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  • 1
    Online Resource
    Online Resource
    Oxford University Press (OUP) ; 2020
    In:  Monthly Notices of the Royal Astronomical Society Vol. 497, No. 3 ( 2020-09-21), p. 2992-3010
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 497, No. 3 ( 2020-09-21), p. 2992-3010
    Abstract: The extreme ultraviolet region (EUV) provides most of the ionization that creates the high equivalent width (EW) broad and narrow emission lines (BELs and NELs) of quasars. Spectra of hypermassive Schwarzschild black holes (HMBHs; MBH ≥ 1010 M⊙) with α-discs, decline rapidly in the EUV suggesting much lower EWs. Model spectra for BHs of mass 106–1012 M⊙ and accretion rates 0.03 ≤ Lbol/LEdd ≤ 1.0 were input to the cloudy photoionization code. BELs become ∼100 times weaker in EW from MBH ∼ 108 M⊙ to MBH ∼ 1010 M⊙. The high-ionization BELs (O vi 1034 Å, C iv 1549 Å, and He ii 1640 Å) decline in EW from MBH ≥ 106 M⊙, reproducing the Baldwin effect, but regain EW for MBH ≥ 1010 M⊙. The low-ionization lines (Mg ii 2798 Å, H β 4861 Å, and H α 6563 Å) remain weak. Lines for maximally spinning HMBHs behave similarly. Line ratio diagrams for the BELs show that high O vi/H β and low C iv/H α may pick out HMBH, although O vi is often hard to observe. In NEL BPT diagrams, HMBHs lie among star-forming regions, except for highly spinning, high accretion rate HMBHs. In summary, the BELs expected from HMBHs would be hard to detect using the current optical facilities. From 100 to 1012 M⊙, the emission lines used to detect active galactic nuclei (AGNs) only have high EW in the 106–109 M⊙ window, where most AGNs are found. This selection effect may be distorting reported distributions of MBH.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2020
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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  • 2
    Online Resource
    Online Resource
    Oxford University Press (OUP) ; 2020
    In:  Monthly Notices of the Royal Astronomical Society Vol. 495, No. 3 ( 2020-07-01), p. 3373-3386
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 495, No. 3 ( 2020-07-01), p. 3373-3386
    Abstract: The primary X-ray emission from active galactic nuclei (AGNs), described by a power-law, irradiates the accretion disc producing reflection features in the spectrum. The reflection features arising from the inner regions of the disc can be significantly modified by the relativistic effects near the black hole. We investigate the relationship between the relativistic reflection fraction Rf, defined as the ratio of the coronal intensity that illuminates the accretion disc to the coronal intensity observed directly, and the hard X-ray photon index Γ of a Nuclear Spectroscopic Telescope Array (NuSTAR) sample of Seyfert 1 galaxies. The X-ray spectra are modelled using relxill code that helps to directly obtain the reflection fraction of a relativistically smeared reflection component. The parameter Rf depends on the amount of Comptonized X-ray emission intercepted by the inner accretion disc. We found a positive correlation between Γ and Rf in our sample. Seed photons from a larger area of an accretion disc entering the corona will result in increased cooling of the coronal plasma, giving rise to steeper X-ray spectrum. The corona irradiating the larger area of the disc will result in higher reflection fraction. Thus, the observed Rf –Γ relation is most likely related to the variations in the disc–corona geometry of AGNs.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2020
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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  • 3
    Online Resource
    Online Resource
    Oxford University Press (OUP) ; 2017
    In:  Monthly Notices of the Royal Astronomical Society Vol. 472, No. 3 ( 2017-12-11), p. 3492-3511
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 472, No. 3 ( 2017-12-11), p. 3492-3511
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2017
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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  • 4
    In: The Astrophysical Journal Letters, American Astronomical Society, Vol. 933, No. 2 ( 2022-07-01), p. L34-
    Abstract: We present a follow-up study on the recent detection of two X-ray flaring events by MAXI/Gas Slit Camera observations in soft and hard X-rays from MAXI J0709–159 in the direction of HD 54786 (LY CMa), on 2022 January 25. The X-ray luminosity during the flare was around 10 37 erg s −1 (MAXI), which got reduced to 10 32 erg s −1 (NuSTAR) after the flare. We took low-resolution spectra of HD 54786 from the 2.01 m Himalayan Chandra Telescope and the 2.34 m Vainu Bappu Telescope (VBT) facilities in India, on 2022 February 1 and 2. In addition to H α emission, we found emission lines of He i in the optical spectrum of this star. By comparing our spectrum of the object with those from the literature we found that He i lines show variability. Using photometric studies we estimate that the star has an effective temperature of 20,000 K. Although HD 54786 is reported as a supergiant in previous studies, our analysis favors it to be evolving off the main sequence in the color–magnitude diagram. We could not detect any infrared excess, ruling out the possibility of IR emission from a dusty circumstellar disk. Our present study suggests that HD 54786 is a Be/X-ray binary system with a compact object companion, possibly a neutron star.
    Type of Medium: Online Resource
    ISSN: 2041-8205 , 2041-8213
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 2006858-X
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  • 5
    Online Resource
    Online Resource
    American Astronomical Society ; 2022
    In:  The Astrophysical Journal Vol. 939, No. 2 ( 2022-11-01), p. 76-
    In: The Astrophysical Journal, American Astronomical Society, Vol. 939, No. 2 ( 2022-11-01), p. 76-
    Abstract: The γ -ray emission from flat-spectrum radio quasars (FSRQs) is thought to be dominated by the inverse Compton scattering of the external sources of photon fields, e.g., accretion disk, broad-line region (BLR), and torus. FSRQs show strong optical emission lines and hence can be a useful probe of the variability in BLR output, which is the reprocessed disk emission. We study the connection between the optical continuum, H γ line, and γ -ray emissions from the FSRQ PKS 1222+216, using long-term (∼2011–2018) optical spectroscopic data from Steward Observatory and γ -ray observations from Fermi Large Area Telescope (LAT). We measured the continuum ( F C,opt ) and H γ ( F H γ ) fluxes by performing a systematic analysis of the 6029–6452 Å optical spectra. We observed stronger variability in F C,opt than F H γ , an inverse correlation between the H γ equivalent width and F C,opt , and a redder-when-brighter trend. Using discrete cross-correlation analysis, we found a positive correlation (DCF ∼ 0.5) between the F γ ‐ray 〉 100 MeV and F C,opt (6024–6092 Å) light curves with a time lag consistent with zero at the 2 σ level. We found no correlation between the F γ ‐ray 〉 100 MeV and F H γ light curves, probably dismissing the disk contribution to the optical and γ -ray variability. The observed strong variability in the Fermi-LAT flux and F γ ‐ray 〉 100 MeV − F C,opt correlation could be due to the changes in the particle acceleration at various epochs. We derived the optical-to- γ -ray spectral energy distributions during the γ -ray flaring and quiescent epochs that show a dominant disk component with no variability. Our study suggests that the γ -ray emission zone is likely located at the edge of the BLR or in the radiation field of the torus.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    RVK:
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2207648-7
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 6
    Online Resource
    Online Resource
    Springer Science and Business Media LLC ; 2021
    In:  Journal of Astrophysics and Astronomy Vol. 42, No. 2 ( 2021-10)
    In: Journal of Astrophysics and Astronomy, Springer Science and Business Media LLC, Vol. 42, No. 2 ( 2021-10)
    Type of Medium: Online Resource
    ISSN: 0250-6335 , 0973-7758
    Language: English
    Publisher: Springer Science and Business Media LLC
    Publication Date: 2021
    detail.hit.zdb_id: 2096381-6
    SSG: 16,12
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  • 7
    Online Resource
    Online Resource
    Wiley ; 2023
    In:  Astronomische Nachrichten Vol. 344, No. 4 ( 2023-05)
    In: Astronomische Nachrichten, Wiley, Vol. 344, No. 4 ( 2023-05)
    Abstract: The soft X‐ray excess, emission below 2 keV over the X‐ray power‐law, is a marked spectral component in the X‐ray spectra of many Seyfert 1 galaxies. We investigate if the observed soft X‐ray excess in a sample of Seyfert 1s is in accordance with the prediction of the relativistic reflection model by analyzing the XMM‐Newton and NuSTAR spectra. The fractional difference in the soft excess (SE) obtained from the blurred reflection emission predicted (from NuSTAR ) and the observed (from XMM‐Newton ) luminosities show that the reflection model underestimates the SE emission in our sample. The results point to alternative models (for example, warm Comptonization) to explain the soft X‐ray excess in AGN.
    Type of Medium: Online Resource
    ISSN: 0004-6337 , 1521-3994
    URL: Issue
    Language: English
    Publisher: Wiley
    Publication Date: 2023
    detail.hit.zdb_id: 2025762-4
    detail.hit.zdb_id: 2171222-0
    SSG: 16,12
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  • 8
    Online Resource
    Online Resource
    Oxford University Press (OUP) ; 2021
    In:  Monthly Notices of the Royal Astronomical Society Vol. 504, No. 4 ( 2021-05-20), p. 5485-5495
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 504, No. 4 ( 2021-05-20), p. 5485-5495
    Abstract: We present the results of the X-ray flaring activity of 1ES 1959+650 during 2017 October 25–26 using AstroSat observations. The source was variable in the X-ray. We investigated the evolution of the X-ray spectral properties of the source by dividing the total observation period (∼130 ks) into time segments of 5 ks, and fitting the Soft X-ray focusing Telescope and Large Area X-ray Proportional Counter spectra for each segment. Synchrotron emission of a broken power-law particle density model provided a better fit than the log-parabola one. The X-ray flux and the normalized particle density at an energy less than the break one were found to anticorrelate with the index before the break. However, a stronger correlation between the density and index was obtained when a delay of ∼60 ks was introduced. The amplitude of the normalized particle density variation |Δnγ/nγ| ∼ 0.1 was found to be less than that of the index ΔΓ ∼ 0.5. We model the amplitudes and the time delay in a scenario where the particle acceleration time-scale varies on a time-scale comparable to itself. In this framework, the rest-frame acceleration time-scale is estimated to be ∼1.97 × 105 s and the emission region size to be ∼6.73 × 1015 cm.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2021
    detail.hit.zdb_id: 2016084-7
    SSG: 16,12
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  • 9
    Online Resource
    Online Resource
    IOP Publishing ; 2016
    In:  Research in Astronomy and Astrophysics Vol. 16, No. 7 ( 2016-07), p. 008-
    In: Research in Astronomy and Astrophysics, IOP Publishing, Vol. 16, No. 7 ( 2016-07), p. 008-
    Type of Medium: Online Resource
    ISSN: 1674-4527
    Language: Unknown
    Publisher: IOP Publishing
    Publication Date: 2016
    detail.hit.zdb_id: 2511247-8
    SSG: 6,25
    SSG: 16,12
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