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Produced by the NASA Center for Aerospace Information (CASI)
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IntrOdUCtion

The purpose of this project was to obtain observations of La in a set of l 

redshift quasars selected from the Palomar Green survey of bright quasars. The

problem that motivated these observations was the well known discrepancies of

the hydrogen line strengths in the broad line regions of quasars. The basic plan

was to combine ultraviolet, optical, and Infrared observations to obtain a data

set sampling as broad a range in hydrogen lines as possible in individual quasars. From the measured La fluxes, coupled with Balmer and Paschen line

fluxes measured in these same objects, it was hoped to establish observational

constraints that would guide models of the broad emission line regions of quasaro. In additic,n to this goal, it was found that the JUE spectra were generally of

sufficiently high quality to derive lire profiles of the ultraviolet lines La and CIV

1550A, which have been compared to the Balmer line profiles. Interesting

results have been derived from this comparison.,

Line fluxes

The quasars that were observed in this program are listed in Table 1, along

with the basic results of the IUE, optical, and infrared observations. The

observed fluxes from the ultraviolet, optical, and infrared lines are listed in

Table 1 for these quasars. In Table 2, the relative strengths of the emission

lines, compared to the nearby continua are listed, as are the relative strengths

of the varJous lines.

The results of Table 2 show that the quasars in this study are far from the

simple Case B results, and indeed strain the current model calculations. This is

shown in Figure 1, where the Balmer/Paschen line ratios for these quasars are

plotted and compared in the other samples of quasars (Soifer, et al., 1581,

., ,

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Figure 1. The Pa/Ha line ratio plotted vs the Ha/Hp line ratio for quasars and

Seyfert galaxies from various samples. The filled circles are Seyfert galaxies,

observed by Lacy et al. (1682), the open circles are quasars observed by Soifer,

et al. (1981), and the open squares are quasars observed by Puetter, et al.

(1981). The open triangles are the quasars observed in this program. The case

R line ratios are represented by the point indicated. The case B result viewed

through different amounts of reddening, in units of E(H-V), is shown by the indicated line, The case Pa/Hp = 0.28 is also shown as a line. The predictions

for these ratios of Krolik and Kwan (1961) are indicated by L es noted as

10 10 , 4 x 108 , and 101 . These indicate electron densities of inaLvicival models,

The predicted lire ratios from the models of Canfield and Puetter (1980) are

ghti,wn at the line CP.
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Puetter, at al., 1981) and Seyfert galaxies (,Lacy, at al., 1982). In this figure the

standard Case B recombination point is indicated, as is the reddened Case B

line. Most of the Seyfert galaxies follow this track, strongly suggesting that

reddening significantly effects the line ratios is these objects. The quasars in

} Figure 1 deviate strongly from this line. The quasars in this present study are

represented by the open triangles. Most of the quasars sbow Pa/Hfl ratios close

4 to the recombination, i.e., optically thin ratio of 0.2 - 0.3. Indeed many of these

quasars are found to have line ratios quite similar to those predicted b q q P y the

°r

models of Krolik and Kwan (1981) and those of Canfield and ;P uetter (1980).

Some of the quasars deviate strongly even from these models, most notably two

of the quasars from this sample PG 0803+76 and PG 1202+26 show significantly 

lower Pa/H"? ratio than can be explained by tiie quasar emission line models. 

This discrepancy is hard to understand on physical grounds, since the HQ and Pa

lines originate in the same level, and the physical mechanisms that have been

invoked to decrease the La flux compared to the Balmer lines would also likely

act to weaken the Balmer lines relative to Paschen a. 

Line Profiles

Because of the high signal to noise of the La and CN emission lines it was

found possible to compare the shape of these lines with the Balmer lines in the

brighter quasars to determine if there are systematic differences between the

rPennsnre lines represented by La and CN, and the Balmer lines, represented

by lip (Hp was chosen because of the contamination produced on the Ha profile

by the atmospheric B band). Figures 2a, b, and c, show the comparisons of the

La, CN, and H(3 line profiles in 3 quasars from the sample observed by NE.

From these data it is clear that there are no clear trends in the line shapes,

that can be used to guide models of the dynamics of the broad line regions. For
6

TABLE 2

RELATIVE EMISSION LINE STRENGTHS

0

Equivalent Width (A) Line Ratio

Object La NV Civ Ha Hs Pa La/Hs WHO Pa/HS

PGO803+76 164 8 53 610 130 56 3.5 9.6 0.11±.02

PG1307+08 81 6 75 570 90 125 2.5 9.3 0.27±.05

PG1202+28 323 36 186 955 197 43 2.8 9.9 0.14±.04

PG1416-12 274 30 412 1150 139 159 0.9 5.6 0.23±.06

PC1309+35 91 12 65 502 64 90 1.1 5.7 0.28±.07

PG111.6+21 89 15 72 535 92 80 3.6 12.2 0.22±.07

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ORMINAL PAGE is

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z

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Figure 2a. The line profiles of La, CIV 1550 A, and HP plotted as intensity vs velocity with respect to the average redshift fcr the quasar PG0803+76. No attempt

has been made to subtract NV from the La. profile, or [01II] from the HP profile.
8

Fz

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ORIGINAL WAGE 19

OF POOR QUAL17Y

PG 1416 -° 12 0

^°--- La + NY

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15 °-10 -5 0 5 I® I

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2b. The line profiles of La, C IV 1550 A, and H P plotted as intensity vs velocity with respect to the average redshift for the quasar PG1416-12. No attempt

nas been made to subtract NV from the Lo. profile, or [0111] from the HP profile,
9

OF 

OF POOR QUALM"!'

PG 1307+08 r--,

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2c. The line profiles of La, CIV 1550 A, and HP plotted as intensity vs velocity with respect to the average redshift for the quasar P1307+80. No attempt

has been made to subtract NV from the La profile, or [OIII] from the HP profile.

.e--

w

z
10

example in PG 0803+76 (Figure 2a) La is broader than CN (16500 which is in

turn broader than HQ, while in PG 1416-12 ( 11 figure 2b) the lines are all of roughly

equal shape, or if anything, CIV 1660 is broader than the hydrogen lines. The

case of PG 1307+08 (Figure 2c) is perhaps the most extreme counter example to

the most simple :ninded models, where La is the narrowest of the permitted

lines, with HP wider, and CN 1550 widest of all.

Conclusion

The results described above demonstrate that the search for guiding physical parameters for modeling the quasar broadline regions is most complex, and

will not yield readily to observations. The observed hydrogen emission line 

ratios have shown that the first order models of the broadline regions, such as

those developed by Canfield and Puetter (1981) and Kwan, Krolik (1981) fit the

data adequately but not well enough to claim clear understanding. In particular

the examples of extremely weak Pa lines in two quasars are quite difficult to

understand based on current models of the broad line regions.

In addition, the line profiles shown in Figure 2 cause significant difficulties

with many of the dynamic models of the permitted line emitting gas, since such 

models predict systematic trends in line shape with line optical depth, as

displayed by the La, CN, and HP lines, whereas the observed profiles show no

such trends.
11

REF.E MCES

Canfield, R. C. and Puetter, R. C. 1980, Ap. J. (Letters), 238, L7.

Kwan, J. and Krolik, J. H. 1981, 250, 478.

Lucy, J. H., at W . , 1982, Ap. J.. 258, 75. 

Puetter, R. C., Smith, H. E., Willner, S. P., and Pipher, J. L. 1981, Ap. J., 243, 345.

Soifer, H. T. , Neugebauer, G., Oke, J. B., and Matthews, K. 1981, Ap. J., 243, 368,