Skip to main content Accessibility help
×
Home

Accretion and outflow of gas in Markarian 509

  • Jelle Kaastra (a1) (a2), Pierre-Olivier Petrucci (a3), Massimo Cappi (a4), Nahum Arav (a5), Ehud Behar (a6), Stefano Bianchi (a7), Graziella Branduardi-Raymont (a8), Elisa Costantini (a1), Jacobo Ebrero (a1), Jerry Kriss (a9) (a10), Missagh Mehdipour (a8), Stephane Paltani (a11), Ciro Pinto (a1), Gabriele Ponti (a12), Katrien Steenbrugge (a13) (a14) and Cor de Vries (a1)...

Abstract

A major uncertainty in models for photoionised outflows in AGN is the distance of the gas to the central black hole. We present 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. Mrk 509 was monitored by XMM-Newton, Integral, Chandra, HST/COS and Swift in 2009. We have studied the response of the photoionised gas to the changes in the ionising flux produced by the central regions. We were able to put tight constraints on the variability of the absorbers from day to year time scales. This allowed us to develop a model for the time-dependent photoionisation in this source. We find that the more highly ionised gas producing most X-ray line opacity is at least 5 pc away from the core; upper limits to the distance of various absorbing components range between 20 pc up to a few kpc. The more lowly ionised gas producing most UV line opacity is at least 100 pc away from the nucleus. These results point to an origin of the dominant, slow (v<1000 km s−1) outflow components in the NLR or torus-region of Mrk 509. We find that while the kinetic luminosity of the outflow is small, the mass carried away is likely larger than the 0.5 Solar mass per year accreting onto the black hole. We also determined the chemical composition of the outflow as well as valuable constraints on the different emission regions. We find for instance that the resolved component of the Fe-K line originates from a region 40–1000 gravitational radii from the black hole, and that the soft excess is produced by Comptonisation in a warm (0.2–1 keV), optically thick (τ~ 10–20) corona near the inner part of the disk.

    • Send article to Kindle

      To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

      Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

      Find out more about the Kindle Personal Document Service.

      Accretion and outflow of gas in Markarian 509
      Available formats
      ×

      Send article to Dropbox

      To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

      Accretion and outflow of gas in Markarian 509
      Available formats
      ×

      Send article to Google Drive

      To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

      Accretion and outflow of gas in Markarian 509
      Available formats
      ×

Copyright

References

Hide All
Arav, N., Edmonds, D., Borguet, B., et al. 2012, A&A, 544, A33
Detmers, R. G., Kaastra, J. S., Steenbrugge, K. C., et al. 2011, A&A, 534, A38
Ebrero, J., Kriss, G. A., Kaastra, J. S., et al. 2011, A&A, 534, A40
Kaastra, J. S., Petrucci, P.-O., Cappi, M., et al. 2011a, A&A, 534, A36
Kaastra, J. S., de Vries, C. P., Steenbrugge, K. C., et al. 2011b, A&A, 534, A37
Kaastra, J. S., Detmers, R. G., Mehdipour, M., et al. 2012, A&A, 539, A117
Kriss, G. A., Arav, N., Kaastra, J. S., et al. 2011, A&A, 534, A41
Mehdipour, M., Branduardi-Raymont, G., Kaastra, J. S., et al. 2011, A&A, 534, A39
Petrucci, P.-O., Paltani, S., Malzac, J., et al. 2012, A&A, in press (arXiv1209.6438)
Phillips, M. M., Bladwin, J. A., Atwood, B., & Carswell, R. F. 1983, ApJ, 274, 558
Pinto, C., Kriss, G. A., Kaastra, J. S., et al. 2012, A&A, 541, A147
Ponti, G., Cappi, M., Costantini, E., et al. 2012, A&A, in press (arXiv1207.0831)
Steenbrugge, K. C., Kaastra, J. S., Detmers, R. G., et al. 2011, A&A, 534, A42
MathJax
MathJax is a JavaScript display engine for mathematics. For more information see http://www.mathjax.org.

Keywords

Accretion and outflow of gas in Markarian 509

  • Jelle Kaastra (a1) (a2), Pierre-Olivier Petrucci (a3), Massimo Cappi (a4), Nahum Arav (a5), Ehud Behar (a6), Stefano Bianchi (a7), Graziella Branduardi-Raymont (a8), Elisa Costantini (a1), Jacobo Ebrero (a1), Jerry Kriss (a9) (a10), Missagh Mehdipour (a8), Stephane Paltani (a11), Ciro Pinto (a1), Gabriele Ponti (a12), Katrien Steenbrugge (a13) (a14) and Cor de Vries (a1)...

Metrics

Full text views

Total number of HTML views: 0
Total number of PDF views: 0 *
Loading metrics...

Abstract views

Total abstract views: 0 *
Loading metrics...

* Views captured on Cambridge Core between <date>. This data will be updated every 24 hours.

Usage data cannot currently be displayed