A High Resolution View of the Warm Absorber in the Quasar MR 2251-178

Reeves, J. N.; Porquet, D.; Braito, V.; Gofford, J.; Nardini, E.; Turner, T. J.; Crenshaw, D. Michael; Kraemer, S. B.

doi:10.1088/0004-637x/776/2/99

Cited by 38 publications

(37 citation statements)

References 135 publications

(178 reference statements)

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“…J.N. Theureau, G., Hanski, M. O., Coudreau, N., Hallet, N., & Martin, J.-M. 2007, A&A, 465, 71 Tombesi, F., Meléndez, M., Veilleux, S., et al 2015 Tombesi, F., Cappi, M., Reeves, J. N., et al 2013, MNRAS, 430, 1102 Tombesi, F., Cappi, M., Reeves, J. N., et al 2010, A&A, 521, A57 Tremaine, S., Gebhardt, K., Bender, R., et al 2002 Tripathi, S., Misra, R., Dewangan, G., & Rastogi, S. 2011, ApJ, 736, L37 Turner, A. K., Fabian, A. C., Lee, J. C., & Vaughan, S. 2004, MNRAS, 353, 319 Turner, T. J., Reeves, J. N., Kraemer, S. B., & Miller, L. 2008, A&A, 483, 161 Walton, D. J., Nardini, E., Fabian, A. C., Gallo, L. C., & Reis, R. C. 2013, MNRAS, 428, 2901 Weisskopf, M. C., Hester, J. J., Tennant, A. F., et al 2000, ApJ, 536, L81 Willingale, R., Starling, R. L. C., Beardmore, A. P., Tanvir, N. R., & O'Brien, P. T. 2013, MNRAS, 431, 394 Wilms, J., Allen, A., & McCray, R. 2000, ApJ, 542, 914 Yaqoob, T., McKernan, B., Kraemer, S. B., et al 2003, ApJ, 582, 105 Zhang, S. N., Ji, L., Marshall, H. L., et al 2011, MNRAS, 410, 2274 Zhou, X.-L., Zhang, S.-N., Wang, D.-X., & Zhu, L. 2010, ApJ, 710, 16 This preprint was prepared with the AAS L A T E X macros v5.2. Table 1.…”

Section: Acknowledgementsmentioning

confidence: 98%

High-resolution X-Ray Spectroscopy of the Seyfert 1 Galaxy Mrk 1040. Revealing the Failed Nuclear Wind with Chandra

Reeves

Braito

Behar

et al. 2017

ApJ

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High resolution X-ray spectroscopy of the warm absorber in the nearby X-ray bright Seyfert 1 galaxy, Mrk 1040 is presented. The observations were carried out in the 2013-2014 timeframe using the Chandra High Energy Transmission Grating with a total exposure of 200 ks. A multitude of absorption lines from Ne, Mg and Si are detected from a wide variety of ionization states. In particular, the detection of inner K-shell absorption lines from Ne, Mg and Si, from charge states ranging from F-like to Li-like ions, suggests the presence of a substantial amount of low ionization absorbing gas, illuminated by a steep soft X-ray continuum. The observations reveal at least 3 warm absorbing components ranging in ionization parameter from log(ξ/erg cm s −1 ) = 0 − 2 and with column densities of N H = 1.5 − 4.0 × 10 21 cm −2 . The velocity profiles imply that the outflow velocities of the absorbing gas are low and within ±100 km s −1 of the systemic velocity of Mrk 1040, which suggests any outflowing gas may have stalled in this AGN on large enough scales. The warm absorber is likely located far from the black hole, within 300 pc of the nucleus and is spatially coincident with emission from an extended Narrow Line Region as seen in the HST images. The iron K band spectrum reveals only narrow emission lines, with Fe Kα at 6.4 keV consistent with originating from reflection off Compton thick pc-scale reprocessing gas.

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Section: Acknowledgementsmentioning

confidence: 98%

High-resolution X-Ray Spectroscopy of the Seyfert 1 Galaxy Mrk 1040. Revealing the Failed Nuclear Wind with Chandra

Reeves

Braito

Behar

et al. 2017

ApJ

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“…A turbulence velocity of σ=300 km s −1 was chosen to account for any narrow absorption lines. The ionization parameter of the absorption table was varied between x = log 0 3 -9 to allow for the typical range in ionization seen toward other Seyfert 1s, with prominent warm absorption components (Kaspi et al 2002;Blustin et al 2005;Detmers et al 2011;Reeves et al 2013;Di Gesu et al 2015). The total N H column was recorded for each value of the ionization parameter, in increments of 0.1 in x log space.…”

Section: Is There Any Warm Absorption Toward Ark 120?mentioning

confidence: 99%

A Deep X-Ray View of the Bare Agn Ark 120. I. Revealing the Soft X-Ray Line Emission

Reeves

Porquet

Braito

et al. 2016

ApJ

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The Seyfert 1 galaxy Ark 120 is a prototype example of the so-called class of bare nucleus active galactic nuclei (AGNs), whereby there is no known evidence for the presence of ionized gas along the direct line of sight. Here deep (>400 ks exposure), high-resolution X-ray spectroscopy of Ark 120 is presented from XMM-Newton observations that were carried out in 2014 March, together with simultaneous Chandra/High Energy Transmission Grating exposures. The high-resolution spectra confirmed the lack of intrinsic absorbing gas associated with Ark 120, with the only X-ray absorption present originating from the interstellar medium (ISM) of our own Galaxy, with a possible slight enhancement of the oxygen abundance required with respect to the expected ISM values in the solar neighborhood. However, the presence of several soft X-ray emission lines are revealed for the first time in the XMM-Newton RGS spectrum, associated with the AGN and arising from the He-and H-like ions of N, O, Ne, and Mg. The He-like line profiles of N, O, and Ne appear velocity broadened, with typical FWHMs of ∼5000 km s −1 , whereas the H-like profiles are unresolved. From the clean measurement of the He-like triplets, we deduce that the broad lines arise from a gas of density n e ∼10 11 cm −3 , while the photoionization calculations infer that the emitting gas covers at least 10% of 4π steradian. Thus the broad soft X-ray profiles appear coincident with an X-ray component of the optical-UV broad-line region on sub-parsec scales, whereas the narrow profiles originate on larger parsec scales, perhaps coincident with the AGN narrow-line region. The observations show that Ark 120 is not intrinsically bare and substantial X-ray-emitting gas exists out of our direct line of sight toward this AGN.

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“…Turner et al 1997Turner et al , 1998 but also type 1 and intermediate Seyferts (e.g., Malizia et al 1997;Pounds et al 2004;Miller et al 2007;Bianchi et al 2009;Turner et al 2009;Risaliti et al 2010;Lobban et al 2011;Marchese et al 2012;Longinotti et al 2009Longinotti et al , 2013Reeves et al 2013;Walton et al 2014;Miniutti et al 2014;Rivers et al 2015). In some cases, the columns are so large that astronomers have called these "changing look" sources (i.e.…”

Section: Introductionmentioning

confidence: 99%

Anatomy of the AGN in NGC 5548

Cappi

Marco

Ponti

et al. 2016

A&A

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In 2013, we conducted a large multi-wavelength campaign on the archetypical Seyfert 1 galaxy NGC 5548. Unexpectedly, this usually unobscured source appeared strongly absorbed in the soft X-rays during the entire campaign, and signatures of new and strong outflows were present in the almost simultaneous UV HST/COS data. Here we carry out a comprehensive spectral analysis of all available XMM-Newton observations of NGC 5548 (precisely 14 observations from our campaign plus three from the archive, for a total of ∼763 ks) in combination with three simultaneous NuSTAR observations. We obtain a best-fit underlying continuum model composed by i) a weakly varying flat (Γ ∼ 1.5-1.7) power-law component; ii) a constant, cold reflection (FeK + continuum) component; iii) a soft excess, possibly owing to thermal Comptonization; and iv) a constant, ionized scattered emission-line dominated component. Our main findings are that, during the 2013 campaign, the first three of these components appear to be partially covered by a heavy and variable obscurer that is located along the line of sight (LOS), which is consistent with a multilayer of cold and mildly ionized gas. We characterize in detail the short timescale (mostly ∼ks-to-days) spectral variability of this new obscurer, and find it is mostly due to a combination of column density and covering factor variations, on top of intrinsic power-law (flux and slope) variations. In addition, our best-fit spectrum is left with several (but marginal) absorption features at rest-frame energies ∼6.7−6.9 keV and ∼8 keV, as well as a weak broad emission line feature redwards of the 6.4 keV emission line. These could indicate a more complex underlying model, e.g. a P-Cygni-type emission profile if we allow for a large velocity and wide-angle outflow. These findings are consistent with a picture where the obscurer represents the manifestation along the LOS of a multilayer of gas, which is also in multiphase, and which is likely outflowing at high speed, and simultaneously producing heavy obscuration and scattering in the X-rays, as well as broad absorption features in the UV.

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A High Resolution View of the Warm Absorber in the Quasar MR 2251-178

Cited by 38 publications

References 135 publications

High-resolution X-Ray Spectroscopy of the Seyfert 1 Galaxy Mrk 1040. Revealing the Failed Nuclear Wind with Chandra

High-resolution X-Ray Spectroscopy of the Seyfert 1 Galaxy Mrk 1040. Revealing the Failed Nuclear Wind with Chandra

A Deep X-Ray View of the Bare Agn Ark 120. I. Revealing the Soft X-Ray Line Emission

Anatomy of the AGN in NGC 5548

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