Atacama Large Millimeter/submillimeter Array (ALMA), by utilizing the <jats:italic>Chandra</jats:italic> 7-Ms data, the deepest X-ray survey to date. Our millimeter galaxy sample comes from the ASAGAO survey covering 26 arcmin<jats:sup>2</jats:sup> (12 sources at a 1.2 mm flux-density limit of <jats:inline-formula>
<jats:tex-math>
<?CDATA $\approx 0.6$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn1.gif" xlink:type="simple" />
</jats:inline-formula> mJy), supplemented by the deeper but narrower 1.3 mm survey of a part of the ASAGAO field by Dunlop et al. Ofthe 25 total millimeter galaxies, 14 have <jats:italic>Chandra</jats:italic> counterparts. The observed AGN fractions at <jats:inline-formula>
<jats:tex-math>
<?CDATA $z=1.5\mbox{--}3$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn2.gif" xlink:type="simple" />
</jats:inline-formula> are found to be <jats:inline-formula>
<jats:tex-math>
<?CDATA ${90}_{-19}^{+8}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn3.gif" xlink:type="simple" />
</jats:inline-formula>% and <jats:inline-formula>
<jats:tex-math>
<?CDATA ${57}_{-25}^{+23}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn4.gif" xlink:type="simple" />
</jats:inline-formula>% for the ultra-luminous and luminous infrared galaxies with log <jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{\mathrm{IR}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn5.gif" xlink:type="simple" />
</jats:inline-formula>/<jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{\odot }$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn6.gif" xlink:type="simple" />
</jats:inline-formula> = 12–12.8 and log <jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{\mathrm{IR}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn7.gif" xlink:type="simple" />
</jats:inline-formula>/<jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{\odot }$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn8.gif" xlink:type="simple" />
</jats:inline-formula> = 11.5–12, respectively. The majority (∼2/3) of the ALMA and/or Herschel detected X-ray AGNs at <jats:italic>z</jats:italic> = 1.5−3 appear to be star-formation-dominant populations, having <jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{{\rm{X}}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn9.gif" xlink:type="simple" />
</jats:inline-formula>/ <jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{\mathrm{IR}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn10.gif" xlink:type="simple" />
</jats:inline-formula> ratios smaller than the “simultaneous evolution” value expected from the local black-hole-mass-to-stellar-mass (<jats:inline-formula>
<jats:tex-math>
<?CDATA ${M}_{\mathrm{BH}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn11.gif" xlink:type="simple" />
</jats:inline-formula>–<jats:italic>M</jats:italic>
<jats:sub>*</jats:sub>) relation. On the basis of the <jats:inline-formula>
<jats:tex-math>
<?CDATA ${L}_{{\rm{X}}}$?>
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<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn12.gif" xlink:type="simple" />
</jats:inline-formula> and stellar mass relation, we infer that a large fraction of star-forming galaxies at <jats:inline-formula>
<jats:tex-math>
<?CDATA $z=1.5\mbox{--}3$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn13.gif" xlink:type="simple" />
</jats:inline-formula> have black hole masses that are smaller than those expected from the local <jats:inline-formula>
<jats:tex-math>
<?CDATA ${M}_{\mathrm{BH}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9f10ieqn14.gif" xlink:type="simple" />
</jats:inline-formula>–<jats:italic>M</jats:italic>
<jats:sub>*</jats:sub> relation. This contrasts previous reports on luminous AGNs at the same redshifts detected in wider and shallower surveys, which are subject to selection biases against lower luminosity AGNs. Our results are consistent with an evolutionary scenario in which star formation occurs first, and an AGN-dominant phase follows later, in objects that finally evolve into galaxies with classical bulges.</jats:p>

• 出版日期2018-1-20