Beschreibung:
<jats:title>Abstract</jats:title>
<jats:p>We present IRAM/NOEMA and JVLA observations of the quasar J1342+0928 at <jats:italic>z</jats:italic> = 7.54 and report detections of copious amounts of dust and [C <jats:sc>ii</jats:sc>] emission in the interstellar medium (ISM) of its host galaxy. At this redshift, the age of the universe is 690 Myr, about 10% younger than the redshift of the previous quasar record holder. Yet, the ISM of this new quasar host galaxy is significantly enriched by metals, as evidenced by the detection of the [C <jats:sc>ii</jats:sc>] 158 <jats:italic>μ</jats:italic>m cooling line and the underlying far-infrared (FIR) dust continuum emission. To the first order, the FIR properties of this quasar host are similar to those found at a slightly lower redshift (<jats:inline-formula>
<jats:tex-math>
<?CDATA $z\sim 6$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn1.gif" xlink:type="simple" />
</jats:inline-formula>), making this source by far the FIR-brightest galaxy known at <jats:inline-formula>
<jats:tex-math>
<?CDATA $z\gtrsim 7.5$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn2.gif" xlink:type="simple" />
</jats:inline-formula>. The [C <jats:sc>ii</jats:sc>] emission is spatially unresolved, with an upper limit on the diameter of 7 kpc. Together with the measured FWHM of the [C <jats:sc>ii</jats:sc>] line, this yields a dynamical mass of the host of <jats:inline-formula>
<jats:tex-math>
<?CDATA $\lt 1.5\times {10}^{11}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn3.gif" xlink:type="simple" />
</jats:inline-formula>
<jats:inline-formula>
<jats:tex-math>
<?CDATA ${M}_{\odot }$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn4.gif" xlink:type="simple" />
</jats:inline-formula>. Using standard assumptions about the dust temperature and emissivity, the NOEMA measurements give a dust mass of <jats:inline-formula>
<jats:tex-math>
<?CDATA $(0.6\mbox{--}4.3)\times {10}^{8}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn5.gif" xlink:type="simple" />
</jats:inline-formula>
<jats:inline-formula>
<jats:tex-math>
<?CDATA ${M}_{\odot }$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn6.gif" xlink:type="simple" />
</jats:inline-formula>. The brightness of the [C <jats:sc>ii</jats:sc>] luminosity, together with the high dust mass, imply active ongoing star formation in the quasar host. Using [C <jats:sc>ii</jats:sc>]–SFR scaling relations, we derive star formation rates of 85–545 <jats:inline-formula>
<jats:tex-math>
<?CDATA ${M}_{\odot }$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa943aieqn7.gif" xlink:type="simple" />
</jats:inline-formula> yr<jats:sup>−1</jats:sup> in the host, consistent with the values derived from the dust continuum. Indeed, an episode of such past high star formation is needed to explain the presence of ∼10<jats:sup>8</jats:sup>
<jats:italic>M</jats:italic>
<jats:sub>☉</jats:sub> of dust implied by the observations.</jats:p>