The Mass Relations between Supermassive Black Holes and Their Host Galaxies at 1 < z < 2 with HST-WFC3

<jats:title>Abstract</jats:title> <jats:p>Correlations between the mass of a supermassive black hole (SMBH) and the properties of its host galaxy (e.g., total stellar mass <jats:italic>M</jats:italic> <jats:sub>*</jats:sub>, luminosity <jats:italic>L</jats:italic> <jats:sub>host</jats:sub>) suggest an evolutionary connection. A powerful test of a coevolution scenario is to measure the relations <jats:inline-formula> <jats:tex-math> <?CDATA ${{ \mathcal M }}_{\mathrm{BH}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab5b90ieqn1.gif" xlink:type="simple" /> </jats:inline-formula>–<jats:italic>L</jats:italic> <jats:sub>host</jats:sub> and <jats:inline-formula> <jats:tex-math> <?CDATA ${{ \mathcal M }}_{\mathrm{BH}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab5b90ieqn2.gif" xlink:type="simple" /> </jats:inline-formula>–<jats:italic>M</jats:italic> <jats:sub>*</jats:sub> at high redshift and compare with local estimates. For this purpose, we acquired <jats:italic>Hubble Space Telescope</jats:italic> (<jats:italic>HST</jats:italic>) imaging with WFC3 of 32 X-ray-selected broad-line (type 1) active galactic nuclei at 1.2 < <jats:italic>z</jats:italic> < 1.7 in deep survey fields. By applying state-of-the-art tools to decompose the <jats:italic>HST</jats:italic> images including available ACS data, we measured the host galaxy luminosity and stellar mass along with other properties through the two-dimensional model fitting. The black hole mass (<jats:inline-formula> <jats:tex-math> <?CDATA ${{ \mathcal M }}_{\mathrm{BH}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab5b90ieqn3.gif" xlink:type="simple" /> </jats:inline-formula>) was determined using the broad H<jats:italic>α</jats:italic> line, detected in the near-infrared with the Subaru Fiber Multi-Object Spectrograph, which potentially minimizes systematic effects using other indicators. We find that the observed ratio of <jats:inline-formula> <jats:tex-math> <?CDATA ${{ \mathcal M }}_{\mathrm{BH}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic"></mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab5b90ieqn4.gif" xlink:type="simple" /> </jats:inline-formula> to total <jats:italic>M</jats:italic> <jats:sub>*</jats:sub> is 2.7× larger at <jats:italic>z</jats:italic> ∼ 1.5 than in the local universe, while the scatter is equivalent between the two epochs. A nonevolving mass ratio is consistent with the data at the 2<jats:italic>σ</jats:italic>–3<jats:italic>σ</jats:italic> confidence level when accounting for selection effects (estimated using two independent and complementary methods) and their uncertain ...