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THE ULTRAVIOLET EXCESS OF QUASARS Ill.

The Highly Polarimed Quasars PKS 0758+017 and PKS 1510-069

(NASA -CR-17555 76) THE ULTRAVIOI,ET EXCESS OF H85-22268

QUASARS 3: THE HIGHLY ECLAFI2ED QUASARS FKS

0736+017 AND PKS 1510-089 (Arizona Univ.,

Tucson.) 33 p HC A03/HP A01 CSCL 03A Unclas

.G3/89 14600

Matthew A. Maikan

Steward Observatory

Richard L. Moore

Aerospace Corporation

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Submitted

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ABSTRACT

We analyze ultraviolet/optical/infrared spectrophotometry of the

highly-polarized quasars (HPQ's) PKS 0736+017 and PKS 1510-089. A "blazar"

continuum component like that in BL Lao objects (e.g. with violent

variability, high polarization, and a steep power-law shape) contributes

about half the visual light of 1510-089, and at least three-quarters of

that in 0736+017. The remaining light has the same spectrum as normal

(low-polarization) quasars, including an "ultraviolet excess" or "blue

bump", which is easily detected in the ME spectra of 1510-089, and weakly

delected in 0736+017. The line fluxes do vary, but not as much as the

continuum. The ratios of the broad emission lines, and the Balmer

continuum are normal in both quasars.
1. INTRODUCTION

Earlier studies of the continuum emission from quasars focussed

considerable attention on the optically violently variable, highly

polarized quasars( IIPQ I s). most of which were selected by their strong, flat

radio spectra. HPQ's share the violent variability and high polarization

of the BL Lac objects, and also have relatively steep optical continua,

which either resemble power-laws, or sometimes curve down at higher

frequencies (Moore and Stockman 1981). Like BL Lac objects, HPQ's have

compact, flat-spectrum radio sources. This suggests that the some steep,

violently variable, highly polarized "blazer" continuum which dominates the

optical light of BL Lac objects, is also seen in HPQ's (Moore and Stockman

1984). Rerently Impey and Malkan (1985) have found that even 3C 273, an

apparently "normal", low polarization, small-amplitude variable quasar,

actually has a highly polarized, violently variable continuum component.

It is extremely week, and even at the peak of an outburst it only produces

-108 of the visual continuum.

Evidently, the ratio of "normal quasar light" to highly polarized

continuum can vary continuously from one quasar to another. The IIPQ's are

simply the extreme end of the distribution, where the polarized blazer

component dominates. This hypothesis implies that HPQ's should also have

a weak underlying continuum component that is the same as that of normal 

quasars, but it would be very difficult to detect due to the strong

dilution from the highly polarized component. 

3
4

The continuum shape of normal quasars and active galactic nuclei does

not vary much from object to object (Malkan 1984). They all have an

"ultraviolet excess" or "bump" which is much too strong to be explained by

Balmer continuum and Fe It line emission alone (Malkan and Sargent 1982,

Paper I; and Malkan and Ftlippenko 1983). This "normal" continuum differs

most significantly from a highly-polarized SL Lao continuum at ultraviolet

wavelengths. For example, the average flux ratios fv4220/fv1770 and

fv4220 /fv1450 are 1.55 and I.S. respectively, for normal, unreddened active

nuclei, whereas they are both roughly two and a half times larger in BL Lao

objects. Thus a search for residual "normal" quasar light in the spectrum

of an IIPQ is most profitably conducted in the ultraviolet.

For this search, we selected two of the brightest HPQ's for our

multi-wavelength continuum study. PKS 0738+017 (Zem = 0.191) and PKS

1510-089 ( Zem = 0.381) were singled out by Moore and Stockman (1981) as

having possible rises at the shortest optical wavelengths. In addition to

their blue colors, these quasars often have relatively low optical

polarizations compared to most HPQ's. Thus, they may not be representative

of the HPQ class as a whole, but are well-suited to our search for UV

excesse,!, Observational obstacles prevented us from obtaining detailed new

polarimetric data to measure the wavelength-dependence of polarization.

Thus the new data presented and analyzed in this study are

epectrophotometric. We showed in Paper I and Paper II (Malkan 1983) that
5

these data alone can yield substantial information about the continuum, if

they span the widest possible wavelength range, at least from the Infrared

to the ultraviolet.

The only previous International Ultraviolet Explorer OUE)

measurements of HPQ's were obtained when the objects were bright or

flaring. The infrared/optical/ultraviolet spectra of 1158 + 295 (Glasegold

at el. 1983; Wills et al. 1983) and 3C 345 and 3C 448 (Bregman at al. 1984)

are indistinguishable from those of BL Lao objects. They resemble smooth

steep power-lawe (with slopes steeper than -1.0), with some downward

curvature at high frequencies. None shows any evidence of the "ultraviolet

excess" seen in normal quasars.
6

11. OBSERVATIONS

Like other highly polarized quasars. 0798+017 and 1510-089 are

optically violently variable. The magnitudes of both objects usually range

from V = 18 to 17, and variations of several tenths of a magnitude have

been seen on timescales as short as a few days (Pica at al. 1980.

Wisnieweki 1985). In 1948, 1510-089 showed a remarkable outburst, reaching

a photographic magnitude of 12, but there is no indication that it has been

nearly so bright in the last several decades (tiller and Liller, 1975).

Thus, it is difficult to obtain tr:ly simultaneous spectrophotometry over

the wide wavelength range needed for a detailed study of the continuum.

We have attempted to overcome this problem by repeating the

observations of each quasar several times over the last few years. These

observations allowed us to piece together infrared/optical/ultraviolet

spectra which, although not completely simultaneous, are continuous at the 

overlaps between each spectral section. We were also aided by Wieslaw

Wisniewski's (1985) unpublished UBVRI monitoring of both quasars over the

last several years, which he generously made available to us. Thus, we

believe that our adopted multi-wavelength spectra of these quasars are

essentially the same as they would have been if all the data had been

obtained simultaneously. This approach eliminates the need to arbitrarily

scale any of the fluxes. Table 1 give the dates of all observations, with
7

references. PKS 1510-089 was observed with both cameras of the 1. U. E. by

Glaesgold at al., and we obtained the reduced spectra from the National

Spaces Sciences Data Center. We obtained the LWR (1900 - 3200A) spectrum

of the 0730+017 with 1. U. E. on 31 December 1983, and have combined it

with SWP (1200 -2000A) spectra obtained by Wampler and Kunth et al. two

years earlier, also supplied by NSSDC.

Although the long and short-wavelength ultraviolet spectra were

obtained at different times, they do overlap for a hundred Angstroms around

1900A. In all cases the ultraviolet spectra at different epochs agree well

with each other. Either we were fortunate to have caught these IIPQ's in

the same state each time or they are intrinsically less variable in the

ultraviolet.

Several low-resolution spectra covering 3500-7000A were obtained on

photometric nights in 1983 and 1984 at the Palomar 1.5m and Steward 2.3m

reflectors. Accurate absolute fluxes were measured with large apertures on

the Palomar SIT spectrograph and on the Steward retieon spectrograph. As

with the I.U.E. spectra, by averaging over bins of a hundred or more

Angstroms, we always achieved a signal/noise ratio of at least 10 and

usually 20. Thus, the typical measuring uncertainties of data points are

about 58, and are comparable to the systematic errors which may exist in

the calibrations. Bach figure shows a bar of + 0.05 dex, somewhat larger

than the error of the worst data points.

Our optical observations span the full range of magnitude variations

that 0738+017 has been observed to undergo (in the last few decades). The

V
8

spectra of 22 April and 14 October 1984 (which is slightly bluer) both

represent the quasar at its brightest, while the 21 November 1976 (Grandi

1981) 10 April 1983 (this paper), and 1980 (Blumenthal, Miller and lel,

1982) spectra were obtained near minimum -ight.

Even between these extremes, the shape of the spectrum did not seem

to vary much--in other words the percentage variability at 3500A is of

almost the same magnitude as that in the far-red: one sigma is 0.2

magnitudes at U, H, V, R and t (Wisniewski, private communication). The

optical spectrum we selected (Baldwin 1975) as the best match to the

ultraviolet observations is almost identical (within - 0.1 mag.) to the

average UBVRI fluxes determined by W. Wisniewski (1985) in ten epochs

spanning the last seven years.

We have one additional reason to believe that our optical and

ultraviolet spectra are well-matched. The SWP spectra, which are

essentially the same. were obtained on the 17th and the 22nd of December

1981. One week later, Wieslaw Wisniewski (1985) obtained UBVRI photometry

of 0736+017 which agrees very well (to within - 0.1 mag. at all

wavelengths) with Baldwin's spectrophotometry. And since we adopted

Baldwin's spectrum in our analysis, it should at least match the SWP

points. The continuity of the LWR spectrum indicates that our adopted

spectrum 1s indeed a good representation of 0736+017 in late December 1981.

Our 7 April 1984 spectrum of 1510-089 is quite similar to that

obtained by Neugebauer et a1. (1979). The quasar was fainter than
9

average, and considerably fainter than when Oke at al. (1970) measured it

in 1967 near maximum. In fact, it was almost as faint as it was on 16 July

1983, when it reached an historical minimum brightness (Malkan 1984). In

the following analysis, we use the 7 April 1984 spectrum, since it gives

the best match to the I.U.E. spectra. The original 200" multichannel

spectra from Neugebauer et al. (1979) are also used to fill in the

0.7--l.05um fluxes. The percentage variability of 1510-089 is slightly

smaller, with a one-sigma magnitude of 0.15 mag., again with no wavelength

dependence.

Unfortunately, the only available infrared photometry was not

obtained in the same years as the spectra. Hyland and Allen (1982)

observed both quasars at 1.2-2.2 um on two occasions each, and found that

both had varied. 1510-089 changed by 0.3 mag. in two days, with its

C

fainter fluxes the same as those. Neugebauer et al. (1979) observed in May

1977. The 2.2 pm flux measured at Palomar in June 1967 (Oke,

Nueugebsuer, and Becklin. 1970) was 0.6 mag. brighter. For 0736+017 we use

the average of the Hyland and Allen measurem`nts of April and November 1979.

In Table 2. we give emission line equivalent widths and, where

available. fluxes. The forbidden lines (e.g. 10111 3727A, (01111 5007A)

were too weak to measure. Although the Balmer line fluxes do not appear to

be constant, they certainly do not vary as strongly as the continuum. Thus

the equivalent widths tend to drop with increasing continuum flux, in. both

quasars. When they change, it is by a roughly wavelength-independent

factor (e.g. the equivalent widths of Mg 11 2800 and lie drop by the same
10

factor). This observation, along with the absence of strong systematic

spectral changes confirms our view that the variability is primarily due to

a component with a roughly power-law shape, with about the same elope as

the overall spectrum, and that this variable component is a major

contributor (at least 508) to the light observed at 0.05-0.85 um.

i
11

I11. ANALYSIS

We analyze the continuous spectra, plotted in Figures 1 - 3 following

the procedures of Papers I and 11. First we make corrections for he

effects of reddening and contamination from the starlight of the underlying

galaxy.

The it I column-densities in the directions to 1510-089 (1 = 353 0 , b =

+38 0 ) and 0738 + 017 (l = 218 4 , b = +11 0 ) imply Milky Way reddenings of EB-V

= O m .01 and Om .12 respectively (Burstein and iteiles 1982). A small amount

of internal reddening (E S -V = 0m .02) is included in the analysis of

1510-089, since it decreases the residuals of the continuum fits slightly.

Direct imaging by Wyckoff at al. (1983) shows that PKS 0738+017 lies

In a faint host galaxy, with a total diameter and red magnitude of 20Tr and

19.9 mag. Our fits include a 0.07 mJy starlight contribution to the

observed visual flux. a very minor correction. The galaxy which is

presumed to harbor PKS 1510-089 is almost too distant to be detectable in

deep photographs of Wyckoff et al. 1981 and Hutchings at at. 1984.

The fitted spectra Included the Balmer emission lines and continuum,

and an extensive tabulation of Fe It emission lines. Their relative

strengths were calculated by Netzer and Wills (1983), who kindly provided a

printout of the results of their "standard model."
12

Since the Balmer continuum is always stronger than the predictions of

Case B recombination, our fits (which assume Case B ratios for the Balmer

lines) fall below the observations between 9900 and 9700A, where

blended Balmer emission produces a strong pseudo-continuum.

(a) 1510-089

The infrared/optical/ultraviolet continuum, shown in Figurealandlcan

certainly not be fitted by a single power-law, even in combination with

strong Balmer conttnuum and blended line emission. The spectrum is similar 

to those of normal quasars: it has strong upward curvature which is even 

visible between H8 and the near-infrared. At these longer wavelengths, the

emission-line and Balmer continuum components are negligible. Thus,

1510-089 has a strong "ultraviolet excess," or "blue bump," which begins to 

contribute noticeably to the continuum below 5000A.

In normal quasars, this bump is broader than a single-temperature

blackbody (as shown in Paper It. and more dramatically for 8201 in Paper

IV). Nonetheless, we first fitted the blue bump in 1510-089 as a single

Planck function because it is a fair approximation over the observed

wavelength range, and can be compared with the blackbody fits in Paper I.

The best fit. and two which closely bracket it, are shown as the solid

lines in Figure 1. The best-fit blackbody temperature Is 99.000 K, and the

other lines show the effect of changing it by t 2,000 K. This temperature

is at the high end of the range of 21,000 - 94,000 K found in Papers 1 and

It.
13

The fitted power-law slope, -1.7, is markedly steeper than those of

normal quasars, but is typical of BL Lao objects and other IIPQ'e. The

total power-law/blackbody ratio at Ao = 5500A is 0.8, nearly twice as

strong as in the average normal quasar. The normal quasar continuum

probably also has a red component resembling a power-law with slope -1.1

(Paper 1). However at long wavelengths, the steeper blazer power-law

dominates the spectrum. Thus, the continuum properties of 1510-089 can be

interpreted as a combination of HL Lac continuum (with high polarization,

violent variability, and a steep power-law slope which extends out to

millimeter wavelengths) and normal quasar light. In the faint state we

observed it in, the ratio of these two components was roughly one-to-one at

5500A.

In .Figure 2, we show the fits to the continuum when we model its

:atrvr'alet excess as light from an accretion disk around a non-rotating

(5chwarzachild) black hole (as in Paper 11). As before we assumed the disk

was in a steady-state. optically thick, geometrically thin, and viewed

face-on. The beat-fit black hole mass is 0x10 7 Me; the two solid

lines show models with hole masses of 5 and 7x10 7 MO, either of which also

fits the data satisfactorily. The best-fit accretion rate corresponds to a

luminosity 408 s 20% that of Eddington limit. Had we assumed that the hole

were rotating rapidly, the inferred mass would nearly triple, while the

inferred accretion rate would drop by a factor of 2 to 3. In this case the

accretion rate would be about 30% of critical (Paper 11).

(b) 0738 + 017

Even after correction for interstellar reddening, the ultraviolet

continuum of 0738 + 017 is much redder than that of 1510 - 089. The
14

optical / ultraviolet colors of 1510 -089 are slightly redder than those of

normal quasars: fv 4220 /fv 1?70 = 2.1 and fv4220 /fv l48U = 1.9. However, the

de-reddened intrinsic colors of 0738 + 017 are 2.7 for both ratios, closer

to the average values for BL Lao objects, Its infrared/optical / ultraviolet

continuum is almost adequately fitted simply by a power -law plus

recombination and Fell line emission ( the flatter fit in Figure 3).

However, this fit would require a power-law slope of a = -0.8,

significantly flatter than the -1.1 index usually seen in the far-red (Ao =

0.8 - 1.8 um) In other quasars. The pure power -law fit is rather poor in

the far-ultraviolet, where it fails to predict the steep fall-off in flax

observed at rest wavelengths shorter than 2000A. Such a flat slope is also

clearly inconsistent with both sets of infrared photometry, which give a

(1.85 - 1.0 um) _ -1.4, and the average R-I color, which corresponds to a

(0.75 - 0.00 um) _ -1.2. This inconsistency is exacerbated when we

remember that the infrared measurements shown in Figure 3 are probably a

little too faint to match the optical data. Phus, we prefer the flt with a

_ -1.0, which must include a blackbody component, although the latter's

presence is not as certain as it is in 1510-089.

The blackbody component is so weak that its strength is poorly

determined. But following the assumption made for 1510-089 (that the

"normal" quasar light has a power-law to blackbody ratio less than 4). we

infer that less than a quarter of the continuum of 0738+017 Is normal

quasar light. More than three-quarters of the ao = 5500A continuum must

belong to the highly polarized, variable, "BL Lac" component.

^'' sar Rai..:..
15

(c) Emission Lines

The optical and ultraviolet broad emission-Une ratios. listed in

Table 2, are indistinguishable from those of normal quasars. The Balmer

lines in 0736 + 017 have unusually small equivalent widths, presumably

because of the dilution from the blazer continuum. Equivalent widths

measured with respect to the normal quasar light alone are at least as

strong in these two IiPQ's as those of normal quasars.

The intrinsic Balmer continuum/line ratios are the same as those seen

in other quasars and Seyfert 1 galaxies (Malkan and Sargent, 1982; Malkan,

1983). For optically thin Balmer continuum emission at Te = 10,000 K, the

ratios Bee/Ha and Bac/H8 are 2.3 and 8.7, respectively, in 0736 + 017 and

1.9 and 6 in 1510-089. Since these emission-line ratios are normal, we

Infer that the shape of the unobserved far-ultraviolet ionizing continuum

cannot be too abnormal. This strengthens our contention that the

broad-line regions in HPQ's are illuminated by the underlying "normal"

quasar spectrum.

The X-ray luminosities of both quasars were measured by Ku et al.

(1980). Comparing the X-ray fluxes to the Infrared fluxes (which may

actually be somewhat low), (the logarithmic elope fromigives aix = -1.15

for 0736 + 017 and -1.1 for 1510-089. These slopes are only marginally

flatter than the average aix for normal AGN, -1.18 (Malkan. 1984x). As

suggested in Paper 1, we see that the violently variable/ polarized

. , «s3 Tom%%^^:(:.. 
16

component in HP@'s does not have a very different infrared/X-ray elope from

that of normal quasars. At moat. for a given infrared flux. the polarized

component might produce twice as much X-ray flux as an unpolarized

continuum.
17

IV. CONCLUSIONS

By analyzing the continuum over a wide range of wavelengths

(ultraviolet, optical, and infrared), we find that the IIPQ's 0798 + 017

and 1510 - 088 have mixtures of "blazer" (highly polarized, violently

variable) light and "normal" quasar light. The blazer component, which

produces about half of the visual light in 1510 - 089, and three-quarters

of that in 0798 + 017, is indistinguishable from that of SL Lao objects,

and is probably generated by the same physical mechanism. Its spectrum is

quite red and is characterized by a power-law with slope -1.1 to -2.0.

The "normal" quasar light is probably the same as that of quasars

studied in Papers I and 1I. It can be further divided into continuum

components; a power-law with slope -1.1 ± 0.1, and a strong "blue hump"

believed to be thermal emission, perhaps from an accretion disk. We

emphasize that this "normal" power-law is different from the blazar

power-law continuum, in having a flatter slope, milder variability, and

lower polarization. It may also be nonthermai, like the blazar continuum,

but these differences indicate that the physical origin is not the same in

detail. Likewise, the weak optical polarization measured in normal quasars

Is very different from that of blazers. It rises significantly at shorter

wavelengths (Stockman. Moore and Angel 1984), and is probably not

AiIwIej

attributable tsynchrotron emission.

In contrast, there are several reasons to believe that the blazar

component is at least antsotropic, and perhaps relativisticaily enhanced.
18

It is usually associated with compact, flat spectrum radio-emission and

with low-radio frequency variability

(Moore and Stockman 1984). In fact. PKS 0736+017 shows strong low

(mr_Ado, iqi&)

/ frequency variability^ It is difficult for the standard incoherent

synchrotron mechanism to explain the small sizes implied by this

variability and the lack of stronger inverse-comptonized X-ray flux without

resorting to bulk realtivistic motions (Marseher 1980). Most models for

the suporluminal expansions detected by VLBI also require beamed.

relativistic outflow (Unwin at al. 1983).

We observe that the line emission (presumed iso(pic) does not vary

nearly as much as the continuum, in contrast to the lines in normal Seyfert

1 nuclei (e.g., Oke, Readhead and Sargent 1980; De Bruyn 1980). This

further suggests that not all of the optical continuum variation is

actually "seen" by the broad-line region, which is expected if the blazer 

component is anistropic.

Our two-component analysis of these HPQ spectra predicts that the

blazer characteristics should be increasingly important at longer

wavelengths, and when the continuum is brighter. The two times 0736 + 017

was seen to be highly polarized (4.38 on 10/27/78, and 5.68 on 11/26/78).

it was indeed unusually bright (visual magnitude estimated at 15.5 - 16.0).

However, even when bright, it sometimes shows a lower polarization. No

brightness/ polarization correlation is evident in 1510-089 (Moore 1981),

At least one wavelength-dependence measurement of 0736+017 by Moore

and Stockman (1981) did show the expected increase in polarization with

-- 
19

wavelength. In November 1978, the blue polarization was 4.97 + 0.278 (9 =

28 0 + 1 0 ) . while the red polarization was 6.12 + 0.208 (9 = 310 + 10). A

marginal effect was seen in October 1978, when the blue polarization was

0.86 + 0.428 ( 9 = 63 0 + 140 ), whle the red polarization was 1.17 + 0.398 (9

= 28 0 + 90).

Recent UBVRI photometry of the low-polarization ( P - 0,58) quasar PKS

2128-123 also supports our two-component analysis. This quasar is a flat

spectrum radio source, but is only moderately variable at blue-visual

wavelengths ( Pica et al. 1980). Moles at al. ( 1985) observed

large-amplitude ( up to Cm = 1.69 mag) night-to-night variability in the I

wowld ^/

band, where we suspect the light of a blazer component AdominateA. At the

same time, the variability of shorter wavelengths was much smaller (a - 0.3

mag), presumably becuase of the dilution from a normal quasar continuum.

Evidently, its ratio of blazer to normal continuum is somewhere between

that of 1510-089 and 3C 273.

Thus our results establish for the first time that a "normal" quasar

continuum is presont in these HPQ ' s, in addition to their emission lines

and highly polarized blazar continuum. This result, combined with the

discovery of a weak blazar component in 3C 273 by Impey and Malkan ( 1985).

demonstrates that HPQ ' s represent one extreme in the relative strength of

blazer to " normal" continuum. The presence of a "normal" continuum in

HPQ's is an important test of an anisotropic model for the optical emission

of quasars, but does not in itself prove the model. The primary arguments

for optical anisotropy remain the statistical connections between optical

blazar properties and the anisotropic ( beamed) radio properties of quasars.
20

ACKNOWLEDGMENTS

We are grateful to Dr. M. Cohen for sponsoring our IUE proposal, and

NASA grant NAG 5-337. We thank Dr. W. Wisniewski for providing us with

his excellent set of photometry, B. Wills and H. Netzer for providing the

Fe lI line strengths from their standard model. and S. Grandi and W. Keel

for supplying plots of some published Lick spectra. We also thank R.

Thompson and K. Feggins at the IUE RDAF for assistance with the ultraviolet

data reduction, and R. Goff'. A. Bauer. M. 7.eitner for assistance at the

2.3m telescope.
21

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^

Dale Telescope

Lag

Wavelength

TADIS 1

of Observations

Spectral

Resolution Aperture Scums

0778 • 017

72 2 Lick 2.9m 3200-02094 7A 2x4" Baldwin 1978

Nov T8 Lick 2.Om 2200-5300A fA 2x4" Orandl 1981

Apr. Nov T9 1' AAT 1.2 — 2.2um O.lum --- Hyland and Allen 1082

19. It Dec 81 2 IUB 1200-2000A 8A 10x15" Oval Womplsr.

Runth et al.l

82 Lick 2.0m 2200-7000A 1A 2x4" BRM

9 Apr 02 Palomar 1.5m 2800-6900A 9A 8x18" This Paper

21 Dee 822 IUB 1900-2200A 1A IOxIS" Oval This Paper

27 Jon 84 Steward 2.2m 0000-9509A 9A S" Circular This Paper

21 Apr 04 Steward 2.3m 2000-0500A BA 5" Circular This Paper

12 Oct 84 Steward 2.2m 0200-0500A 9A 9" Circular This Paper

EI 14. 15 Feb 08 Slewnrd 2.3m 2000-0700A 9A 8" Circular This Paper

Mar 77-Afar 84 2 Steward L.Sm 2900-SOOOA I500A 12"7 Circular Wlaniewski 1988

1510-089

Jun 78 Lick O.Om 5200-t000A to 2x4" BRM 1982

Feb 77 Palomar 5.0m 2200-10.000A 40100A 10" Circular Neugebauer

at al. 1979

May 77 2 Palomar 8.0m 1.2 — 2.2um O.lum 10" Circular Neugebauer

at el. 1979

Mar 792 AAT 1.2 -- 2.2um O.lum Byland and Allen 1982

8 Jun W lug 1900-3200A 7A IOxIS" Oval Glasngold at al.l

21 Jan 802 lug 1200-2000A 9A IOxIS" Oval Glassfold at al .I

T Apr 83 2 Palomar L.Sm 2500-6900A 9A 9x10" This Pspor

21 Apr 84 Steward 2.2m 2500-OSODA 8A S" Circular This Paper

I 14 FPb 85 Steward 2.2m 2300-9700A 9A 9" Circular This Paper

F Feb 82-May 04 Steward 1.5m 2500-ROOOA 1500A 12"7 Circular Wisniewski 1908

I These reduced IUB spectra were obtained from the National Space Sciences Data Center.

2 These spectra were used In the multi-wavelength continuum titling described In the text. They are also

plotted In the figures.
Table 2

Emission Line Fluxes (in 10' 14 erg seo-1 cm-2)

and

Equivalent Widths 1 (in A)

Spectrum Lye CIV Mgli fly 118 He

0736 • 017

12/81 15 9

/72 12 2.8 7.0 30

51 23 63 310

11/76 --- --- 67 39 91 374

/ 1 18 45 250

1/84 2.1 5.8

17 52

4/84 2.7 7.6

14 45

10/84 3.0 7.7

18 55

2/85 2.5 6.2

18 54

8

31

6/76

/77

2/77

1/83

4/84

2/85

1 corrected to zero-redshift

1510-089

55 38

6.5 ---

57 ---

9 4.5

66 66

7.2

47

78

115

5.3 18

110 530

7.0

115
Table 3

ultraviolet Fluxes (in m.ly)

Corrected for Redshlft

log vo 0738+017 1510-089

15.508 ---- 0.15

15.428 0.08 0.18

15.352 0.12 0.28

15.320 --- 0.28

15.310 0.15 0.24

15.229 0.18 0.18

15.189 0.23 0.27

15.142 0.29 0.33

15.122 0.32 0.28

15.095 0.33 0.30

15.084 0.34 0.32
Table 4

Optical Continuum Flu0es

Correoted for 1ledehlft

tin mJF • 10-t6 erg seo' 1 am', HO)

log vo 0726 • Oil ISl0 - 089

#4 ^}

14.15 Feb 95 21 Apr 94 17 Jan!- 9 Apr. 14 Feb 85

1

V Apr. 84 7 Apr 92

15.017 - 0.76 --- 0.29 0.42 0.28 0.40

15.001 --- 0.65 ---- 0.28 0.42 0.20 0.44

14.988 -- 0.82 0.67 0.21 0.42 0.27 0.45

14.975 0.70 0.80 0.60 0.42 0.40 0.42 0.41

!4.962 0.81 0.90 0.11 0.44 0.50 0.46 0.49

14.951 0.80 0.92 0.71 0.45 0.49 0.47 0.50

14.942 0.84 9.99 0.75 0.46 0.50 0.48 0.50

14.922 0.88 1.01 0.75 0.47 0.50 0.49 0.51

14.924 0.84 1.01 0.12 0.49 0.49 0.46 0.50

14.912 - 1.02 0.15 0.40 0.50 0.48 0d7

14.095 0.84 1.05 0.76 0.48 0.49 0.40 0.48

14.872 0.81 1.02 0.72 6.40 0.48 0.44 0.40

14.951 0.81 1.04 0.16 0.50 0.51 0.46 0.40

14.628 0.89 1.10 0.86 0.57 0.52 0.52 0.57

14.801 0.92 1.20 0.90 0.58 -- 0.45 0.66

14.790 - ---- --- --- 0.55 0.49 -

14.772 0.98 ---- I.OI 0.76 -- ---- 0.72

14.758 --- --- ---- 0.87 - 0.52 ---

14.744 1.07 1.26 -- 0.95 -- 0.46 ---

14.720 1.08 1.42 --- 1.05 -- 0.56 --

14.712 1.08 ---- ---- 1.15 --- 0.52 --

14.690 - --^- --- --' --- 0.58 0.96

14.612 - --- -^ --- --- 0.65 ----

14.652 -+ ---- ---- ---_ - 0.84 -

14.626 0.79 --

14.610 -'- --- ---- ---' -- 0.99 -

14 .800 -» --- ---- --- --- 0.77 -

14.580 -- ---- ---- -_ - 1.04 -

r-

._.....
Table 5

Model-Fitting Results

Balmer Accretion

QSQ Continuuma Power-Law Blackbody Disk

Ha a fvob

No Temp (K) Mbh(M(9) M(Mp/yr)

0736+017 24 -1.0 0.90 0.05 26.000 ---c ---c

1510-089 1.9 -1.7 0.46 0.07 33,000 6x107 1.0

a Balmer continuum was assumed optically thin, at 10,000K.

b All fluxes refer to rest frequency of i( — vo = 14.74, and are given In

mJy (10-26 erg em-2 e-1 Hz-1 ), reddening-corrected.

e The ultraviolet excess in 0736 + 017 is too weak to allow accurate

estimation of disk parameters.
FIGURE CAPTIONS

Figure 1. Fits to the infrared/optical/ultraviolet spectrum of 1510-088,

with a power-law, blackbody, and contributions from Balmer and

Fe 11 emission lines, and Balmer continua. The three curves

are for blackbody temperatures of 31,000, 33,000, and 35,000K.

The bar which shows 0.1 dex in flux, is larger than the errors

of the worst data points. The curve with the hottest

blackbody temperature has the most flux in the far ultraviolet.

Figure 2. Fits to the same multi-wavelength data as shown in Figure 1.

Here the blackbody component was replaced by the spectrum

emitted from an optically-thick, geometrically thin, face-on

accretion disk. The two curves, which fit the data better

than the blackbody fits in Figure 1, are for Schwarzechild

black hole masses of 5 and 7 x 107 %1@. The curve with the

stronger far ultraviolet flux is for the smaller hole mass.

Figure 3. Fits to the multi-wavelength spectrum of 0738 + 017. The

flatter curve, which is a slightly worse match to the

shortest-wavelength points, is for a power-law of slope -0.8,

plus Balmer continuum, and Balmer and Fe 11 emission lines.

The steeper curve has a power-law slope of -1.0 and a weak

28,000 K blackbody component. This blackbody curve has a

higher flux in the infrared, and lower flux in the far

ultraviolet, and is crossed twice by the pure power-law curve.

—.1— -
-25, C

1510-089

BLACKBODY FITS

I II

I

I

I/

I I

I

I

II I

I I

I

I ;^

10.1

C%

u -26.0

1

V

d

f/1

V

v

a0

J

-27.0

14.0 14.5 15.0 15.5 16.0

Log V. (Hz)

1

N

M

1

Aa
-25.

N

T.

a

I

u

ra

a>' M

OI V

V41

a°

of

27.t

14.0 14.5 15.0 15.5 16,0

Log V. (Hz)
-25.0

0736+017

10.1

N

a

iE -26.0

v

i

vdN

v

L

a

J

- 27.0

14.5 14.0 14.5

Log Vo (Hz)

I J.V 1
A-tth l

re' Addreeeeet Moo • hw A Me'kevt

CA nrrrh

R l rhoird L Mire.

gn01A.

0.1

Dep'+. n' Aetr„- y^ UCLA, L'se Awet.ee^

P c 3cX I'Z'i^7

Aer+epere C'>trpore t +ni, Los Ai o el.ee, CA

rn •c - M4-'IOLA

OF p^R QU^rY