The Kinematics and Physical Conditions of the Ionized Gas in Markarian 509. II. STIS Echelle Observations

Kraemer, S. B.; Crenshaw, D. Michael; Yaqoob, T.; McKernan, Barry; Gabel, J. R.; George, I. M.; Turner, T. J.; Dunn, Jay P.

doi:10.1086/344542

Cited by 41 publications

(97 citation statements)

References 37 publications

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“…The absorption component with the highest redshift relative to the systemic velocity is only observed in the UV and is likely to be a high velocity cloud near the host galaxy . From studying the absorption troughs either at rest or outflowing in the UV, it appears that these are clustered around −300 and +16 km s −1 (Kriss et al 2000;Kraemer et al 2003;Kriss et al 2011). Fitting model 2, Detmers et al (2011) finds outflow velocities of −13 ± 11 km s −1 and −319 ± 14 km s −1 , consistent with the main absorption troughs detected in the UV.…”

Section: Spectral Modelsmentioning

confidence: 54%

Multiwavelength campaign on Mrk 509

Steenbrugge

Kaastra

Detmers

et al. 2011

A&A

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Context. The study of abundances in the nucleus of active galaxies allows us to investigate the evolution of the abundance by comparing local and higher redshift galaxies. However, the methods used so far have substantial drawbacks or rather large uncertainties. Some of the measurements are at odds with the initial mass function derived from the older stellar population of local elliptical galaxies. Aims. We determine accurate and reliable abundances of C, N, Ne, and Fe relative to O from the narrow absorption lines observed in the X-ray spectra of Mrk 509. Methods. We use the stacked 600 ks XMM-Newton RGS and 180 ks Chandra LETGS spectra. Thanks to simultaneous observations with INTEGRAL and the optical monitor on-board XMM-Newton for the RGS observations and HST-COS and Swift for the LETGS observations, we have an individual spectral energy distribution for each dataset. Owing to the excellent quality of the RGS spectrum, the ionisation structure of the absorbing gas is well constrained, allowing for a reliable abundance determination using ions over the whole observed range of ionisation parameters. Results. We find that the relative abundances are consistent with the proto-solar abundance ratios: C/O = 1.19 ± 0.08, N/O = 0.98 ± 0.08, Ne/O = 1.11 ± 0.10, Mg/O = 0.68 ± 0.16, Si/O = 1.3 ± 0.6, Ca/O = 0.89 ± 0.25, and Fe/O = 0.85 ± 0.06, with the exception of S, which is slightly under-abundant, S/O = 0.57 ± 0.14. Our results, and their implications, are discussed and compared to the results obtained using other techniques to derive abundances in galaxies.

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Section: Spectral Modelsmentioning

confidence: 54%

Multiwavelength campaign on Mrk 509

Steenbrugge

Kaastra

Detmers

et al. 2011

A&A

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“…Yaqoob et al (2003) also applied a curve of growth analysis to deduce a velocity width of 100 km s −1 , quite similar to what we find and fully in agreement with the recent analysis of the data gathered during our 2009 multi-wavelength campaign (Kaastra et al 2011a, hereafter Paper II). The velocity widths found in X-rays are, in general, broader than those found in the UV (Kriss et al 2000;Kraemer et al 2003) which may provide some hints on the nature of the X-ray/UV absorbing gas. Note, however, that the UV absorption is characterized by more components at velocities too close to be resolved in the X-rays.…”

Section: Comparison With Previous X-ray Observationsmentioning

confidence: 82%

“…Making direct comparisons between the UV observations of O vi and the X-ray, even among the individual O vi components seen with FUSE is difficult because of the high level of saturation in most of these features, as pointed out by Kraemer et al (2003). The quoted column densities from Kriss et al (2000) for the strongest components should be treated as lower limits.…”

Section: Column Densitiesmentioning

confidence: 99%

“…It is particularly suitable for an extensive multi-wavelength campaign because of its brightness and confirmed presence of an intrinsic WA (Pounds et al 2001;Yaqoob et al 2003;Smith et al 2007;Detmers et al 2010) in X-rays, as well as a variety of UV absorption lines (Crenshaw et al 1995Savage et al 1997;Kriss et al 2000;Kraemer et al 2003) and slow variability, which makes it particularly suited to reverberation studies. This paper is devoted to the analysis of the Chandra-LETGS observation of Mrk 509, which is part of an unprecedented multiwavelength campaign of observations carried out at the end of 2009, aiming at determining the location of the warm absorber and the physics of its ionized outflow.…”

Section: Introductionmentioning

confidence: 99%

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Multiwavelength campaign on Mrk 509

Ebrero

Kriss

Kaastra

et al. 2011

A&A

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Context. We present here the results of a 180 ks Chandra-LETGS observation as part of a large multi-wavelength campaign on Mrk 509. Aims. We study the warm absorber in Mrk 509 and use the data from a simultaneous HST-COS observation in order to assess whether the gas responsible for the UV and X-ray absorption are the same. Methods. We analyzed the LETGS X-ray spectrum of Mrk 509 using the SPEX fitting package. Results. We detect several absorption features originating in the ionized absorber of the source, along with resolved emission lines and radiative recombination continua. The absorption features belong to ions with, at least, three distinct ionization degrees. The lowest ionized component is slightly redshifted (Δv = 73 km s −1 ) and is not in pressure equilibrium with the others, and therefore it is not likely part of the outflow, possibly belonging to the interstellar medium of the host galaxy. The other components are outflowing at velocities of −196 and −455 km s −1 , respectively. The source was observed simultaneously with HST-COS, finding 13 UV kinematic components. At least three of them can be kinematically associated with the observed X-ray components. Based on the HST-COS results and a previous FUSE observation, we find evidence that the UV absorbing gas might be co-located with the X-ray absorbing gas and belong to the same structure.

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“…They manifest themselves through blueshifted absorption lines imprinted in the UV and X-ray continuum of AGN spectra (e.g. Kraemer & Crenshaw 2003, Krongold et al 2003, Andrade-Velazquez et al 2010, Gupta et al 2013a. They have been classified as having Narrow Absorption Lines These outflows are thought to be strong driving agents of galaxy evolution, producing the AGN feedback required to stop the growth of their host galaxies, heating their interstellar medium and quenching star formation (di Matteo et al 2005, Silk 2011, Kormendy & Ho 2013.…”

Section: Introductionmentioning

confidence: 99%

Hubble Space Telescope observations of BALQSO Ton 34 reveal a connection between the broad-line region and the BAL outflow

Krongold¹,

Binette²,

Bohlin³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Ton 34 recently transitioned from non-absorbing quasar into a BALQSO.Here, we report new HST-STIS observations of this quasar. Along with CIV absorption, we also detect absorption by NV+Lyα and possibly O VI+Lyβ. We follow the evolution of the CIV BAL, and find that, for the slower outflowing material, the absorption trough varies little (if at all) on a rest-frame timescale of ∼ 2 yr. However, we detect a strong deepening of the absorption in the gas moving at larger velocities (−20, 000 -−23, 000 km s −1 ). The data is consistent with a multistreaming flow crossing our line of sight to the source. The transverse velocity of the flow should be ∼ few thousand km s −1 , similar to the rotation velocity of the BLR gas (≈ 2, 600 km s −1 ). By simply assuming Keplerian motion, these two components must have similar locations, pointing to a common outflow forming the BLR and the BAL. We speculate that BALs, mini-BALs, and NALs, are part of a common, ubiquitous, accretion-disk outflow in AGN, but become observable depending on the viewing angle towards the flow. The absorption troughs suggests a wind covering only ∼20 % of the emitting source, implying a maximum size of 10 −3 pc for the clouds forming the BAL/BLR medium. This is consistent with constraints of the BLR clouds from X-ray occultations. Finally, we suggest that the low excitation broad emission lines detected in the spectra of this source lie beyond the wind, and this gas is probably excited by the shock of the BAL wind with the surrounding medium.

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The Kinematics and Physical Conditions of the Ionized Gas in Markarian 509. II. STIS Echelle Observations

Cited by 41 publications

References 37 publications

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

Hubble Space Telescope observations of BALQSO Ton 34 reveal a connection between the broad-line region and the BAL outflow

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