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Cr> Γ- ΟΟ [ Publications of the Astronomical Society of the Pacific cr> - ΟΟΓ [ Publications of the Astronomical Society of the Pacific cs] 102:379-411, April 1990 \—I0 ωCu 1 PUBLICATIONS OF THE 2 ASTRONOMICAL SOCIETY OF THE PACIFIC Vol. 102 April 1990 No. 650 CONTEMPORARY OPTICAL SPECTRAL CLASSIFICATION OF THE OB STARS: A DIGITAL ATLAS* NOLAN R. WALBORNt Space Telescope Science Institute, φ 3700 San Martin Drive, Baltimore, Maryland 21218 AND EDWARD L. FITZPATRICKf Princeton University Observatory, Peyton Hall, Princeton, New Jersey 08544 Received 1990 ABSTRACT Some recent developments in the optical classification of OB spectra are reviewed in terms of a comprehensive atlas of new blue-violet digital data from the CTIO 1-meter photon-counting system. These developments include the OS spectral type; luminosity criteria for the O stars; OBN/OBC anomalies; and refined, interpolated late-O/early-B types. Examples of these phenom- ena are included among extensive spectral- and luminosity-class sequences, comprising 75 standard objects arranged into 27 montages and covering the wavelength range 3950 Â-4750 A for types OS-BS (-B8 at Iö). It is intended that this atlas serve a reference function analogous to that of the printed MK atlases, for morphological investigations of OB spectra based on digital data, which will supersede photographic techniques in most future applications. Key words: spectral atlas-OB stars 1. Introduction and Background The Μ Κ classification was based on blue-violet The system of spectral classification provided one (3900 Â-4900 A) photographic spectrograms of disper- Μ Κ -1 of the foundations of stellar astrophysics. Far from being sion ~ 100 A mm (resolution ~ 2 A) and widening at rendered obsolete by the development of the latter, how- least 0.5 mm. This wavelength range represented a happy ever, morphological techniques maintain a vital system- correspondence between the sensitivity maximum of atic role as modern astronomical spectroscopy expands photographic emulsions and the highest density of optical wavelength, information content, and apparent-magni- absorption lines offered by stellar spectra. The widening tude limits, revealing ever more of the phenomenological permitted reliable results at a relatively low formal S/N by intricacies inherent in stellar spectra. The difficult task of providing a third dimension which allowed ready discrim- extracting the physical information contained in these ination between weak lines and noise of comparable am- phenomena is usually facilitated by prior morphological plitude. One of the precepts of Μ Κ classification was that analysis. the defining standard objects be obtained with the same instrumental characteristics as the unknowns, the latter *One in a series of invited review papers currently appearing in these then being described differentially relative to the stan- Publications. tVisiting Astronomer, Cerro Tololo Inter-American Observatory, dards, which provided an approximate photographic as National Optical Astronomy Observatories, operated by the Association well as empirical line-ratio calibration. Nevertheless, the of Universities for Research in Astronomy, Inc., under contract with the practical application of the system benefited greatly from National Science Foundation. extensive printed atlases, which both guided the selec- ^Operated by the Association of Universities for Research in Astron- omy, Inc., under contract with the National Aeronautics and Space tion of standards and criteria, and supported interpola- Administration. tions among them when the complete grid could not be 379 © Astronomical Society of the Pacific · Provided by the NASA Astrophysics Data System 380 WALBORN AND FITZPATRICK observed (Morgan, Keenan, and Kellman 1943; Abt et al. telescopes do not permit the acquisition of extensive 1968; Yamashita, Nariai, and Norimoto 1977; Morgan, standard sets, the more so if the detector has a count-rate Abt, andTapscott 1978). limit. The availability of very similar detector systems at The OB blue-violet domain was reexamined with a the CTIO 1-meter and 4-meter telescopes has encour- greater resolution (60 A mm-1, 1.2 A) and widening (1.2 aged us to address this problem for the OB stars. Indeed, mm) by Walborn (1970, 1971a,fc,c). The increased infor- the high quality of initial results from the 1-meter for a mation content of these spectrograms allowed the detec- systematic program on LMC B-supergiants (Fitzpatrick tion and description of several new phenomena: O stars in 1988a; Walborn et al. 1989; Fitzpatrick 1990) directly the Carina nebula with spectral types earlier than the inspired the present project. The objects observed here earliest previous MK standard, for which the extrapolated were either standards or otherwise well observed in the type 03 was introduced (see also Walborn 1982); luminos- previous photographic work; most of them are morpho- ity classification criteria for the early O stars, which did logically normal, although a substantial sample of ON/OC not exist in the Μ Κ system earlier than 09 (Walborn spectra is also included. Hence, this paper transfers the 1973); CNO absorption-line anomalies in OB spectra, previous photographic systematics to the digital data, leading to the OBN and OBC categories (Walborn 1976); providing a comprehensive reference atlas for future and additional interpolated spectral types in the complex, work. Users should still obtain as many key overlap line-rich 09.5-B1 range (09.7, B0.2, and B0.7), which standards as is feasible with their own instrumental sys- sharpened the discrimination between the two funda- tems, but the Atlas should reduce the number required mental (temperature-luminosity) classification dimen- for reliable results. Related atlases for the Ofpe/WN9 sions there. Correlative atlases including illustrations of class in the LMC have been presented by Bohannan these phenomena were presented for the yellow-red and Walborn (1989), for a new Β Ν supergiant with appro- (5400 Â-6600 A) wavelength range by Walborn (1980) priate comparison objects by Walborn, Fitzpatrick, and and for the space UV (1200 Â-1900 A) by Walborn, Nichols-Bohlin (1990), and will be presented for several Nichols-Bohlin, and Panek (1985) and by Walborn and categories of peculiar emission-line OB and WN spectra Nichols-Bohlin (1987). Independently and simulta- by Walborn and Fitzpatrick (1990). An additional cur- neously with this work, P. S. Conti and collaborators rent digital investigation of O-type spectra which, al- developed a quantitative classification for O-type spectra though based on a relatively restricted wavelength range based on equivalent-width measurements in high-resolu- (4300 A-4800 A), should be mentioned because of its ex- tion spectrograms (Conti and Alschuler 1971; Conti tent and quality, is that by Mathys (1988, 1989) who has 1973a,fo, 1974; Conti and Leep 1974; Conti and Frost already discovered several new ON objects. 1977). While operationally distinct from the Μ Κ method- ology, this work shows good systematic agreement with 2. Observations and Reductions the morphological results and provides a vital point of The new digital data were obtained with the Shectman/ contact with the model atmospheres. Heathcote two-dimensional, photon-counting detector Currently, digital detector systems are supplanting on the Cassegrain spectrograph at the CTIO 1-meter photography for most astronomical spectroscopy; indeed, telescope during October 1988 and March 1989. The many of the instruments used in the earlier work are no 3-pixel resolution is 1.5 A, and the full wavelength cover- longer available. Fortunately, several of the new systems age is 3800 A-5000 A. Four observations at different loca- now provide the combination of wavelength coverage and tions along the slit are added to reduce fixed-pattern resolution, S/N, and definition of weak absorption lines in noise. All stars except for a few in the Magellanic Clouds faint objects required for spectral classification work, were neutral-density filtered as closely as possible to the which until recently could be achieved only photographi- bright limit of ß ~ 11 for this system, which required a cally. A higher formal S/N is required in the digital data total exposure time of 40 minutes. The typical maximum for comparable results, in lieu of the third dimension. S/N is about 80 per resolution element, being somewhat With the added advantages of speed, sky subtraction, degraded as is the resolution itself at the extremes of the linear response, and multiple-object capabilities, these wavelength range. systems offer high promise for future morphological stud- The data were extracted and rectified (not flux cali- ies, including faint extragalactic objects. However, the brated) with IRAF1 software at CTIO and subsequently methodological considerations which led to the success of 3-pixel smoothed and plotted with the DISSPLA graphics the photographic work apply fully to the digital data and package at the Joint Institute for Laboratory Astrophysics have not yet been extensively addressed. In particular, a of the University of Colorado. Considerable care was well-defined reference frame of standard objects, relative to which unknowns are described differentially with simi- ^RAF is distributed by National Optical Astronomy Observatories, lar observational parameters, remains essential for sys- which is operated by the Association of Universities for Research in tematically reliable results. Of course, short runs on large Astronomy, Inc., under contract to the National Science Foundation. © Astronomical Society of the Pacific · Provided by the NASA Astrophysics Data System OB SPECTRAL ATLAS 381 taken in the spline-based rectification process in order to 08.5 V is more clear. Type 07 is defined by He II X4541 preserve broad, low-intensity emission features found to = He I X4471. Also by definition, the O-type luminosity underlie the Of lines in some objects (see also Underbill, class V spectra all have strong He π λ.4686 absorption; Gilroy, and Hill 1989). A high-order spline fit, required to the notation ((f)) signifies that in addition weak Ν III rectify the spectrograms completely, would tend to dis- λλ4634-4640-4642 emission is present. Among the spec- tort or eliminate such features.
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