Deep Hubble Space Telescope Imaging on the Extended Ly$alpha$ Emission of a QSO at $z = 2.19$ with Damped Lyman Alpha System as a Natural Coronagraph. (arXiv:2002.05179v1 [astro-ph.GA])

Deep Hubble Space Telescope Imaging on the Extended Ly$alpha$ Emission of a QSO at $z = 2.19$ with Damped Lyman Alpha System as a Natural Coronagraph. (arXiv:2002.05179v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ding_J/0/1/0/all/0/1">Jiani Ding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_Z/0/1/0/all/0/1">Zheng Cai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prochaska_J/0/1/0/all/0/1">J. Xavier Prochaska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finley_H/0/1/0/all/0/1">H.Finley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_X/0/1/0/all/0/1">Xiaohui Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_Z/0/1/0/all/0/1">Zheng Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fathivavsari_H/0/1/0/all/0/1">H. Fathivavsari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petitjean_P/0/1/0/all/0/1">P. Petitjean</a>

Recent observations suggest that proximate damped Ly$alpha$ (PDLA) systems
can be used to study the host galaxies of Quasi-stellar objects (QSOs), because
the PDLAs can block the bright point-spread-function (PSF) from central QSOs.
Using six-orbits of narrowband imaging with $it{HST}$/WFC3, we present the
first high resolution narrowband image of the Ly$alpha$ emission in the PDLA
trough of the QSO SDSSJ115432.67-021537.9 . We detect one major component and
one minor component in the narrowband imaging. Combining the $it{HST}$/WFC3
imaging with deep Magellan/MagE spectra, we measure that the Ly$alpha$ flux
F$_{rm{Lyalpha}}$ = 1.56$pm0.10 times10^{-16}$ $rm{erg s^{-1} cm^{-2}}$,
which is among the luminous ($approx$ 2.7 L$^{star}_{rm{Lyalpha}}$)
Ly$alpha$ emitters at $it{z} =$ 2.19. The $rm{Lyalpha}$-based star
formation rate (SFR) is $sim$ 7 $textrm{M_{sun} yr^{-1}}$. These
observational results favor that the star formation from the host galaxy could
be the main mechanism to power the Ly$alpha$ emission. This new method sheds
new light on the study of the kinematic structure and the spatial distribution
of the extended Ly$alpha$ emitting regions around the QSO host.

Recent observations suggest that proximate damped Ly$alpha$ (PDLA) systems
can be used to study the host galaxies of Quasi-stellar objects (QSOs), because
the PDLAs can block the bright point-spread-function (PSF) from central QSOs.
Using six-orbits of narrowband imaging with $it{HST}$/WFC3, we present the
first high resolution narrowband image of the Ly$alpha$ emission in the PDLA
trough of the QSO SDSSJ115432.67-021537.9 . We detect one major component and
one minor component in the narrowband imaging. Combining the $it{HST}$/WFC3
imaging with deep Magellan/MagE spectra, we measure that the Ly$alpha$ flux
F$_{rm{Lyalpha}}$ = 1.56$pm0.10 times10^{-16}$ $rm{erg s^{-1} cm^{-2}}$,
which is among the luminous ($approx$ 2.7 L$^{star}_{rm{Lyalpha}}$)
Ly$alpha$ emitters at $it{z} =$ 2.19. The $rm{Lyalpha}$-based star
formation rate (SFR) is $sim$ 7 $textrm{M_{sun} yr^{-1}}$. These
observational results favor that the star formation from the host galaxy could
be the main mechanism to power the Ly$alpha$ emission. This new method sheds
new light on the study of the kinematic structure and the spatial distribution
of the extended Ly$alpha$ emitting regions around the QSO host.

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