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Astronomical Data Analysis Software and Systems VI

ASP Conference Series, Vol. 125, 1997

Editors: Gareth Hunt and H. E. Payne

**G. J. Ferland, K. T. Korista, and D. A. Verner**

Physics & Astronomy, University of Kentucky, Lexington, KY 40506

A complete simulation involves many hundreds of stages of ionization, many thousands of levels, with populations determined by a vast sea of atomic/molecular processes, many with accurate cross sections and rate coefficients only now becoming available. The scope of the calculations and the numerical techniques they use, can be improved as computers grow ever faster, since previous calculations were naturally limited by the available hardware. The final part is the application to observations, driven in part by the revolution in quality of spectra made possible by advances in instrumentation. The galactic nebulae represent laboratories for checking whether the physics of nebulae is complete and for testing galactic chemical evolution theories, and can validate the analysis methods to be used on the quasars. Models of ablating molecular clouds, the likely origin of some gas in quasars, are tested by studies of the Orion complex. Finally, the quasars themselves present the ultimate challenge: to deduce the composition of their emitting gas from the spectrum, determine the dependencies of this spectrum on the shape of the ionizing continuum, correlating this with observed changes in the spectral energy distribution, and finally to understand its dependencies on luminosity (the Baldwin effect). Once the emission line regions of quasars are understood, we will have a direct probe of the universe.

Cloudy is widely used in the astronomical community, with roughly 50 papers per year employing it. The code is a general spectroscopic tool whose development has an impact well beyond out specific studies.

*
*

The quasars are the most luminous objects in the universe and the highest redshift objects we can observe directly. Understanding their emission lines has a cosmological imperative, since their spectra depend on luminosity (Baldwin 1977; Boroson & Green 1992; Osmer et al. 1994). Once we can directly measure their luminosity, the quasars will gauge the expansion of the universe at redshifts . At the same time, the origin of the chemical elements remains a central theme across much of stellar, galactic, and extragalactic astrophysics. Quasars probe early epochs in the formation of massive galaxies and their emission lines can reveal the composition of the interstellar medium (ISM) when the universe had an age well under a billion years. Within our galaxy, HII regions and planetary nebulae define the end points of stellar evolution. Detailed analysis of their emission line spectra can reveal both the nebula's composition and the luminosity and temperature of the central star(s), and can validate the analysis methods to be used for the quasars.

Deducing reliable abundances and luminosities of galactic and extragalactic
emission line objects is
the central theme of the development of Cloudy. Emission lines are produced
by warm (~10^{4}K) gas
with moderate to low density ( cm^{-3}).
Such gas is far from equilibrium, and its physical
conditions cannot be known from analytical theory.
Rather, the observed spectrum is the result of a
host of microphysical processes which must be simulated numerically.

The ionization, level populations, and electron temperature are determined self-consistently by solving the equations of statistical and thermal equilibrium. Lines and continua are optically thick and their transport must be treated in detail. Predictions of the intensities of thousands of lines and the column densities of all constituents result from the specification of only the incident continuum, gas density, and its composition. By their nature, such calculations involve enormous quantities of atomic/molecular data describing a host of microphysical processes, and the codes involved are at the forefront of modern computational astrophysics. Although the task is difficult, the rewards are great, since numerical simulations make it possible to interpret the spectrum of non-equilibrium gas on a physical basis. Cloudy has been developed as an aid to this interpretation, much as an observer might build a spectrometer.

The next few years will witness first light of a large number of new optical to infrared observational facilities, and we will be in a position to obtain spectra of faint objects with unprecedented precision. The basic atomic data base is growing in both precision and size, and high-end workstations have the power of yesterday's supercomputers-large scale numerical simulations and spectral synthesis can now be done with unprecedented precision and facility. Cloudy is openly available, and other astronomers use it to publish roughly 50 refereed papers per year. It is a general spectroscopic tool whose development has an impact well beyond the specific studies undertaken here.

Cloudy's source (about 110,000 lines of FORTRAN) and its documentation
* Hazy, a Brief Introduction
to Cloudy* (UK Physics Internal Report, 461 pages), are freely available on
the
Cloudy home
page.
This Web page also has group preprints, and Dima Verner's
Atomic Data for Astrophysics
(ADfA) Web page provides
public access to the numerical forms of the atomic data used by
Cloudy.

A major use of spectral synthesis calculations is to deduce the conditions and abundances in the matter producing a spectrum. There is always a question of uniqueness since there may be more than one way to get any particular result, and we must work backwards to deduce the question (properties of the object) from the answer (the spectrum). Examining predictions over the very broadest possible range of physical parameters is vital to really understand what a spectrum is telling us. Today we usually use the code to generate very large grids, involving thousands of complete simulations, to generate contour or 3-D plots like that shown in Figure 1.

**Figure:** CIV 1549 equivalent width for a wide
range of densities and flux of photons.
Original PostScript figure (488kB).

This is an example, based on Baldwin et al. (1995), showing that one of the strongest quasar emission lines is most efficiently produced over a very narrow range of conditions. The peak visibility occurs for the parameters long ago deduced as ``standard'' quasar conditions. We argued that this is just a selection effect.

A * major* effort has gone into making it possible to generate such large
grids on a routine basis.
Issues include the following:

** The code must have enough intelligence to autonomously converge
for models
with very different
conditions, without user intervention.**
This goal has largely been realized. All of the predictions
shown here are the result of fully autonomous calculations with
no outside intervention.

** The code must respond appropriately, no matter what conditions it is
asked to compute.** It goes to
the Compton, molecular, ISM, and LTE limits. The temperature limits are
2.8K**<**T**<**10^{9}K, and
density limit cm^{-3}
because of the approximate treatment of line transfer, and since most ions
are treated as two-level systems. The code will identify conditions which
are inappropriate for its use.

** The code must examine its results and predictions to confirm that
the simulation is valid.**
It simply is not possible to go over the many tens of megabytes of results
generated in large grids, after
the fact, to confirm that all went well. As the code is developed, potential
problems are identified and
logic written to check for this in future calculations.

The code * will probably* converge a simulation with no problems, and it
* will certainly* identify any
problems at the end of the calculation. These are essential core
features-vital if very large grids are to
be computed reliably. Each simulation ends with a summary of all remarkable
or surprising features,
an analysis of any convergence problems, and checks that the range of
validity was not exceeded. One
specific example of these internal checks is that the code now tracks
timescales for all heating-cooling
and ionization-recombination reactions. At the end of the calculation
the code will identify the longest
timescale. A warning is produced if the time-steady assumption is not valid.

The code includes ~10^{4} resonance lines from the 495 possible stages
of ionization of the lightest 30
elements-an extension that required several steps. The charge transfer data
base was expanded to
complete the needed reactions between hydrogen and the first 4 ions and fit
all reactions with a
common approximation (Kingdon & Ferland 1996). Radiative recombination rate
coefficients were
derived for recombination from all closed shells, where this process should
dominate (Verner &
Ferland 1996). Analytical fits to Opacity Project (OP) and other recent
photoionization cross sections
were produced (Verner et al. 1996). Finally, rescaled OP oscillator
strengths were used to compile a
complete set of data for 5971 resonance lines (Verner, Verner, & Ferland
1996).

**Figure:** Cloudy's size as a function of time. This shows only the number
of executable lines of FORTRAN. The
total distributed source now constitutes
~110,000 lines of code.
Original PostScript figure (8kB).

Many other improvements are summarized in Ferland et al. (1997). Figure 2 shows a partial indicator of the scope of this activity, the number of lines of executable FORTRAN, as a function of time. The growth of the code in the past few years has been explosive, thanks to modern workstations.

This is the central difficulty in any large simulation since analytical answers are seldom known. Predictions are affected by the numerical approximations and atomic data used, as well as the presence of bugs which are certainly present in any large program. The best way to verify results is to compare completely independent calculations. We organized a workshop in 1994 to bring together researchers who have developed nebular codes. The result was the set of benchmarks published in the STScI Osterbrock-Seaton commemoration (Ferland et al. 1995). These benchmarks provide reference points to aid validation of any plasma code. We also make a continuous comparison of Cloudy with another independently written photoionization code, LineSpec (Verner & Yakovlev 1990).

Cloudy is widely used by others in their analysis and theory of spectroscopic observations. Figure 3 shows the number of refereed papers acknowledging the use of Cloudy through 1995.

**Figure:** Refereed papers acknowledging Cloudy.
Original PostScript figure (5kB).

At least 138 papers were published in 1993-1995. Although I was not a co-author on these projects, the code did play some role in their execution.

The long-term goal is for the ionization and thermal equilibria of all species and the radiative transfer of continua and lines to be exact for all conditions. By this standard, the code is well over half-way complete.

A major effort has gone into Verner's * Atomic Data for Astrophysics*
(ADfA) database. The results of any
fully non-equilibrium
calculation are no better than the underlying atomic data. New data appear
throughout the physics and
chemistry literature; maintaining the data base is a major ongoing effort,
but one that does not directly
result in publications. The ADfA contains basic atomic data required for
calculation of the ionization
state of astrophysical plasmas and for quantitative spectroscopy. The home
page had more than 3000
visits and more than 4000 data files were retrieved during
October 1995-October 1996. The contents of
ADfA are driven by Cloudy's needs, which are defined by the spectroscopic
problems. Because of
this, and the public access we provide to our data, it has broad application
to anyone working in
quantitative spectroscopy.

We have placed a great deal of effort into deriving accurate fits to the best photoionization cross sections (Verner et al. 1996), the corresponding radiative recombination coefficients (Verner & Ferland 1996), and incorporating them into Cloudy. This effort is continuing, with the eventual goal of a complete photoionization cross section database, for all energies, of all atoms and ions of the first thirty elements. We plan the following developments:

- For some elements, accurate experimental data on the ground-state
photoionization cross sections
are only now becoming available. We are replacing the fits to the smoothed
Opacity Project (OP)
data by the fits to experimental data for such species.
- Some photoionization cross sections include strong and wide resonances
which cannot be
smoothed, and energy positions of these resonances are accurately known by
experiment. We are
extending the treatment of such resonances in our fits.
- We are improving our current photoionization fits for the outer shells
of non-OP elements up to
zinc (
**Z=30**) by use of isoelectronic interpolation of the fits for the OP elements. - Our current fits reproduce theoretical non-relativistic high-energy
asymptotes which cannot be
applied for energies above 50keV. We plan extensions to relativistic cross
sections based on
available X-ray experimental data (see, e.g., Veigele 1973).
- We are creating fits for excited shell photoionization cross sections
of atoms and ions based on
the OP data near thresholds, and on new Hartree-Dirac-Fock calculations far
from threshold. The
new data are being calculated by Band and Trzhaskovskaya (St. Petersburg).
This is needed for
dense environments, and for accurate radiative recombination rate coefficients.

We have calculated radiative recombination rates for all H-like, He-like,
Li-like and Na-like ions of
elements from H through Zn, and fitted them with convenient analytical
formulae (Verner & Ferland 1996). Using our new fits to the excited shell
photoionization cross section data described above, we
shall complete the calculations of radiative recombination rates for ions of
all isoelectronic sequences
of all elements up to zinc (**Z=30**), and fit them by analytical formulae.
This requires partial cross
sections, and cannot be done with total cross sections, such as those
available from the Opacity
Project.

The majority of the ~10^{4} heavy element lines now use collision
strengths from g-approximations
(Gaetz & Salpeter 1983; Mewe 1972). These can be computed on the fly for
any line, but should
only be used for transitions with no quantal calculations. The Iron Project
(IP; Hummer et al. 1993) is
producing large numbers of collision strengths which must be fitted and
incorporated, if this
remarkable data set is to be exploited. We will fit the IP data with
a procedure drawing on our
previous work on photoionization cross sections (Verner et al. 1996) and
the asymptotic limits of
Burgess & Tully (1992). We will develop a generalized scheme to represent
the full temperature
dependence in terms of analytical fits, with coefficients that can be stored
along with other line
information.

We have compiled accurate wavelengths, energy levels, and atomic transition probabilities for the permitted resonance lines of all ionization states of astrophysically important elements (Verner, Verner, & Ferland 1996), and these data are in Cloudy. Thus, the resonance line list is fairly complete. However, the set of forbidden and intercombination lines is not complete, especially for high ionization transitions of 3rd row and higher elements. Using our compilation of experimental energy levels, we will calculate accurate wavelengths for a complete list of forbidden and intercombination transitions between the lowest levels of all ions and elements included in Cloudy. We will compile atomic transition probabilities and collision strengths for them from literature and from available atomic databases, including the very recent database CHIANTI (Dere et al. 1996). All the collision strengths will be averaged over Maxwellian electron distribution, checked for asymptotic behavior by use of the Burgess & Tully (1992) method, and fitted over temperature with analytical formulae.

The ``Locally Optimally-emitting Clouds'' (LOC) model is outlined in Baldwin et al. (1995). The homogeneity of AGN spectra was long a mystery (Baldwin & Netzer 1978). Baldwin et al. (1995) showed that the average quasar spectrum can be produced by simply integrating over all possible clouds. Selection effects due to the line visibility function (Figure 1) ensure that most quasars will have very similar spectra even if their distributions of cloud properties are different.

The new aspect of this approach is allowing a range of cloud properties at a given radius, including ranges in column density and gas density. This seems much more realistic than just single-valued functions. Clouds of different gas densities could exist side-by-side for several viable confinement mechanisms (magnetically or shock confined, or dissipating clouds).

These integrations have been carried out over the full range of possible parameters. The line visibility functions are so strongly peaked that the spectrum of a typical quasar can be easily matched. This is not an entirely positive conclusion-we want to be able to deduce conditions in the quasar from the observations. The advantage is that there is no longer any hidden hand needed to adjust cloud parameters-we are dealing with a known, calculable, set of line visibility functions, which introduce powerful selection effects.

Two approaches are being taken. First we set up specific ``straw man'' distribution functions, compute the resulting spectrum, and compare this with observations. As an example, Broad Line Region (BLR) clouds could be radiatively driven outflows; we find that this can drive mass from main sequence stars near quasars. Such winds are Rayleigh-Taylor unstable, and they should cut off at an optical depth of unity in the Lyman continuum. We have carried out such an LOC integration, and find that the predicted lines can match observations. Radiatively driven winds are consistent with the observations.

The second approach is to use observations to try placing limits on possible distribution functions. We are working with Keith Horne (St. Andrews) to adopt our LOC grids, Keith's maximum entropy techniques (Horne 1994), and Jack Baldwin's line profile observations, to deduce the cloud distribution function. An integration over the full LOC plane produces results which are in good agreement with ``typical'' spectra of quasars (Baldwin et al. 1995). There is a large dispersion from object to object about this mean, which, together with detailed line profile studies, suggests that this plane is not necessarily fully populated in a given object. A goal is to determine observational limits to the cloud distribution functions. The combination of Keith's methods, Jack's observations, and our cloud simulations makes it possible to quantify which portions of the plane are populated, and whether this depends on luminosity.

For both approaches, we will first generate large data cubes containing predicted line equivalent widths as a function of gas density, column density, and flux at the illuminated face of the cloud. There will be a large number of these data cubes, with various continuum shapes and metallicities. Each will be incorporated into an interpolating routine, so that arbitrary parameters can be specified and the resulting spectrum obtained. Calculations of this core set of predictions is now underway and an initial atlas has been produced (Korista et al. 1997).

Our goal in these data cubes is to explore the implications of the LOC. However, this work has application well beyond our specific LOC models. Any other model of the BLR is only a subset of the LOC. Our grids will be made publicly available, so it will be possible for anyone to predict the spectrum resulting from a favored kinematic-spatial-magneto-hydrodynamic model, without becoming involved in the details of photoionization modeling.

The long-term emphasis is to use luminous quasars to probe the high redshift universe. The basic problem is to understand luminosity correlations such as those in Baldwin, Wampler, & Gaskell (1989), and Osmer et al. (1994), on a physical basis. Luminosity-line correlations are complicated by other correlations, such as luminosity with continuum shape, most obviously (Avni & Tananbaum 1986; Worrall et al. 1987; however LaFranca et al. 1995 find no dependence, and Avni, Worrall, & Morgan 1995 find a complicated dependence). The NV/CIV relation discussed by Hamann & Ferland (1992, 1993) suggests a metallicity-luminosity correlation (Ferland et al. 1996; Korista et al. 1997).

The LOC data cubes will be generated for many different continuum shapes, which we characterize by a Big Bump temperature, , and slopes for the bump and X-ray continuum. From this set, we can search for line ratios more sensitive to the continuum shape than to the LOC integration or metallicity. The large data sets available from CTIO will be used, together with our theoretical data sets, archival X-ray and IR observations, to establish constraints on the change in the continuum shape. The CIV/Ly ratio is an example of lines that are sensitive to changes in the ~30eV continuum (Clavel & Santos-Lleo 1990). For the high redshift quasars, the high energy end of the Big Bump is a more important ingredient than the X-rays, and we can make explicit predictions for how line equivalent widths change with continuum shape. This work will be extended using cloud distribution functions, and the absence/presence of Baldwin effects in various lines, to quantify changes in the Big Bump with luminosity.

The development of Cloudy would not have been possible without the continued support of NASA and the NSF.

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Table of Contents - Index - PS reprint

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