5 research outputs found
Narrow absorption line Outflow in Seyfert 1 galaxy J1429+4518: Outflow's distance from the central source and its energetics
In the HST/COS spectrum of the Seyfert 1 galaxy 2MASX J14292507+4518318, we
have identified a narrow absorption line (NAL) outflow system with a velocity
of -151 km s This outflow exhibits absorption troughs from the resonance
states of ions like CIV, NV, SiIV, and SiII, as well as excited states from
CII*, and SiII*. Our investigation of the outflow involved measuring ionic
column densities and conducting photoionization analysis. These yield the total
column density of the outflow to be estimated as =19.84
[cm, its ionization parameter to be =2.0 and its
electron number density equal to = 2.75[cm]. These
measurements enabled us to determine the mass-loss rate and the kinetic
luminosity of the outflow system to be =0.22[] and
=39.3 [erg s], respectively. We have also measured the
location of the outflow system to be at 275 pc from the central source.
This outflow does not contribute to the AGN feedback processes due to the low
ratio of the outflow's kinetic luminosity to the AGN's Eddington luminosity
(). This outflow is remarkably similar to
the two bipolar lobe outflows observed in the Milky Way by XMM-Newton and
Chandra.Comment: 11 pages, 8 figures, accepted for publication in MNRA
An Extreme FeLoBAL Outflow in the VLT/UVES Spectrum of Quasar SDSS J1321-0041
Context. Quasar outflows are often analyzed to determine their ability to
contribute to active galactic nucleus (AGN) feedback. We have identified a
broad absorption line (BAL) outflow in the VLT/UVES spectrum of the quasar SDSS
J1321-0041. The outflow shows troughs from Fe II, and is therefore identified
as an FeLoBAL. It is quite extreme among that population, as it shows C II and
Si II BALs. Aims. Outflow systems require a kinetic luminosity above
of the quasar's luminosity to contribute to AGN feedback. For this
reason, we analyzed the spectrum of J1321-0041 to determine the outflow's
kinetic luminosity, as well as the quasar's bolometric luminosity. Methods. We
measured the ionic column densities from the absorption troughs in the
spectrum, and determined the Hydrogen column density and ionization parameter
using those column densities as our constraints. We also determined the
electron number density based on the ratios between excited state and
resonance state column densities of Fe II and Si II. This allowed us to find
the distance of the outflow from its central source, as well as its kinetic
luminosity. Results. We determined the kinetic luminosity of the outflow to be
, and the quasar's
bolometric luminosity to be ,
resulting in a ratio of . We conclude
that this outflow has sufficient kinetic luminosity to contribute to AGN
feedback.Comment: 6 pages, 5 figures, 2 tables. Submitted to A&
AGN STORM 2. I. First results: A Change in the Weather of Mrk 817
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. Unified
AGN STORM 2. III. A NICER View of the Variable X-Ray Obscurer in Mrk 817
The AGN STORM 2 Collaboration targeted the Seyfert 1 galaxy Mrk 817 for a year-long multiwavelength, coordinated reverberation mapping campaign including Hubble Space Telescope, Swift, XMM-Newton, NICER, and ground-based observatories. Early observations with NICER and XMM revealed an X-ray state 10 times fainter than historical observations, consistent with the presence of a new dust-free, ionized obscurer. The following analysis of NICER spectra attributes variability in the observed X-ray flux to changes in both the column density of the obscurer by at least one order of magnitude (NH ranges from to ) and the intrinsic continuum brightness (the unobscured flux ranges from 10−11.8 to 10−10.5 erg s−1 cm−2). While the X-ray flux generally remains in a faint state, there is one large flare during which Mrk 817 returns to its historical mean flux. The obscuring gas is still present at lower column density during the flare, but it also becomes highly ionized, increasing its transparency. Correlation between the column density of the X-ray obscurer and the strength of UV broad absorption lines suggests that the X-ray and UV continua are both affected by the same obscuration, consistent with a clumpy disk wind launched from the inner broad-line region
AGN STORM 2. III. A NICER view of the variable x-ray obscurer in Mrk 817
The AGN STORM 2 Collaboration targeted the Seyfert 1 galaxy Mrk 817 for a year-long multiwavelength, coordinated reverberation mapping campaign including Hubble Space Telescope, Swift, XMM-Newton, NICER, and ground-based observatories. Early observations with NICER and XMM revealed an X-ray state 10 times fainter than historical observations, consistent with the presence of a new dust-free, ionized obscurer. The following analysis of NICER spectra attributes variability in the observed X-ray flux to changes in both the column density of the obscurer by at least one order of magnitude (NH ranges from 2.85−0.33+0.48×1022cm−2 to 25.6−3.5+3.0×1022cm−2 ) and the intrinsic continuum brightness (the unobscured flux ranges from 10−11.8 to 10−10.5 erg s−1 cm−2). While the X-ray flux generally remains in a faint state, there is one large flare during which Mrk 817 returns to its historical mean flux. The obscuring gas is still present at lower column density during the flare, but it also becomes highly ionized, increasing its transparency. Correlation between the column density of the X-ray obscurer and the strength of UV broad absorption lines suggests that the X-ray and UV continua are both affected by the same obscuration, consistent with a clumpy disk wind launched from the inner broad-line region