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We present the analysis of the absorption troughs of six outflows observed in quasar SDSS J1130+0411 ($z \approx 3.98$) with radial velocities ranging from $-2400$ to $-15,400$ km s$^{-1}$. These spectra were taken with the Very Large Telescope/Ultraviolet and Visual Echelle Spectrograph over the rest frame wavelength range of $1135-1890$ \r{A}. In the main outflow system ($v \approx -3200$ km s$^{-1}$), we identify Fe II and several Fe II* absorption troughs as well as Si II and Si II* troughs, which we use to determine the electron number density $\log n_e = 2.6_{-0.7}^{+0.8}$ cm$^{-3}$. Using the column densities of these and other ions, we determine a photoionization solution with hydrogen column density $\log N_H = 21.44_{-0.33}^{+0.24}$ cm$^{-2}$ and ionization parameter $\log U_H = -1.75_{-0.45}^{+0.28}$. From these values we derive the distance $R = 16_{-11}^{+23}$ kpc, the average mass flow rate $\dot{M} = 4100_{-2400}^{+6600}$ $M_{\odot}$ yr$^{-1}$, and the kinetic luminosity $\log \dot{E}_k = 46.13_{-0.37}^{+0.41}$ erg s$^{-1}$. This $\dot{E}_k$ is $1.4_{-0.8}^{+2.2}$% of the quasar's Eddington luminosity, and therefore contributes significantly to AGN feedback., Comment: 8 pages, 5 figures, 3 tables, published in MNRAS

We found a broad absorption line (BAL) outflow in the VLT/UVES spectrum of the quasar SDSS J235702.54-004824.0, in which we identified four subcomponents. We measured the column densities of the ions in one of the subcomponents ($v$ = -1600 km s$^{-1}$), which include O I and Fe II. We found the kinetic luminosity of this component to be at most ~2.4% of the quasar's Eddington luminosity. This is near the amount required to contribute to AGN feedback. We also examined the time-variability of a C IV mini-BAL found at $v$ = -8700 km s$^{-1}$, which shows a shallower and narrower absorption feature attached to it in previous SDSS observations from 2000 and 2001, but not in the spectra from 2005 and onwards., 10 pages, 6 figures. Accepted for publication on MNRAS

We analyze Very Large Telescope/UVES observations of the quasar SDSS J024221.87+004912.6. We identify four absorption outflow systems: a C iv broad absorption line (BAL) at v approximate to -18,000 km s(-1) and three narrower low-ionization systems with centroid velocities ranging from -1200 to -3500 km s(-1). These outflows show similar physical attributes to the [O iii] outflows studied by Liu et al. (2013). We find that two of the systems are energetic enough to contribute to active galactic nucleus feedback, with one system reaching above 5% of the quasar's Eddington luminosity. We also find that this system is at a distance of 67 kpc away from the quasar, the farthest detected mini-BAL absorption outflow from its central source to date. In addition, we examine the time-variability of the BAL and find that its velocity monotonically increases, while the trough itself becomes shallower over time. NSF [AST 2106249]; NASA STScI [14777, 14242, 14054, 14176, AR-15786]; Virginia Space Grant Consortium Graduate Research Fellowship Program [200009-010] Published version N.A. and D.B. acknowledge support from NSF grant No. AST 2106249, as well as NASA STScI grant Nos. GO 14777, 14242, 14054, 14176, and AR-15786. D.B. acknowledges support from the Virginia Space Grant Consortium Graduate Research Fellowship Program (award number 200009-010).

Full list of authors: Kara, Erin; Mehdipour, Missagh; Kriss, Gerard A.; Cackett, Edward M.; Arav, Nahum; Barth, Aaron J.; Byun, Doyee; Brotherton, Michael S.; De Rosa, Gisella; Gelbord, Jonathan; Hernández Santisteban, Juan V.; Hu, Chen; Kaastra, Jelle; Landt, Hermine; Li, Yan-Rong; Miller, Jake A. ; Montano, John; Partington, Ethan; Aceituno, Jesús; Bai, Jin-Ming; Bao, Dongwei; Bentz, Misty C.; Brink, Thomas G.; Chelouche, Doron; Chen, Yong-Jie; Colmenero, Encarni Romero; Dalla Bontà, Elena; Dehghanian, Maryam; Du, Pu; Edelson, Rick; Ferland, Gary J.; Ferrarese, Laura; Fian, Carina; Filippenko, Alexei V.; Fischer, Travis; Goad, Michael R.; González Buitrago, Diego H.; Gorjian, Varoujan; Grier, Catherine J.; Guo, Wei-Jian; Hall, Patrick B.; Ho, Luis C.; Homayouni, Y.; Horne, Keith; Ilić, Dragana; Jiang, Bo-Wei; Joner, Michael D.; Kaspi, Shai; Kochanek, Christopher S.; Korista, Kirk T.; Kynoch, Daniel; Li, Sha-Sha; Liu, Jun-Rong; McHardy, Ian M.; McLane, Jacob N.; Mitchell, Jake A. J.; Netzer, Hagai; Olson, Kianna A.; Pogge, Richard W.; Popović, Luka Č.; Proga, Daniel; Storchi-Bergmann, Thaisa; Strasburger, Erika; Treu, Tommaso; Vestergaard, Marianne; Wang, Jian-Min; Ward, Martin J.; Waters, Tim; Williams, Peter R.; Yang, Sen; Yao, Zhu-Heng; Zastrocky, Theodora E.; Zhai, Shuo; Zu, Ying, We present the first results from the ongoing, intensive, multiwavelength monitoring program of the luminous Seyfert 1 galaxy Mrk 817. While this active galactic nucleus was, in part, selected for its historically unobscured nature, we discovered that the X-ray spectrum is highly absorbed, and there are new blueshifted, broad, and narrow UV absorption lines, which suggest that a dust-free, ionized obscurer located at the inner broad-line region partially covers the central source. Despite the obscuration, we measure UV and optical continuum reverberation lags consistent with a centrally illuminated Shakura-Sunyaev thin accretion disk, and measure reverberation lags associated with the optical broad-line region, as expected. However, in the first 55 days of the campaign, when the obscuration was becoming most extreme, we observe a de-coupling of the UV continuum and the UV broad emission-line variability. The correlation recovered in the next 42 days of the campaign, as Mrk 817 entered a less obscured state. The short C iv and Lyα lags suggest that the accretion disk extends beyond the UV broad-line region. © 2021. The American Astronomical Society. All rights reserved., E.K. acknowledges support from NASA grant GO1-22116X. E.M.C. and J.A.M. gratefully acknowledge support from NSF grant AST-1909199. Research at UC Irvine was supported by NSF grant AST-1907290. H.L. acknowledges a Daphne Jackson Fellowship sponsored by the Science and Technology Facilities Council (STFC), UK. J.A.J.M. and M.J.W. acknowledge support from STFC grants ST/P000541/1 and ST/T000244/1. G.J.F. and M.D. acknowledge support by NSF (1816537, 1910687), NASA (ATP 17-ATP17-0141, 19-ATP19-0188), and STScI (HST-AR- 15018 and HST-GO-16196.003-A). Y.H. acknowledges support from NASA grants HST-GO-15650 and HST-GO-16-196. D.I. and L.Č. P. acknowledge funding provided by the Astronomical Observatory Belgrade (the contract 451-03-68/2020-14/200002), University of Belgrade—Faculty of Mathematics (the contract 451-03-9/2021-14/200104) through the grants by the Ministry of Education, Science, and Technological Development of the Republic of Serbia. D.I. acknowledges the support of the Alexander von Humboldt Foundation. M.V. gratefully acknowledges financial support from the Independent Research Fund Denmark via grant No. DFF 8021-00130. J.M.W. acknowledges financial support by the National Science Foundation of China (NSFC) through grants NSFC-11833008 and -11991054. P.D. acknowledges financial support from NSFC grants NSFC-12022301, -11873048, and -11991051, and from the Strategic Priority Research Program of the CAS (XDB23010400). C.H. acknowledges financial support from the grant NSFC-11773029 and from the National Key R&D Program of China (2016YFA0400701). Y.R.L. acknowledges financial support from the grant NSFC-11922304 and from the Youth Innovation Promotion Association CAS. J.V.H.S. and K.H. acknowledge support from STFC grant ST/R000824/1. P.B.H. is supported by NSERC. Support for A.V.F.'s group at U.C. Berkeley is provided by the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (A.V.F. is a Senior Miller Fellow). M.C.B. gratefully acknowledges support from the NSF through grant AST-2009230. D.K. acknowledges support from the Czech Science Foundation project No. 19-05599Y. L.C.H. was supported by the National Key R&D Program of China (2016YFA0400702) and the National Science Foundation of China (11721303, 11991052). J.G. gratefully acknowledges support from NASA under the ADAP award 80NSSC17K0126., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.