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Journal articles on the topic 'NGC 5548'

Author: Grafiati

Published: 4 June 2021

Last updated: 3 February 2022

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1

Kaastra, J. S., R. Mewe, J. Heise, F. J. M. Alkemade, C. J. Schrijver, and T. Carone. "EUVE Observations of NGC 5548." Symposium - International Astronomical Union 159 (1994): 325. http://dx.doi.org/10.1017/s0074180900175308.

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2

Kollatschny, W., and M. Dietrich. "Emission line variability in NGC 4593 and NGC 5548." Astrophysics and Space Science 205, no. 1 (1993): 179–84. http://dx.doi.org/10.1007/bf00657974.

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3

Rosenblatt, Edward I., and Matthew A. Malkan. "Broad Line Variations in NGC 5548." Symposium - International Astronomical Union 134 (1989): 114–15. http://dx.doi.org/10.1017/s0074180900140549.

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Since broad line variations can, in principle, constrain the structure and kinematics of the broad line region in active galaxies we have conducted a monitoring program of 20 Seyfert galaxies over a 5 year period in order to study broad line flux and profile changes. Included in our sample is the Seyfert 1.5 galaxy NGC 5548. Fifteen observations were taken from 1979 to 1984 mainly with the 60″ Palomar telescope and a SIT vidicon spectrograph. Measurements show (Fig. 1) that both the Hβ and Hγ line flux varied by 200% and the continuum varied by 300%. Furthermore, these changes were positively correlated as one would expect from photoionization by a central continuum source.

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4

Kaastra, J. S., K. C. Steenbrugge, A. J. J. Raassen, R. L. J. van der Meer, A. C. Brinkman, D. A. Liedahl, E. Behar, and A. de Rosa. "X-ray spectroscopy of NGC 5548." Astronomy & Astrophysics 386, no. 2 (May 2002): 427–45. http://dx.doi.org/10.1051/0004-6361:20020235.

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5

Nandra, K., A. C. Fabian, I. M. George, G. Branduardi-Raymont, A. Lawrence, K. O. Mason, I. M. McHardy, et al. "A ROSAT observation of NGC 5548." Monthly Notices of the Royal Astronomical Society 260, no. 3 (February 1, 1993): 504–12. http://dx.doi.org/10.1093/mnras/260.3.504.

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6

Kallman, T., and M. Elitzur. "Broad-line variability in NGC 5548." Astrophysical Journal 328 (May 1988): 523. http://dx.doi.org/10.1086/166310.

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7

Detmers, R. G., J. S. Kaastra, E. Costantini, I. M. McHardy, and F. Verbunt. "The warm absorber in NGC 5548." Astronomy & Astrophysics 488, no. 1 (June 16, 2008): 67–72. http://dx.doi.org/10.1051/0004-6361:200809862.

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8

Chiang, J., C. S. Reynolds, O. M. Blaes, M. A. Nowak, N. Murray, G. Madejski, H. L. Marshall, and P. Magdziarz. "SimultaneousEUVE/ASCA/RXTEObservations of NGC 5548." Astrophysical Journal 528, no. 1 (January 2000): 292–305. http://dx.doi.org/10.1086/308178.

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9

Bottorff, M. C., K. T. Korista, I. Shlosman, and R. D. Blandford. "Hydromagnetic Wind Model for the Broad-Line Region of NGC 5548." International Astronomical Union Colloquium 159 (1997): 215–16. http://dx.doi.org/10.1017/s0252921100040082.

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AbstractA hydromagnetic wind model from a dusty molecular disk (Emmering, Blandford, & Shlosman 1992) was applied to the BLR in NGC 5548 and produced synthetic C IV line profiles as a function of time. The model C IV profiles are compared to data from the 1993 IUE/HST campaign and properties of the the BLR of NGC 5548 are inferred.

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10

Panagiotou, C., I. E. Papadakis, E. S. Kammoun, and M. Dovčiak. "Multiwavelength power-spectrum analysis of NGC 5548." Monthly Notices of the Royal Astronomical Society 499, no. 2 (September 28, 2020): 1998–2006. http://dx.doi.org/10.1093/mnras/staa2920.

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ABSTRACT NGC 5548 was recently monitored intensively from NIR to X-rays as part of the STORM campaign. Its disc emission was found to lag behind the observed X-rays, while the measured time lag was increasing with wavelength. These results are consistent with the assumption that short-term variability in AGN emission is driven by the X-ray illumination of the accretion disc. In this work, we studied the power spectrum of UV/optical and X-ray emission of NGC 5548, using the data of the STORM campaign as well as previous Swift data, in order to investigate the relation between the UV/optical and X-ray variability and to examine its consistency with the above picture. We demonstrate that even the power spectrum results are compatible with a standard disc being illuminated by X-rays, with low accretion rates, but the details are not entirely consistent with the results from the modelling of the ‘τ versus λ’ relation. The differences indicate that the inner disc might be covered by a ‘warm corona’ which does not allow the detection of UV/optical emission from the inner disc. Finally, we found strong evidence that the UV emission of NGC 5548 is not stationary.

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11

Mao, Junjie, J. S. Kaastra, M. Mehdipour, Liyi Gu, E. Costantini, G. A. Kriss, S. Bianchi, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 612 (April 2018): A18. http://dx.doi.org/10.1051/0004-6361/201732162.

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The X-ray narrow emission line region (NELR) of the archetypal Seyfert 1 galaxy NGC 5548 has been interpreted as a single-phase photoionized plasma that is absorbed by some of the warm absorber components. This scenario requires those overlaying warm absorber components to have larger distance (to the central engine) than the X-ray NELR, which is not fully consistent with the distance estimates found in the literature. Therefore, we reanalyze the high-resolution spectra obtained in 2013–2014 with the Reflection Grating Spectrometer (RGS) aboard XMM-Newton to provide an alternative interpretation of the X-ray narrow emission features. We find that the X-ray narrow emission features in NGC 5548 can be described by a two-phase photoionized plasma with different ionization parameters (logξ = 1.3 and 0.1) and kinematics (vout = −50 and −400 km s−1), and no further absorption by the warm absorber components. The X-ray and optical NELR might be the same multi-phase photoionized plasma. Both X-ray and optical NELR have comparable distances, asymmetric line profiles, and the underlying photoionized plasma is turbulent and compact in size. The X-ray NELR is not the counterpart of the UV/X-ray absorber outside the line of sight because their distances and kinematics are not consistent. In addition, X-ray broad emission features that we find in the spectrum can be accounted for by a third photoionized emission component. The RGS spectrum obtained in 2016 is analyzed as well, where the luminosity of most prominent emission lines (the O VII forbidden line and O VIII Lyα line) are the same (at a 1σ confidence level) as in 2013–2014.

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12

Cappi, M., B. De Marco, G. Ponti, F. Ursini, P. O. Petrucci, S. Bianchi, J. S. Kaastra, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 592 (July 7, 2016): A27. http://dx.doi.org/10.1051/0004-6361/201628464.

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13

Arav, N., C. Chamberlain, G. A. Kriss, J. S. Kaastra, M. Cappi, M. Mehdipour, P. O. Petrucci, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 577 (April 28, 2015): A37. http://dx.doi.org/10.1051/0004-6361/201425302.

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14

Mehdipour, M., J. S. Kaastra, G. A. Kriss, M. Cappi, P. O. Petrucci, K. C. Steenbrugge, N. Arav, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 575 (February 13, 2015): A22. http://dx.doi.org/10.1051/0004-6361/201425373.

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15

Ursini, F., R. Boissay, P. O. Petrucci, G. Matt, M. Cappi, S. Bianchi, J. Kaastra, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 577 (April 28, 2015): A38. http://dx.doi.org/10.1051/0004-6361/201425401.

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16

Di Gesu, L., E. Costantini, J. Ebrero, M. Mehdipour, J. S. Kaastra, F. Ursini, P. O. Petrucci, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 579 (June 24, 2015): A42. http://dx.doi.org/10.1051/0004-6361/201525934.

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17

Whewell, M., G. Branduardi-Raymont, J. S. Kaastra, M. Mehdipour, K. C. Steenbrugge, S. Bianchi, E. Behar, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 581 (September 2015): A79. http://dx.doi.org/10.1051/0004-6361/201526742.

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18

Mehdipour, M., J. S. Kaastra, G. A. Kriss, M. Cappi, P. O. Petrucci, B. De Marco, G. Ponti, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 588 (April 2016): A139. http://dx.doi.org/10.1051/0004-6361/201527729.

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19

Ebrero, J., J. S. Kaastra, G. A. Kriss, L. Di Gesu, E. Costantini, M. Mehdipour, S. Bianchi, et al. "Anatomy of the AGN in NGC 5548." Astronomy & Astrophysics 587 (March 2016): A129. http://dx.doi.org/10.1051/0004-6361/201527808.

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20

Kollatschny, W., and M. Dietrich. "Line-Profile Variations in AGN." International Astronomical Union Colloquium 159 (1997): 201–2. http://dx.doi.org/10.1017/s0252921100040021.

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21

Shomshekova, S. A., E. K. Denissyuk, R. R. Valiullin, I. V. Reva, and A. V. Kusakin. "Photometric Studies of the Seyfert Galaxies NGC 3516, NGC 5548, NGC 3227, NGC 4051, NGC 4151, and NGC 7469." Astrophysics 62, no. 2 (May 10, 2019): 163–76. http://dx.doi.org/10.1007/s10511-019-09571-w.

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22

Kaastra, J. S., R. Mewe, and N. Roos. "Line Emission from Warm Material in NGC 5548." International Astronomical Union Colloquium 152 (1996): 51–55. http://dx.doi.org/10.1017/s0252921100035740.

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EUVE observations of the Seyfert 1 galaxy NGC 5548 have shown the presence of line emission features identified as a Ne VII/Ne VIII blend at 88 Å and Si VII emission at 70 Å. The lines show significant broadening (FWHM 3800 km s−1) placing the emitting region at the same distance as the inner broad-line region. A fit to a thermal plasma yields a temperature of 6 × 105 K. The line emission can be attributed to the warm absorbing material discovered before from oxygen and iron absorption features, which appears to be an optically thin (for the Lyman continuum), highly ionized phase of the broad-line region.

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23

Steenbrugge, K. C., J. S. Kaastra, C. P. de Vries, and R. Edelson. "XMM-NEWTON High resolution spectroscopy of NGC 5548." Astronomy & Astrophysics 402, no. 2 (April 14, 2003): 477–86. http://dx.doi.org/10.1051/0004-6361:20030261.

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24

Cackett, Edward M., and Keith Horne. "Photoionized Hβ emission in NGC 5548: it breathes!" Monthly Notices of the Royal Astronomical Society 365, no. 4 (December 15, 2005): 1180–90. http://dx.doi.org/10.1111/j.1365-2966.2005.09795.x.

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25

Pronik, I. "Emission Lines Variations in the Spectra of Seyfert Galaxies Nuclei. Observational Data." Symposium - International Astronomical Union 121 (1987): 169–84. http://dx.doi.org/10.1017/s0074180900155081.

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The emission lines variability in the spectra of Seyfert galaxies nuclei has been known for more than 20 years. The first report on the problem under consideration was made by Bardin et al.(1967). They published the data on the variation of relative intensities of forbidden 4959+5007 A and 4363 A [OIII] lines in the spectrum of NGC 5548 galaxy nucleus that exceed the errors of observations. It was noticed also that NGC 5548 was the second galaxy where the considered lines show variability. At least four review papers have been published: Lyutyi and V. Pronik (1975), Collin-Souffrin(1980), I. Pronik (1980), Penston(1982).

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26

Pronik, I. I. "Flows and Shocks in Variable Fluxes of Seyfert galaxies." Symposium - International Astronomical Union 217 (2004): 360–61. http://dx.doi.org/10.1017/s0074180900197931.

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Data collected from the optical through infrared to the radio show that the Seyfert galaxies NGC 1275, NGC 3227, NGC 4151, NGC 5548 and NGC 7469 exhibit signs of flows or jets. The characteristics of night-to-night variations of Balmer line profiles and/or intranight continuum variations were obtained and investigated at the Crimean Astrophysical Observatory. They permit to suppose, that short term variability of the Balmer lines and intranight continuum variations can be produced in short lived shocks as a result of strong energy output in the form of gas flows or jets.

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27

Orr, A., R. Walter, T. J. L. Courvoisier, H. H. Fink, F. Makino, C. Otani, and W. Wamsteker. "Simultaneous Observations of Seyfert 1 Galaxies by IUE, ROSAT and GINGA." Symposium - International Astronomical Union 159 (1994): 330. http://dx.doi.org/10.1017/s0074180900175357.

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Simultaneous observations of 8 Seyfert 1 type AGN (Fairall-9, Mrk 590, NGC 4051, 3C 273, NGC 5548, Mrk 841, Q 1821+643 and 3C 390.3) obtained with ROSAT and IUE (RIASS program), and for 5 sources (Fairall-9, NGC 4051, 3C 273, Mrk 841 and Q 1821+643) with Ginga, have been analysed with the aim of describing the UV to soft X-ray spectral component in these sources.

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28

Steenbrugge, K. C., and J. S. Kaastra. "Warm Winds in the Seyfert 1 Galaxy NGC 5548." Symposium - International Astronomical Union 217 (2004): 356–57. http://dx.doi.org/10.1017/s0074180900197918.

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We present the results of a recent long XMM-Newton and Chandra observation on the Seyfert 1 galaxy NGC 5548. This galaxy has a warm absorber with a wide range of ionization stages. The detection of O VI in both the UV and X-rays allows for a direct comparison of the measured column density in both wavelength bands. We also comment on the detection of O V, and its newly measured wavelength.

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29

ISMAILOV, NARIMAN Z., and ULVIYYE Z. BASHIROVA. "ON THE LONG TIME SPECTRAL VARIABILITY OF NGC 5548." Publications of The Korean Astronomical Society 30, no. 2 (September 30, 2015): 531–33. http://dx.doi.org/10.5303/pkas.2015.30.2.531.

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30

Peterson, B. M., and G. J. Ferland. "An accretion event in the Seyfert galaxy NGC 5548." Nature 324, no. 6095 (November 1986): 345–47. http://dx.doi.org/10.1038/324345a0.

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31

Crenshaw, D. M., S. B. Kraemer, H. R. Schmitt, J. S. Kaastra, N. Arav, J. R. Gabel, and K. T. Korista. "MASS OUTFLOW IN THE SEYFERT 1 GALAXY NGC 5548." Astrophysical Journal 698, no. 1 (May 20, 2009): 281–92. http://dx.doi.org/10.1088/0004-637x/698/1/281.

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32

Koen, C. "Transfer function analysis of ultraviolet observations of NGC 5548." Monthly Notices of the Royal Astronomical Society 262, no. 4 (June 15, 1993): 823–30. http://dx.doi.org/10.1093/mnras/262.4.823.

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33

Iijima, T. "Recent spectral variations of the Seyfert galaxy NGC 5548." Astrophysics and Space Science 206, no. 2 (1993): 235–48. http://dx.doi.org/10.1007/bf00658148.

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34

Collin-Souffrin, S., A. M. Dumont, and L. Nazarova. "Inconsistency of Photoionization Models for NGC 5548: Proof of Mechanical Heating?" International Astronomical Union Colloquium 159 (1997): 217–19. http://dx.doi.org/10.1017/s0252921100040094.

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AbstractIt is shown that, in the case of NGC 5548, photoionization models cannot account for line fluxes, line ratios, and line variations. The assumption that a fraction of the broad-line region is mechanically heated can solve the problem.

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35

Ma, Zhen Guo. "Fe Kα Lines of Seyfert I Galaxies: Thin-Torus Model." Symposium - International Astronomical Union 214 (2003): 275–80. http://dx.doi.org/10.1017/s0074180900194562.

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In order to elucidate the physics of the Fe Kα line emissions from Seyfert (-like) AGNs, we propose a thin-torus model in Kerr metric and fit it to three galaxies (i.e., NGC 3516, 3C 273, and NGC 5548). It is found that only spinning-BH galaxies radiate observable line flux from a region within tens of gravitational radii of a central BH. Besides, the observer's inclination angle is around 30°.

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36

Bochkarev, N. G., A. I. Shapovalova, A. N. Burenkov, and V. V. Vlasyuk. "11.6. Spectral monitoring of AGN at the 6 meter telescope." Symposium - International Astronomical Union 184 (1998): 467–68. http://dx.doi.org/10.1017/s0074180900085600.

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To study broad line region (BLR) size and kinematics spectral monitoring of NGC 3516, NGC 4151, NGC 5548, NGC 7469 and 3C390.3 has been performed with the 6 m telescope of the Special Astrophysical Observatory (N. Arkhyz- North Caucasus) in 1986–1996. The spectra are obtained in the Nasmyth focus using the TV scanner with a resolution of 3–4Å and S/N= 10–25 within 4000–5200ÅÅ (1986–94, 500 spectra), and in the prime focus with the spectrograph UAGS (a long-slit mode) + CCD (resolution 5–10Å) or multi-pupil field spectrograph (MPFS) + CCD (resolution 4Å) within 4000–7000ÅÅ and S/N=50–100 (1995–96, 270 spectra).

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37

Belete, A. Bewketu, L. J. Goicoechea, I. C. Leão, B. L. Canto Martins, and J. R. De Medeiros. "A Novel Approach to Study the Variability of NGC 5548." Astrophysical Journal 879, no. 2 (July 12, 2019): 113. http://dx.doi.org/10.3847/1538-4357/ab2457.

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38

Peterson, B. M., and K. T. Korista. "Intensive Spectroscopic Monitoring of NGC 5548 with HST and IUE." Symposium - International Astronomical Union 159 (1994): 177–80. http://dx.doi.org/10.1017/s0074180900174984.

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We present preliminary results on a combined HST/IUE/ground-based monitoring campaign on the Seyfert 1 galaxy NGC 5548 undertaken by the International AGN Watch in order to answer questions that require both high temporal resolution (one day) and high signal-to-noise ratios. Our preliminary conclusions are (1) the ultraviolet and optical continuum variations are simultaneous to within a day (2) the He II λ1640 variations lag behind the continuum by about 1.7 days, and (3) the velocity field of the C IV-emitting region is not characterized by bulk by radial motion, but the higher velocity gas seems to originate closer to the continuum source than the lower velocity gas.

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39

Iwasawa, K., A. C. Fabian, and K. Nandra. "ASCA and ROSAT observations of NGC 5548: discrepant spectral indices." Monthly Notices of the Royal Astronomical Society 307, no. 3 (August 11, 1999): 611–18. http://dx.doi.org/10.1046/j.1365-8711.1999.02664.x.

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40

Clavel, J., K. Nandra, F. Makino, K. A. Pounds, G. A. Reichert, C. M. Urry, W. Wamsteker, M. Peracaula-Bosch, G. C. Stewart, and C. Otani. "Correlated hard X-ray and ultraviolet variability in NGC 5548." Astrophysical Journal 393 (July 1992): 113. http://dx.doi.org/10.1086/171490.

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41

Horne, Keith, William F. Welsh, and Bradley M. Peterson. "Echo mapping of broad H-beta emission in NGC 5548." Astrophysical Journal 367 (January 1991): L5. http://dx.doi.org/10.1086/185919.

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42

Bottorff, Mark C., Kirk T. Korista, and Isaac Shlosman. "Dynamics of Warm Absorbing Gas in Seyfert Galaxies: NGC 5548." Astrophysical Journal 537, no. 1 (July 2000): 134–51. http://dx.doi.org/10.1086/309006.

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43

Magdziarz, P., and O. Blaes. "A Model of the Broad-Band Continuum of NGC 5548." Symposium - International Astronomical Union 188 (1998): 430–31. http://dx.doi.org/10.1017/s0074180900115876.

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We discuss a model of the central source in Seyfert 1 galaxy NGC 5548. The model assumes a three phase disk structure consisting of a cold outer disk, a hot central disk constituting a Comptonizing X/γ source, and an intermediate unstable and complex phase emitting a soft excess component. The model qualitatively explains broad-band spectrum and variability behavior assuming that the soft excess contributes significantly to the continuum emission and drives variability by geometrical changes of the intermediate disk zone.

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44

Gardner, Emma, and Chris Done. "The origin of the UV/optical lags in NGC 5548." Monthly Notices of the Royal Astronomical Society 470, no. 3 (April 21, 2017): 3591–605. http://dx.doi.org/10.1093/mnras/stx946.

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45

Done, C., K. A. Pounds, K. Nandra, and A. C. Fabian. "The complex variable soft X-ray spectrum of NGC 5548." Monthly Notices of the Royal Astronomical Society 275, no. 2 (July 1995): 417–28. http://dx.doi.org/10.1093/mnras/275.2.417.

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46

Mathur, Smita, Martin Elvis, and Belinda Wilkes. "Testing Unified X-Ray/Ultraviolet Absorber Models with NGC 5548." Astrophysical Journal 452 (October 1995): 230. http://dx.doi.org/10.1086/176294.

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47

Done, Christine, and Julian H. Krolik. "Kinematics of the Broad Emission Line Region in NGC 5548." Astrophysical Journal 463 (May 1996): 144. http://dx.doi.org/10.1086/177230.

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48

Mathur, Smita, Martin Elvis, and Belinda Wilkes. "Multiple Velocity Components in the CivAbsorption Line of NGC 5548." Astrophysical Journal 519, no. 2 (July 10, 1999): 605–9. http://dx.doi.org/10.1086/307416.

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49

Landt, Hermine, Martin J. Ward, Katrien C. Steenbrugge, and Gary J. Ferland. "Strong variability of the coronal line region in NGC 5548." Monthly Notices of the Royal Astronomical Society 454, no. 4 (October 20, 2015): 3688–96. http://dx.doi.org/10.1093/mnras/stv2176.

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50

Srianand, R. "High‐Resolution Study of Associated CivAbsorption Systems in NGC 5548." Astrophysical Journal 528, no. 2 (January 10, 2000): 617–25. http://dx.doi.org/10.1086/308214.

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