AGNs with hard γ-ray emission identified so far are radio-loud. Ⅲ Zw 2 is a radio intermediate AGN with a relativistic jet. We study its spectral energy distribution （SED） and find that the broad band emissions ar...AGNs with hard γ-ray emission identified so far are radio-loud. Ⅲ Zw 2 is a radio intermediate AGN with a relativistic jet. We study its spectral energy distribution （SED） and find that the broad band emissions are dominated by the nonthermal emissions from the jet. We model its SED through a synchrotron ＋ inverse Compton （IC） model. The results show that the IC component of Ⅲ Zw 2 peaks at a few MeV, and the flux density drops rapidly at higher energy with photon index F 3.3 above 0.1 GeV. The predicted flux is slightly over the sensitivity of Fermi/LAT, but it was not included in the first Fermi/LAT AGN catalog. The reason for this may be： 1） that the IC peak is low and the spectrum is very steep above 0.1 GeV, 2） that Ⅲ Zw 2 is in the low state during the period of the Fermi/LAT operation. We also find that Ⅲ Zw 2 follows similar jet processes as those in γ-ray AGNs, e.g., the relation between jet power and radiation power, which is called the blazar sequence. We suggest that Ⅲ Zw 2 may be a young source at an earlier stage of jet activity.展开更多
We investigate the spatially resolved specific star formation rate （SSFR） in the inner -40 pc for a nearby Seyfert 2 galaxy, M51 （NGC 5194） by analyzing spectra obtained with the Hubble Space Telescope （HST） Spa...We investigate the spatially resolved specific star formation rate （SSFR） in the inner -40 pc for a nearby Seyfert 2 galaxy, M51 （NGC 5194） by analyzing spectra obtained with the Hubble Space Telescope （HST） Space Telescope Imaging Spectrograph （STIS）. We present 24 radial spectra measured along the STIS long slit in M51, extending - 1＂ from the nucleus （i.e., -41.5 pc to 39.4 pc）. By simple stellar population synthesis, the stellar contributions in these radial optical spectra are modeled. It is found that the mean flux fraction of young stellar populations （younger than 24.5 Myr） is about 9%. Excluding some regions with zero young flux fraction near the center （from -6 pc to 2 pc）, the mean mass fraction is about 0.09%. The young stellar populations are not required in the center inner -8 pc in M51, suggesting a possible SSFR suppression in the circumnuclear region （- 10 pc） from the feedback of active galactic nuclei （AGNs）. The radial distribution of SSFR in M51 is not symmetrical with respect to the long slit in STIS. This unsymmetrical SSFR distribution is possibly due to the unsymmetrical AGN feedback in M51, which is related to its jet.展开更多
We found a NLS1 nucleus in the extensively studied eruptive BL Lac object, 0846+51W1, out of a large sample of NLS1s compiled from the spectroscopic dataset of SDSS DR1. Its optical spectrum can be well decomposed int...We found a NLS1 nucleus in the extensively studied eruptive BL Lac object, 0846+51W1, out of a large sample of NLS1s compiled from the spectroscopic dataset of SDSS DR1. Its optical spectrum can be well decomposed into three components: a power law component from the relativistic jet, a stellar component from the host galaxy, and a component from a typical NLS1 nucleus. The emission line properties of 0846+51W1, FWHM (Hβ) (?) 1710 km s-1 and [OⅢ]λ5007/Hβ(?)0.32 from its SDSS spectrum observed when it was in the faint state, fulfil the conventional definition of NLS1. Strong Fell emission is detected in the SDSS spectrum, which is also typical of NLS1s. We tried to estimate its central black hole mass using various techniques and found that 0846+51W1 is very likely emitting at a few ×10% of the Eddington luminosity. We speculate that Seyfert-like nuclei, including NLS1s, might be concealed in a significant fraction of BL Lacs but have remained largely unobserved because, often, their optical-UV continuum is overwhelmed by the synchrotron emission.展开更多
We examined the correlation between the ROSAT Hardness Ratio 1 and Count Rates eight Narrow-line Seyfert 1 Galaxies (NLSls) and 14 Broad-line Seyfertl Galaxies (BLSls). We found that six of the NLSls show a positive H...We examined the correlation between the ROSAT Hardness Ratio 1 and Count Rates eight Narrow-line Seyfert 1 Galaxies (NLSls) and 14 Broad-line Seyfertl Galaxies (BLSls). We found that six of the NLSls show a positive HR1-CTs correlation, and seven of the BLSls, a negative correlation. The other two NLSls and seven BLSls do not show any clear HR1-CTs correlation. Thus, the spectral behavior is statistically different for the NLSls and BLSls. The different behaviors can possibly be interpreted in terms of a stable 'soft excess' that is strong in NLSls and weak in BLSls, plus a power law component, common to both, which softens with increasing flux.展开更多
We present a study of the nearby Seyfert galaxy NGC 3982 using optical, infrared and X-ray data acquired by SDSS, Spitzer and Chandra. Our main results are as follows： （1） A simple stellar population synthesis on t...We present a study of the nearby Seyfert galaxy NGC 3982 using optical, infrared and X-ray data acquired by SDSS, Spitzer and Chandra. Our main results are as follows： （1） A simple stellar population synthesis on the nuclear and circumnuclear SDSS spectra gives unambiguous evidence of young stellar components in both the nuclear and circumnuclear regions. （2） The Spitzer Infrared Spectrograph （IRS） spectrum of the central region （∽ 3＂） shows a power-law continuum, a silicate emission feature at 9.7μm, and significant PAH emission features at 7.7, 8.6, 11.3 and 12.7 pro, suggesting the coexistence of AGN and starburst activities in the central region of NGC 3982. （3） We estimate the star formation rate （SFR） of the circumnuclear （∽ 5＂ - 20＂） region from the Hα luminosity to be SFRHα = 0.52 M⊙ yr^-1, which is consistent with the result from the Spitzer IRAC 8 μm luminosity, SFR8.0μm = 0.57 M⊙ yr^-1. （4） We measure the spectral energy distribution for the active nucleus of NGC 3982 from radio to X-ray, and obtain a bolometric luminosity of Lbol 4.5 × 10^42 erg s-1, corresponding to an Eddington ratio （Lbol//LEdd） of 0.014 The HST image of NGC 3982 shows a nuclear mini-spiral between the circumnuclear starforming region and the nucleus, which could be the channel through which gas is transported to the supermassive black hole from the circumnuclear star-forming region.展开更多
We report on the results of cross-correlation of a sample of 903 Ultraluminous IRAS galaxies (ULIRGs) with the ROSAT-All Sky Survey Bright Source Catalogue and the ROSAT archived pointing observations. The sample of ...We report on the results of cross-correlation of a sample of 903 Ultraluminous IRAS galaxies (ULIRGs) with the ROSAT-All Sky Survey Bright Source Catalogue and the ROSAT archived pointing observations. The sample of ULIRGs has been compiled from the recently released PSCz redshift survey. In total, 35 ULIRGs are securely detected by the ROSAT All-Sky Survey and pointing observations, five of which are blazars. The statistical properties of these sources in the soft X-ray band are determined and compared with their properties in other wavebands. We find that the ratio of the soft X-ray to the far-infrared flux spans about five orders of magnitude and reaches Values of about unity. This ratio is a good indicator of the main energy source of ULIRGs. Those with soft X-ray to far-infrared flux exceeding 0.01 are probably powered by accretion onto central supermassive black holes while those with ratios smaller than 0.001 are probably powered by starbursts or other heating processes, or are Compton thick sources. Some ULIRGs have energy contributions from both. This ratio is low for most ULIRGs and hyperluminous infrared galaxies, which explains their low detection rate by ROSAT and ASCA. We also find that some ULIRGs have a similar soft X-ray luminosity vs. temperature relation to that for groups of galaxies and elliptical galaxies, suggesting a common origin of these systems. Our study also reveals a tight correlation between the hardness ratio and the soft X-ray luminosity for Seyfert 1s/QSOs.展开更多
By checking DSS optical images and NVSS radio images, 782 Markarian galaxies were identified to be NVSS radio sources. A comparison of the radio luminosity at 1.4GHz and the far-infrared （FIR） luminosity for 468 “n...By checking DSS optical images and NVSS radio images, 782 Markarian galaxies were identified to be NVSS radio sources. A comparison of the radio luminosity at 1.4GHz and the far-infrared （FIR） luminosity for 468 “normal” galaxies shows a tight correlation. Most of the Seyfert galaxies and quasars follow the radio-FIR relation deduced from the “normal” galaxy sample, but with a somewhat larger scatter. A total 167 Markarian galaxies, comprising 100 “normal” galaxies, 66 Seyfert galaxies and one quasar, have either excess radio emission or much lower FIR spectral index α（25 μm, 60 μm）. These galaxies may be classified as “AGN-powered”. For “normal” galaxies, the average q value （defined as the log ratio between FIR and radio luminosities） is 2.3. There seems a trend for q to slightly decrease with increasing radio luminosity. This may imply that the ongoing active star formation in galaxies with higher radio luminosities is more efficient in heating the cosmic-ray electrons.展开更多
We used multi-component profiles to model the HE and [O Ⅲ]λλ4959,5007 lines of SDSS J143030.22-001115.1, a narrow-line Seyfert 1 galaxy （NLS1） in a sample of 150 NLS1 candidates selected from the Sloan Digital Sk...We used multi-component profiles to model the HE and [O Ⅲ]λλ4959,5007 lines of SDSS J143030.22-001115.1, a narrow-line Seyfert 1 galaxy （NLS1） in a sample of 150 NLS1 candidates selected from the Sloan Digital Sky Survey （SDSS）, Early Data Release （EDR）. After subtracting the HE contribution from narrow line regions （NLRs）, we found that its full width half maximum （FWHM） of broad H/3 line is nearly 2900km s^-1, significantly larger than the customarily adopted criterion of 2000 km s^-1. With its weak Fe II multiples, we believe that SDSS J143030.22-001115.1 should not be classified as a genuine NLS1. When we calculate the virial black hole masses of NLSls, we should use the Hβ linewidth after subtracting the NLR component.展开更多
Warm absorption is a common phenomenon in Seyfert 1 s and quasars, but is rare in Seyfert 2s. We report the detection of warm absorbers with high energy resolution in the Seyfert 2 galaxy IRAS 18325-5926 for the first...Warm absorption is a common phenomenon in Seyfert 1 s and quasars, but is rare in Seyfert 2s. We report the detection of warm absorbers with high energy resolution in the Seyfert 2 galaxy IRAS 18325-5926 for the first time with Chandra HETGS spectra. An intrinsic absorbing line system with an outflow velocity - 400 km s^-1 was found, which is contributed by two warm absorbers with FWHM of 570 km s^-1 and 1360 km s^-1, respectively. The two absorbers were adjacent, and moving transversely across our line of sight. We constrained the distance between the center and the absorbers to be a small value, suggesting that the absorbers may originate from the highly ionized accretion disk wind ejected five years ago. The perspective of this type 2 Seyfert provides the best situation in which to investigate the vertical part of the funnel-like outflows. Another weak absorbing line system with zero redshift was also detected, which could be due to Galactic absorption with very high temperature or an intrinsic outflow with a very high velocity - 6000 km s^-1.展开更多
We analyze eight XMM-Newton observations of the bright Narrow Line Seyfert 1 galaxy Arakelian 564（Ark 564）. These observations, separated bye^6 days, allow us to look for correlations between the simultaneous ultrav...We analyze eight XMM-Newton observations of the bright Narrow Line Seyfert 1 galaxy Arakelian 564（Ark 564）. These observations, separated bye^6 days, allow us to look for correlations between the simultaneous ultraviolet（UV） emission（from th Optical Monitor） with not only the X-ray flux but also with different X-ray spectral parameters. The X-ray spectra from all the observations are found to be adequately fitted by a double Comptonization model where the soft excess and the hard X-ray power law are represented by thermal Comptonization in a low temperature plasma and hot corona, respectively. Apart from the fluxes of each component, the hard X-ray power law index is found to be variable. These results suggest that the variability is associated with changes in the geometry of the inner region. The UV emission is found to be variable and well correlated with the high energy index while the correlations with the fluxes of each component are found to be weaker. Using viscous timescale arguments we rule out the possibility that the UV variation is due to the fluctuating accretion rate in the outer disk. If the UV variation is driven by X-ray reprocessing, then our results indicate that the strength of the X-ray reprocessing depends more on the geometry of the X-ray producing inner region rather than on the X-ray luminosity alone.展开更多
Low-ionization nuclear emission regions （LINERs） are present in a large fraction of local galaxies, while their connection to the more luminous active galactic nuclei （AGN） remains elusive. We analyze the narrow b...Low-ionization nuclear emission regions （LINERs） are present in a large fraction of local galaxies, while their connection to the more luminous active galactic nuclei （AGN） remains elusive. We analyze the narrow band images obtained by the Hubble Space Telescope （HST） in Hα＋[NII] and/or [OIII] band for 23 LINERs and low luminosity Seyfert galaxies in the sample of the Palomar Optical Spectroscopic Survey of nearby galaxies in an attempt to resolve the structure of Narrow Emission Line Regions （NLRs） of these objects. In all cases, NLRs are well resolved and their morphology differs from object to object. Clumps, linear structure, spiral arms or a ring are detected in a large fraction of the objects, while there is no significant difference between Seyfert galaxies and LINERs. We find that the NLR size and the narrow line luminosity are strongly correlated for both LINERs and low luminosity Seyfert galaxies, and that the size of Ha＋[NII] emission line region scales with Ha luminosity as RNLR ∝ LHα^0.44＋0.06, consistent with an extension of the NLR size-luminosity relation defined for luminous Seyfert galaxies and quasars, to two orders of magnitude lower in luminosity and to lower activity levels. Our results suggest that NLRs in LINERs are similar to those of Seyfert galaxies, and they are powered by the central active galactic nucleus.展开更多
We compile the observed intensity ratios of the Balmer lines for low redshift quasars and Seyfert Ⅰ galaxies. In the framework of the Cerenkov line emission theory, we compare the theoretical intensity ratios with th...We compile the observed intensity ratios of the Balmer lines for low redshift quasars and Seyfert Ⅰ galaxies. In the framework of the Cerenkov line emission theory, we compare the theoretical intensity ratios with those of observations, and find that the observed intensity ratios for the radio-loud quasars and the Seyfert Ⅰ galaxies are nearer to the theoretical expectation than those for the radio-quiet sources. It seems that for the radio-loud AGNs, the characteristics of the Cerenkov line emission are more remarkable because of the existence of a great number of relativistic electrons. We also discuss the reddening by dust in quasars and the Seyfert galaxies. The fact that the reddening of the Seyfert galaxies is more serious than quasars shows that the Seyfert galaxies have more dust than quasars. This is in agreement with the present point of view.展开更多
基金the West Ph.D. project of the Training Programme for the Talents of the West Light Foundation of the CASthe National Natural Science Foundation of China (NSFC+2 种基金Grant Nos.10903025 and 10778702) for financial supportthe National Natural Science Foundation of China (Grant No.10973034)the 973 Program (Grant No.2009CB824800)
文摘AGNs with hard γ-ray emission identified so far are radio-loud. Ⅲ Zw 2 is a radio intermediate AGN with a relativistic jet. We study its spectral energy distribution （SED） and find that the broad band emissions are dominated by the nonthermal emissions from the jet. We model its SED through a synchrotron ＋ inverse Compton （IC） model. The results show that the IC component of Ⅲ Zw 2 peaks at a few MeV, and the flux density drops rapidly at higher energy with photon index F 3.3 above 0.1 GeV. The predicted flux is slightly over the sensitivity of Fermi/LAT, but it was not included in the first Fermi/LAT AGN catalog. The reason for this may be： 1） that the IC peak is low and the spectrum is very steep above 0.1 GeV, 2） that Ⅲ Zw 2 is in the low state during the period of the Fermi/LAT operation. We also find that Ⅲ Zw 2 follows similar jet processes as those in γ-ray AGNs, e.g., the relation between jet power and radiation power, which is called the blazar sequence. We suggest that Ⅲ Zw 2 may be a young source at an earlier stage of jet activity.
基金Supported by the National Natural Science Foundation of China
文摘We investigate the spatially resolved specific star formation rate （SSFR） in the inner -40 pc for a nearby Seyfert 2 galaxy, M51 （NGC 5194） by analyzing spectra obtained with the Hubble Space Telescope （HST） Space Telescope Imaging Spectrograph （STIS）. We present 24 radial spectra measured along the STIS long slit in M51, extending - 1＂ from the nucleus （i.e., -41.5 pc to 39.4 pc）. By simple stellar population synthesis, the stellar contributions in these radial optical spectra are modeled. It is found that the mean flux fraction of young stellar populations （younger than 24.5 Myr） is about 9%. Excluding some regions with zero young flux fraction near the center （from -6 pc to 2 pc）, the mean mass fraction is about 0.09%. The young stellar populations are not required in the center inner -8 pc in M51, suggesting a possible SSFR suppression in the circumnuclear region （- 10 pc） from the feedback of active galactic nuclei （AGNs）. The radial distribution of SSFR in M51 is not symmetrical with respect to the long slit in STIS. This unsymmetrical SSFR distribution is possibly due to the unsymmetrical AGN feedback in M51, which is related to its jet.
文摘We found a NLS1 nucleus in the extensively studied eruptive BL Lac object, 0846+51W1, out of a large sample of NLS1s compiled from the spectroscopic dataset of SDSS DR1. Its optical spectrum can be well decomposed into three components: a power law component from the relativistic jet, a stellar component from the host galaxy, and a component from a typical NLS1 nucleus. The emission line properties of 0846+51W1, FWHM (Hβ) (?) 1710 km s-1 and [OⅢ]λ5007/Hβ(?)0.32 from its SDSS spectrum observed when it was in the faint state, fulfil the conventional definition of NLS1. Strong Fell emission is detected in the SDSS spectrum, which is also typical of NLS1s. We tried to estimate its central black hole mass using various techniques and found that 0846+51W1 is very likely emitting at a few ×10% of the Eddington luminosity. We speculate that Seyfert-like nuclei, including NLS1s, might be concealed in a significant fraction of BL Lacs but have remained largely unobserved because, often, their optical-UV continuum is overwhelmed by the synchrotron emission.
文摘We examined the correlation between the ROSAT Hardness Ratio 1 and Count Rates eight Narrow-line Seyfert 1 Galaxies (NLSls) and 14 Broad-line Seyfertl Galaxies (BLSls). We found that six of the NLSls show a positive HR1-CTs correlation, and seven of the BLSls, a negative correlation. The other two NLSls and seven BLSls do not show any clear HR1-CTs correlation. Thus, the spectral behavior is statistically different for the NLSls and BLSls. The different behaviors can possibly be interpreted in terms of a stable 'soft excess' that is strong in NLSls and weak in BLSls, plus a power law component, common to both, which softens with increasing flux.
基金the National Natural Science Foundation of China
文摘We present a study of the nearby Seyfert galaxy NGC 3982 using optical, infrared and X-ray data acquired by SDSS, Spitzer and Chandra. Our main results are as follows： （1） A simple stellar population synthesis on the nuclear and circumnuclear SDSS spectra gives unambiguous evidence of young stellar components in both the nuclear and circumnuclear regions. （2） The Spitzer Infrared Spectrograph （IRS） spectrum of the central region （∽ 3＂） shows a power-law continuum, a silicate emission feature at 9.7μm, and significant PAH emission features at 7.7, 8.6, 11.3 and 12.7 pro, suggesting the coexistence of AGN and starburst activities in the central region of NGC 3982. （3） We estimate the star formation rate （SFR） of the circumnuclear （∽ 5＂ - 20＂） region from the Hα luminosity to be SFRHα = 0.52 M⊙ yr^-1, which is consistent with the result from the Spitzer IRAC 8 μm luminosity, SFR8.0μm = 0.57 M⊙ yr^-1. （4） We measure the spectral energy distribution for the active nucleus of NGC 3982 from radio to X-ray, and obtain a bolometric luminosity of Lbol 4.5 × 10^42 erg s-1, corresponding to an Eddington ratio （Lbol//LEdd） of 0.014 The HST image of NGC 3982 shows a nuclear mini-spiral between the circumnuclear starforming region and the nucleus, which could be the channel through which gas is transported to the supermassive black hole from the circumnuclear star-forming region.
文摘We report on the results of cross-correlation of a sample of 903 Ultraluminous IRAS galaxies (ULIRGs) with the ROSAT-All Sky Survey Bright Source Catalogue and the ROSAT archived pointing observations. The sample of ULIRGs has been compiled from the recently released PSCz redshift survey. In total, 35 ULIRGs are securely detected by the ROSAT All-Sky Survey and pointing observations, five of which are blazars. The statistical properties of these sources in the soft X-ray band are determined and compared with their properties in other wavebands. We find that the ratio of the soft X-ray to the far-infrared flux spans about five orders of magnitude and reaches Values of about unity. This ratio is a good indicator of the main energy source of ULIRGs. Those with soft X-ray to far-infrared flux exceeding 0.01 are probably powered by accretion onto central supermassive black holes while those with ratios smaller than 0.001 are probably powered by starbursts or other heating processes, or are Compton thick sources. Some ULIRGs have energy contributions from both. This ratio is low for most ULIRGs and hyperluminous infrared galaxies, which explains their low detection rate by ROSAT and ASCA. We also find that some ULIRGs have a similar soft X-ray luminosity vs. temperature relation to that for groups of galaxies and elliptical galaxies, suggesting a common origin of these systems. Our study also reveals a tight correlation between the hardness ratio and the soft X-ray luminosity for Seyfert 1s/QSOs.
文摘By checking DSS optical images and NVSS radio images, 782 Markarian galaxies were identified to be NVSS radio sources. A comparison of the radio luminosity at 1.4GHz and the far-infrared （FIR） luminosity for 468 “normal” galaxies shows a tight correlation. Most of the Seyfert galaxies and quasars follow the radio-FIR relation deduced from the “normal” galaxy sample, but with a somewhat larger scatter. A total 167 Markarian galaxies, comprising 100 “normal” galaxies, 66 Seyfert galaxies and one quasar, have either excess radio emission or much lower FIR spectral index α（25 μm, 60 μm）. These galaxies may be classified as “AGN-powered”. For “normal” galaxies, the average q value （defined as the log ratio between FIR and radio luminosities） is 2.3. There seems a trend for q to slightly decrease with increasing radio luminosity. This may imply that the ongoing active star formation in galaxies with higher radio luminosities is more efficient in heating the cosmic-ray electrons.
基金Supported by the National Natural Science Foundation of China.
文摘We used multi-component profiles to model the HE and [O Ⅲ]λλ4959,5007 lines of SDSS J143030.22-001115.1, a narrow-line Seyfert 1 galaxy （NLS1） in a sample of 150 NLS1 candidates selected from the Sloan Digital Sky Survey （SDSS）, Early Data Release （EDR）. After subtracting the HE contribution from narrow line regions （NLRs）, we found that its full width half maximum （FWHM） of broad H/3 line is nearly 2900km s^-1, significantly larger than the customarily adopted criterion of 2000 km s^-1. With its weak Fe II multiples, we believe that SDSS J143030.22-001115.1 should not be classified as a genuine NLS1. When we calculate the virial black hole masses of NLSls, we should use the Hβ linewidth after subtracting the NLR component.
基金provided by the Program for New Century Excellent Talents in University (NCET)the National Natural Science Foundation of China (Grant Nos. 10878010, 10221001 and 10633040)the National Basic Research Program of China (GrantNo. 2007CB815405)
文摘Warm absorption is a common phenomenon in Seyfert 1 s and quasars, but is rare in Seyfert 2s. We report the detection of warm absorbers with high energy resolution in the Seyfert 2 galaxy IRAS 18325-5926 for the first time with Chandra HETGS spectra. An intrinsic absorbing line system with an outflow velocity - 400 km s^-1 was found, which is contributed by two warm absorbers with FWHM of 570 km s^-1 and 1360 km s^-1, respectively. The two absorbers were adjacent, and moving transversely across our line of sight. We constrained the distance between the center and the absorbers to be a small value, suggesting that the absorbers may originate from the highly ionized accretion disk wind ejected five years ago. The perspective of this type 2 Seyfert provides the best situation in which to investigate the vertical part of the funnel-like outflows. Another weak absorbing line system with zero redshift was also detected, which could be due to Galactic absorption with very high temperature or an intrinsic outflow with a very high velocity - 6000 km s^-1.
基金based on observations obtained with the XMM-Newton satellite,an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA(NASA)made use of the NASA/IPAC Extragalactic Data base which is operated by the Jet Propulsion Laboratory,California Institute of Technology and data obtained through the High Energy Astrophysics Science Archive Research Center Online Service,provided by NASA/GSFCthe Department of Science and Technology of India for the grant(No.SR/S2/HEP-07/2012)that supported this work
文摘We analyze eight XMM-Newton observations of the bright Narrow Line Seyfert 1 galaxy Arakelian 564（Ark 564）. These observations, separated bye^6 days, allow us to look for correlations between the simultaneous ultraviolet（UV） emission（from th Optical Monitor） with not only the X-ray flux but also with different X-ray spectral parameters. The X-ray spectra from all the observations are found to be adequately fitted by a double Comptonization model where the soft excess and the hard X-ray power law are represented by thermal Comptonization in a low temperature plasma and hot corona, respectively. Apart from the fluxes of each component, the hard X-ray power law index is found to be variable. These results suggest that the variability is associated with changes in the geometry of the inner region. The UV emission is found to be variable and well correlated with the high energy index while the correlations with the fluxes of each component are found to be weaker. Using viscous timescale arguments we rule out the possibility that the UV variation is due to the fluctuating accretion rate in the outer disk. If the UV variation is driven by X-ray reprocessing, then our results indicate that the strength of the X-ray reprocessing depends more on the geometry of the X-ray producing inner region rather than on the X-ray luminosity alone.
文摘Low-ionization nuclear emission regions （LINERs） are present in a large fraction of local galaxies, while their connection to the more luminous active galactic nuclei （AGN） remains elusive. We analyze the narrow band images obtained by the Hubble Space Telescope （HST） in Hα＋[NII] and/or [OIII] band for 23 LINERs and low luminosity Seyfert galaxies in the sample of the Palomar Optical Spectroscopic Survey of nearby galaxies in an attempt to resolve the structure of Narrow Emission Line Regions （NLRs） of these objects. In all cases, NLRs are well resolved and their morphology differs from object to object. Clumps, linear structure, spiral arms or a ring are detected in a large fraction of the objects, while there is no significant difference between Seyfert galaxies and LINERs. We find that the NLR size and the narrow line luminosity are strongly correlated for both LINERs and low luminosity Seyfert galaxies, and that the size of Ha＋[NII] emission line region scales with Ha luminosity as RNLR ∝ LHα^0.44＋0.06, consistent with an extension of the NLR size-luminosity relation defined for luminous Seyfert galaxies and quasars, to two orders of magnitude lower in luminosity and to lower activity levels. Our results suggest that NLRs in LINERs are similar to those of Seyfert galaxies, and they are powered by the central active galactic nucleus.
基金Project supported by the National Natural Science Foundation of China.
文摘We compile the observed intensity ratios of the Balmer lines for low redshift quasars and Seyfert Ⅰ galaxies. In the framework of the Cerenkov line emission theory, we compare the theoretical intensity ratios with those of observations, and find that the observed intensity ratios for the radio-loud quasars and the Seyfert Ⅰ galaxies are nearer to the theoretical expectation than those for the radio-quiet sources. It seems that for the radio-loud AGNs, the characteristics of the Cerenkov line emission are more remarkable because of the existence of a great number of relativistic electrons. We also discuss the reddening by dust in quasars and the Seyfert galaxies. The fact that the reddening of the Seyfert galaxies is more serious than quasars shows that the Seyfert galaxies have more dust than quasars. This is in agreement with the present point of view.
