192 kB PostScript reprint
R. K. Gulati and R. Gupta
IUCAA, Post Bag 4, Ganeshkhind, Pune 411 007, India
P. Gothoskar and S. Khobragade
NCRA, TIFR Center, P.O. Box 3, Pune 411 007, India
We have implemented ANN to classify stellar spectra from large spectral databases. We present here the Multilayer Back Propagation Network (MBPN), which is used to classify stellar spectra obtained in the optical and ultraviolet regions. The performance of MBPN shows that the ANN is capable of classifying ultraviolet stellar spectra to an accuracy of about one spectral subclass for most of the cases. The scope of this technique is expected to be expanded with the availability of large homogeneous digitized stellar spectral databases.
Progress in ground based and space instrumentation has brought us to a new era of spectroscopy, where a large quantity of good quality stellar spectra has started becoming available through well organized data centers. In order to analyze these spectra and extract useful physical information about stars and stellar systems, we need to develop fast and accurate methods. One way to analyze these spectra is to classify them in terms of common visible properties.
Spectral classification, which conventionally has been done by human classifiers (Houk 1983; Houk & Smith-Moore 1988), involves large, time-consuming efforts. We now require automation of the classification process. The main advantages of automated over human classification is not only the speed with which it can be done, but also accuracy, detection of variability, the elimination of personal error, and the possibility of classification of higher dimensionality.
We (Gulati et al. 1994) have initiated a project to implement automated classification schemes to digitized databases of optical and UV spectra by using conventional metric distance minimization methods and Artificial Neural Networks. We have been using the Multilayer Back Propagation Network (MBPN). Similar efforts have also been employed by another group to classify the stellar spectra of high-dispersion objective prism plates using a neural network scheme (von Hippel et al. 1994). ANN has also been applied to classify a near infra-red database (Weaver 1994).
Here we present the performance of the ANN scheme on libraries of optical and ultraviolet stellar spectra by comparing classifications determined by ANN with those of human classifiers (i.e., catalog classifications).
The optical data were taken from Silva (Silva & Cornell 1992)
and Jacoby (Jacoby et al. 1984) libraries.
A set of 55 spectra selected from the
former library was treated as the template database, and the test database
was a set of 158 spectra from the latter library. Both sets were brought to
a uniform wavelength range of 3510--6800Å with 5Å sampling
and 11Å resolution,
and normalized to a value of 100 at
5450Å . Instead of using the full spectral information, a set of 161 wavelength
positions was used to monitor the fluxes which are diagnostic of the spectral
classes as given by human experts (Jaschek and Jaschek 1990).
Catalog classifications of the spectra were taken from the respective libraries.
The spectra covered
stars of solar metallicity, types O--M, and luminosity classes I--V. Each
spectro-luminosity class was coded with a number
,
where A1 was the main spectral type of the star (i.e., O to M types
coded from 0.0 to 9.5), A2 was the sub-spectral type (coded from 0.0 to 9.5)
and A3 the luminosity class (i.e., classes I to V coded as 0 to 4).
For example, a B2I star and a G9.5V star would be coded as 2201.5 and 5959.5,
respectively.
The input database for the UV data was the IUE Low Resolution Spectra
(Heck et al. 1984). A set of 128 spectra spanning 75 spectro-luminosity
classes was selected as the template and another set of 83 spectra was used as
the test set. The catalog classification was taken from this catalog, where
like MK classification, the UV classification
is given as O, B, F, etc.,
as main classes, subclasses ranging from 0.0 to 9.5,
and luminosity classes represented as s, g, and d for super-giants, giants,
and dwarfs, respectively.
The wavelength range of the UV spectra is 1213--3201Å with 2Å
sampling and 6Å resolution. The spectra were monitored
at 35 wavelength positions which are the diagnostic of these spectral classes as
given in Table 1 of the IUE catalog (Heck et al. 1984). Here, too, the
spectral coding was done
by using a number 
, where A1 was the main spectral type of the star (i.e., O to F types
coded as 1 to 4), A2 was the sub-spectral type of the star (coded
from 0.0 to 9.5), and A3 the luminosity class of the star (i.e., 2,
5, or 8 for s, g, or d). For example, stars dB2.5, gO9.5 and sF7
(ultraviolet classes) were coded as 2258, 1955, and 4702, respectively.
We used the standard feedforward supervised neural network, known as ``multilayer backpropagation network (MBPN)'' (Rumelhart et al. 1986), for classifying the databases of optical and ultraviolet stellar spectra into different classes of stars. As mentioned earlier, the number of output classes was 55 in the optical case and 75 in the UV case. The input data points for optical and UV data classifiers were different, so the ANN classifiers were selected with different architectures for optical and UV data. The optical classifier was found to be optimal with the configuration 161:64:64:55 and the UV classifier was configured as 35:71:75. The configuration numbers show the input size, hidden nodes, and, at the end, the output nodes, respectively. Once the training was over, the networks could classify the large databases of stellar spectra within a minute, without any human intervention.
The performance of the ANN technique can be judged from Figure 1, which shows the 3D plots of classification errors in luminosity and spectral type on x and y axes and the percentage of total test sample along the z axis, respectively, for optical and UV data. In these plots an ideal classification would appear as a single peak of 100% value in the center of the (x,y) plane, signifying that all spectra are classified correctly with no errors in either luminosity or spectral type. One sub-spectral type error means 100 units error along the y-axis of these 3D plots. Statistical parameters, such as linear correlation coefficients and standard deviations, were computed on the scatter plots (for details see Gulati et al. 1994), and it was found that the classification error for optical was about two subclasses and for UV it is about one subclass, barring a few stars which clearly show more than 100 units of error. These stars require further detailed studies.
Figure: 3D plots for classification errors in luminosity (x-axis) and
spectral type (y-axis) vs. the % of total number of test spectra
for Optical and UV data.
Original PostScript figures
(71 kB),
(47 kB)
We do not see any gross mis-classification with the automated ANN scheme and the schemes are quite efficient for large databases. However, we feel that a more homogeneous and complete database is required for the ANN training to perform better. The implementation of ANN on a parallel computer would significantly reduce the training time. In the future, we plan to use a library of synthetic spectra based on stellar atmosphere models (Gulati et al., 1993) to tag information on the stellar physical parameters.
R. K. Gulati wishes to acknowledge the generous financial support from the organizing committees of ADASS IV, which allowed him to present this paper at the conference.
Gulati, R. K., Gupta, R., Gothoskar, P., & Khobragade, S. 1994, ApJ, 426, 340
Heck, A., Egret, D., Jaschek, M., & Jaschek, C. 1984, in IUE Low-Resolution Spectra: A Reference Atlas--Part I, Normal Stars, ESA SP-1052
Houk, N. 1983, in The MK Process and Stellar Classification, ed. R. F. Garrison, (Toronto, David Dunlop Observatory), p. 85
Houk, N., & Smith-Moore, M. 1988, in University of Michigan Catalogue of Two-Dimensional Spectral Types for the HD Stars, 1988, Vol. 4
Jacoby, G. H., Hunter, D. A., & Christian, C. A. 1984, ApJS, 56, 257
Jaschek, C., & Jaschek, M. 1990, The Classification of Stars, (Cambridge, Cambridge Univ. Press)
Rumelhart, D. E., Hinton, G. E., & Williams, R. J. 1986, Nature, 323, 533
Silva, D. R., & Cornell, M. E. 1992, ApJS, 81, 865
von Hippel, T., Storrie-Lombardi, L. J., Storrie-Lombardi, M. C. & Irwin, M. J. 1994, MNRAS, 269, 97
Weaver, Wm. B. 1994, in The MK Process at 50 Years: A Powerful tool for Astrophysical Insight, ASP Conf. Series, Vol. 60, eds. C. J. Corbally, R. O. Gray, and R. F. Garrison (San Francisco, ASP), p. 303
192 kB PostScript reprint