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IRAS F11119+3257 is a quasar-dominated Ultra-Luminous InfraRed Galaxy, with apartially obscured narrow-line seyfert 1 nucleus. In this paper, we present theNIR spectroscopy of F11119+3257, in which we find unusual Paschen emissionlines, and metastable He I* $\lambda$10830 absorption associated with thepreviously reported atomic sodium and molecular OH mini-BAL (Broad AbsorptionLine) outflow. Photo-ionization diagnosis confirms previous findings that theoutflows are at kilo-parsec scales. Such large-scale outflows should produceemission lines. We indeed find that high-ionization emission lines ([O III],[Ne III], and [Ne V]) are dominated by blueshifted components at similar speedsto the mini-BALs. The blueshifted components are also detected in somelow-ionization emission lines, such as [O II] $\lambda$3727 and some Balmerlines (H$\alpha$, H$\beta$, and H$\gamma$), even though their cores aredominated by narrow ($FWHM_{\rm NEL} = 570\pm40$km s$^{-1}$) or broadcomponents at the systemic redshift of $z=0.18966\pm0.00006$. The mass flowrate (230-730$~M_\odot \rm yr^{-1}$) and the kinetic luminosity ($\dot{E}_k\sim 10^{43.6-44.8} $erg s$^{-1}$) are then inferred jointly from theblueshifted emission and absorption lines. In the NIR spectrum of F11119+3257,we also find that the Paschen emission lines are unique, in which a very narrow($FWHM=260\pm20~$km s$^{-1}$) component is shown in only Pa$\alpha$. Thisnarrow component most probably comes from heavily obscured star formation.Based on the Pa$\alpha$ and Pa$\beta$ emissions, we obtain an extinction at the$H$ band, $A_H~>~2.1$ (or a reddenning of $E_{B-V}~>~$3.7), and a starformation rate of $SFR~>~130\rm M_\odot yr^{-1}$ that resembles the estimatesinferred from the FIR emissions ($SFR_{\rm FIR} = 190\pm90$ $M_\odot$yr$^{-1}$).

astrophysical journal/the astrophysical journal

Discovery of Metastable He I* $\lambda$10830 Mini-broad Absorption Lines  and Very Narrow Paschen $\alpha$ Emission Lines in the ULIRG Quasar IRAS  F11119+3257