The outflow in Mrk 509

Detmers, R. G.; Kaastra, J. S.; Costantini, E.; Verbunt, F.; Cappi, M.; Vries, C. de

doi:10.1051/0004-6361/200913879

Cited by 17 publications

(30 citation statements)

References 28 publications

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“…A simultaneous fit to the pn and RGS data of these spectra showed three ionisation components that correspond to our components B, C, and a blend of D and E. Components B and C did not show any significant variability between the observations. The fits of Detmers et al (2010) indicate that the ionisation parameter for component D/E had decreased from 3.29 ± 0.04 in the first observation of 2005 to 3.01 ± 0.06 in the 2006 observation. From this change within 0.5 year an upper limit to the distance of 0.5 pc was derived.…”

Section: Discussionmentioning

confidence: 95%

“…Our present estimates are more direct. Detmers et al (2010) analysed the XMM-Newton spectra of Mrk 509 taken in 2005 and 2006. A simultaneous fit to the pn and RGS data of these spectra showed three ionisation components that correspond to our components B, C, and a blend of D and E. Components B and C did not show any significant variability between the observations.…”

Section: Discussionmentioning

confidence: 99%

“…Such a value clearly contradicts our lower limit of about 5 pc for components D and E. With our present model, however, a change in 0.5 year would correspond to a distance of about 15 pc, much larger than 0.5 pc. The discrepancy can be traced down to the use of Fe xii to estimate the recombination time scale by Detmers et al (2010). This ion has its peak concentration near the ionisation parameter for component D/E.…”

Section: Discussionmentioning

confidence: 99%

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Multiwavelength campaign on Mrk 509

Kaastra

Detmers

Mehdipour

et al. 2012

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Aims. More than half of all active galactic nuclei show strong photoionised outflows. A major uncertainty in models for these outflows is the distance of the gas to the central black hole. We use the results of a massive multiwavelength monitoring campaign on the bright Seyfert 1 galaxy Mrk 509 to constrain the location of the outflow components dominating the soft X-ray band. Methods. Mrk 509 was monitored by XMM-Newton and other satellites in 2009. We have studied the response of the photoionised gas to the changes in the ionising flux produced by the central regions. We used the five discrete ionisation components A-E that we detected in the time-averaged spectrum taken with the RGS instrument. By using the ratio of fluxed EPIC-pn and RGS spectra, we were able to put tight constraints on the variability of the absorbers. Monitoring with the Swift satellite started six weeks before the XMM-Newton observations. This allowed us to use the history of the ionising flux and to develop a model for the time-dependent photoionisation in this source. Results. Components A and B are too weak for variability studies, but the distance for component A is already known from optical imaging of the [O iii] line to be about 3 kpc. During the five weeks of the XMM-Newton observations we found no evidence of changes in the three X-ray dominant ionisation components C, D, and E, despite a huge soft X-ray intensity increase of 60% in the middle of our campaign. This excludes high-density gas close to the black hole. Instead, using our time-dependent modelling, we find that the density is very low, and we derive firm lower limits to the distance of these components. For component D we find evidence for variability on longer time scales by comparing our spectra to archival data taken in 2000 and 2001, yielding an upper limit to the distance. For component E we derive an upper limit to the distance based on the argument that the thickness of the absorbing layer must be less than its distance to the black hole. Combining these results, at the 90% confidence level, component C has a distance of >70 pc, component D is between 5-33 pc, and component E has a distance >5 pc but smaller than 21-400 pc, depending upon modelling details. These results are consistent with the upper limits that we derived from the HST/COS observations of our campaign and point to an origin of the dominant, slow (v < 1000 km s −1 ) outflow components in the NLR or torus-region of Mrk 509.

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Section: Discussionmentioning

confidence: 95%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Multiwavelength campaign on Mrk 509

Kaastra

Detmers

Mehdipour

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“…For both sources, the presence of a warm absorber was confirmed, and its features could explain the residuals of the fit. The most complete studies of the warm absorber of these two objects were done using XMM/RGS data by Smith et al (2007) and Detmers et al (2010) for Mrk 509, and by Longinotti et al (2010) for Mrk 841.…”

Section: Additional Contribution Of the Warm Absorbermentioning

confidence: 99%

“…Using Ginga, Singh et al (1990) revealed a hardening of the power law at energies greater than 10 keV. BeppoSAX observations (Perola et al 2000) showed a power-law cut-off at 70 keV and revealed information about the warm absorber (Dadina et al 2005), which since has been studied in depth by Smith et al (2007) and Detmers et al (2010), with XMM-Newton/RGS data. Ponti et al (2009) presented the most complete study to date of the Fe K complex, using XMM-Newton data and the same Suzaku observations we present here.…”

Section: Introductionmentioning

confidence: 96%

Suzakubroad-band observations of the Seyfert 1 galaxies Mrk 509 and Mrk 841

Cerruti¹,

Ponti²,

Boisson³

et al. 2011

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Context. Markarian 509 and Markarian 841 are two bright Seyfert 1 galaxies with X-ray spectra characterised by a strong soft excess and a variable Fe Kα line, as shown by several X-ray observatories in the past. Aims. We report an analysis and modelling of new Suzaku observations of these sources, taken between April and November, 2006, for Mrk 509, and between January and July, 2007, for Mrk 841, for a total exposure time of ≈100 ks each. Data from XIS and HXD/PIN instruments, going from 0.5 to 60 keV, represent the highest spectral resolution simultaneous broad-band X-ray spectrum for these objects, and provide the strongest constraints yet on the origin of the soft excess emission. Methods. We fitted the broad-band spectrum of both sources with a double Comptonisation model, adding neutral reflection from distant material and a two-phase warm absorber. We then studied the two competing models developed to explain the soft excess in terms of atomic processes: a blurred ionised disc reflection and an ionised absorption by a high velocity material. Results. When fitting the data in the 3-10 keV range with a power law spectrum, and extrapolating this result to low energies, a soft excess is clearly observed below 2 keV, although its strength is weak compared to previous observations of both sources. A moderate hard excess is seen at energies higher than 10 keV, together with a neutral Fe Kα narrow emission line at E 0 ≈ 6.4 keV and a broad Fe emission line. For Mrk 509, the broad Fe emission line is required in all the three physical models to ensure a good fit to the data: this finding suggests that the blurred reflection model correctly describes the soft excess, but that it underestimates the broad Fe emission line. For the smeared absorption model, this suggests instead that the continuum spectrum absorbed by the outflowing gas should indeed contain a reflected component. For Mrk 841, all three models that we tested provide a good fit to the data, and we cannot rule out any of them. A broad emission line is required in the double Comptonisation and smeared absorption models, while the blurred reflection model consistently fits the broad-band spectrum, without adding any extra emission-line component.

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Multiwavelength campaign on Mrk 509

Kaastra

Petrucci

Cappi

et al. 2011

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Context. Active galactic nuclei (AGN) show a wealth of interesting physical processes, some of which are poorly understood. In a broader context, they play an important role in processes that are far beyond their immediate surroundings, owing to the high emitted power. Aims. We want to address a number of open questions, including the location and physics of the outflow from AGN, the nature of the continuum emission, the geometry and physical state of the X-ray broad emission line region, the Fe-K line complex, the metal abundances of the nucleus, and finally the interstellar medium of our own Galaxy as seen through the signatures it imprints on the X-ray and UV spectra of AGN. Methods. We study one of the best targets for these aims, the Seyfert 1 galaxy Mrk 509 with a multiwavelength campaign using five satellites (XMM-Newton, INTEGRAL, Chandra, HST, and Swift) and two ground-based facilities (WHT and PAIRITEL). Our observations cover more than five decades in frequency, from 2 μm to 200 keV. The combination of high-resolution spectroscopy and time variability allows us to disentangle and study the different components. Our campaign covers 100 days from September to December 2009, and is centred on a simultaneous set of deep XMM-Newton and INTEGRAL observations with regular time intervals, spanning seven weeks. Results. We obtain a continuous light curve in the X-ray and UV band, showing a strong, up to 60% flux increase in the soft X-ray band during the three weeks in the middle of our deepest monitoring campaign, and which is correlated with an enhancement of the UV flux. This allows us to study the time evolution of the continuum and the outflow. By stacking the observations, we have also obtained one of the best X-ray and UV spectra of a Seyfert galaxy ever obtained. In this paper we also study the effects of the spectral energy distribution (SED) that we obtained on the photo-ionisation equilibrium. Thanks to our broad-band coverage, uncertainties on the SED do not strongly affect the determination of this equilibrium. Conclusions. Here we present our very successful campaign and in a series of subsequent papers we will elaborate on different aspects of our study.

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The outflow in Mrk 509

Cited by 17 publications

References 28 publications

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

Suzakubroad-band observations of the Seyfert 1 galaxies Mrk 509 and Mrk 841

Multiwavelength campaign on Mrk 509

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