High resolution optical spectroscopy of the $mathrm{N_2}$-rich comet C/2016 R2 (PanSTARRS). (arXiv:1901.00657v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Opitom_C/0/1/0/all/0/1">C. Opitom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hutsemekers_D/0/1/0/all/0/1">D. Hutsemékers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jehin_E/0/1/0/all/0/1">E. Jehin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rousselot_P/0/1/0/all/0/1">P. Rousselot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pozuelos_F/0/1/0/all/0/1">F. J. Pozuelos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manfroid_J/0/1/0/all/0/1">J. Manfroid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moulane_Y/0/1/0/all/0/1">Y. Moulane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gillon_M/0/1/0/all/0/1">M. Gillon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benkhaldoun_Z/0/1/0/all/0/1">Z. Benkhaldoun</a>
Early observations of comet C/2016 R2 (PanSTARRS) have shown that the
composition of this comet is very peculiar. We obtained high resolution spectra
of the comet in February when it was at 2.8 au from the Sun. We used the UVES
spectrograph of the ESO VLT, complemented with narrow-band images obtained with
the TRAPPIST telescopes. We detect strong emissions from the ions
$mathrm{N_2^+}$ and $mathrm{CO^+}$, but also $mathrm{CO_2^+}$, emission from
the CH radical, and much fainter emissions of the CN, $mathrm{C_2}$, and
$mathrm{C_3}$ radicals which were not detected in previous observations of
this comet. We do not detect OH or $mathrm{H_2O^+}$, and derive an upper limit
of the $mathrm{H_2O^+/CO^+}$ ratio of 0.4, implying that the comet has a low
water abundance. We measure a $mathrm{N_2^+/CO^+}$ ratio of $0.06pm0.01$. The
non-detection of $mathrm{NH_2}$ indicates that most of the nitrogen content of
the comet lies within $mathrm{N_2}$. Together with the high
$mathrm{N_2^+/CO^+}$ ratio, this could indicate a low formation temperature of
the comet, or that the comet is a fragment of a large differentiated Kuiper
Belt object. The $mathrm{CO_2^+/CO^+}$ ratio is $1.1pm0.3$. We do not detect
$mathrm{^{14}N^{15}N^+}$ lines, and can only put a lower limit on the
$mathrm{^{14}N/^{15}N}$ ratio measured from $mathrm{N_2^+}$ of about 100,
compatible with measurements of the same isotopic ratio for $mathrm{NH_2}$ and
CN in other comets. Finally, in addition to the [OI] and [CI] forbidden lines,
we detect for the first time the forbidden nitrogen lines [NI] doublet at
519.79 and 520.04 nm in the coma of a comet.
Early observations of comet C/2016 R2 (PanSTARRS) have shown that the
composition of this comet is very peculiar. We obtained high resolution spectra
of the comet in February when it was at 2.8 au from the Sun. We used the UVES
spectrograph of the ESO VLT, complemented with narrow-band images obtained with
the TRAPPIST telescopes. We detect strong emissions from the ions
$mathrm{N_2^+}$ and $mathrm{CO^+}$, but also $mathrm{CO_2^+}$, emission from
the CH radical, and much fainter emissions of the CN, $mathrm{C_2}$, and
$mathrm{C_3}$ radicals which were not detected in previous observations of
this comet. We do not detect OH or $mathrm{H_2O^+}$, and derive an upper limit
of the $mathrm{H_2O^+/CO^+}$ ratio of 0.4, implying that the comet has a low
water abundance. We measure a $mathrm{N_2^+/CO^+}$ ratio of $0.06pm0.01$. The
non-detection of $mathrm{NH_2}$ indicates that most of the nitrogen content of
the comet lies within $mathrm{N_2}$. Together with the high
$mathrm{N_2^+/CO^+}$ ratio, this could indicate a low formation temperature of
the comet, or that the comet is a fragment of a large differentiated Kuiper
Belt object. The $mathrm{CO_2^+/CO^+}$ ratio is $1.1pm0.3$. We do not detect
$mathrm{^{14}N^{15}N^+}$ lines, and can only put a lower limit on the
$mathrm{^{14}N/^{15}N}$ ratio measured from $mathrm{N_2^+}$ of about 100,
compatible with measurements of the same isotopic ratio for $mathrm{NH_2}$ and
CN in other comets. Finally, in addition to the [OI] and [CI] forbidden lines,
we detect for the first time the forbidden nitrogen lines [NI] doublet at
519.79 and 520.04 nm in the coma of a comet.
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