We present a database of 908 stellar spectra of 709 stars in the wavelength range 410 to 680 nm obtained with the ELODIE spectrograph. The archive provides a large coverage of the space of stellar parameters: Spectral types O to M, luminosity classes V to I and metallicities [Fe/H] from -3.0 to +0.8. At the nominal resolution, R=42000, the mean signal-to-noise ratio is 150 per pixel. The spectra given at this resolution are normalized to their pseudo-continuum and are intended to serve for abundance studies, spectral classification and tests of stellar atmosphere models. A lower resolution version of the archive, R=10000, is calibrated in physical flux with a broad-band photometric precision of 2.5% and narrow-band precision of 0.5%. It is scoped for stellar population synthesis of galaxies and clusters, and for kinematical investigations of stellar systems. The archive is also distributed in FITS format through the HYPERCAT database http://www-obs.univ-lyon1.fr/hypercat/spectrophotometry.html .
ELODIE.3.1 is an updated release of the library published in Prugniel & Soubiran (2001A&A...369.1048P, Cat. III/218; and 2004 version, in astro-ph/0409214). The library includes 1959 spectra of 1388 stars obtained with the ELODIE spectrograph at the Observatoire de Haute-Provence 193cm telescope in the wavelength range 390 to 680 nm. It provides a wide coverage of atmospheric parameters: Teff from 3100K to 50000K, logg from -0.25 to 4.9 and [Fe/H] from -3 to +1. The library is given at two resolutions: R around 42000, with the flux normalized to the pseudo-continuum. A lower resolution version of the spectra (R around 10000), is calibrated in physical flux (reduced above earth atmosphere) with a broad-band photometric precision of 2.5% and narrow-band precision of 0.5%. In this new release the data-reduction (flux calibration, reconnection of the echelle orders) has been improved, and in particular the blue region, between 390 and 400nm has been added. The FITS files for each spectra, and the measured atmospheric parameters are publicly available. See the ELODIE.3.1 page for more details: http://www.obs.u-bordeaux1.fr/m2a/soubiran/elodie library.html
Globular clusters produce many exotic stars due to a much higher frequency of dynamical interactions in their dense stellar environments. Some of these objects were observed together with several hundred thousand other stars in our MUSE survey of 26 Galactic globular clusters. Assuming that at least a few exotic stars have exotic spectra (i.e. spectra that contain emission lines), we can use this large spectroscopic data set of over a million stellar spectra as a blind survey to detect stellar exotica in globular clusters. To detect emission lines in each spectrum, we modelled the expected shape of an emission line as a Gaussian curve. This template was used for matched filtering on the differences between each observed 1D spectrum and its fitted spectral model. The spectra with the most significant detections of H{alpha} emission are checked visually and cross-matched with published catalogues. We find 156 stars with H{alpha} emission, including several known cataclysmic variables (CV) and two new CVs, pulsating variable stars, eclipsing binary stars, the optical counterpart of a known black hole, several probable sub-subgiants and red stragglers, and 21 background emission-line galaxies. We find possible optical counterparts to 39 X-ray sources, as we detected H_alpha emission in several spectra of stars that are close to known positions of Chandra X-ray sources. This spectral catalogue can be used to supplement existing or future X-ray or radio observations with spectra of potential optical counterparts to classify the sources.
Several studies have appeared in the literature describing methods for deriving stellar continuum fluxes as simple functions of Johnson color indices. In previous papers, we have used similar relations to derive Ca II H & K line core fluxes for dwarf stars on Lowell Observatory's Solar-Stellar Spectrograph (SSS) program. Our desire is to present our data, and complementary data from the Mt. Wilson and National Solar Observatory stellar and solar programs, in terms of physical fluxes. However, our existing relations break down for mid-K and later stars and for giant stars, which form an important element of our target list. In this work I have used a broader range of spectrophotometry and angular diameters than in our previous work to derive empirical flux scales for spectral types A to early M, luminosity classes I to V, and for four color indices, Johnson B-V, V-R, R-I, and Stromgren b-y. In this paper I describe the methods I used and present the derived flux scales. I compare the results with those from earlier studies and present examples of the use of the flux scales. The data and results are available on the World Wide Web home page. Access <http://www.lowell.edu>, select "Lowell staff", and select the author's home page.
The intrinsic energy distribution for 41 spectral subclasses in the range of wavelengths of 320-760 nm are derived in the following way: (1) The sources of the spectrophotometric data were taken from three catalogues published in FSU (Kharitonov et al. 1988, Glushneva, ed., 1982, Alekseeva et al. 1992), containing energy distributions of about 2000 stars of different spectral types. (2) MK spectral classes were taken from the Bright Star Catalogue (Hoffleit 1982; hereafter BSC). The paper by Gray and Garrison (1987) was took into account to examine the influence of errors in spectral classification. (3) The quality of stars selected for each subclass was estimated by comparison of the observed and synthetic (U-B) and (B-V) color indices calculated for our energy distributions. The results have been published by Knyazeva and Kharitonov (1993, 1994a, 1994b, 1996a, 1996b)
The normal spectral energy distribution for spectral subtypes from O4 to O8 and O9 to B5 for luminosity classes V,IV and III are derived. Three photometrically uniform catalogs served as the source of the spectrophotometric data used. Synthetic color indices for all spectral types are calculated using the energy distribution curves obtained.
The normal spectral energy distribution for spectral subtypes from O4 to O8 for luminosity classes V,IV and III are derived. Three photometrically uniform catalogs served as the source of the spectrophotometric data used. Synthetic color indices for all spectral types are calculated using the energy distribution curves obtained.
Spectral energy distributions for 41 stars, 7-8mag, near the celestial equator (DE=+/-3{deg}) were obtained. The 3100-7600{AA} spectral range is studied with a spectral resolution of 50{AA}.
We present two-dimensional stellar and gaseous kinematics of the inner 0.7x1.2kpc^2^ of the Seyfert 1.5 galaxy ESO 362-G18, derived from optical (4092-7338{AA}) spectra obtained with the GMOS integral field spectrograph on the Gemini South telescope at a spatial resolution of 170 pc and spectral resolution of 36km/s. ESO 362-G18 is a strongly perturbed galaxy of morphological type Sa or S0/a, with a minor merger approaching along the NE direction. Previous studies have shown that the [OIII] emission shows a fan-shaped extension of ~10" to the SE. We detect the [OIII] doublet, [NII] and H{alpha} emission lines throughout our FOV. The stellar kinematics is dominated by circular motions in the galaxy plane, with a kinematic position angle of ~137{deg} and is centred approximately on the continuum peak. The gas kinematics is also dominated by rotation, with kinematic position angles ranging from 122{deg} to 139{deg}, projected velocity amplitudes of the order of 100km/s, and a mean velocity dispersion of 100km/s. A double-Gaussian fit to the [OIII]{lambda}5007 and H{alpha} lines, which have the highest signal to noise ratios of the emission lines, reveal two kinematic components: (1) a component at lower radial velocities which we interpret as gas rotating in the galactic disk; and (2) a component with line of sight (LOS) velocities 100-250km/s higher than the systemic velocity, interpreted as originating in the outflowing gas within the AGN ionization cone. We estimate a mass outflow rate of 7.4x10^-2^M_{sun}_/yr in the SE ionization cone (this rate doubles if we assume a biconical configuration), and a mass accretion rate on the supermassive black hole (SMBH) of 2.2x10^-2^M_{sun}_/yr. The total ionized gas mass within 84pc of the nucleus is 3.3x10^5^M_{sun}_; infall velocities of ~34km/s in this gas would be required to feed both the outflow and SMBH accretion.
This is a collection of line indices in the Lick system (and others) for a collection of Galactic, M31, M33 and other globular clusters plus bright and dwarf galaxies observed primarily at the MMT over the period 1980-1992 by J. Huchra, J. Brodie, N. Caldwell, R. Schommer, C. Christian and G. Bothun. The paper describing this catalog of indices is published in Huchra, Harris & Schommer (1996, in prep). Table 1 lists the definition of the indices used, Table 2 lists the line indices and errors, Table 3 lists multiple measurements for individual objects (plus dispersions and means) to give the reader a sense of the precision and accuracy of individual measures, and Table 4 lists index measurements from higher dispersion spectra. Each of the index tables generally has two lines, the first are the index values and the second are the statistical (calculated from photon counts) errors. An estimate of the external error in each index can be gotten from the multiple measurements given in Table 3. "AV" in Table 2 indicates that the measurement given is the average of multiple individual spectra give in Table 3. Otherwise the "RFN" number refers to the serial number of the MMT spectrum.
