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|The Dynamics of Poor Systems of Galaxies|
We assemble and observe a sample of poor galaxy systems that is suitablefor testing N-body simulations of hierarchical clustering and otherdynamical halo models. We (1) determine the parameters of the densityprofile rho(r) and the velocity dispersion profile sigma_p(R), (2)separate emission-line galaxies from absorption-line galaxies, examiningthe model parameters and as a function of spectroscopic type, and (3)for the best-behaved subsample, constrain the velocity anisotropyparameter, beta, which determines the shapes of the galaxy orbits. Oursample consists of 20 systems, 12 of which have extended X-ray emissionin the ROSAT All-Sky Survey. We measure the 877 optical spectra ofgalaxies brighter than m_R~15.4 within 1.5 h^-1 Mpc of the systemcenters (we take H_0=100 h km s^-1 Mpc^-1). Thus, we sample the systemmembership to a radius typically three times larger than other recentoptical group surveys. The average system population is 30 galaxies, andthe average line-of-sight velocity dispersion is ~300 km s^-1. TheNavarro, Frenk, & White universal profile and the Hernquist modelboth provide good descriptions of the spatial data. In most cases anisothermal sphere is ruled out. Systems with declining sigma_p(R) arewell-matched by theoretical profiles in which the star-forming galaxieshave predominantly radial orbits (beta>0) many of these galaxies areprobably falling in for the first time. There is significant evidencefor spatial segregation of the spectroscopic classes regardless ofsigma_p(R).
|An image database. II. Catalogue between δ=-30deg and δ=70deg.|
A preliminary list of 68.040 galaxies was built from extraction of35.841 digitized images of the Palomar Sky Survey (Paper I). For eachgalaxy, the basic parameters are obtained: coordinates, diameter, axisratio, total magnitude, position angle. On this preliminary list, weapply severe selection rules to get a catalog of 28.000 galaxies, wellidentified and well documented. For each parameter, a comparison is madewith standard measurements. The accuracy of the raw photometricparameters is quite good despite of the simplicity of the method.Without any local correction, the standard error on the total magnitudeis about 0.5 magnitude up to a total magnitude of B_T_=17. Significantsecondary effects are detected concerning the magnitudes: distance toplate center effect and air-mass effect.
|On the excess of physical companions among Seyfert galaxies|
The results of a search for close companions in two magnitude limitedsamples (mB less than or equal to 15.5) of 99 Seyfert 1 and98 Seyfert 2 galaxies are presented. It is found that there is an excessof physical companions in both samples of galaxies, compared with twocontrol samples of normal field spiral galaxies. The calculated lowerlimit percentages of physical companions are (12 +/- 3)% and (12 +/- 4)%for Seyfert 1 and Seyfert 2, respectively, while the upper limits on thepercentage of galaxies with physical companions are in the range (0%-5%)in both control samples. The excess is confirmed by analysis of theredshifts for all pairs found in the complete, magnitude limited (B(O)less than or equal to 14.5) CfA sample of Seyfert galaxies.
|An optical catalog of extragalactic emission-line objects similar to quasi-stellar objects|
A catalog of 935 galaxies which have optical properties similar to thoseof QSOs is given. A subsidiary table of cross-identifications enablesthe reader to relate the name of a given object to its coordinate name.Most of the objects appear to be nonstellar. The majority, more than700, have redshifts z = 0.2 or less, and have mostly been classified asSeyfert galaxies, N systems, or radio galaxies. The Hubble diagram forall of the objects with z = 0.2 or less is shown. The redshiftdistribution peaks at z = 0.025, but there are about 200 powerful radiogalaxies in the extended tail of the distribution which have z greaterthan 0.2. There is a separate and distinct peak in the redshiftdistribution at z = 0.06.
|The Wasilewski sample of emission-line galaxies - Follow-up CCD imaging and spectroscopic and IRAS observations|
The results of an extensive imaging and spectroscopic follow-up of theobjective prism-selected emission line galaxy (ELG) sample of Wasilewski(1982) are presented. Fluxes at 12, 25, 60, and 100 microns were alsoobtained from the coadded IRAS survey data. ELGs found by objectiveprism surveys are found to be generally small and underluminous galaxieswhich usually have higher than average optical surface brightness. TheSeyfert detection rate in objective prism surveys is roughly 10 percentand the ratio of the space densities of Seyfert 2 to Seyfert 1 galaxiesis significantly larger than unity. Most of the galaxies selected byobjective prism surveys are star-forming, late-type spirals which oftenshow disturbed morphology. About 25 percent of the galaxies detected bythe surveys are faint, high-excitation metal-poor compact H II regions.
|A catalogue of Seyfert galaxies.|
|The Case low-dispersion Northern Sky Survey. V.|
Positions, estimated magnitudes, and finding charts (when necessary) areprovided for 143 blue and/or emission-line galaxies, probable H IIregions in 11 galaxies, 149 blue and/or emission-line stellar objectsincluding QSO candidates, and 36 known and suspected blue stars in theR.A. region between 10 h 10 m and 12 h 15 m and declination between +33.0 and .38.0 deg (1950). The objects, whose blue magnitudes are mostlywithin the range 15-18, were identified on low-dispersionobjective-prism plates taken with the Burrel Schmidt telescope at KittPeak.
|The relative number of Seyfert 2 galaxies. I - Spectra of emission-line galaxies in the Wasilewski field|
Slit spectra were obtained of all the Seyfert galaxy candidates and manyother emission-line galaxies discovered by Wasilewski (1982), and theresults are reported. Relative emission line fluxes, redshifts andextinctions, emission line widths and diagnostic ratios, and spectralscans are shown. An activity classification of the galaxies is made. Itis confirmed that the relative number of Seyfert 2 galaxies down to agiven apparent magnitude is large in H II region. Per unit volume ofspace, the relative number of Seyfert (1 + 1.5) to Seyfert (1.8 + 1.9)to Seyfert 2 is approximately 0.1/0.1/0.8.
|The space density and spectroscopic properties of a new sample of emission-line galaxies|
A 4-deg objective prism survey for low redshift emission line galaxiesconducted over an 825 sq deg region of the sky indicates that a newsample of emission line galaxies is available even in areas which havebeen well searched with the 'excess UV-continuum' technique. Thesegalaxies commonly occur in systems with peculiar morphology, indicatinggravitational interaction with a close companion or other disturbance.The space density of the new galaxies is found to be similar to thespace density of the Markarian galaxies. The present galaxies representabout 8 percent of all nearby galaxies in the -16.5 to -22.5 absolutemagnitude range, and are composed of a population which is completelyindependent of the Markarian sample.
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