SCATTERING AND INFLOWING BROAD-LINE REGIONS

Line Shifts, Broad-Line Region Inflow, and the Feeding of AGNs

Abstract

Velocity-resolved reverberation mapping suggests that the broad-line regions (BLRs) of AGNs can have significant net inflow. We use the STOKES radiative transfer code to show that electron and Rayleigh scattering off the BLR and torus naturally explains the blueshifted profiles of high-ionization lines and the ionization dependence of the blueshifts. This result is insensitive to the geometry of the scattering region. If correct, this model resolves the long-standing conflict between the absence of outflow implied by velocity-resolved reverberation mapping and the need for outflow if the blueshifting is the result of obscuration. The accretion rate implied by the inflow is sufficient to power the AGN. We suggest that the BLR is part of the outer accretion disk and that similar MHD processes are operating. In the scattering model the blueshifting is proportional to the accretion rate so high-accretion-rate AGNs will show greater high-ionization line blueshifts as is observed. Scattering can lead to systematically too high black hole mass estimates from the C IV line. We note many similarities between narrow-line region (NLR) and BLR blueshiftings, and suggest that NLR blueshiftings have a similar explanation. Our model explains the higher blueshifts of broad absorption line QSOs if they are more highly inclined. Rayleigh scattering from the BLR and torus could be more important in the UV than electron scattering for predominantly neutral material around AGNs. The importance of Rayleigh scattering versus electron scattering can be assessed by comparing line profiles at different wavelengths arising from the same emission-line region.

Subject headings:
accretion, accretion disks — black hole physics — galaxies:active — galaxies:quasars:emission lines — line: profiles — scattering
6

1. Introduction

The structure and kinematics of the broad-line region (BLR) of thermal active galactic nuclei7 (AGNs) has long been a subject of much debate, and a wide range of structures and velocities have been considered (for reviews see Mathews & Capriotti 1985; Osterbrock & Mathews 1986; Osterbrock 1993; Gaskell et al. 1999; Sulentic, Marziani, & Dultzin-Hacyan 2000; Gaskell 2009). Because of these uncertainties, for a long time it was not clear where the BLR is located, what it is doing, and hence, what role it plays in the AGN phenomenon. Reverberation mapping (Lyutyi & Cherepashchuk, 1972; Cherepashchuk & Lyutyi, 1973; Blandford & McKee, 1982; Gaskell & Sparke, 1986) has enabled us to probe the structures of the BLR and dusty torus, and it is argued elsewhere (see Gaskell, Klimek, & Nazarova 2007, hereinafter “GKN”; and Gaskell 2009) that the BLR and torus share a similar flattened toroidal structure with a high covering factor and self shielding.

A major reason for the uncertainty over the structure and kinematics of the BLR has been the conflicting pictures of the velocity field in AGNs field given by varying lines of observational evidence. First, the discovery of broad absorption lines (Lynds, 1967) was unequivocal evidence that at least some gas is outflowing from AGNs. Radiatively-driven outflows could also naturally explain the symmetric “logarithmic” BLR line profiles seen in a large fraction of AGNs (Blumenthal & Mathews, 1975). The outflow picture was supported by the discovery (Gaskell, 1982) of the blueshifting of the high-ionization BLR lines with respect to the low-ionization lines and the rest frame of the host galaxy by km s. This effect, which for brevity we will refer to here simply as “blueshifting”, required physical separation of the high- and low-ionization BLR clouds, a component of radial motions, and an opacity source. Gaskell (1982) proposed a “disk-wind” model where the blueshifting could be explained by having the high-ionization clouds be radially outflowing, with obscuration in the equatorial plane blocking our view of the receding clouds (i.e., of the redshifted side of the line profile). Although the blueshifting is usually of the order of km s, it can exceed 4000 km s (Corbin, 1990). The blueshifting is not only found when comparing the profiles of high- and low-ionization lines in individual AGNs, but also when using spectral principal component analysis (SPCA) of samples of AGNs to separate out line profiles into possible independent components such as an “intermediate-line region” (ILR) and a “very broad line region” (VBLR) (see Brotherton et al. 1994). The magnitude of the blueshifting is roughly in order of increasing ionization potential (Tytler & Fan, 1992). It also tends to be strongest in luminous, radio-quiet AGNs (Corbin, 1990; Tytler & Fan, 1992; Sulentic et al., 1995; Richards et al., 2002), especially in broad absorption line QSOs (BALQSOs; Corbin 1990; Richards et al. 2002), and in AGNs with a high accretion rate (Sulentic et al., 2000; Xu et al., 2003; Leighly & Moore, 2004). The large blueshifts in high-accretion-rate AGNs have been taken as an indication of strong outflowing winds in these AGNs (e.g., Leighly & Moore 2004; Komossa et al. 2008).

Gaskell (1988) pointed out that the outflowing high-ionization BLR scenario predicted strong velocity-dependent time delays in the wings of the high-ionization lines (the blue wing should lead the red wing by twice the line–continuum delay), and showed that such a signature of outflowing winds was absent at a high confidence level in velocity-resolved reverberation mapping of NGC 4151. This has subsequently been found to be the case in many other AGNs where velocity-dependent time delays have been studied (Koratkar & Gaskell 1989; Crenshaw & Blackwell 1990; Koratkar & Gaskell 1991a, b; Korista et al. 1995; see Gaskell 2010b for more detailed discussion). With only a couple of exceptions discussed below, the wings of BLR lines either vary simultaneously (as would be expected from Keplerian motion of the clouds or isotropic motions), or show slight evidence for inflow (i.e., the red wings vary first). Because of the strong evidence for gravitational domination of the motions, Gaskell (1988) argued that motions of BLR clouds were gravitationally dominated, and hence that they could be used for determining black hole masses. Furthermore, Krolik et al. (1991) showed from an analysis of the Clavel et al. (1991) observations of NGC 5548 that broad line widths are consistent with the fall off with radius expected when motions are virialized. The Krolik et al. result has been confirmed for other objects (Peterson & Wandel, 2000; Onken & Peterson, 2002; Kollatschny, 2003) covering a wide range of black hole masses and Eddington ratios.

There has thus long been little doubt that low-ionization BLR clouds (i.e., those producing Mg II and the Balmer lines) are predominantly orbiting the black hole. Other lines of evidence point to this orbital motion being Keplerian motion in the equatorial plane. Despite the significant covering factor of the BLR, we never see the BLR in absorption (see GKN), Balmer line widths show the expected correlation with the orientation of the rotation axis (Wills & Browne, 1986; Rokaki et al., 2003), disk-like line profiles are common (e.g., Eracleous & Halpern 1994; Gaskell & Snedden 1999), and evidence of orbital motion of emission regions has been detected (Gaskell, 1996; Sergeev et al., 2002; Pronik & Sergeev, 2006). It has been suggested that double-peaked line profiles are due to separate BLRs around two supermassive black holes in a binary (Gaskell, 1983) but variability observations strongly support a disk origin instead (see Gaskell 2010a and references therein). Gaskell (2010c, 2011) shows that apparently extreme double BLR peaks can readily by explained with the same gas distribution and kinematics as for single-peaked BLRs seen from a slightly higher inclination. The question of the detectability of close supermassive binary black holes remains an active area of investigation, however (see Popović 2012 for an extensive review).

It can be seen that there is considerable confidence that black hole masses can reliably be estimated from low-ionization lines (see Marziani & Sulentic 2012 for a review of AGN black hole mass determinations). However, for the high-ionization lines, the conflict between the kinematics implied by the blueshifted absorption lines and the blueshifting of the emission lines on the one hand, and the velocity-resolved reverberation mapping on the other, has raised serious doubts about the suitability of high-ionization lines such as C IV 1549 for estimating black hole masses. Further evidence for a difference in the kinematics of high- and low-ionization lines comes from the different velocity dependencies of the physical conditions (Snedden & Gaskell, 2004). The ionizing flux received by low-ionization BLR lines shows the dependence on velocity one would expect as a result of virialization and the inverse-square law, while the ionizing flux received by the high-ionization clouds appears to be almost independent of velocity.

This conflict between BLR kinematic indicators cannot simply be reconciled by assuming that the low-ionization lines arise in a disk while the high-ionization lines arise in a wind (e.g., Collin-Souffrin et al. 1988) because the velocity-resolved reverberation mapping specifically shows (Gaskell, 1988; Koratkar & Gaskell, 1989; Crenshaw & Blackwell, 1990; Koratkar & Gaskell, 1991a) that the high-ionization BLR gas is not outflowing. Also, the fall off of line widths with radius (Krolik et al., 1991) includes the high-ionization C IV line. Furthermore, disk–wind models have a problem of explaining why line profiles of different ions are so similar if they have very different origins (Tytler & Fan, 1992). While winds necessarily exist in AGNs in order to remove angular momentum so that material can accrete, and they could be energetically important as well, the amount of mass involved is small. The density in a wind is more than an order of magnitude lower than in the disk, and emissivity goes as the square of the density, so emission from a wind is negligible.

In this paper we will argue that the velocity-resolved reverberation mapping results are correct, and that the entire BLR has a net inflow. In section 2 we summarize the evidence for an inward spiraling of the BLR and estimate the inflow component of velocity. In section 3 we argue that scattering is consistent with producing a blueshifting when the BLR is inflowing, and in section 4 we use the STOKES Monte Carlo radiative transfer code to show that scattering off an inflowing medium reproduces observed blueshifted line profiles and also explains the dependence of blueshifting on ionization. We consider the implications of the inflowing BLR scenario for the energy generation mechanism in AGNs in section 5. In section 6 we offer an explanation of why high-accretion-rate AGNs (“Narrow-line Seyfert 1s” = NLS1s) show a stronger blueshifting, we point out potential systematic effects when the C IV emission line is used to estimate masses of high-redshift AGNs, we suggest an extension of our model to the narrow-line region, and we offer an explanation of why the blueshifting is enhanced in broad absorption line QSOs.

2. Inflowing BLR Gas

2.1. The Evidence for an Inflow Velocity Component

Although it has generally been assumed in estimating black hole masses that the BLR gas is in near-Keplerian or quasi-random orbits (i.e., there is no net radial motion), Gaskell (1988) found that for NGC 4151 inflow was favored and that purely Keplerian or random orbits were excluded at the 97% (single-tailed) confidence level. Koratkar & Gaskell (1989) similarly found that non-inflowing motion was excluded in Fairall 9 at the % confidence level. From the intensive 1989 IUE monitoring of NGC 5548 (Clavel et al., 1991), Crenshaw & Blackwell (1990) and Done & Krolik (1996) also favored a net inflow of the C IV emitting gas in NGC 5548. From the estimated errors in the lags given by Crenshaw & Blackwell (1990), non-inflowing motion is excluded at the 93% confidence level. The 1993 combined HST and IUE campaign (Korista et al., 1995) showed a similar degree of inflow (see their Table 25). The only bright AGN for which the variability of C IV has been studied is 3C 273 where Koratkar & Gaskell (1991b) and Paltani & Türler (2003) find an inflowing velocity component at two separate epochs. As Gaskell & Snedden (1997) point out, although the statistical significance of inflow C IV for one line in any one observing campaign of any individual AGN is not necessarily strong, the case is much stronger when all the AGNs are considered together.8 The aforementioned analyses are mostly for C IV 1549, but Gaskell (1988) found inflow of Mg II 2798 in NGC 4151, and Welsh et al. (2007) have recently found that H in NGC 5548 has an inflow component of velocity.

Two contradictory velocity-resolved reverberation mapping results must be mentioned. The first is an event in NGC 5548 which temporarily showed an apparent outflow kinematic signature (Kollatschny & Dietrich, 1996). The second is a similar conflicting signature seen in one season of monitoring of NGC 3227 (Denney et al., 2009). The temporary NGC 5548 apparent outflow signature certainly does not represent a systematic outflow because only three months later an inflow signature was seen in the same object (Kollatschny & Dietrich, 1996). Gaskell (2010c, 2011) has shown that transient apparent outflow signatures are a natural consequence of off-axis variability for which there is considerable other evidence.

Independent evidence for inflow comes from high-resolution spectropolarimetry (Smith et al., 2005). The systematic change in polarization as a function of velocity across the Balmer lines suggests a net inflow of a scattering region somewhat exterior to the Balmer lines.

In summary, we believe that there is significant observational evidence for gas producing both the high- and low-ionization BLR lines to be inflowing.

2.2. The Inflow Velocity

We can estimate the ratio of net inflow velocities to random velocities along the line of sight from the positions of the peaks of the red-wing/blue-wing cross correlation functions (CCFs). The positions of the expected peaks in the wing-wing CCFs are marked in Gaskell (1988) and Koratkar & Gaskell (1989). The observed peak positions, and the one found by Crenshaw & Blackwell (1990) are all consistent with the net inflow velocities being several times smaller than the non-inflow velocities. Done & Krolik (1996) reach a similar conclusion from more detailed modelling of the velocity-dependent delays in NGC 5548. For each object this suggests that the net inflow velocity of C IV is km s. In a totally independent analysis of the polarization structure of Balmer lines, Smith et al. (2005) suggest an inflow velocity of the scattering region of 900 km s. We will therefore adopt an inflow velocity of 1000 km s. However, we will see below that the precise value of the inflow velocity is not critical for our modelling and that the blueshifting can be obtained with much lower velocities.

3. Producing a Blueshift from Inflowing Gas

There are two main ways of producing a blueshift of a line from inflowing gas. One is by having anisotropic emission from the gas clouds (Gaskell, 1982; Wilkes, 1984), and the other is by having scattering off inflowing material (e.g., Auer & van Blerkom 1972). Although the emission from BLR clouds is certainly expected to be anisotropic, the anisotropy is much greater for some lines than for others. As discussed by Wilkes & Carswell (1982) and Kallman et al. (1993), this creates a problem in explaining all line profiles with an inflowing anisotropic emitting cloud model. Lyman has particularly strongly asymmetric emission compared with other lines when clouds are optically thick, which is almost certainly the case for the BLR clouds of relevance here (see Snedden & Gaskell 2007 for evidence against a significant optically-thin contribution to the BLR). There is no evidence that Lyman is more asymmetric than other lines (Wilkes & Carswell, 1982), so it would be hard for anisotropic emission from inflowing clouds to explain the blueshifting.

Electron scattering has long been considered to be a significant source of line broadening in AGNs in general (Kaneko & Ohtani, 1968; Weymann, 1970; Mathis, 1970), and from time to time it has been invoked to explain the line profiles of individual objects (Shields & McKee, 1981; Laor, 2006).9 Scattering regions with a net radial motion were considered by Auer & van Blerkom (1972). If the scattering region is outflowing, scattered photons are redshifted, while if it is inflowing, the photons are blueshifted. This can easily be understood by considering one´s reflection in a moving mirror (see Fig. 10 of Gaskell 2009). If the mirror is moving towards you your image appears to be approaching at twice the speed of the mirror. Such shifts have already been shown in simulations of electron scattering in AGNs by Kallman & Krolik (1986) and Ferrara & Pietrini (1993) and it has been suggested that this could be a cause of the blueshifting of high-ionization lines (Corbin, 1990; Mathews, 1993).

4. Scattering in an Inflowing Medium

4.1. Spherical Scattering Shells

We have modelled the effects of an inflowing scattering medium using the STOKES Monte Carlo radiative transfer code, which is described in Goosmann & Gaskell (2007) and Marin et al. (2012). Detailed documentation, sample input, source code, and executables for different computer platforms can be freely downloaded.10 The optical depths, , to scattering by free electrons along our line of sight are not expected to be much greater than unity inside the high-ionization BLR of an AGN. Shields & McKee (1981) estimate for electrons between BLR clouds, and Laor (2006) estimates for typical BLR clouds. Modelling of BLR clouds with the photoionization code CLOUDY (Ferland et al., 1998) gave similar values of . We therefore investigated quasi-spherical external scattering regions with = 0.5, 1, and 2. We also modelled = 10 to investigate effects of significantly larger optical depths. The inflow velocity was taken to be 1000 km s in all models. Since in this paper we are interested in modeling just the inflow and line asymmetry, we simply assumed that the unscattered line had an intrinsic broadening due to bulk motions. The assumed unbroadened profile is shown as a solid black line in Fig. 1. We considered inflowing scattering shells both inside and outside the BLR. The results are shown in Fig. 1.

Figure 1.— Calculated shifts of the C IV line by electron or Rayleigh scattering. The top black solid curve shows a Lorentzian line profile before scattering. The other solid curves show the blueshifting caused by an external spherical shell of scatterers with an inflow velocity of 1000 km s. The areas under all curves are the same. In order of increasing blueshifting and decreasing peak flux, the curves show the effects of = 0.5 (red), 1.0 (green), 2.0 (blue), and 10 (purple). The dots show the blueshifting caused by an inflowing flared disk with a radial optical depth of 5, a half-opening angle of 60 degrees, and an inflow velocity of 1000 km s, when the BLR is viewed from a “type-1” viewing position.

Our first result is that for a line-emitting region outside an inflowing scattering shell there was a negligible effect on the line profile (differences mostly smaller than the plotting lines and symbols in the figures). This thus verifies that when there is strong radial stratification of the BLR (see GKN and Gaskell 2009), only the innermost high-ionization lines (those within the scattering region) are blueshifted. This gives a natural explanation of the difference in blueshift with ionization and is a big advantage of our scattering model over the outflowing-wind-plus-obscuration model of Gaskell (1982) because in the latter model one has to contrive to have the obscuration affect the outer low-ionization lines less. In our scattering model the blueshift of a line only depends on the optical depth and velocity of material outside where the line is emitted. As discussed in section 4.4 below, we can therefore easily predict blueshifting as a function of ionization. For example, C III] 1909 will have a blueshifting about half that of C IV 1549, as is observed to be the case (Corbin, 1990; Steidel & Sargent, 1991).

In Fig. 2 we show a comparison with the blueshifted C IV profiles in a typical AGN, and in Fig. 3 we show a comparison with the VBLR line profile given by SPCA of a sample of AGNs by Brotherton et al. (1994) in. In Fig. 4 we show the blueshifts for composite SDSS spectra (Richards et al., 2002) sorted by blueshift.

It can be seen in Fig. 1 that for a spherical shell, the blueshifting and asymmetry increase with . For (a much greater electron-scattering optical depth than has been considered for the line of sight to a BLR), both the blueshifting and the asymmetry become much greater than is observed (see Figs. 2 – 4), so we can rule out such high optical depths along the line of sight.

Figure 2.— The profiles of O I 1305 (narrow symmetric profile shown in red) and C IV 1549 (thick blue line) for the quasar PKS 0304-392. The thin black line is the blueshifted profile produced by a spherical distribution of scatters with = 0.5, and the dashed green line is the profile produced by the same distribution with = 1. The brown dots are the profile produced by a = 20 inflowing cylindrical distribution. PKS 0304-392 observations taken from Wilkes (1984).
Figure 3.— The mean intermediate line region (ILR) profiles (narrow red profile), and very broad line region (VBLR) profiles (thick blue line) given by SPCA of the ALS sample of Brotherton et al. (1994). The solid line shows the shifting caused by an external spherical shell of scatters with = 2 inflowing at 1000 km s as shown in Fig. 1. The dotted green line is for a similar shell with = 1.
Figure 4.— Shifts in composite SDSS spectra binned by C IV blueshift. Each curve is based on approximately 50 AGNs (see Richards et al. 2002 for details). The blueshifts of each sample are 197, 606, 1003, and 1526 km s for the black, red, green, and blue curves respectively. No attempt has been made to remove blending with He II 1640 or O III] 1663. To match Fig 1, the areas under all curves are the same – i.e., they have been normalized to the same combined flux in the C IV, He II, and O III] blend. These line profiles can be compared with the model predictions of Fig. 1.

4.2. Rayleigh Scattering in the BLR and Torus

While large electron scattering optical depths are not likely along our line of sight to the BLR or within the inner BLR, our modelling of BLR clouds with CLOUDY showed that for clouds of sufficiently large neutral column densities to produce the significant Fe II emission seen in many AGNs, Rayleigh scattering was over an order of magnitude more important than electron scattering in the UV. This is not surprising for a region where hydrogen, which is the main provider of electrons, is mostly neutral, since a typical Rayleigh cross section is larger in the UV than the Thomson cross section. The potential importance of Rayleigh scattering in modifying the spectra of AGNs has been discussed in detail by Korista & Ferland (1998), and Lee (2005) has considered the effect of Rayleigh scattering on the polarization of Lyman .

STOKES does not explicitly handle Rayleigh scattering at present, but the angular dependence of Rayleigh scattering and electron scattering is identical, and the variation of scattering cross section across an emission line is unimportant, so Rayleigh scattering can be treated as electron scattering. The effect of Rayleigh scattering off an inflowing medium completely covering the source will be to give a very large blueshift as shown in Fig. 1 for . Such Rayleigh scattering would, however, be accompanied by substantial blueshifted low-ionization absorption which is never observed. We can therefore strongly rule out such a spherical shell which is optically thick to Rayleigh scattering.

4.3. Scattering off a Flattened BLR and Torus

Although it is unlikely that our direct line of sight to the BLR has a high optical depth to electron scattering, as one goes away from the black hole the BLR must become optically thick (in order to explain the strong optical Fe II emission) and merge with the torus (see GKN), so the optical depth to both electron and Rayleigh scattering will become substantial in the equatorial plane (Korista & Ferland, 1998). The existence of Compton-reflection humps (Pounds et al., 1990) is evidence that that there are substantial electron scattering optical depths. Reprocessing of X-rays requires (see Goosmann et al. 2007). It is also well known that half of all Seyfert 2 galaxies are observed to be “Compton thick” (Risaliti, Maiolino, & Salvati, 1999), so most or all AGNs are probably optically thick to electron scattering in the equatorial plane. Gaskell, Klimek, & Nazarova (2007) have argued that in a typical AGN, the BLR, like the torus, has a covering factor of 40% or so. As Smith et al. (2004) and Smith et al. (2005) point out, a significant scale height of the scattering region is also necessary in order to explain the polarization of type-1 AGNs. The broad-band polarization properties as a function of opening angle are considered in detail in Marin et al. (2012). We therefore modelled an inflowing scattering cylindrical torus with a half-opening angle of 60 degrees, an optical depth of 5, and an inflow velocity of 1000 km s. The viewing position is within the half-opening angle (i.e., as required for a type-1 viewing position). We show the profiles arising from such a model by the dotted curve in Figs. 1.

It can be seen from Fig. 1 that the blueshifting produced by such a model differs insignificantly from that produced by the purely spherical scattering model with or 2. However, unlike the spherical model, the shift produced in the torus model depends only on the inflow velocity, and except for small opening angles (where the flared disk begins to approximate a shell) the shift is less sensitive to large optical depths. This is because in the torus case, after one or two scatterings a photon has a high probability of escape within the half-opening angle. The main difference between the quasi-spherical scattering case and the torus case is that the former produces more blueward asymmetry for a given inflow velocity and optical depths. For most objects, such as the AGN shown in Fig. 2, the difference between the two models is negligible. The advantages of such a flattened BLR and torus are that there is no need to fine tune , and high Rayleigh scattering optical depths are permitted.

The precise geometry of the inflowing region is not important, only the covering factor. As an illustration of this the dots in Fig. 2 show the profile resulting from scattering off an optically-thick cylindrical inflow. This can again be seen to give a line profile similar to an inflowing shell of 1. The similarity of line profiles for a range of geometries is easy to understand because the observed profile is simply the sum of the unscattered profile plus a scattered blueshifted profile. The size of the scattered component depends on the covering factor, and its shift depends on the inflow velocity and the number of scatterings.

Note that in all our models there is some degeneracy between inflow velocity and covering factor, and, if the covering factor is large, with the optical depth as well (see Figs. 1 and 2). This means that our adopted of 1000 km s is not critical. If km s the observed blueshifts can readily be reproduced by increasing the covering factor and/or of the scattering medium. For example, with a scattering region with a half-opening angle of 60 degrees = 700 km s and gives essentially identical profiles as = 100 km s and . On the other hand, it is not likely that km s or else the blueshifting predicted will exceed the observed shifts.

4.4. Blueshifting as a Function of Emission Radius

Our scattering model predicts that the blueshift of a line depends on the inflow velocity immediately outside the radius, , the line is produced at. The radii that given lines are produced at are known approximately from reverberation mapping, and the GKN self-shielding photoionization model also predicts relative radii which agree well with the observed radii for NGC 5548 and other objects. For an inflowing BLR we expect the net inflow velocity, . In Fig. 5 we compare the relative radii, , at which lines are emitted in the GKN model with the mean observed blueshifting velocities for AGNs. The mean blueshift velocity of C III] 1909 has been taken as half the blueshifting of C IV relative to Mg II (see Fig. 3 of Corbin 1990), and other blueshift velocities have been taken from Tytler & Fan (1992). The predicted radii (in light days) are scaled to NGC 5548. While the blueshifts are for the large samples of AGNs studied by Corbin (1990) and Tytler & Fan (1992) rather than for NGC 5548 itself, there is a similar correlation if the mean blueshifts are plotted against the measured lags for NGC 5548. The least-squares fit line in Fig. 5 gives which is consistent with the expected slope of -0.50.

Figure 5.— Mean blueshifts of emission lines (see text for details) versus the radii, , of maximum emission predicted in the GKN model. The line is a least squares fit showing as a function of .

The SDSS sample of Richards et al. (2002) provides additional support for increasing blueshifting with ionization. Fig. 6 shows the He II 1640 and C IV blueshifts which we have derived from the composite SDSS profiles. It can be see that for the sample with the highest blueshifts, the He II 1640 blueshift is approximately twice that of the C IV line as is predicted from the GKN model.

Figure 6.— He II 1640 profiles estimated from composite profiles of SDSS AGNs with low blueshifting (red lines) and high blueshifting (double blue line). The C IV profiles for the same samples are shown as dotted and solid thin black lines respectively. The red side of He II 1640 is heavily contaminated by O III] 1640 and is shown by the dashed red line. It is similar for both samples. The high-velocity blue wing of He II is dominated by C IV.

5. Implications

5.1. Mass Inflow Rate

It has long been noted that, for pure radial motion, the mass transfer rate across the BLR is comparable to the accretion rate. Padovani & Rafanelli (1988) have argued, for example, that if the BLR is purely inflowing, then the mass inflow rate in AGNs correlates well with the accretion rate. Calculating the mass inflow rate is straight forward. We illustrate this by considering the C IV emitting region of the well-studied AGN NGC 5548. The sizes of the emitting regions are known in NGC 5548 from reverberation mapping and the continuum shape is also relatively well known. After reddening correction (Gaskell et al., 2004; Gaskell & Benker, 2007), GKN get a bolometric luminosity of ergs s during the high state of NGC 5548 observed by Korista et al. (1995). (This is only slightly greater than the ergs s estimated by Padovani & Rafanelli 1988). Using the GKN continuum, an observed C IV-emitting radius of 8 light-days, and an electron density , CLOUDY photoionization models give a thickness of cm for the C IV emitting region, and a mass of 1 solar mass. For an inflow velocity of 1000 km s the inflow time from 8 light days is years. Adopting a 50% covering factor (see GKN), this gives a mass inflow rate of 0.08 solar masses per year.

If we adopt a black hole mass of solar masses from the average of the many NGC 5548 black hole mass estimates given by Vestergaard & Peterson (2006), and assume a standard radiative efficiency of 10%, then the Eddington accretion rate is 0.8 solar masses per year, and the accretion rate during the high state studied by GKN is 0.1 solar masses per year. This is comparable to the accretion rate we have calculated from the C IV emitting gas, so we can see that the BLR mass inflow can readily provide the mass inflow rate needed to power NGC 5548. Since the size of the C IV emitting region is well known from reverberation mapping and we know the covering factor to %, the main uncertainty in this calculation is the mean density. If the inflow velocities is less than hundreds of km s then one requires mean densities of the inflowing material of  cm or more.

Although we have calculated the mass inflow rate just for NGC 5548, it should be noted that there is no reason to think that NGC 5548 is unusual in this regard. Padovani & Rafanelli (1988) have shown that their estimated mass flow rates (calculated assuming that the entire BLR is moving radially) are proportional to the accretion rate needed to produce the bolometric luminosity for a wide variety of AGNs, including objects such as I Zw 1, which we now recognize as a high-accretion-rate narrow-line Seyfert 1.

5.2. Producing Inflow

Because of the degeneracy with the optical depth the inflow velocity is not well constrained. However, the inflow velocity needed to explain the blueshifting is likely to be higher than the sound speed at the radius of the BLR. Is it possible to obtain such a net inflow velocity? In the classic Bondi solution there is no problem in having supersonic infall at large distances, but this is unlikely to be relevant to what we are considering since the accreted material has angular momentum.

As is well known, to get a net inflow of matter there must be outward transport of angular momentum. This means that something must apply a torque on the gas. This could be magnetic breaking caused by a wind (Blandford &Payne, 1982) or a viscosity providing a torque between material at different radii. The nature of the viscosity was a long-standing problem for accretion disk modelling, since ordinary gas viscosity is far too low, but it is now recognized that the necessary viscosity comes from the magneto-rotational instability (MRI) (Balbus & Hawley, 1991).

If we have inflow in the BLR, there is the same need for a torque to provide the necessary angular momentum transfer in the BLR gas. It would be natural for this to provided by the same mechanisms as for the disk, i.e., magnetic breaking by a wind, or the MRI.

Visual inspection of MHD simulations of AGN accretion suggests that the turbulent and inflow velocities are roughly of the same magnitude, which is in qualitative agreement with our estimate of the inflow velocity. However, while there can be highly supersonic inflow in the “plunging region” (a few Schwarzschild radii from the black hole), the turbulent and inflow velocities in typical MHD simulations of rotationally-supported Keplerian disks are subsonic at the radius of the BLR. There are however some simulations of gas with sub-Keplerian rotation with substantial inflow velocities. One example is Proga & Begelman (2003) where the inflow velocity in the outer part of the simulations is 10% of the Keplerian velocity (see the upper right panels in their figures 9 and 10). Another possibility (Giri & Chakrabarti, 2013) is that there is a two-component advective flow where a Keplerian disk is surrounded by a rapidly infalling sub-Keplerian halo.

Flares due to the tidal disruption of stars are a valuable laboratory for testing models of accretion disks because they arise from a well-defined injection of mass ( one solar mass) in a one-off event. Cannizzo et al. (1990) used a time-dependent alpha-disk model to study the subsequent evolution of the accretion disk created. They concluded that the disk remained luminous for several thousand years. However, more recent work by Montesinos & de Freitas (2011) shows that the duration of the flare (and disk) is of the order of only a few years to a few decades. This much shorter lifetime means that the inflow velocity is a couple of orders of magnitude higher than in the Cannizzo et al. (1990) model. Now that a number of tidal disruption events have been observed we know that the duration is as in the Montesinos & de Freitas (2011) models and hence that the inflow velocities are higher than in earlier models.

Although there is theoretical and observational support for relatively rapid (supersonic) inflow, more modelling of the motions around supermassive black holes is clearly needed.

5.3. The Relationship Between the BLR and the Accretion Disk

It is now recognized that we are viewing most type-1 AGNs within degrees of the axis (see Antonucci 1993 for a review), and hence that we view the BLR close to face on. Even when we see disk-like line profiles, the inclinations are still not great (see, for example, Eracleous & Halpern 1994 and Fig. 2 of Gaskell 2011). Because the observed broad-line widths are substantial, and the BLR has to be flattened (see GKN), there must be a substantial component of random BLR velocity out of the plane (Gaskell, 2009). Such a velocity is also necessary to maintain the thickness of the BLR needed to provide the observed covering factor.

The overall motion of the BLR (see Gaskell 2009) has to be as follows: the main motion is rotational but there is a vertical random (“turbulent”) component of velocity (Osterbrock, 1978) that is almost as great as the rotational velocity. Then, as argued above, there is an additional, slower, net inflow. As we have noted, this overall structure of the velocity field in the BLR is qualitatively similar to the results of accretion disk magnetohydrodynamic (MHD) calculations (see, for example the simulations of Hawley & Krolik 2001). Gaskell (2008) points out that the size of the accretion disk is such that its outer parts (those generating the optical and IR emission) must extend out to within the BLR. We therefore propose on the basis of the similarities of the size, physical processes needed, kinematics, and mass inflow rates, that the BLR and the outer part of the accretion disk are one and the same. The accretion disk is the part which is optically thick in the continuum and closest to the equatorial plane.

The magnetic fields generated by the MRI potentially solve two major problems. The first is the long-standing “confinement problem” (see Mathews & Capriotti 1985 for a review). Rees (1987) has shown how magnetic fields can confine the BLR clouds. A second problem is the survival problem. Clouds with a random velocity component (e.g., as proposed by Osterbrock 1978) have a mean time between collisions comparable to the orbital timescale (see Osterbrock & Mathews 1986). Cloud–cloud collisions will produce very high Mach number shocks which will immediately destroy the colliding clouds. Strong magnetic fields can prevent shocks from occurring, just as they prevent such shocks in MHD simulations of accretion disks.

6. Discussion

6.1. High-Accretion-Rate AGNs

As discussed in the introduction, it is well established that high-accretion-rate AGNs (such as NLS1s) show strong blueshifting, and this has been interpreted as evidence for strong outflowing winds in high-accretion-rate AGNs (e.g., Leighly & Moore 2004; Komossa et al. 2008). However, the blueshiftings in NLS1s are merely the extreme of the distribution for AGNs in general, so there is no reason to think that they have a different cause from the shifts in other AGNs. We therefore propose that the greater blueshifts in NLS1 imply greater inflow rates. This result follows quite naturally from our STOKES modelling shown in Fig. 1. The amplitude of the blueshifting obviously depends linearly on the inflow velocity, but as shown in Fig. 1, it also depends on the optical depth and covering factor. An inflow velocity of 1000 km s, as we have assumed above, is adequate to explain the typical blueshiftings, but for the most extreme examples, such as Q1338+416, where the shift is almost 5000 km s (Corbin, 1990), a higher inflow velocity is needed. In Fig. 1 the blueshifting is roughly proportional to the product of the scattering optical depth and the inflow velocity. For a given column length the optical depth depends on the filling factor and density. The mass inflow rate is proportional to the mean density and inflow rate. Thus, whether a greater optical depth or a greater inflow velocity is responsible for the increased blueshifts, the blueshift is proportional to the mass inflow rate.

6.2. Estimating Black Hole Masses from C IV Widths

There is considerable interest in estimating black holes masses at high redshifts. Because it is difficult to measure H at high redshift, it has been suggested that the FWHM of C IV 1549 can be used instead of the FWHM of H (Vestergaard, 2002; Warner, Hamann, & Dietrich, 2003). Our conclusion that the C IV-producing region has a net inflow rather than an outflow in a wind is good news for such endeavors. However, the FWHM of C IV needs to be used with caution because, not only does scattering cause blueshifting, but it also broadens the lines (see Fig. 1). The width of C IV can therefore give an overestimate of the virial velocity in the C IV emitting region. Since it is the square of the line width which enters into the equation for the virial mass, significant systematic errors in the black hole mass can be introduced. We have noted above that the blueshifting increases with accretion rate, and that it has also been found to be correlated with radio loudness and the presence of broad absorption lines, so there is a danger of systematic errors when using the FWHM of C IV to estimate masses. It should, however, be possible to empirically correct for these systematic errors by investigating the differences in masses estimated from high- and low-ionization lines as a function of the blueshifting.

6.3. Blueshifts of Narrow Lines

It has long been known (Burbidge, Burbidge, & Prendergast, 1959) that narrow lines in AGNs are blueshifted, and it has been widely assumed that this is a consequence of outflow of the NLR gas and dust (e.g., Dahari & de Robertis 1988). Zamanov et al. (2002) showed that the blueshifting of [O III] 5007 is correlated with the blueshifting of broad C IV line and that both blueshiftings are strongest NLS1s. This is confirmed by Komossa et al. (2008) who have also shown that the blueshiftings of the narrow lines increase with ionization potential. Corbin (1990, 1992) found that the blueshiftings of C IV were related to the C IV Baldwin effect (Baldwin, 1977; Baldwin et al., 1978). This is also very obvious in Fig. 4 of Richards et al. (2002). Zhang et al. (2011) show that the O [III] blueshiftings are similarly related to the O [III] Baldwin effect The NLR blueshiftings thus show many striking similarities to the BLR blueshiftings. Zamanov et al. (2002) argue that the correlation of blueshiftings points to a kinematic connection between the BLR and NLR. We therefore suggest that if the BLR blueshiftings are due to inflow and scattering, then so too are the NLR blueshiftings.

6.4. Broad Absorption Line QSOs and Orientation Effects

Corbin (1990) discovered that his sample of BALQSOs showed unusually large blueshiftings of C IV with respect to Mg II ( km s). Furthermore, he found that the BALQSOs also deviated from the correlation between blueshifting and the Baldwin effect found for non-BALQSOs. This is in the sense that their blueshifts are too large for their equivalent widths. This suggests that there is some additional factor influencing the blueshifting. Since BALQSOs are believed to be seen at higher inclinations (Hines & Wills, 1995; Goodrich & Miller, 1995; Cohen et al., 1995; Elvis, 2000) orientation could be the factor enhancing or even causing the blueshifting of high-ionization lines in BALQSOs (Richards et al., 2002). Our simulations verify that in our scattering+inflow model there is indeed an enhancement of the blueshifting at high inclinations. We find a negligible dependence of the blueshifting on viewing angle within the half-opening angle of the torus (i.e., from any type-1 viewing position), but that there is a strong increase of the blueshifting as we start seeing through the scattering medium (see Fig. 7). The increase in blueshift is because the scattered light becomes more important. In our models this is a relatively abrupt transition (i.e., from all type-1 viewing positions the predicted line profile is like the solid black line in Fig. 7 while for all lines of sight passing through the scattering disk the profiles are like the blue dashed line). In a real AGN the material will be clumpy and the transition will probably not be as abrupt.

Figure 7.— Theoretical C IV line profiles for electron or Rayleigh scattering off a inflowing flared disk of half-opening angle 60 degrees, an inflow velocity of 1000 km s, and a radial optical depth of 5. The solid black curve shows the profile predicted when the system is viewed away from the disk. The dashed blue line shows the profile predicted when the system is viewed from just inside the disk surface as could be the case in a BALQSO.

For the models show in this paper we have used an unchanging unscattered profile, but since observations strongly point to the BLR being flattened and rotating (see introduction) the unscattered profile will actually be broader when seen at higher inclinations. Our model thus also predicts that when high-ionization lines are highly blueshifted because the inclination is higher, there will be further broadening in addition to that caused by the scattering. Inspection of Table 2 of Richards et al. (2002) shows that the more blueshifted C IV lines are indeed broader.

Note that we do not predict that a large blueshift will be observed in type-2 AGNs. This is because the central region is, by definition, obscured by the torus and if the BLR is detectable in polarized light, the scatterers sending light into our line of sight are located far from the central region.

6.5. Determining the Structure of the Scattering Region(s)

The ease with which scattering off inflowing material with differing geometries reproduces the observed blueshifting provides gratifying support for our inwardly spiraling BLR picture. However, a disappointment is that the blueshifting is insensitive to the geometry (see Figs. 1 and 2), and because there is some degeneracy between the inflow rate, covering factor, and optical depth, we cannot get a strong constraint on the geometry and kinematics because of the limited accuracy with which line profiles can be measured. Fortunately, other observations provide constraints on the geometry and kinematics. Two promising ways of studying the distribution and kinematics of the scatters are spectropolarimetry (e.g., Smith et al. 2004, 2005; Goosmann & Gaskell 2007; Marin et al. 2012) and polarimetric reverberation mapping (Gaskell et al. 2012). The combination of the two methods (i.e., high-resolution spectropolarimetric reverberation mapping) promises to be particularly powerful.

7. Conclusions

We have pointed out the problems with the popular outflow/wind explanation (Gaskell, 1982) for the blueshifting and blueward asymmetry of the high-ionization lines, and shown that velocity-resolved reverberation mapping supports the velocity field of the BLR having an inflow velocity component. We have demonstrated using the STOKES Monte Carlo radiative transfer code that electron or Rayleigh scattering off an inflowing medium readily reproduces the blueshifts and asymmetries of the high-ionization lines. Our model also predicts that the relative blueshifts for different lines in the same AGN should be proportional to the inverse square root of the radius the lines are expected to be formed at. Available estimates of relative blueshiftings support this.

If the BLR is indeed inwardly spiraling this has many important implications. Viscosity is required to transport angular momentum outwards. As with traditional accretion disks, this is presumably due to the magneto-rotational instability. As the BLR inflows it releases energy. The deduced mass inflow rates are comparable to the mass accretion rate needed to power AGNs. We have therefore proposed that the broad-line region could be a major part of the material accreting onto the black hole. Taken together these conclusions suggest a picture where the BLR is part of the outer region of the accretion disk.

We have argued that the magnitude of the high-ionization blueshifting effect is proportional to the mass-inflow rate. The inflowing BLR picture thus naturally explains why high-accretion-rate AGNs (NLS1s) show the largest high-ionization-line blueshifts. Our models also gives an explanation of why BALQSOs can show higher blueshifts if they are seen at higher inclinations.

The inwardly spiraling BLR picture supports use of C IV to measure black hole masses in high-redshift AGNs but, because scattering broadens lines as well as blueshifting them, caution is necessary when using C IV line widths. A systematic correction could be necessary as a function of the blueshifting.

Similarities between NLR and BLR blueshiftings suggest that NLR blueshiftings might also due to an inflow velocity component and scattering.

Finally, as Korista & Ferland (1998) have pointed out, Rayleigh scattering could be important in AGNs in the ultraviolet, and we have proposed a simple observational test for the degree to which Rayleigh scattering influences the blueshifting.

RG is grateful to the Astronomy Department of the University of Texas for its hospitality during his time as a Tinsley scholar where this work was begun. We would like to thank Philip Hardee, Liz Klimek, Julian Krolik, Bill Mathews, Matias Montesinos, Ramesh Narayan, Daniel Proga, and Greg Shields, for helpful discussions of various issues. This research has been supported in part by the US National Science Foundation through grants AST 03-07912 and AST 08-03883, by the Space Telescope Science Institute through grant AR-09926.01, the GEMINI-CONICYT Fund of Chile through project N°32070017, FONDECYT of Chile through project N° 1120957, French grant ANR-11-JS56-013-01, the French GdR PCHE, and from the Center for Theoretical Astrophysics (CTA) through Czech Ministry of Education, Youth and Sports programme LC06014. Finally, we would like to thank the anonymous referee for his/her helpful comments.

Footnotes

  1. affiliation: Department of Astronomy, University of Texas, Austin, TX 78712-0259.
  2. affiliation: Centro de Astrofísica de Valparaíso y Departamento de Física y Astronomía, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile. (Present address)
  3. affiliation: Astronomical Institute of the Academy of Sciences, Bocni II 1401, 14131 Prague, Czech Republic.
  4. affiliation: Tinsley Visiting Scholar, Department of Astronomy, University of Texas, Austin, TX 78712-0259.
  5. affiliation: Observatoire astronomique de Strasbourg, 11 rue de l’Université, F-67000 Strasbourg, France. (Present address)
  6. slugcomment: Accepted for publication in the Astrophysical Journal
  7. For a review of the differences between thermal and non-thermal AGNs see Antonucci (2012).
  8. Koratkar & Gaskell (1991b) also find non-statistically significant C IV inflow in four additional AGNs.
  9. Note however, that the apparent extended wings in the AGN considered by Shields & McKee (1981) are actually due to red continuum being too low in the Baldwin (1975) spectrum (J. M. Shuder - private communication).
  10. www.stokes-program.info

References

  1. Antonucci, R. R. J 1993, ARA&A, 31, 473
  2. Antonucci, R. R. J 2012, Astron. & Ap. Trans., 27, 557
  3. Auer, L. H., & van Blerkom, D. 1972, ApJ, 178, 175
  4. Balbus, S. A., & Hawley, J. F. 1991, ApJ, 376, 214
  5. Baldwin, J. A. 1975, ApJ, 201, 26
  6. Baldwin, J. A. 1977, ApJ, 214, 679
  7. Baldwin, J. A., Burke, W. L., Gaskell, C. M., & Wampler, E. J. 1978, Nature, 273, 431
  8. Blandford, R. D., & Payne, D. G. 1982, MNRAS, 199, 883
  9. Blandford, R. D., & McKee, C. F. 1982, ApJ, 255, 419
  10. Blumenthal, G. R., & Mathews, W. G. 1975, ApJ, 198, 517
  11. Brotherton, M. S., Wills, B. J., Francis, P. J., & Steidel, C. C. 1994, ApJ, 430, 495
  12. Burbidge, E. M., Burbidge, G. R., & Prendergast, K. H. 1959, ApJ, 130, 26
  13. Cannizzo, J. K., Lee, H. M., & Goodman, J. 1990, ApJ, 351, 38
  14. Cherepashchuk, A. M., & Lyutyi, V. M. 1973, Astrophys. Lett., 13, 165
  15. Clavel, J., et al. 1991, ApJ, 366, 64
  16. Cohen, M. H., Ogle, P. M., Tran, H. D., et al. 1995, ApJ, 448, L77
  17. Collin-Souffrin, S., Dyson, J. E., McDowell, J. C., & Perry, J. J. 1988, MNRAS, 232, 539
  18. Corbin, M. R. 1990, ApJ, 357, 346
  19. Corbin, M. R. 1992, ApJ, 391, 577
  20. Crenshaw, D. M., & Blackwell, J. H., Jr. 1990, ApJ, 358, L37
  21. Dahari, O., & De Robertis, M. M. 1988, ApJ, 331, 727
  22. Denney, K. D., et al. 2009, ApJ. Letts. 704, L80
  23. Done, C., & Krolik, J. H. 1996, ApJ, 463, 144
  24. Elvis, M. 2000, ApJ, 545, 63
  25. Eracleous, M., & Halpern, J. P. 1994, ApJS, 90, 1
  26. Ferland, G. J., Korista, K. T., Verner, D. A., Ferguson, J. W., Kingdon, J. B., & Verner, E. M. 1998, PASP, 110, 761
  27. Ferrara, A., & Pietrini, P. 1993, ApJ, 405, 130
  28. Gaskell, C. M. 1982, ApJ, 263, 79
  29. Gaskell, C. M. 1983, Liege Intl. Astrophys. Colloq, 24, 473
  30. Gaskell, C. M. 1988, ApJ, 325, 114
  31. Gaskell, C. M. 1996, ApJ, 464, L107
  32. Gaskell, C. M. 2008, Rev. Mex. A&A Conf. Ser. 32, 1
  33. Gaskell, C. M. 2009, New Astron. Rev, 53, 140
  34. Gaskell, C. M. 2010a, Nature, 463, E1
  35. Gaskell, C. M. 2010b in Accretion and Ejection in AGN: a Global View, 427, 68
  36. Gaskell, C. M. 2010c, ApJ, submitted [arXiv:1008.1057]
  37. Gaskell, C. M. 2011, Baltic Astron., 20, 000.
  38. Gaskell, C. M., Brandt, W. N., Dietrich, M., Dultzin-Hacyan, D., & Eracleous, M. 1999, Structure and Kinematics of Quasar Broad Line Regions, ASP Conf. Ser, 175
  39. Gaskell, C. M. & Benker, A. J. 2007, ApJ, submitted [arXiv:0711.1013]
  40. Gaskell, C. M., Goosmann, R. W., Antonucci, R. R. J., & Whysong, D. H. 2004, ApJ, 616, 147
  41. Gaskell, C. M., Goosmann, R. W., Merkulova, N. I., Shakhovskoy, N. M., & Shoji, M. 2012, ApJ, 749, 148
  42. Gaskell, C. M., Klimek, E. S., & Nazarova, L. S. 2007, ApJ, submitted [arXiv:0711.1025] (GKN)
  43. Gaskell, C. M., & Snedden, S. A. 1997, BAAS, 29, 1252
  44. Gaskell, C. M., & Snedden, S. A. 1999, in Structure and Kinematics of Quasar Broad Line Regions, ed. C. M. Gaskell, W. N. Brandt, M. Dietrich, D. Dultzin-Hacyan, & M. Eracleous, ASP Conf. Ser, 175, 157
  45. Gaskell, C. M. & Sparke, L. S. 1986, ApJ, 305, 175
  46. Giri, K., & Chakrabarti, S. K. 2013, MNRAS, in press [arXiv:1212.6493]
  47. Goodrich, R. W., & Miller, J. S. 1995, ApJ, 448, L73
  48. Goosmann, R. W., & Gaskell, C. M. 2007, A&A, 465, 129
  49. Goosmann, R. W., Mouchet, M., Czerny, B., Dovčiak, M., Karas, V., Róžańska, A., & Dumont, A.-M. 2007, A&A, 475, 155
  50. Hawley, J. F., & Krolik, J. H. 2001, ApJ, 548, 348
  51. Hines, D. C., & Wills, B. J. 1995, ApJ, 448, L69
  52. Kallman, T. R., & Krolik, J. H. 1986, ApJ, 308, 805
  53. Kallman, T. R., Wilkes, B. J., Krolik, J. H., & Green, R. 1993, ApJ, 403, 45
  54. Kaneko, N., & Ohtani, H. 1968, AJ, 73, 899
  55. Kollatschny, W. & Dietrich, M. 1996, A&A, 314, 43
  56. Kollatschny, W. 2003, A&A, 407, 461
  57. Komossa, S., Xu, D., Zhou, H., Storchi-Bergmann, T., & Binette, L. 2008, ApJ, 680, 926
  58. Koratkar, A. P. & Gaskell, C. M. 1989, ApJ, 345, 637
  59. Koratkar, A. P., & Gaskell, C. M. 1991a, ApJ, 375, 85
  60. Koratkar, A. P., & Gaskell, C. M. 1991b, ApJS, 75, 719
  61. Korista, K. T., et al. 1995, ApJS, 97, 285
  62. Korista, K. T., & Ferland, G. J. 1998, ApJ, 495, 672
  63. Krolik, J. H., Horne, K., Kallman, T. R., Malkan, M. A., Edelson, R. A., & Kriss, G. A. et al. 1991, ApJ, 371, 541
  64. Laor, A. 2006, ApJ, 643, 112
  65. Lee, H.-W. 2005, in Astronomical Polarimetry: Current Status and Future Directions, eds. A. Adamson, C. Aspin, C. J. Davis, & T. Fujiyoshi, ASP Conf. Ser., 343, 441
  66. Leighly, K. M., & Moore, J. R. 2004, ApJ, 611, 107
  67. Lynds, C. R. 1967, ApJ, 147, 396
  68. Lyutyi, V. M., & Cherepashchuk, A. M. 1972, Astronomicheskij Tsirkulyar, 688, 1
  69. Marin, F., Goosmann, R. W., Gaskell, C. M., Porquet, D., & Dovčiak, M. 2012, A&A, 548, A121
  70. Marziani, P., & Sulentic, J. W. 2012, New Ast. Rev., 56, 49
  71. Mathews, W. G., & Capriotti, E. R. 1985, in Astrophysics of Active Galaxies and Quasi-Stellar Objects, ed. J. S. Miller (Mill Valley, CA: University Science Books), p. 185
  72. Mathews, W. G. 1993, ApJ., 412, L17
  73. Mathis, J. S. 1970, ApJ, 162, 761
  74. Montesinos Armijo, M. & de Freitas Pacheco, J. A. 2011, ApJ, 736, 126
  75. Onken, C. A., & Peterson, B. M. 2002, ApJ, 572, 746
  76. Osterbrock, D. E. 1978, Proc. Natl. Acad. Sci., 75, 540
  77. Osterbrock, D. E. 1993, ApJ, 404, 551
  78. Osterbrock, D. E., & Mathews, W. G. 1986, ARA&A, 24, 171
  79. Padovani, P., & Rafanelli, P. 1988, A&A, 205, 53
  80. Paltani, S. & Türler, M. 2003, ApJ, 583, 659
  81. Peterson, B. M., & Wandel, A. 2000, ApJ, 540, L13
  82. Popović, L. Č. 2012, New Ast. Rev., 56, 74
  83. Pounds, K. A., Nandra, K., Stewart, G. C., George, I. M., & Fabian, A. C. 1990, Nature, 344, 132
  84. Proga, D., & Begelman, M. C. 2003, ApJ, 592, 767
  85. Pronik, V. I., & Sergeev, S. G. 2006, in AGN Variability from X-Rays to Radio Waves, ed. C. M. Gaskell, I. M. McHardy, B. M. Peterson, & S. G. Sergeev, ASP Conf. Ser., 360, 13
  86. Rees, M. J. 1987, MNRAS, 228, 47P
  87. Richards, G. T., Vanden Berk, D. E., Reichard, T. A., Hall, P. B., Schneider, D. P., SubbaRao, M., Thakar, A. R., & York, D. G. 2002, AJ, 124, 1
  88. Risaliti, G., Maiolino, R., & Salvati, M. 1999, ApJ, 522, 157
  89. Rokaki, E., Lawrence, A., Economou, F., & Mastichiadis, A. 2003, MNRAS, 340, 1298
  90. Sergeev, S. G., Pronik, V. I., Peterson, B. M., Sergeeva, E. A., & Zheng, W. 2002, ApJ, 576, 660
  91. Shields, G. A., & McKee, C. F. 1981, ApJ, 246, L57
  92. Smith, J. E., Robinson, A., Alexander, D. M., Young, S., Axon, D. J., & Corbett, E. A. 2004, MNRAS, 350, 140
  93. Smith, J. E., Robinson, A., Young, S., Axon, D. J., & Corbett, E. A. 2005, MNRAS, 359, 846
  94. Snedden, S. A., & Gaskell, C. M. 2004, in AGN Physics with the Sloan Digital Sky Survey, eds. G. T. Richards & P. B. Hall, ASP Conf. Ser., 311, 197
  95. Snedden, S. A., & Gaskell, C. M. 2007, ApJ, 669, 126
  96. Steidel, C. C., & Sargent, W. L. W. 1991, ApJ, 382, 433
  97. Sulentic, J. W., Marziani, P., & Dultzin-Hacyan, D. 2000, ARA&A, 38, 521
  98. Sulentic, J. W., Marziani, P., Dultzin-Hacyan, D., Calvani, M., & Moles, M. 1995, ApJ, 445, L85
  99. Sulentic, J. W., Zwitter, T., Marziani, P., & Dultzin-Hacyan, D. 2000, ApJ, 536, L5
  100. Tytler, D., & Fan, X.-M. 1992, ApJS, 79, 1
  101. Vestergaard, M. 2002, ApJ, 571, 733
  102. Vestergaard, M., & Peterson, B. M. 2006, ApJ, 641, 689
  103. Warner, C., Hamann, F., & Dietrich, M. 2003, ApJ, 596, 72
  104. Welsh, W. F., Martino, D. L., Kawaguchi, G., & Kollatschny, W. 2007, in The Central Engine of Active Galactic Nuclei, ed. L. C. Ho & J.-M. Wang, ASP Conf. Ser., 373, 29
  105. Weymann, R. J. 1970, ApJ, 160, 31
  106. Wilkes, B. J. 1984, MNRAS, 207, 73
  107. Wilkes, B. J., & Carswell, R. F. 1982, MNRAS, 201, 645
  108. Wills, B. J., & Browne, I. W. A. 1986, ApJ, 302, 56
  109. Xu, D. W., Komossa, S., Wei, J. Y., Qian, Y., & Zheng, X. Z. 2003, ApJ, 590, 73
  110. Zamanov, R., Marziani, P., Sulentic, J. W., Calvani, M., Dultzin-Hacyan, D., & Bachev, R. 2002, ApJ, 576, L9
  111. Zhang, K., Dong, X.-B., Wang, T.-G., & Gaskell, C. M. 2011, ApJ, 737, 71
100091
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
Edit
-  
Unpublish
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel
Comments 0
Request comment
""
The feedback must be of minumum 40 characters
Add comment
Cancel
Loading ...

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description