Optical Continuum and Emission‐Line Variability of the Seyfert 1 Galaxy Markarian 509

Carone, T. E.; Peterson, B. M.; Bechtold, Jill; Bertram, R.; Bischoff, K.; Dietrich, M.; Filippenko, A. V.; Ho, Luis C.; Huchra, J. P.; Kollatschny, W.; Korista, K. T.; Matheson, T.; Pogge, Richard W.; Shields, J. C.; Smith, Paul S.; Wagner, R. M.; Wilkes, B. J.

doi:10.1086/178002

Cited by 29 publications

(28 citation statements)

References 7 publications

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“…2). This is consistent with the results of the monitoring program of Mrk 509 by Carone et al (1996) who found the Hβ λ4861 and He ii λ4686 emission lines to respond to continuum variations with time lags of about 80 and 60 days respectively, considerably longer than the emission line lags measured for other Seyfert galaxies and also longer than the duration of the XMM-Newton campaign. Finally, we proceeded to correct the OM and UVOT filter data (described in Sect.…”

Section: Correction For Emission From the Broad Line Region (Blr) Andsupporting

confidence: 91%

Multiwavelength campaign on Mrk 509

Mehdipour

Branduardi‐Raymont

Kaastra

et al. 2011

A&A

173

225

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We present the analysis of XMM-Newton and Swift optical-UV and X-ray observations of the Seyfert-1/QSO Mrk 509, part of an unprecedented multi-wavelength campaign, investigating the nuclear environment of this AGN. The XMM-Newton data are from a series of 10 observations of about 60 ks each, spaced from each other by about 4 days, taken in Oct.-Nov. 2009. During our campaign, Mrk 509 was also observed with Swift for a period of about 100 days, monitoring the behaviour of the source before and after the XMM-Newton observations. With these data we have established the continuum spectrum in the optical-UV and X-ray bands and investigated its variability on the timescale of our campaign with a resolution time of a few days. In order to measure and model the continuum as far as possible into the UV, we also made use of Hubble Space Telescope (HST) cosmic origin spectrograph (COS) observations of Mrk 509 (part of our coordinated campaign) and of an archival Far Ultraviolet Spectroscopic Explorer (FUSE) observation. We have found that in addition to an X-ray power-law, the spectrum displays soft X-ray excess emission below 2 keV, which interestingly varies in association with the thermal optical-UV emission from the accretion disc. The change in the X-ray power-law component flux (albeit smaller than that of the soft excess), on the other hand, is uncorrelated to the flux variability of the soft X-ray excess and the disc component on the probed timescale. The results of our simultaneous broad-band spectral and timing analysis suggest that, on a resolution time of a few days, the soft X-ray excess of Mrk 509 is produced by the Comptonisation of the thermal optical-UV photons from the accretion disc by a warm (0.2 keV) optically thick (τ ∼ 17) corona surrounding the inner regions of the disc. This makes Mrk 509, with a black hole mass of about 1-3 × 10 8 M , the highest mass known system to display such behaviour and origin for the soft X-ray excess.

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Section: Correction For Emission From the Broad Line Region (Blr) Andsupporting

confidence: 91%

Multiwavelength campaign on Mrk 509

Mehdipour

Branduardi‐Raymont

Kaastra

et al. 2011

A&A

173

225

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“…This method is not exactly the same as usually used; the usually used interpolation method only interpolates one lightcurve and the other lightcurve is paired with this interpolated lightcurve [1] . However, our method gives nearly the same CCF as Carone et al (2006) [7] , who obtained a lag of about 80 days, within the uncertainty region of our result. The uncertainty for each centroid is obtained as described in Peterson et al (1998) [8] .…”

Section: Mrk 509supporting

confidence: 89%

“…We acquire about five years' data of Mrk 509 from AGN watch website; they are the data used in Carone et al (1996) [7] . All of their 151 Hβ spectra are decomposed as described in the last section.…”

Section: Mrk 509mentioning

confidence: 99%

Diagnostics for the structure of AGNs’ broad line regions with reverberation mapping data: confirmation of the two-component broad line region model

Zhu

Zhang

2010

Sci. China Phys. Mech. Astron.

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“…This broad-emission-line gas is emitted within 0.1 pc of the central black hole (Peterson & Wandel 2000). In Mrk 509, the size of the broad line region (BLR) determined from Hβ measurements is 80 light-days (0.067 pc) (Carone et al 1996). The absorbing gas is probably located at a somewhat larger distance, although both aspects of the AGN phenomenon are likely to have similar abundances because of their close origin.…”

Section: Rgsmentioning

confidence: 99%

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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Optical Continuum and Emission‐Line Variability of the Seyfert 1 Galaxy Markarian 509

Cited by 29 publications

References 7 publications

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

Diagnostics for the structure of AGNs’ broad line regions with reverberation mapping data: confirmation of the two-component broad line region model

Multiwavelength campaign on Mrk 509

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